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1. MAGIC and Fermi-LAT gamma-ray results on unassociated HAWC sources

Author: M. L. Ahnen, S. Ansoldi, L. A. Antonelli, C. Arcaro, D. Baack, A. Babic, B. Banerjee, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, R. Ch. Berse, A. Berti, W. Bhattacharyya, A. Biland, O. Blanch, G. Bonnoli, R. Carosi, A. Carosi, G. Ceribella, A. Chatterjee, S. M. Colak, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Cumani, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, F. Di Pierro, A. Domınguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Elsaesser, V. Fallah Ramazani, A. Fernandez-Barral, D. Fidalgo, M. V. Fonseca, L. Font, C. Fruck, D. Galindo, R. J. Garcıa Lopez, M. Garczarczyk, M. Gaug, P. Giammaria, N. Godinovic, D. Gora, D. Guberman, D. Hadasch, A. Hahn, T. Hassan, M. Hayashida, J. Herrera, J. Hose, D. Hrupec, K. Ishio, Y. Konno, H. Kubo, J. Kushida, D. Kuvezdic, D. Lelas, E. Lindfors, S. Lombardi, F. Longo, M. Lopez, C. Maggio, P. Majumdar, M. Makariev, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martınez, S. Masuda, D. Mazin, K. Mielke, M. Minev, J. M. Miranda, R. Mirzoyan, A. Moralejo, V. Moreno, E. Moretti, T. Nagayoshi, V. Neustroev, A. Niedzwiecki, M. Nievas Rosillo, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, L. Nogues, S. Paiano, J. Palacio, D. Paneque, R. Paoletti, J. M. Paredes, G. Pedaletti, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, J. R. Garcia, I. Reichardt, W. Rhodes, M. Ribo, J. Rico, C. Righi, A. Rugliancich, T. Saito, K. Satalecka, T. Schweizer, J. Sitarek, I. Snidaric, D. Sobczynska, A. Stamerra, M. Strzys, T. Suric, M. Takahashi, L. Takalo, F. Tavecchio, P. Temnikov, T. Terzic, M. Teshima, N. Torres-Alba, A. Treves, S. Tsujimoto, G. Vanzo, M. Vazquez Acosta, I. Vovk, J. E. Ward, M. Will, D. Zaric, A. Albert, R. Alfaro, C. Alvarez, R. Arceo, J. C. Arteaga-Velazquez, D. Avila Rojas, H. A. Ayala Solares, A. Becerril, E. Belmont-Moreno, S. Y. BenZvi, A. Bernal, J. Braun, K. S. Caballero-Mora, T. Capistran, A. Carraminana, S. Casanova, M. Castillo, U. Cotti, J. Cotzomi, S. Coutino de Leon, C. De Leon, E. De la Fuente, R. Diaz Hernandez, S. Dichiara, B. L. Dingus, M. A. DuVernois, J. C. Dıaz-Velez, R. W. Ellsworth, K. Engel, O. Enriquez-Rivera, D. W. Fiorino, H. Fleischhack, N. Fraija, J. A. Garcıa-Gonzalez, F. Garfias, A. Gonzalez-Munoz, M. M. Gonzalez, J. A. Goodman, Z. Hampel-Arias, J. P. Harding, S. Hernandez, F. Hueyotl-Zahuantitla, C. M. Hui, P. Huntemeyer, A. Iriarte, A. Jardin-Blicq, V. Joshi, S. Kaufmann, A. Lara, R. J. Lauer, W. H. Lee, D. Lennarz, H. Leon Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, R. Luna-Garcıa, R. Lopez-Coto, K. Malone, S. S. Marinelli, O. Martinez, I. Martinez-Castellanos, J. Martınez-Castro, H. Martınez-Huerta, J. A. Matthews, P. Miranda-Romagnoli, E. Moreno, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, R. Pelayo, J. Pretz, E. G. Perez-Perez, Z. Ren, C. D. Rho, C. Riviere, D. Rosa-Gonzalez, M. Rosenberg, E. Ruiz-Velasco, F. Salesa Greus, A. Sandoval, M. Schneider, M. Seglar Arroyo, G. Sinnis, A. J. Smith, R. W. Springer, P. Surajbali, I. Taboada, O. Tibolla, K. Tollefson, I. Torres, T. N. Ukwatta, G. Vianello, L. Villasenor, F. Werner, S. Westerhoff, J. Wood, T. Yapici, G. Yodh, A. Zepeda, H. Zhou, J. D. Alvarez, M. Ajello, L. Baldini, G. Barbiellini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, T. J. Brandt, J. Bregeon, P. Bruel, R. A. Cameron, R. Caputo, P. A. Caraveo, D. Castro, E. Cavazzuti, G. Chiaro, S. Ciprini, D. Costantin, F. D'Ammando, F. de Palma, A. Desai, N. Di Lalla, M. Di Mauro, L. Di Venere, C. Favuzzi, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, D. Green, I. A. Grenier, S. Guiriec, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, G. Johannesson, M. Kuss, S. Larsson, I. Liodakis, F. Loparco, P. Lubrano, J. D. Magill, S. Maldera, A. Manfreda, M. N. Mazziotta, I. Mereu, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, M. Palatiello, V. S. Paliya, M. Pesce-Rollins, V. Petrosian, F. Piron, T. A. Porter, G. Principe, S. Raino, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, C. Sgro, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, J. B. Thayer, David J Thompson, D. F. Torres, E. Torresi, E. Troja, J. Valverde, K. Wood, and M. Yassine
Subjects: Astronomy, Astrophysics
Abstract: The HAWC Collaboration released the 2HWC catalogue of TeV sources, in which 19 show no association with any known high-energy (HE; E ≳ 10 GeV) or very-high-energy (VHE; E ≳ 300 GeV) sources. This catalogue motivated follow-up studies by both the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) and Fermi-LAT (Large Area Telescope) observatories with the aim of investigating gamma-ray emission over a broad energy band. In this paper, we report the results from the first joint work between High Altitude Water Cherenkov (HAWC), MAGIC, and Fermi-LAT on three unassociated HAWC sources: 2HWC J2006+341, 2HWC J1907+084*, and 2HWC J1852+013*. Although no significant detection was found in the HE and VHE regimes, this investigation shows that a minimum 1° extension (at 95 per cent confidence level) and harder spectrum in the GeV than the one extrapolated from HAWC results are required in the case of 2HWC J1852+013*, whilst a simply minimum extension of 0.16° (at 95 per cent confidence level) can already explain the scenario proposed by HAWC for the remaining sources. Moreover, the hypothesis that these sources are pulsar wind nebulae is also investigated in detail.
Published: 2019
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2. Study of the variable broadband emission of Markarian 501 during the most extreme Swift X-ray activity

Author: Francesco Longo, Yuki Iwamura, Susumu Inoue, L. Nogués, M. I. Martínez, G. Pedaletti, Thomas Bretz, J. Buss, A. Rugliancich, Marina Manganaro, D. Galindo, Merja Tornikoski, Sabrina Einecke, Martin Makariev, Oscar Blanch, C. Leto, Ciro Bigongiari, Adrian Biland, D. Zarić, Andrii Neronov, M. Garczarczyk, Sargis Gasparyan, Konstancja Satalecka, Michele Doro, Marc Ribó, M. Noethe, J. Becerra González, Kazuma Ishio, J. Rico, Christian Fruck, Kyoshi Nishijima, Abelardo Moralejo, E. Moretti, Wolfgang Rhode, Christoph Wendel, Dominik Baack, Satoshi Masuda, Hidetoshi Kubo, Nikola Godinovic, B. Machado de Oliveira Fraga, Alexander Hahn, Manuel Delfino, Daniela Dorner, P. Giammaria, A. Niedzwiecki, Alessio Berti, U. Barres de Almeida, F. Verrecchia, G. Busetto, Lena Linhoff, D. Fidalgo, Damir Lelas, G. Ferrara, Alicia Fattorini, D. Hildebrand, David Paneque, V. A. Acciari, Bernd Schleicher, Gaia Vanzo, M. Peresano, Rodolfo Carosi, M. Perri, Alessandra Lamastra, John Hoang, Marcel Strzys, M. Gaug, Chiara Righi, M. Armas Padilla, D. Ninci, Ana Babić, Michael Blank, Dorota Sobczyńska, D. Dominis Prester, A. De Angelis, Vitaly Neustroev, I. Snidaric, F. Schulz, E. von Willert, D. Guberman, A. Y. Lien, J. Herrera, Juan Abel Barrio, B. Banerjee, J. van Scherpenberg, V. D'Elia, Narek Sahakyan, P. Temnikov, Stefano Ansoldi, R. J. García López, G. Maneva, E. Do Souto Espiñera, B. De Lotto, Elisa Bernardini, Riccardo Paoletti, S. Paiano, Karl Mannheim, Pablo Peñil, A. Shukla, Ivica Puljak, Jose Luis Contreras, D. Neise, Andrea Tramacere, Manuela Mallamaci, A. López-Oramas, Jordi Delgado, V. Fallah Ramazani, Juan Cortina, J. Palacio, P. Colin, R. Walter, J. M. Paredes, F. Di Pierro, Antonio Stamerra, Pratik Majumdar, Camilla Maggio, M. V. Fonseca, Ievgen Vovk, Francesco Dazzi, A. Fernández-Barral, Cosimo Nigro, P. Munar-Adrover, Massimo Persic, Dario Hrupec, L. A. Antonelli, Martin Will, D. Kuveždić, T. Schweizer, F. Leone, Anne Lähteenmäki, Tarek M. Hassan, Fabrizio Tavecchio, Masahiro Teshima, A. Somero, Kari Nilsson, Ll. Font, M. Bulinski, Wlodek Bednarek, Vitalii Sliusar, P. G. Prada Moroni, Junko Kushida, P. Da Vela, E. Prandini, N. Torres-Albà, Joni Tammi, Sebastian Achim Mueller, J. R. Garcia, Giacomo Bonnoli, Manuel Doerr, Stefano Gallozzi, Jose Miguel Miranda, Wrijupan Bhattacharyya, Julian Sitarek, T. Surić, Shimpei Tsujimoto, K. Bruegge, D. Elsaesser, Tomislav Terzić, Jürgen Besenrieder, E. Molina, E. Colombo, Lab Saha, Luca Foffano, Mosè Mariotti, A. Paravac, Saverio Lombardi, M. Nievas Rosillo, M. Minev, M. Balbo, D. Hadasch, R. Mirzoyan, A. Arbet-Engels, K. Sedlaczek, L. Maraschi, Elina Lindfors, Daniel Mazin, Stefan Cikota, M. Vazquez Acosta, Victoria Moreno, Stefano Covino, Tomoki Saito, Giovanni Ceribella, Aaron Dominguez, K. Noda, Sidika Merve Colak, M. López, German Research Foundation, Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Croatian Science Foundation, University of Rijeka, Polish National Agency for Academic Exchange, Ministério da Ciência, Tecnologia e Inovação (Brasil), National Aeronautics and Space Administration (US), Department of Energy (US), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), Centre National de la Recherche Scientifique (France), Institut National de Physique Nucléaire et de Physique des Particules (France), Agenzia Spaziale Italiana, High Energy Accelerator Research Organization (Japan), Japan Aerospace Exploration Agency, Knut and Alice Wallenberg Foundation, Swedish Research Council, Swedish National Space Board, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Babic, A., Banerjee, B., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Blanch, O., Bonnoli, G., Busetto, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., DI Pierro, F., Do Souto Espinera, E., Dominguez, A., Dominis Prester, D., Doro, M., Fallah Ramazani, V., Fattorini, A., Fernandez-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., Garcia Lopez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giammaria, P., Godinovic, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuvecdic, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Oramas, A., MacHado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Maraschi, L., Mariotti, M., Martinez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Penil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Suric, T., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tsujimoto, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vovk, I., Will, M., Zaric, D., Arbet-Engels, A., Baack, D., Balbo, M., Biland, A., Blank, M., Bretz, T., Bruegge, K., Bulinski, M., Buss, J., Doerr, M., Dorner, D., Einecke, S., Elsaesser, D., Hildebrand, D., Linhoff, L., Mannheim, K., Mueller, S., Neise, D., Neronov, A., Noethe, M., Paravac, A., Rhode, W., Schleicher, B., Schulz, F., Sedlaczek, K., Shukla, A., Sliusar, V., Von Willert, E., Walter, R., Wendel, C., Tramacere, A., Lien, A., Perri, M., Verrecchia, F., Armas Padilla, M., Leto, C., Lahteenmaki, A., Tornikoski, M., Tammi, J., Department of Electronics and Nanoengineering, Metsähovi Radio Observatory, Aalto-yliopisto, and Aalto University
Subjects: galaxies: active, BL Lacertae objects: individual: Mrk 501, gamma rays: galaxies, X-rays: galaxies, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Power law, Spectral line, Galaxies: active, Gamma rays: galaxies, individual: Mrk 501 [BL Lacertae objects], 0103 physical sciences, MAGIC (telescope), Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, galaxie [Gamma rays], 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, galaxies [X-rays], Crab Nebula, Space and Planetary Science, active [galaxies], galaxies [gamma rays], ddc:520, Física nuclear, High Energy Astrophysical Phenomena, Astrophysics - High Energy Astrophysical Phenomena
Abstract: [Context] Markarian 501 (Mrk 501) is a very high-energy (VHE) gamma-ray blazar located at z = 0:034, which is regularly monitored by a wide range of multi-wavelength instruments, from radio to VHE gamma rays. During a period of almost two weeks in July 2014, the highest X-ray activity of Mrk 501 was observed in -14 years of operation of the Neil Gehrels Swift Gamma-ray Burst Observatory., [Aims] We characterize the broadband variability of Mrk 501 from radio to VHE gamma rays during the most extreme X-ray activity measured in the last 14 years, and evaluate whether it can be interpreted within theoretical scenarios widely used to explain the broadband emission from blazars., [Methods] The emission of Mrk 501 was measured at radio with Metsähovi, at optical–UV with KVA and Swift/UVOT, at X-ray with Swift/XRT and Swift/BAT, at gamma ray with Fermi-LAT, and at VHE gamma rays with the FACT and MAGIC telescopes. The multi-band variability and correlations were quantified, and the broadband spectral energy distributions (SEDs) were compared with predictions from theoretical models., [Results] The VHE emission of Mrk 501 was found to be elevated during the X-ray outburst, with a gamma-ray flux above 0.15 TeV varying from ∼0.5 to ∼2 times the Crab nebula flux. The X-ray and VHE emission both varied on timescales of 1 day and were found to be correlated. We measured a general increase in the fractional variability with energy, with the VHE variability being twice as large as the X-ray variability. The temporal evolution of the most prominent and variable segments of the SED, characterized on a day-by-day basis from 2014 July 16 to 2014 July 31, is described with a one-zone synchrotron self-Compton model with variations in the break energy of the electron energy distribution (EED), and with some adjustments in the magnetic field strength and spectral shape of the EED. These results suggest that the main flux variations during this extreme X-ray outburst are produced by the acceleration and the cooling of the high-energy electrons. A narrow feature at ∼3 TeV was observed in the VHE spectrum measured on 2014 July 19 (MJD 56857.98), which is the day with the highest X-ray flux (>0.3 keV) measured during the entire Swift mission. This feature is inconsistent with the classical analytic functions to describe the measured VHE spectra (power law, log-parabola, and log-parabola with exponential cutoff) at more than 3σ. A fit with a log-parabola plus a narrow component is preferred over the fit with a single log-parabola at more than 4σ, and a dedicated Monte Carlo simulation estimated the significance of this extra component to be larger than 3σ. Under the assumption that this VHE spectral feature is real, we show that it can be reproduced with three distinct theoretical scenarios: (a) a pileup in the EED due to stochastic acceleration; (b) a structured jet with two-SSC emitting regions, with one region dominated by an extremely narrow EED; and (c) an emission from an IC pair cascade induced by electrons accelerated in a magnetospheric vacuum gap, in addition to the SSC emission from a more conventional region along the jet of Mrk 501., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Instituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. The important contributions from ETH Zurich grants ETH-10.08-2 and ETH-27.12-1 as well as the funding by the Swiss SNF and the German BMBF (Ver-bundforschung Astro-und Astroteilchenphysik) and HAP (Helmoltz Alliance for Astroparticle Physics) are gratefully acknowledged. Part of this work is supported by Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center SFB 876, project C3. We thank the Instituto de Astrofisica de Canarias for allowing us to operate the telescope at the Observatorio del Roque de los Muchachos in La Palma, the Max-Planck-Institut fur Physik for providing us with the mount of the former HEGRA CT3 telescope, and the MAGIC Collaboration for their support. JBG acknowledges the support of the Viera y Clavijo program funded by ACIISI and ULL. C. W. is grateful for the support by the project “Promotion inklusive” of the Universität zu Köln and the German Bundesmin-isterium für Arbeit und Soziales. This publication makes use of data obtained at Metsähovi Radio Observatory, operated by Aalto University, Finland.
Published: 2020

3. Statistics of VHE gamma-Rays in Temporal Association with Radio Giant Pulses from the Crab Pulsar

Author: J. Palacio, J. M. Paredes, Antonio Stamerra, L. Maraschi, Elina Lindfors, Daniel Mazin, Chiara Righi, Wlodek Bednarek, Alessandro Carosi, P. Temnikov, Pratik Majumdar, N. Torres-Albà, M. V. Fonseca, S. N. Shore, Martin Will, Jose Miguel Miranda, E. Colombo, E. Prandini, Aaron Dominguez, Kari Nilsson, L. O. Takalo, Francesco Longo, Juan Abel Barrio, Masahiro Teshima, Nikola Godinovic, U. Menzel, L. A. Antonelli, Mosè Mariotti, D. Hadasch, J. E. Ward, Alba Fernández-Barral, M. Engelkemeier, Stefano Covino, Martin Makariev, Alexander Hahn, P. Colin, Saverio Lombardi, Andrea Rugliancich, Sidika Merve Colak, Oscar Blanch, Arka Chatterjee, Adrian Biland, Christian Fruck, Tomoki Saito, M. Doert, T. Surić, Shimpei Tsujimoto, M. Garczarczyk, Ana Babić, D. Fidalgo, M. Peresano, Camilla Maggio, J. Rico, S. Schroeder, Ivica Puljak, Ievgen Vovk, M. Vazquez Acosta, D. Dominis Prester, Tarek M. Hassan, B. Biasuzzi, Victoria Moreno, Fabrizio Tavecchio, L. Nogués, E. Moretti, D. Kuveždić, Jose Luis Contreras, Abelardo Moralejo, F. Di Pierro, Yusuke Konno, Juan Cortina, T. Schweizer, J. R. Garcia, Giacomo Bonnoli, A. De Angelis, A. Treves, Vitaly Neustroev, V. Fallah Ramazani, Max Ludwig Ahnen, Wrijupan Bhattacharyya, T. Nagayoshi, Daniela Dorner, Dariusz Gora, Gaia Vanzo, G. Maneva, Junko Kushida, P. Da Vela, Kyoshi Nishijima, U. Barres de Almeida, M. Minev, I. Reichardt, P. Giammaria, A. Niedzwiecki, R. Smits, M. Gaug, Damir Lelas, D. Elsaesser, I. Snidaric, Dorota Sobczyńska, J. Herrera, B. De Lotto, Julian Sitarek, Koji Noda, J. Hose, Elisa Bernardini, Stefano Ansoldi, David Paneque, M. I. Martínez, Riccardo Paoletti, D. Guberman, Marina Manganaro, Sabrina Einecke, D. Galindo, P. Cumani, Konstancja Satalecka, Michele Doro, Dario Hrupec, M. A. Lopez, S. Paiano, Karl Mannheim, P. G. Prada Moroni, Tomislav Terzić, Francesco Dazzi, J. Becerra González, Alessio Berti, Natalia Lewandowska, L. Perri, D. Eisenacher Glawion, Cosimo Nigro, M. Nievas Rosillo, B. Banerjee, C. Arcaro, Lluis Font, Marcel Strzys, R. J. García López, G. Pedaletti, Massimo Persic, Wolfgang Rhode, D. Ninci, M. Hayashida, D. Zarić, Marc Ribó, P. Bangale, Hidetoshi Kubo, R. Mirzoyan, Kazuma Ishio, Rodolfo Carosi, German Research Foundation, Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Ministerio de Economía y Competitividad (España), Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Universidad de Barcelona, Croatian Science Foundation, University of Rijeka, Foundation for Polish Science, Ministério da Ciência, Tecnologia e Inovação (Brasil), Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bernardini, E., Berti, A., Bhattacharyya, W., Biasuzzi, B., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Di Pierro, F., Doert, M., Dominguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., Fernandez-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Garcia Lopez, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinovic, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuvez Dic, D., Lelas, D., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Menzel, U., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Shore, S. N., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Strzys, M., Suric, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zaric, D., and Smits, R.
Subjects: Photon, Radiation mechanisms: non-thermal, Radio continuum: stars, VHE [gamma ray], Astrophysics, 01 natural sciences, Cherenkov, individual, 010303 astronomy & astrophysics, Pulsars: individual: Crab pulsar, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), photon, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, pulsed, Gamma rays: stars, pulsars: individual: Crab pulsar - gamma-rays: stars - radio continuum: stars - radiation mechanics: non-thermal, detector [radio wave], statistics, Crab pulsar, Global Positioning System, stars [Radio continuum], Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, stars, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, pulsars, gamma rays, radio continuum, radiation mechanisms, non-thermal, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, star [Gamma rays], Pulsar, emission [gamma ray], 0103 physical sciences, 010306 general physics, enhancement, Astrophysics::Galaxy Astrophysics, Cherenkov radiation, non-thermal [Radiation mechanisms], business.industry, Crab Pulsar, stars [Gamma rays], Astronomy and Astrophysics, individual: Crab pulsar [Pulsars], MAGIC, flux, Stars, Space and Planetary Science, correlation, ddc:520, business, statistical
Abstract: [Aims] The aim of this study is to search for evidence of a common emission engine between radio giant pulses (GPs) and very-high-energy (VHE, E > 100 GeV) γ-rays from the Crab pulsar., [Methods] We performed 16 h of simultaneous observations of the Crab pulsar at 1.4 GHz with the Effelsberg radio telescope and the Westerbork Synthesis Radio Telescope (WSRT), and at energies above 60 GeV we used the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes. We searched for a statistical correlation between the radio and VHE γ-ray emission with search windows of different lengths and different time lags to the arrival times of a radio GP. A dedicated search for an enhancement in the number of VHE γ-rays correlated with the occurrence of radio GPs was carried out separately for the P1 and P2 phase ranges, respectively., [Results] In the radio data sample, 99444 radio GPs were detected. We find no significant correlation between the GPs and VHE photons in any of the search windows. Depending on phase cuts and the chosen search windows, we find upper limits at a 95% confidence level on an increase in VHE γ-ray events correlated with radio GPs between 7% and 61% of the average Crab pulsar VHE flux for the P1 and P2 phase ranges, respectively. This puts upper limits on the flux increase during a radio GP between 12% and 2900% of the pulsed VHE flux, depending on the search window duration and phase cuts. This is the most stringent upper limit on a correlation between γ-ray emission and radio GPs reported so far., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ.
Published: 2019
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4. Deep observations of the globular cluster M15 with the MAGIC telescopes

Author: B. Machado de Oliveira Fraga, A. Lamastra, Jordi Delgado, P. Giammaria, Razmik Mirzoyan, D. Baack, D. Galindo, Massimo Persic, John Hoang, E. Moretti, J. Palacio, Pablo Peñil, Chiara Righi, A. Hahn, R. J. García López, Kari Nilsson, P. Majumdar, J. M. Paredes, Antonio Stamerra, J. Becerra González, Dorota Sobczyńska, Francesco Longo, Satoshi Masuda, D. Dominis Prester, Adrian Biland, S. Gasparyan, Y. Iwamura, M. Strzys, J. Kushida, S. M. Colak, Abelardo Moralejo, Jose Luis Contreras, Juan Cortina, A. Fernández-Barral, N. Godinović, Takashi Saito, Pierre Colin, Tihomir Surić, Francesco Leone, W. Rhode, M. V. Fonseca, I. Puljak, P G Prada Moroni, N. Sahakyan, W. Bhattacharyya, V. Fallah Ramazani, J. Rico, P. Munar-Adrover, Oscar Blanch, A. Somero, Saverio Lombardi, Louis Antonelli, U. Barres de Almeida, A. Niedzwiecki, D. Fidalgo, M. Will, David H. Green, Edgar Molina, V. D'Elia, E. Colombo, S. Gallozzi, A. De Angelis, G. Vanzo, Petar Temnikov, Koji Noda, Ana Babić, Stefan Cikota, A. Fattorini, D. Ninci, Shimpei Tsujimoto, M. I. Martínez, M. Vazquez Acosta, Stefano Ansoldi, Elisa Bernardini, Masahiro Teshima, M. Peresano, Giovanni Busetto, M. Mallamaci, F. Di Pierro, Lab Saha, B. De Lotto, D. Dorner, Markus Gaug, M. López, Elisa Prandini, A. Arbet Engels, D. Hadasch, Sabrina Einecke, Victoria Moreno, D. Kuveždić, Julian Sitarek, Rodolfo Carosi, D. Lelas, Vitaly Neustroev, Francesco Dazzi, Darko Zarić, Jürgen Besenrieder, K. Mannheim, Juan Abel Barrio, D. Elsaesser, I. Vovk, M. Makariev, Ciro Bigongiari, Aaron Dominguez, M. Nöthe, S. Paiano, B. Banerjee, K. Ishio, C. Nigro, G. Ceribella, G. Pedaletti, W. Bednarek, C. Maggio, G. Maneva, E. Do Souto Espiñera, Fabrizio Tavecchio, Ll. Font, Tomislav Terzić, Susumu Inoue, M. Nievas Rosillo, Dario Hrupec, R. Paoletti, A. López-Oramas, L. Foffano, L. Maraschi, M. Delfino, Marc Ribó, Jose Carlos Herrera, Elina Lindfors, Daniel Mazin, A. Berti, J. R. Garcia, Stefano Covino, M. Minev, Hidetoshi Kubo, G. Bonnoli, T. Schweizer, L. Nogués, M. Mariotti, M. Garczarczyk, V. A. Acciari, J. van Scherpenberg, K. Nishijima, P. Da Vela, Iva Šnidarić, A. Rugliancich, Marina Manganaro, G. Ferrara, D. Paneque, Konstancja Satalecka, Michele Doro, C. Fruck, D. Guberman, N. Torres-Albà, Jose Miguel Miranda, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babic, A., Banerjee, B., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Busetto, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Do Souto Espinera, E., Dominguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Fernandez-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., Garcia Lopez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giammaria, P., Godinovic, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuvezdic, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Oramas, A., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Nothe, M., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Penil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Suric, T., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tsujimoto, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vovk, I., Will, M., and Zaric, D.
Subjects: Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, Population, general [Pulsars], Globular clusters: general, FOS: Physical sciences, astro-ph.HE, Astrophysics, 01 natural sciences, 7. Clean energy, stars [gamma-rays], Pulsar, Millisecond pulsar, 0103 physical sciences, Gamma-rays: stars, Globular clusters: individual: M15, Pulsars: general, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, star [Gamma-rays], education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, individual: M15 [Globular clusters], non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Compton scattering, Stars, Crab Nebula, Globular cluster, ddc:520, High Energy Physics::Experiment, Electrónica, general [Globular clusters], radiation mechanisms: non-thermal, pulsars: general, globular clusters: general, globular clusters: individual: M15, gamma-rays: stars, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Lepton
Abstract: A population of globular clusters (GCs) has been recently established by the Fermi-LAT telescope as a new class of GeV $\gamma$-ray sources. Leptons accelerated to TeV energies, in the inner magnetospheres of MSPs or in their wind regions, should produce $\gamma$-rays through the inverse Compton scattering in the dense radiation field from the huge population of stars. We have conducted deep observations of the globular cluster M15 with the MAGIC telescopes and used 165 hrs in order to search for $\gamma$-ray emission. A strong upper limit on the TeV $\gamma$-ray flux $, Comment: 11 pages, 7 figures, accepted for publication in MNRAS
Published: 2019

5. Discovery of TeV γ-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC

Author: R. J. García López, P G Prada Moroni, C. Arcaro, M. Vazquez Acosta, Masahiro Teshima, Elina Lindfors, Nikola Godinovic, Victoria Moreno, Daniel Mazin, Saverio Lombardi, A. Fernández-Barral, Chiara Righi, Pratik Majumdar, M. V. Fonseca, L. Nogués, Cosimo Nigro, M. Nievas Rosillo, Lluis Font, D. Dorner, A. Lamastra, M. Minev, R. Zanin, P. Temnikov, D. Elsaesser, J. Palacio, J. M. Paredes, Antonio Stamerra, Marcel Strzys, V. D'Elia, Martin Will, Stefano Covino, D. Zarić, Adrian Biland, D.F. Torres, Dario Hrupec, R. Paoletti, Wrijupan Bhattacharyya, B. Banerjee, A. Fattorini, Marc Ribó, S. Ansoldi, P. Giammaria, M. A. Lopez, Karl Mannheim, P. Bangale, Junko Kushida, J. Delgado, J. Rico, Kyoshi Nishijima, Tomoki Saito, Giovanni Ceribella, Satoshi Masuda, John Hoang, U. Barres de Almeida, Arka Chatterjee, Tarek M. Hassan, Hidetoshi Kubo, S. Paiano, Aaron Dominguez, F. Di Pierro, D. Kuveždić, Jürgen Besenrieder, Alexander Hahn, D. Hadasch, A. Rugliancich, Marina Manganaro, Fabrizio Tavecchio, M. I. Martínez, D. Fidalgo, Juan Abel Barrio, J. Becerra González, J. E. Ward, Damir Lelas, Francesco Longo, I. Snidaric, Sidika Merve Colak, G. Ferrara, E. Colombo, Sabrina Einecke, M. Delfino, Lab Saha, D. Dominis Prester, Alessio Berti, Ievgen Vovk, Louis Antonelli, A. Arbet Engels, S. Gallozzi, Gaia Vanzo, P. Cumani, Konstancja Satalecka, A. De Angelis, D. Ninci, Michele Doro, Dorota Sobczyńska, Martin Makariev, Ana Babić, Oscar Blanch, R. Mirzoyan, Vitaly Neustroev, W. Bednarek, T. Schweizer, Jose Luis Contreras, Christian Fruck, Julian Sitarek, Juan Cortina, J. Herrera, V. Fallah Ramazani, G. Bonnoli, David Paneque, M. Mariotti, Koji Noda, A. López-Oramas, Ivica Puljak, D. Guberman, Elisa Bernardini, G. Pedaletti, G. Maneva, D. Baack, M. Persic, P. Colin, V. A. Acciari, P. Da Vela, L. Foffano, L. Maraschi, Tomislav Terzić, Kari Nilsson, Yuki Iwamura, Susumu Inoue, J. R. Garcia, Camilla Maggio, Kazuma Ishio, E. de Oña Wilhelmi, A. Niedzwiecki, Elisa Prandini, Rodolfo Carosi, M. Peresano, N. Torres-Albà, Jose Miguel Miranda, D. Galindo, Francesco Leone, T. Surić, Shimpei Tsujimoto, Abelardo Moralejo, E. Moretti, Edgar Molina, B. De Lotto, Markus Gaug, Ciro Bigongiari, M. Garczarczyk, W. Rhode, Francesco Dazzi, A. Somero, Pablo Peñil, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., De Almeida, U Barre, Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., De Oña Wilhelmi, E., Torres, D. F., and Zanin, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, cloud [ISM], ISM:supernova remnants, acceleration of particles, ISM: clouds, cosmic rays, ISM: supernova remnants, gamma-rays: general, astro-ph.HE, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy and Astrophysics, Space and Planetary Science, 01 natural sciences, Spectral line, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, acceleration of particle, cosmic ray, Cherenkov radiation, Physics, Spectral index, 010308 nuclear & particles physics, supernova remnants [ISM], Spectral density, Astronomy and Astrophysic, acceleration of particles, cosmic rays, ISM:supernova remnants, ISM: clouds, gamma-rays: general, Acceleration of particles, cosmic rays, gamma-rays: general, ISM: clouds, ISM: supernova remnants, Supernova, 13. Climate action, ddc:520, supernova remnant [ISM], Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, clouds [ISM], general [gamma-rays], Radio wave
Abstract: SNR G24.7+0.6 is a 9.5 kyrs radio and $\gamma$-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL\,J1834.1--0706e/FGES\,J1834.1--0706) shows a hard spectral index ($\Gamma$$\sim$2) up to $200$\,GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of \snr\ with the MAGIC telescopes for a total of 31 hours. We detect very high energy $\gamma$-ray emission from an extended source located 0.34\degr\ away from the center of the radio SNR. The new source, named \mgc\ is detected up to 5\,TeV, and its spectrum is well-represented by a power-law function with spectral index of $2.74 \pm 0.08$. The complexity of the region makes the identification of the origin of the very-high energy emission difficult, however the spectral agreement with the LAT source and overlapping position at less than 1.5$\sigma$ point to a common origin. We analysed 8 years of \fermi-LAT data to extend the spectrum of the source down to 60\,MeV. \fermi-LAT and MAGIC spectra overlap within errors and the global broad band spectrum is described by a power-law with exponential cutoff at $1.9\pm0.5$\,TeV. The detected $\gamma$-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding., Comment: accepted for publication by MNRAS
Published: 2019

6. Detection of persistent VHE gamma-ray emission from PKS 1510–089 by the MAGIC telescopes during low states between 2012 and 2017

Author: M. I. Martínez, P. Bangale, Sabrina Einecke, Jae-Young Kim, M. Makariev, Aaron Dominguez, Alicia Fattorini, G. Pedaletti, Ivica Puljak, Stefano Covino, B. De Lotto, Pierre Colin, J. Kushida, Jose Luis Contreras, Walter Max-Moerbeck, J. Becerra González, A. Arbet Engels, A. De Angelis, Vitaly Neustroev, M. Peresano, Chiara Righi, Juan Abel Barrio, D. Elsaesser, J. Palacio, Satoshi Masuda, J. E. Ward, Juan Cortina, Takashi Saito, Wrijupan Bhattacharyya, P. Temnikov, Sidika Merve Colak, Wolfgang Rhode, Giovanni Ceribella, I. Agudo, José L. Gómez, V. A. Acciari, Antonio Stamerra, D. Hadasch, D. Fidalgo, Camilla Maggio, Abelardo Moralejo, A. López-Oramas, P. Munar-Adrover, E. Moretti, Daniela Dorner, Pablo Peñil, Alexander Hahn, Dominik Baack, Gaia Vanzo, G. Maneva, E. Do Souto Espiñera, Joni Tammi, Adrian Biland, Elina Lindfors, Jürgen Besenrieder, C. M. Raiteri, Louis Antonelli, Sol N. Molina, Daniel Mazin, Ievgen Vovk, A. Berti, Francesco Dazzi, A. Fernández-Barral, K. Nishijima, Manuel Delfino, M. Gaug, R. J. García López, Nikola Godinovic, D. Dominis Prester, J. Rico, V. Ramakrishnan, Francesco Longo, Pratik Majumdar, D. Zarić, M. V. Fonseca, J. Herrera, T. Schweizer, Antonio Fuentes, Sebastian Kiehlmann, Marc Ribó, Ana Babić, A. Somero, Koji Noda, L. Maraschi, E. Prandini, Elisa Bernardini, P. Giammaria, V. Fallah Ramazani, John Hoang, Massimo Persic, Stefano Ansoldi, S. Paiano, Efthalia Traianou, Riccardo Paoletti, Tomislav Terzić, Ciro Bigongiari, Clemens Thum, B. Banerjee, P. G. Prada Moroni, Hidetoshi Kubo, C. Arcaro, J. van Scherpenberg, Karl Mannheim, I. Snidaric, Oscar Blanch, D. Kuveždić, Razmik Mirzoyan, U. Barres de Almeida, F. Leone, Carolina Casadio, Kari Nilsson, Damir Lelas, Anne Lähteenmäki, Masahiro Teshima, Stefan Cikota, M. Strzys, M. Will, Markus Garczarczyk, Dorota Sobczyńska, D. Ninci, M. Vazquez Acosta, Angela Sandrinelli, Cosimo Nigro, M. Nievas Rosillo, G. Ferrara, M. Minev, Victoria Moreno, G. Bonnoli, Kazuma Ishio, Yuki Iwamura, Susumu Inoue, Tarek M. Hassan, W. Bednarek, Fabrizio Tavecchio, Dario Hrupec, Luca Foffano, Ll. Font, L. Nogués, M. A. Lopez, Rodolfo Carosi, Mosè Mariotti, J. M. Paredes, J. R. Garcia, V. D'Elia, Saverio Lombardi, A. Rugliancich, Marina Manganaro, Ioannis Myserlis, D. Galindo, Merja Tornikoski, E. Molina, E. Colombo, Konstancja Satalecka, Michele Doro, Lab Saha, A. Niedzwiecki, David Paneque, D. Guberman, Jordi Delgado, F. Di Pierro, Talvikki Hovatta, P. Da Vela, Julian Sitarek, C. Fruck, N. Torres-Albà, Stefano Gallozzi, Jose Miguel Miranda, Alessandra Lamastra, T. Surić, Shimpei Tsujimoto, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., DI Pierro, F., Do Souto Espiñera, E., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Becerra González, J., Raiteri, C. M., Sandrinelli, A., Hovatta, T., Kiehlmann, S., Max-Moerbeck, W., Tornikoski, M., Lähteenmäki, A., Tammi, J., Ramakrishnan, V., Thum, C., Agudo, I., Molina, S. N., Gómez, J. L., Fuentes, A., Casadio, C., Traianou, E., Myserlis, I., Kim, J. -Y., Metsähovi Radio Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, Federal Ministry of Education and Research (Germany), Max Planck Society, Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, and Junta de Andalucía
Subjects: galaxies [Gamma rays], Astrophysics, 01 natural sciences, 7. Clean energy, jet [Galaxies], law.invention, Raigs gamma, law, Jets (Astrofísica), Broadband, 010303 astronomy & astrophysics, Physics, galaxies: active, galaxies: jets, gamma rays: galaxies, quasars: individual: PKS 1510-089, galaxie [Gamma rays], Gamma ray, Galaxies: active, 3. Good health, Magnetic field, Gamma rays: galaxies, Spectral energy distribution, Física nuclear, Galaxies: jets, Quasars: individual: PKS 1510-089, Astronomy and Astrophysics, Space and Planetary Science, Flare, Spectral shape analysis, active [Galaxies], astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, individual: PKS 1510-089 [Quasars], Quasars, Quàsars, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Gamma rays, Quasar, Plasma, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Astrophysical jets, Astrophysics of Galaxies (astro-ph.GA), Galàxies actives, Active galaxies, ddc:520, jets [Galaxies]
Abstract: PKS 1510-089 is a flat spectrum radio quasar strongly variable in the optical and GeV range. To date, very high-energy (VHE, > 100 GeV) emission has been observed from this source either during long high states of optical and GeV activity or during short flares. Aims. We search for low-state VHE gamma-ray emission from PKS 1510-089. We characterize and model the source in a broadband context, which would provide a baseline over which high states and flares could be better understood. Methods. PKS 1510-089 has been monitored by the MAGIC telescopes since 2012. We use daily binned Fermi-LAT flux measurements of PKS 1510-089 to characterize the GeV emission and select the observation periods of MAGIC during low state of activity. For the selected times we compute the average radio, IR, optical, UV, X-ray, and gamma-ray emission to construct a low-state spectral energy distribution of the source. The broadband emission is modeled within an external Compton scenario with a stationary emission region through which plasma and magnetic fields are flowing. We also perform the emission-model-independent calculations of the maximum absorption in the broad line region (BLR) using two different models. Results. The MAGIC telescopes collected 75 hr of data during times when the Fermi-LAT flux measured above 1 GeV was below 3? × 10 -8 ? cm -2 ? s -1 , which is the threshold adopted for the definition of a low gamma-ray activity state. The data show a strongly significant (9.5¿) VHE gamma-ray emission at the level of (4.27 ± 0.61 stat ) × 10 -12 ? cm -2 ? s -1 above 150 GeV, a factor of 80 lower than the highest flare observed so far from this object. Despite the lower flux, the spectral shape is consistent with earlier detections in the VHE band. The broadband emission is compatible with the external Compton scenario assuming a large emission region located beyond the BLR. For the first time the gamma-ray data allow us to place a limit on the location of the emission region during a low gamma-ray state of a FSRQ. For the used model of the BLR, the 95% confidence level on the location of the emission region allows us to place it at a distance > 74% of the outer radius of the BLR. © ESO 2018., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Exce-lencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and by the Brazilian MCTIC, CNPq and FAPERJ. IA acknowledges support from a Ramón y Cajal grant of the Ministerio de Economía, Industria, y Competitividad (MINECO) of Spain. Acquisition and reduction of the POLAMI and MAPCAT data was supported in part by MINECO through grants AYA2010-14844, AYA2013-40825-P, and AYA2016-80889-P, and by the Regional Government of Andalucía through grant P09-FQM-4784.
Published: 2018

7. The Blazar TXS 0506+056 associated with a high-energy neutrino: insights into extragalactic jets and cosmic-ray acceleration

Author: M. Makariev, John Hoang, J. Besenrieder, J. Rico, W. Rhode, M. Vazquez Acosta, L. Nogués, J. Kushida, Simona Paiano, D. Hadasch, R. Ch. Berse, Jose Luis Contreras, Abelardo Moralejo, E. Moretti, K. Mielke, P. Da Vela, Ievgen Vovk, Francesco Dazzi, A. Fernández-Barral, M. I. Martínez, Juan Cortina, P. Bangale, A. Hahn, W. Bhattacharyya, K. Pfrang, F. Di Pierro, D. Fidalgo, M. Mariotti, K. Nishijima, G. Pedaletti, V. Moreno, G. Vanzo, S. Gallozzi, Sabrina Einecke, K. Mannheim, T. Saito, D. Dorner, C. Maggio, D. Dominis Prester, Stefano Covino, Matteo Cerruti, Marina Manganaro, Juan Abel Barrio, P. G. Prada Moroni, M. Strzys, S. Lombardi, P. Cumani, Konstancja Satalecka, Michele Doro, J. R. Garcia, P. Peñil, M. Minev, D. Lelas, F. Leone, B. De Lotto, Elisa Prandini, Rodolfo Carosi, Dario Hrupec, R. Paoletti, S. M. Colak, C. Arcaro, M. A. Lopez, M. Peresano, G. Ceribella, A. Niedzwiecki, M. V. Fonseca, Tarek M. Hassan, W. Bednarek, Ana Babić, David Paneque, Ciro Bigongiari, Petar Temnikov, Koji Noda, Elisa Bernardini, Stefano Ansoldi, Fabrizio Tavecchio, I. Šnidarić, Eduardo Colombo, Razmik Mirzoyan, Elina Lindfors, Ll. Font, Markus Gaug, D. Guberman, Daniel Mazin, A. Berti, J. Palacio, Christian Fruck, A. Fattorini, Tomislav Terzić, B. Banerjee, Dorota Sobczyńska, J. M. Paredes, Antonio Stamerra, Y. Iwamura, M. Hayashida, P. Giammaria, R. J. García López, Markus Garczarczyk, Francesco Longo, N. Godinović, Lab Saha, Pierre Colin, Kari Nilsson, G. Maneva, V. Fallah Ramazani, Marc Ribó, Massimo Persic, M. Will, Hidetoshi Kubo, Pratik Majumdar, D. Elsaesser, Jose Carlos Herrera, G. Ferrara, G. Bonnoli, Oscar Blanch, Jordi Delgado, M. Delfino, Julian Sitarek, Masahiro Teshima, T. Schweizer, D. Ninci, Chiara Righi, Satoshi Masuda, Arka Chatterjee, Yusuke Konno, I. Puljak, Laura Maraschi, C. Nigro, Darko Zarić, Luca Foffano, Aaron Dominguez, A. Lamastra, J. E. Ward, Shimpei Tsujimoto, A. Rugliancich, Vitaly Neustroev, Susumu Inoue, N. Torres-Albà, Valerio D'Elia, Dominik Baack, Adrian Biland, Jose Miguel Miranda, Tihomir Surić, Louis Antonelli, A. De Angelis, U. Barres de Almeida, M. Nievas Rosillo, K. Ishio, J. Becerra González, Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Vela, P. Da, Dazzi, F., Angelis, A. De, Lotto, B. De, Delfino, M., Delgado, J., Pierro, F. Di, Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Konno, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Pfrang, K., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albá, N., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Cerruti, Matteo, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), MAGIC, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: neutrino: energy: high, jets [galaxies], Electron, Astrophysics, individual (TXS 0506+056) [BL Lacertae objects], 01 natural sciences, neutrino, Absorption (logic), MAGIC (telescope), 010303 astronomy & astrophysics, interaction [electron], cosmic ray, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, photon, neutrinos, 520 Astronomie und zugeordnete Wissenschaften, non-thermal [radiation mechanisms], Neutrino detector, inverse [Compton scattering], electron: interaction, galaxies [gamma rays], acceleration [cosmic radiation], Física nuclear, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, VHE, energy [p], blazar, X-ray, cosmic rays, 0103 physical sciences, gamma rays: galaxies, ddc:530, galaxie [gamma rays], energy: high [neutrino], cosmic radiation: acceleration, Blazar, plasma, BL Lacertae objects: individual, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, galaxies: jets, radiation mechanisms: non-thermal, 530 Physik, MAGIC, BL Lacertae objects: individual (TXS 0506+056), cosmic rays, galaxies: jets, gamma rays: galaxies, neutrinos, radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, BL Lacertae objects: individual (TXS 0506+056), messenger, electromagnetic, Compton scattering: inverse, p: energy, jet [galaxies], gamma ray, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], absorption
Abstract: A neutrino with energy of $\sim$290 TeV, IceCube-170922A, was detected in coincidence with the BL Lac object TXS~0506+056 during enhanced gamma-ray activity, with chance coincidence being rejected at $\sim 3\sigma$ level. We monitored the object in the very-high-energy (VHE) band with the MAGIC telescopes for $\sim$41 hours from 1.3 to 40.4 days after the neutrino detection. Day-timescale variability is clearly resolved. We interpret the quasi-simultaneous neutrino and broadband electromagnetic observations with a novel one-zone lepto-hadronic model, based on interactions of electrons and protons co-accelerated in the jet with external photons originating from a slow-moving plasma sheath surrounding the faster jet spine. We can reproduce the multiwavelength spectra of TXS 0506+056 with neutrino rate and energy compatible with IceCube-170922A, and with plausible values for the jet power of $\sim 10^{45} - 4 \times 10^{46} {\rm erg \ s^{-1}}$. The steep spectrum observed by MAGIC is concordant with internal $\gamma\gamma$ absorption above a few tens of GeV entailed by photohadronic production of a $\sim$290 TeV neutrino, corroborating a genuine connection between the multi-messenger signals. In contrast to previous predictions of predominantly hadronic emission from neutrino sources, the gamma-rays can be mostly ascribed to inverse Compton up-scattering of external photons by accelerated electrons. The X-ray and VHE bands provide crucial constraints on the emission from both accelerated electrons and protons. We infer that the maximum energy of protons in the jet co-moving frame can be in the range $\sim 10^{14}$ to $10^{18}$ eV., Comment: 11 pages, 3 figues, 3 tables, Accepted for publication in ApJL. Major changes in the revised Version: corrected author list
Published: 2018

8. Multi-wavelength characterization of the blazar S5 0716+714 during an unprecedented outburst phase

Author: Mark Gurwell, Max Ludwig Ahnen, Elina Lindfors, D. Gasparrini, Antonio Stamerra, Daniel Mazin, J. Becerra González, Alessandro Carosi, B. De Lotto, Francesco Longo, A. Berti, Ievgen Vovk, G. A. Borman, Rodrigo Reeves, Abelardo Moralejo, M. Peresano, N. Torres-Albà, P. Giammaria, Helen Jermak, V. Fallah Ramazani, Juan Abel Barrio, G. Pedaletti, Adrian Biland, G. Bonnoli, M. Minev, I. Reichardt, T. Schweizer, D. Bastieri, I. Snidaric, Takashi Saito, I. Agudo, Stefano Gallozzi, Jose Miguel Miranda, Satoshi Masuda, R. J. García López, Alexander Hahn, Stefano Covino, Dario Hrupec, J. Kushida, J. Rico, J. Anton Zensus, Arka Chatterjee, Alan P. Marscher, Mosè Mariotti, M. A. Lopez, Dominik Baack, Yu. V. Troitskaya, Mitsunari Takahashi, A. C. S. Readhead, J. E. Ward, K. Mielke, D. Galindo, Aaron Dominguez, Jose Luis Contreras, Svetlana G. Jorstad, J. R. Garcia, D. Fidalgo, Massimo Persic, Pratik Majumdar, M. V. Fonseca, L. Maraschi, D. Kuveždić, K. Nishijima, D. Dominis Prester, J. M. Paredes, Sidika Merve Colak, E. N. Kopatskaya, D. J. Thompson, Juan Cortina, P. G. Prada Moroni, Giovanni Ceribella, Julian Sitarek, Stefano Ansoldi, Oscar Blanch, T. S. Grishina, Emmanouil Angelakis, Wrijupan Bhattacharyya, C. Fruck, Tomislav Terzić, Riccardo Paoletti, Chiara Righi, B. Lott, Jordi Delgado, A. Niedzwiecki, G. M. Madejski, D. Hadasch, F. Di Pierro, Saverio Lombardi, A. De Angelis, M. Strzys, Talvikki Hovatta, M. Vazquez Acosta, A. Treves, Vitaly Neustroev, L. V. Larionova, Ivan S. Troitsky, David Paneque, Yusuke Konno, L. Nogués, P. Temnikov, Andrea Rugliancich, Tarek M. Hassan, Krzysztof Nalewajko, W. Bednarek, Thomas P. Krichbaum, Sergey S. Savchenko, Victoria Moreno, Francesco Dazzi, A. Fernández-Barral, Ryosuke Itoh, P. Da Vela, Alexander Kraus, E. Moretti, Louis Antonelli, Fabrizio Tavecchio, Ll. Font, Bindu Rani, T. J. Pearson, Valeri M. Larionov, T. Nagayoshi, G. Maneva, D. Guberman, Manuel Delfino, Camilla Maggio, Daniela Dorner, Dariusz Gora, Gaia Vanzo, M. Gaug, S. Paiano, T. Surić, J. Herrera, Marina Manganaro, Shimpei Tsujimoto, Koji Noda, Ana Babić, Elisa Bernardini, Emilia Järvelä, Carolina Casadio, Anne Lähteenmäki, Masahiro Teshima, Karl Mannheim, Kari Nilsson, M. Will, Nikola Godinovic, Ioannis Myserlis, Merja Tornikoski, E. Colombo, Markus Garczarczyk, N. P. M. Kuin, L. O. Takalo, P. Cumani, Kazuma Ishio, Konstancja Satalecka, Michele Doro, Cosimo Nigro, M. Nievas Rosillo, Rodolfo Carosi, J. Palacio, V. Ramakrishnan, M. I. Martínez, P. Bangale, Sabrina Einecke, M. Makariev, E. Prandini, Iain A. Steele, Razmik Mirzoyan, U. Barres de Almeida, Damir Lelas, A. A. Vasilyev, Dorota Sobczyńska, Ivica Puljak, Pierre Colin, Sol N. Molina, D. A. Morozova, D. Ninci, A. Y. Lien, J. Hose, D. Elsaesser, Walter Max-Moerbeck, R. Ch. Berse, M. Hayashida, D. Zarić, Wolfgang Rhode, Marc Ribó, Hidetoshi Kubo, B. Banerjee, C. Arcaro, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), MAGIC, MWL, Fermi-LAT, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Ch Berse, R., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Bastieri, D., Gasparrini, D., Lott, B., Rani, B., Thompson, D. J., Agudo, I., Angelakis, E., Borman, G. A., Casadio, C., Grishina, T. S., Gurwell, M., Hovatta, T., Itoh, R., Järvelä, E., Jermak, H., Jorstad, S., Kopatskaya, E. N., Kraus, A., Krichbaum, T. P., Kuin, N. P. M., Lähteenmäki, A., Larionov, V. M., Larionova, L. V., Lien, A. Y., Madejski, G., Marscher, A., Myserlis, I., Max-Moerbeck, W., Molina, S. N., Morozova, D. A., Nalewajko, K., Pearson, T. J., Ramakrishnan, V., Readhead, A. C. S., Reeves, R. A., Savchenko, S. S., Steele, I. A., Tornikoski, M., Troitskaya, Yu. V., Troitsky, I., Vasilyev, A. A., Anton Zensus, J., Japanese Government, Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, Istituto Nazionale di Astrofisica, Federal Ministry of Education and Research (Germany), Croatian Science Foundation, Polish Academy of Sciences, Centre National de la Recherche Scientifique (France), Ministério da Ciência e Tecnologia (Brasil), National Aeronautics and Space Administration (US), Academy of Finland, Smithsonian Institution, Academia Sinica (Taiwan), Russian Science Foundation, Junta de Andalucía, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: BL Lacertae objects: individual: S5 0716+714, galaxies: active, galaxies: jets, gamma rays: galaxies, galaxies [Gamma rays], active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: active, Galaxies: jets, Gamma rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, 7. Clean energy, 01 natural sciences, jet [Galaxies], Radio spectrum, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Superluminal motion, galaxie [Gamma rays], 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysic, Light curve, Redshift, ddc:520, jets [Galaxies], Física nuclear, individual: S5 0716+714 [BL Lacertae objects], gamma-rays: galaxies, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BL Lac object, Fermi Gamma-ray Space Telescope
Abstract: Context. The BL Lac object S5 0716+714, a highly variable blazar, underwent an impressive outburst in January 2015 (Phase A), followed by minor activity in February (Phase B). The MAGIC observations were triggered by the optical flux observed in Phase A, corresponding to the brightest ever reported state of the source in the R-band. Aims.The comprehensive dataset collected is investigated in order to shed light on the mechanism of the broadband emission. Methods. Multi-wavelength light curves have been studied together with the broadband spectral energy distributions (SEDs). The sample includes data from Effelsberg, OVRO, Metsähovi, VLBI, CARMA, IRAM, SMA, Swift-UVOT, KVA, Tuorla, Steward, RINGO3, KANATA, AZT-8+ST7, Perkins, LX-200, Swift-XRT, NuSTAR, Fermi-LAT and MAGIC. Results. The flaring state of Phase A was detected in all the energy bands, providing for the first time a multi-wavelength sample of simultaneous data from the radio band to the very-high-energy (VHE, E > 100 GeV). In the constructed SED, the Swift-XRT+NuSTAR data constrain the transition between the synchrotron and inverse Compton components very accurately, while the second peak is constrained from 0.1 GeV to 600 GeV by Fermi+MAGIC data. The broadband SED cannot be described with a one-zone synchrotron self-Compton model as it severely underestimates the optical flux in order to reproduce the X-ray to -ray data. Instead we use a two-zone model. The electric vector position angle (EVPA) shows an unprecedented fast rotation. An estimation of the redshift of the source by combined high-energy (HE, 0.1 GeV < E < 100 GeV) and VHE data provides a value of z = 0:31 ± 0:02 ± 0:05, confirming the literature value. Conclusions. The data show the VHE emission originating in the entrance and exit of a superluminal knot in and out of a recollimation shock in the inner jet. A shock-shock interaction in the jet seems responsible for the observed flares and EVPA swing. This scenario is also consistent with the SED modeling. © ESO 2018., We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia "Maria de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Universities Space Research Association through a contract with NASA. We thank the Swift team duty scientists and science planners., The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The VLBA is an instrument of the Long Baseline Observatory. The Long Baseline Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. The Sub-millimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G, NNX11A043G and NNX14AQ89G, and NSF grants AST-0808050 and AST-1109911. The St. Petersburg University team acknowledges support from Russian Science Foundation grant 17-12-01029. The BU group acknowledges support by NASA under Fermi Guest Investigator grant NNX14AQ58G and by NSF under grant AST-1615796. Part of this work was done with funding by the UK Space Agency. The VLBA is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The PRISM (Perkins Re-Imaging SysteM) camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. This paper makes use of data obtained with the 100m Effelsberg radio-telescope, which is operated by the Max-Planck-Institut fur Radioastronomy (MPIfR) in Bonn (Germany). Part of this work is based on archival data, software or online services provided by the ASI Science Data Center (ASDC). PYRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. This paper is partly based on observations carried out with the IRAM 30 m. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). IA acknowledges support by a Ramon y Cajal grant of the Ministerio de Economia, Industria y Competitividad (MINECO) of Spain. The research at the IAA-CSIC was supported in part by the MINECO through grants AYA2016-80889-P, AYA2013-40825-P, and AYA2010-14844, and by the regional government of Andalucia through grant P09-FQM-4784. The Liverpool Telescope is operated by JMU with financial support from the UK-STFC.
Published: 2018

9. Limits on the flux of tau neutrinos from 1 PeV to 3 EeV with the MAGIC telescopes

Author: Christian Fruck, L. Nogués, E. Moretti, Francesco Longo, Alba Fernández-Barral, Kazuma Ishio, Satoshi Masuda, Arka Chatterjee, D. Fidalgo, Yusuke Konno, M. Garczarczyk, L. Maraschi, Elina Lindfors, Ievgen Vovk, Ivica Puljak, Pierre Colin, J. R. Garcia, Daniel Mazin, A. Berti, M. I. Martínez, Rodolfo Carosi, Mosè Mariotti, Louis Antonelli, T. Schweizer, K. Mielke, Alessandro Carosi, B. De Lotto, Aaron Dominguez, Cosimo Nigro, M. Nievas Rosillo, T. Nagayoshi, Martin Makariev, N. Torres-Albà, M. Minev, Sabrina Einecke, Pratik Majumdar, M. V. Fonseca, Nikola Godinovic, J. E. Ward, J. Becerra González, Stefano Ansoldi, Riccardo Paoletti, Jose Miguel Miranda, Saverio Lombardi, Andrea Rugliancich, Abelardo Moralejo, Sidika Merve Colak, Stefano Covino, Tomislav Terzić, Oscar Blanch, P. G. Prada Moroni, G. Pedaletti, E. Colombo, Marcel Strzys, Masahiro Teshima, Wrijupan Bhattacharyya, J. Palacio, Julian Sitarek, J. Hose, K. Nishijima, Daniela Hadasch, R. Mirzoyan, Adrian Biland, Martin Will, J. M. Paredes, U. Barres de Almeida, I. Reichardt, L. O. Takalo, Antonio Stamerra, Tomoki Saito, Giovanni Ceribella, D. Elsaesser, R. Ch. Berse, Damir Lelas, M. Peresano, Marina Manganaro, D. Galindo, Shimpei Tsujimoto, Dominik Baack, Tihomir Surić, J. Rico, Dorota Sobczyńska, Wolfgang Rhode, S. Paiano, Chiara Righi, P. Cumani, Konstancja Satalecka, Michele Doro, Karl Mannheim, P. Temnikov, Dario Hrupec, Francesco Dazzi, M. Vazquez Acosta, Juan Abel Barrio, M. A. Lopez, Mitsunari Takahashi, Victoria Moreno, A. Niedzwiecki, R. J. García López, David Paneque, B. Banerjee, C. Arcaro, D. Guberman, E. Prandini, A. De Angelis, A. Treves, Vitaly Neustroev, Massimo Persic, D. Kuveždić, Jordi Delgado, G. Bonnoli, F. Di Pierro, Manuel Delfino, Camilla Maggio, Daniela Dorner, Dariusz Gora, Gaia Vanzo, M. Gaug, J. Herrera, G. Maneva, Koji Noda, Elisa Bernardini, P. Da Vela, Ana Babić, Kari Nilsson, J. Kushida, Jose Luis Contreras, Juan Cortina, Tarek M. Hassan, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Max Ludwig Ahnen, P. Giammaria, I. Snidaric, M. Hayashida, D. Zarić, Marc Ribó, P. Bangale, Hidetoshi Kubo, D. Ninci, Alexander Hahn, D. Dominis Prester, V. Fallah Ramazani, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Vela, P. Da, Dazzi, F., Angelis, A. De, Lotto, B. De, Delfino, M., Delgado, J., Pierro, F. Di, Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Góra, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., and Zarić, D.
Subjects: Point source, Astrophysics::High Energy Astrophysical Phenomena, Tau neutrinos, FOS: Physical sciences, Astrophysics, Cherenkov telescopes, 01 natural sciences, law.invention, law, Tau neutrino, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma-ray astronomy, tau neutrinos, Spectral index, ta115, 010308 nuclear & particles physics, Horizon, High Energy Physics::Phenomenology, Astronomy and Astrophysics, Cherenkov telescope, ddc:540, High Energy Physics::Experiment, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Lepton, Flare
Abstract: Astroparticle physics 102, 77 - 88 (2018). doi:10.1016/j.astropartphys.2018.05.002, A search for tau neutrino induced showers with the MAGIC telescopes is presented. The MAGIC telescopes located at an altitude of 2200 m a.s.l. in the Canary Island of La Palma, can point towards the horizon or a few degrees below across an azimuthal range of about 80°. This provides a possibility to search for air showers induced by tau leptons arising from interactions of tau neutrinos in the Earth crust or the surrounding ocean. In this paper we show how such air showers can be discriminated from the background of very inclined hadronic showers by using Monte Carlo simulations. Taking into account the orography of the site, the point source acceptance and the event rates expected have been calculated for a sample of generic neutrino fluxes from photo-hadronic interactions in AGNs. The analysis of about 30 h of data taken towards the sea leads to a 90% C.L. point source limit for tau neutrinos in the energy range from 1.0 × 10$^{15}$ eV to 3.0 × 10$^{18}$ eV of about $E^{2}_{\nu_{\tau}} \times \phi (E_{\nu_{\tau}}) < 2.0 \times 10^{-4}$ GeV cm$^{-2} s^{-1}$ for an assumed power-law neutrino spectrum with spectral index $\gamma =−2$. However, with 300 h and in case of an optimistic neutrino flare model, limits of the level down to $E^{2}_{\nu_{\tau}} \times \phi (E_{\nu_{\tau}}) < 8.4 \times 10^{-6}$ GeV cm$^{-2} s^{-1}$ can be expected., Published by Elsevier Science, Amsterdam [u.a.]
Published: 2018

10. The broad-band properties of the intermediate synchrotron peaked BL Lac S2 0109+22 from radio to VHE gamma rays

Author: F. Wierda, M. Peresano, Cosimo Nigro, Alexander Hahn, M. Nievas Rosillo, R. Reinthal, M. Hayashida, M. Minev, N. Mankuzhiyil, Julian Sitarek, Razmik Mirzoyan, U. Barres de Almeida, Nikola Godinovic, Damir Lelas, J. M. Paredes, Tomislav Terzić, Marc Ribó, Kazuma Ishio, Antonio Stamerra, Ievgen Vovk, Dorota Sobczyńska, M. Delfino, Wrijupan Bhattacharyya, Juan Abel Barrio, P. Bangale, Francesco Longo, D. Dominis Prester, Hidetoshi Kubo, B. De Lotto, J. E. Ward, Rodolfo Carosi, Camilla Maggio, Jenni Jormanainen, S. Paiano, M. Lopez, Karl Mannheim, P. G. Prada Moroni, Marcel Strzys, Ivica Puljak, John Hoang, Stefano Ciprini, Pierre Colin, Daniela Dorner, Gaia Vanzo, Dominik Baack, R. Desiante, Jordi Delgado, T. Schweizer, Fallah Ramazani, F. Di Pierro, M. Gaug, G. Ferrara, Anthony C. S. Readhead, D. Elsaesser, J. Becerra González, J. Herrera, G. Bonnoli, M. Vazquez Acosta, Talvikki Hovatta, Neustroev, L. Nogués, R. J. García López, Martin Makariev, Koji Noda, Elisa Bernardini, L. Maraschi, A. Niedzwiecki, Francesco Dazzi, A. Fernández-Barral, Elina Lindfors, K. Pfrang, Oscar Blanch, E. Moretti, Dario Hrupec, P. Da Vela, Pratik Majumdar, M. V. Fonseca, Darko Zarić, Aaron Dominguez, Daniel Mazin, A. Berti, Ciro Bigongiari, J. Palacio, Massimo Persic, F. Leone, Anne Lähteenmäki, Stefano Ansoldi, S Barcewicz, M. Garczarczyk, David Paneque, Masahiro Teshima, Martin Will, Riccardo Paoletti, Stefano Covino, Walter Max-Moerbeck, R. Ch. Berse, Sidika Merve Colak, Yuki Iwamura, Kyoshi Nishijima, D. Ninci, Abelardo Moralejo, J. R. Garcia, Susumu Inoue, D. Guberman, E. Prandini, Louis Antonelli, R. J. C. Vera, Alessandra Lamastra, M. I. Martínez, Tomoki Saito, Giovanni Ceribella, Marina Manganaro, Merja Tornikoski, Joni Tammi, Sabrina Einecke, P. Cumani, Chiara Righi, Konstancja Satalecka, Wolfgang Rhode, Michele Doro, P. Temnikov, K. Mielke, Iva Šnidarić, Sebastian Kiehlmann, B. Banerjee, Alicia Fattorini, C. Arcaro, Pablo Peñil, Shimpei Tsujimoto, Jürgen Besenrieder, Adrian Biland, Moreno, Tihomir Surić, J. Rico, Satoshi Masuda, Arka Chatterjee, P. Giammaria, D. Fidalgo, N. Torres-Albà, Tarek M. Hassan, G. Pedaletti, Yusuke Konno, W. Bednarek, Fabrizio Tavecchio, Ll. Font, A. De Angelis, Stefano Gallozzi, Jose Miguel Miranda, G. Maneva, Ana Babić, J. Kushida, Jose Luis Contreras, Juan Cortina, Kari Nilsson, E. Colombo, Lab Saha, Luca Foffano, L. O. Takalo, D. Hadasch, Mosè Mariotti, Saverio Lombardi, Andrea Rugliancich, D’Elia, Christian Fruck, Department of Electronics and Nanoengineering, Metsähovi Radio Observatory, Aalto-yliopisto, Aalto University, Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Gallozzi, S., García Łópez, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Konno, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Łópez, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Pfrang, K., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Ciprini, S., Desiante, R., Barcewicz, S., Hovatta, T., Jormanainen, J., Takalo, L., Reinthal, R., Mankuzhiyil, N., Wierda, F., Lähteenmäki, A., Tammi, J., Tornikoski, M., Vera, R. J. C., Kiehlmann, S., Max-Moerbeck, W., Readhead, A. C. S., Ciprini , S., and Desiante , R.
Subjects: galaxie [Gamma-rays], active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, jet [Galaxies], Luminosity, 0103 physical sciences, BL Lacertae objects: individual: S2 0109+22, Galaxies: active, Galaxies: jets, Gamma-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, MAGIC (telescope), Blazar, education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, ta115, 010308 nuclear & particles physics, galaxies: active, galaxies: jets, gamma-rays: galaxies, Optical polarization, individual: S2 0109+22 [BL Lacertae objects], Astronomy and Astrophysic, Redshift, 13. Climate action, ddc:520, Spectral energy distribution, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract: The MAGIC telescopes observed S2 0109+22 in 2015 July during its flaring activity in high energy gamma rays observed by Fermi-LAT. We analyse the MAGIC data to characterise the very high energy (VHE) gamma-ray emission of S2 0109+22, which belongs to the subclass of intermediate synchrotron peak (ISP) BL Lac objects. We study the multi-frequency emission in order to investigate the source classification. Finally, we compare the source long-term behaviour to other VHE gamma-ray emitting (TeV) blazars. We performed a temporal and spectral analysis of the data centred around the MAGIC interval of observation (MJD 57225-57231). Long-term radio and optical data have also been investigated using the discrete correlation function. The redshift of the source is estimated through optical host-galaxy imaging and also using the amount of VHE gamma-ray absorption. The quasi-simultaneous multi-frequency spectral energy distribution (SED) is modelled with the conventional one-zone synchrotron self-Compton (SSC) model. MAGIC observations resulted in the detection of the source at a significance level of $5.3\,\sigma$. The VHE gamma-ray emission of S2 0109+22 is variable on a daily time scale. VHE gamma-ray luminosity of the source is lower than the average of TeV BL Lacs. The optical polarization, and long-term optical/radio behaviour of the source are different from the general population of TeV blazars. All these findings agree with the classification of the source as an ISP BL Lac object. We estimate the source redshift as $z = 0.36 \pm 0.07$. The SSC parameters describing the SED are rather typical for blazars., Comment: 15 pages, 10 figures, Corresponding authors: Fallah Ramazani, V. (vafara@utu.fi), Hovatta, T. (talvikki.hovatta@utu.fi), Lindfors, E. (elilin@utu.fi) and Nilsson, K. (kani@utu.fi)
Published: 2018
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11. Constraining very-high-energy and optical emission from FRB 121102 with the MAGIC telescopes

Author: D. Elsaesser, Satoshi Masuda, Alessandra Lamastra, A. Hahn, Stefano Covino, K. Nishijima, Francesco Longo, Kazumi Kashiyama, Arka Chatterjee, Marc Ribó, Pierre Colin, D. Hadasch, J. Becerra González, Oscar Blanch, Julian Sitarek, P. Bangale, Abelardo Moralejo, Hidetoshi Kubo, W. Bhattacharyya, W. Rhode, J. Kushida, Jose Luis Contreras, J. Rico, P. Giammaria, Laura Spitler, F. Leone, M. Minev, L. Maraschi, E. Colombo, Juan Cortina, I. Puljak, Masahiro Teshima, G. Ferrara, Jordi Delgado, M. Vazquez Acosta, M. López, G. Bonnoli, J. Palacio, T. Schweizer, E. Molina, Victoria Moreno, Chiara Righi, J. M. Paredes, Antonio Stamerra, M. Delfino, Francesco Dazzi, A. Fernández-Barral, Jason W. T. Hessels, N. Torres-Albà, B. Banerjee, C. Arcaro, J. R. Garcia, Darko Zarić, P. Da Vela, Iva Šnidarić, D. Baack, D. Ninci, Jürgen Besenrieder, Alicia Fattorini, D. Dominis Prester, F. Di Pierro, M. Peresano, M. Makariev, A. Arbet Engels, Vitaly Neustroev, Lab Saha, Luca Foffano, Pablo Peñil, R. J. García López, Stefano Gallozzi, Jose Miguel Miranda, A. Somero, V. D'Elia, Aaron Dominguez, A. Niedzwiecki, J. E. Ward, C. Fruck, Ciro Bigongiari, Kari Nilsson, P. Majumdar, C. Nigro, G. Ceribella, Elina Lindfors, Juan Abel Barrio, L. Nogués, D. Dorner, M. Nievas Rosillo, M. Mariotti, S. M. Colak, M. Garczarczyk, D. Guberman, Kohta Murase, A. Rugliancich, Marina Manganaro, V. Fallah Ramazani, C. Maggio, G. Maneva, Daniel Mazin, Tomislav Terzić, Dario Hrupec, R. Paoletti, A. Berti, M. Will, A. López-Oramas, D. Paneque, N. Godinović, B. De Lotto, K. Mannheim, Tarek M. Hassan, W. Bednarek, Andrew Seymour, G. Pedaletti, Shimpei Tsujimoto, P. Cumani, Konstancja Satalecka, Michele Doro, Fabrizio Tavecchio, M. I. Martínez, Massimo Persic, V. A. Acciari, Ll. Font, Razmik Mirzoyan, P G Prada Moroni, Adrian Biland, Louis Antonelli, D. Lelas, G. Vanzo, E. Moretti, Ana Babić, Sabrina Einecke, A. De Angelis, Tihomir Surić, S. Paiano, K. Ishio, Dorota Sobczyńska, Benito Marcote, Stefano Ansoldi, D. Fidalgo, Markus Gaug, M. V. Fonseca, Saverio Lombardi, John Hoang, Takashi Saito, U. Barres de Almeida, Elisa Prandini, Rodolfo Carosi, Susumu Inoue, Daniele Michilli, Y. Iwamura, M. Strzys, D. Kuveždić, I. Vovk, Valentí Bosch-Ramon, Jose Carlos Herrera, Petar Temnikov, Koji Noda, Elisa Bernardini, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Marcote, B., Spitler, L. G., Hessels, J. W. T., Kashiyama, K., Murase, K., Bosch-Ramon, V., Michilli, D., Seymour, A., Universitat de Barcelona, and ITA
Subjects: High energy, Photon, Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radiació, Raigs gamma, radiation mechanisms: non-thermal, methods: data analysis, methods: observational, gamma-rays: general, Methods: observational, Methods: data analysis, 0103 physical sciences, Gamma ray astronomy, Astronomia de raigs gamma, observational [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Millisecond, general [Gamma-rays], ta115, Radiation, non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Astronomy and Astrophysic, Galaxy, Redshift, data analysi [Methods], Wavelength, 13. Climate action, Space and Planetary Science, Gamma-rays: general, ddc:520, Física nuclear, Optical emission spectroscopy, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Fast radio bursts (FRBs) are bright flashes observed typically at GHz frequencies with millisecond duration, whose origin is likely extragalactic. Their nature remains mysterious, motivating searches for counterparts at other wavelengths. FRB 121102 is so far the only source known to repeatedly emit FRBs and is associated with a host galaxy at redshift $z \simeq 0.193$. We conducted simultaneous observations of FRB 121102 with the Arecibo and MAGIC telescopes during several epochs in 2016--2017. This allowed searches for millisecond-timescale burst emission in very-high-energy (VHE) gamma rays as well as the optical band. While a total of five FRBs were detected during these observations, no VHE emission was detected, neither of a persistent nature nor burst-like associated with the FRBs. The average integral flux upper limits above 100 GeV at 95% confidence level are $6.6 \times 10^{-12}~\mathrm{photons\ cm^{-2}\ s^{-1}}$ (corresponding to luminosity $L_{\rm VHE} \lesssim 10^{45}~\mathrm{erg\ s^{-1}}$) over the entire observation period, and $1.2 \times 10^{-7}~ \mathrm{photons\ cm^{-2}\ s^{-1}}$ ($L_{\rm VHE} \lesssim 10^{49}~\mathrm{erg\ s^{-1}}$) over the total duration of the five FRBs. We constrain the optical U-band flux to be below 8.6 mJy at 5-$\sigma$ level for 1-ms intervals around the FRB arrival times. A bright burst with U-band flux $29~\mathrm{mJy}$ and duration $\sim 12$ ms was detected 4.3 s before the arrival of one FRB. However, the probability of spuriously detecting such a signal within the sampled time space is 1.5% (2.2 $\sigma$, post-trial), i.e. consistent with the expected background. We discuss the implications of the obtained upper limits for constraining FRB models., Comment: 9 pages, 3 figures. Accepted for publication in MNRAS the 2nd September 2018
Published: 2018

12. Detection of the blazar S4 0954+65 at very-high-energy with the MAGIC telescopes during an exceptionally high optical state

Author: M. Hayashida, Satoshi Masuda, Arka Chatterjee, Juan Abel Barrio, D. Fidalgo, Yu. V. Troitskaya, Svetlana G. Jorstad, Emilia Järvelä, Marc Ribó, J. A. Acosta Pulido, Wrijupan Bhattacharyya, L. Maraschi, Kari Nilsson, P. Bangale, Hidetoshi Kubo, J. Hose, Stefano Ansoldi, Yusuke Konno, D. Elsaesser, Riccardo Paoletti, Tomislav Terzić, Francesco Longo, Elina Lindfors, P. G. Prada Moroni, Daniel Mazin, G. A. Borman, Alessandro Carosi, V. Fallah Ramazani, J. Palacio, D. Ninci, Kazuma Ishio, Pratik Majumdar, A. Berti, J. M. Paredes, Antonio Stamerra, N. Torres-Albà, J. Kushida, M. V. Fonseca, Jose Luis Contreras, M. Peresano, M. Makariev, G. Bonnoli, D. Kuveždić, Tarek M. Hassan, W. Bednarek, G. Pedaletti, Juan Cortina, Fabrizio Tavecchio, Martin Will, Chiara Righi, R. Ch. Berse, Ll. Font, Razmik Mirzoyan, Rodolfo Carosi, Dario Hrupec, Jose Miguel Miranda, J. Becerra González, M. A. Lopez, J. R. Garcia, Marina Manganaro, U. Barres de Almeida, P. Temnikov, E. Colombo, Oscar Blanch, T. S. Grishina, Mitsunari Takahashi, Stefano Covino, Louis Antonelli, Damir Lelas, Valeri M. Larionov, Aaron Dominguez, D. Galindo, Merja Tornikoski, Sergey S. Savchenko, Francesco Dazzi, Manuel Delfino, D. Dominis Prester, Wolfgang Rhode, Nikola Godinovic, Shimpei Tsujimoto, Tomoki Saito, Giovanni Ceribella, A. A. Vasilyev, Ana Babić, P. Cumani, L. O. Takalo, Konstancja Satalecka, L. Nogués, Michele Doro, Max Ludwig Ahnen, Dorota Sobczyńska, R. Ojha, K. Mielke, J. Finke, E. Moretti, Ievgen Vovk, P. Giammaria, Jordi Delgado, F. Di Pierro, Camilla Maggio, Daniela Dorner, Dariusz Gora, M. Gaug, G. Vanzo, C. Protasio, J. Herrera, D. Hadasch, Alba Fernández-Barral, Carolina Casadio, Anne Lähteenmäki, Mosè Mariotti, Masahiro Teshima, Alexander Hahn, E. Prandini, Cosimo Nigro, M. Nievas Rosillo, T. Nagayoshi, Kyoshi Nishijima, M. Minev, Iva Šnidarić, T. Schweizer, J. E. Ward, Sidika Merve Colak, E. N. Kopatskaya, A. Niedzwiecki, Koji Noda, Elisa Bernardini, Ivan S. Troitsky, David Paneque, D. Guberman, Saverio Lombardi, Andrea Rugliancich, V. Ramakrishnan, M. I. Martínez, Sabrina Einecke, Ivica Puljak, Pierre Colin, Markus Garczarczyk, M. I. Carnerero, Talvikki Hovatta, Sol N. Molina, P. Da Vela, Julian Sitarek, S. Paiano, Karl Mannheim, D. A. Morozova, A. De Angelis, A. Treves, Vitaly Neustroev, M. Vazquez Acosta, L. V. Larionova, G. Maneva, I. Agudo, Adrian Biland, Tihomir Surić, J. Rico, Dominik Baack, Alan P. Marscher, Christian Fruck, Victoria Moreno, Darko Zarić, B. De Lotto, Abelardo Moralejo, I. Reichardt, Mark Gurwell, B. Banerjee, Marcel Strzys, C. Arcaro, R. J. García López, Massimo Persic, Yasuyuki T. Tanaka, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Becerra González, J., Tanaka, Y., Ojha, R., Finke, J., Lähteenmäki, A., Järvelä, E., Tornikoski, M., Ramakrishnan, V., Hovatta, T., Jorstad, S. G., Marscher, A. P., Larionov, V. M., Borman, G. A., Grishina, T. S., Kopatskaya, E. N., Larionova, L. V., Morozova, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., Agudo, I., Molina, S. N., Casadio, C., Gurwell, M., Carnerero, M. I., Protasio, C., Acosta Pulido, J. A., Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, Federal Ministry of Education and Research (Germany), Junta de Andalucía, Max Planck Society, Universitat de Barcelona, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: individual: S4 0954+65 [BL Lacertae objects], Active galactic nucleus, active [Galaxies], BL Lacertae objects: individual: S4 0954+65, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxies: active, Gamma rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, Gamma ray astronomy, Astronomia de raigs gamma, gamma rays:galaxies, galaxies:active, BL Lacertae objects:individual:S40954+65, Blazar, 010303 astronomy & astrophysics, Quasars, Astrophysics::Galaxy Astrophysics, Quàsars, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, gamma rays: galaxies, galaxies: active, galaxie [Gamma rays], 010308 nuclear & particles physics, Compton scattering, Optical polarization, Quasar, Astronomy and Astrophysic, Galaxies, Redshift, Galàxies, galaxies [gamma rays], ddc:520, Spectral energy distribution, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Radio wave
Abstract: The very high energy (VHE ¿ 100 GeV) -ray MAGIC observations of the blazar S4 0954+65, were triggered by an exceptionally high flux state of emission in the optical. This blazar has a disputed redshift of z = 0.368 or z ¿ 0.45 and an uncertain classification among blazar subclasses. The exceptional source state described here makes for an excellent opportunity to understand physical processes in the jet of S4 0954+65 and thus contribute to its classification. Methods. We investigated the multiwavelength (MWL) light curve and spectral energy distribution (SED) of the S4 0954+65 blazar during an enhanced state in February 2015 and have put it in context with possible emission scenarios. We collected photometric data in radio, optical, X-ray, and ¿-ray. We studied both the optical polarization and the inner parsec-scale jet behavior with 43 GHz data. Results. Observations with the MAGIC telescopes led to the first detection of S4 0954+65 at VHE. Simultaneous data with Fermi-LAT at high energy ¿-ray(HE, 100 MeV < E < 100 GeV) also show a period of increased activity. Imaging at 43 GHz reveals the emergence of a new feature in the radio jet in coincidence with the VHE flare. Simultaneous monitoring of the optical polarization angle reveals a rotation of approximately 100. Conclusions. The high emission state during the flare allows us to compile the simultaneous broadband SED and to characterize it in the scope of blazar jet emission models. The broadband spectrum can be modeled with an emission mechanism commonly invoked for flat spectrum radio quasars (FSRQs), that is, inverse Compton scattering on an external soft photon field from the dust torus, also known as external Compton. The light curve and SED phenomenology is consistent with an interpretation of a blob propagating through a helical structured magnetic field and eventually crossing a standing shock in the jet, a scenario typically applied to FSRQs and low-frequency peaked BL Lac objects (LBL). © ESO 2018., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq, and FAPERJ. IA acknowledges support by a Ramón y Cajal grant of the Ministerio de Economía, Industria y Competitividad (MINECO) of Spain. The research at the IAA–CSIC was supported in part by the MINECO through grants AYA2016–80889–P, AYA2013–40825–P, and AYA2010–14844, and by the regional government of Andalucía through grant P09–FQM–4784.
Published: 2018

13. Probing high-energy acceleration processes in S5 0716+714 using combined Fermi-LAT and MAGIC observations

Author: Fermi-LAT, Bindu Rani, Magic collaborations, G. Pedaletti, Martina Manganaro, and E. Lindfors
Subjects: Physics, 0209 industrial biotechnology, Photon, Astrophysics::High Energy Astrophysical Phenomena, 02 engineering and technology, Astrophysics, Light curve, 7. Clean energy, Synchrotron, law.invention, 020901 industrial engineering & automation, law, 0202 electrical engineering, electronic engineering, information engineering, Spectral energy distribution, 020201 artificial intelligence & image processing, MAGIC (telescope), Blazar, Fermi Gamma-ray Space Telescope, BL Lac object
Abstract: The BL Lac object S5 0716+714 underwent an impressive outburst in January/February 2015, being detected by many instruments spanning from radio to very high energy gamma-rays (VHE, E > 100 GeV). The multi-wavelength dataset collected made possible a deep study of the broad- band Spectral Energy Distribution (SED), which in blazars is described by two components. The low-energy component, in case of S5 0716+714 peaked between 1014 - 1015 Hz, is generated by synchrotron emission from relativistic electrons in the jet, while the high-energy one is in general attributed to inverse-Compton (IC) up-scattering of soft synchrotron photons off the same elec- trons that have undergone synchrotron cooling. For the first time for this source, the high energy (HE, 0.1 GeV < E < 100 GeV) and VHE gamma-ray data have been collected simultaneously, from Fermi-LAT and MAGIC respectively, allowing the possibility to study the whole high en- ergy part of the broadband SED in an unprecedented high state. In this contribution we will report on the broadband activity of the source during its strongest outburst ever detected so far, focus- ing on the GeV-TeV connection, described by the multi-wavelength light curves and the SED. A combined spectrum of Fermi-LAT and MAGIC will be presented, in the frame of a two-zone modelling.
Published: 2017

14. Multiwavelength observations of the blazar BL Lacertae in June 2015

Author: G. Pedaletti, Julian Sitarek, Vandad Fallah Ramazani, J. Kushida, Elina Lindfors, Daniel Mazin, Fermi-LAT Collaborations, Monica Vazquez Acosta, Shimpei Tsujimoto, Filippo D'Ammando, and Kyoshi Nishijima
Subjects: Physics, Crab Nebula, law, Flux, MAGIC (telescope), Astrophysics, Blazar, Light curve, Redshift, Radio wave, Flare, law.invention
Abstract: BL Lacertae is a blazar at the redshift of z = 0.069, eponym of the BL Lac blazar type. It is also a prototype of the low-frequency-peaked BL Lac (LBL) subclass. It was first detected in sub-TeV gamma-ray range by MAGIC in 2005. In 2015, MAGIC observations of BL Lacertae were triggered by the Fermi-LAT analysis report in the MAGIC group, and were performed during 10 individual nights between 15th and 28th June for a total of 8.6 h. The measured gamma-ray flux varied from 40% to 10% of the Crab nebula flux above 200 GeV in the nights from 15th to 17th June. In particular, a fast variability was found during the nights of 15th and 17th June. We also performed multi-wavelength (MWL) observations in the radio, optical, UV, X-ray and gamma-ray bands, and the MWL light curves indicate that no apparent simultaneous activity in other wavebands accompanying the very high energy gamma-ray flare in June 2015 like an another occurrence of an orphan very high energy flare. In this proceedings we will present the results of the campaign and discuss their implications on our understanding of the object.
Published: 2017

15. Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes

Author: K. Mallot, F. Di Pierro, Francesco Longo, R. J. García López, D. Hadasch, Daniela Dorner, U. Barres de Almeida, Damir Lelas, S. Paiano, Karl Mannheim, W. Idec, Mosè Mariotti, Dariusz Gora, Gaia Vanzo, D. Nakajima, D. Elsaesser, Dorota Sobczyńska, P. Da Vela, M. Gaug, Arka Chatterjee, R. Zanin, Adrian Biland, Saverio Lombardi, Abelardo Moralejo, Wlodek Bednarek, Alessandro Carosi, Max Ludwig Ahnen, J. Becerra González, M. Palatiello, M. Hayashida, Ruben Lopez-Coto, J. Herrera, D. Fidalgo, Martin Makariev, Pratik Majumdar, M. V. Fonseca, Massimo Persic, Alessio Berti, Marc Ribó, P. Bangale, Hidetoshi Kubo, E. Moretti, Alexander Hahn, Dario Hrupec, M. A. Lopez, Francesco Dazzi, A. Fernández-Barral, M. Vazquez Acosta, J. Rico, I. Reichardt, Rodolfo Carosi, Oscar Blanch, E. Colombo, P. Giammaria, P. Temnikov, Gareth Hughes, J. M. Paredes, L. Nogués, B. Biasuzzi, Koji Noda, Stefano Covino, U. Menzel, Antonio Stamerra, K. Kodani, L. O. Takalo, Elisa Bernardini, Kyoshi Nishijima, Nikola Godinovic, Benito Marcote, Jose Miguel Miranda, E. Prandini, L. Perri, Yusuke Konno, Diego F. Torres, M. Doert, M. H. Wu, L. A. Antonelli, M. I. Martínez, M. Garczarczyk, A. La Barbera, Marcel Strzys, S. Bonnefoy, Julian Sitarek, D. Eisenacher Glawion, X. Paredes-Fortuny, M. Peresano, D. Dominis Prester, Sabrina Einecke, B. De Lotto, Kari Nilsson, D. Tescaro, J. Hose, A. Niedzwiecki, C. Fruck, M. Engelkemeier, F. Borracci, M. Nievas Rosillo, M. Will, A. De Angelis, A. Treves, Vitaly Neustroev, R. Mirzoyan, T. Toyama, Fabrizio Tavecchio, T. Surić, J. R. Garcia, David Paneque, A. Sillanpää, Ll. Font, S. Schroeder, Giacomo Bonnoli, L. Maraschi, D. Guberman, D. Garrido Terrats, Ivica Puljak, Pierre Colin, I. Snidaric, V. Fallah Ramazani, Elina Lindfors, Takashi Saito, G. Maneva, J. Palacio, J. E. Ward, Masahiro Teshima, Daniel Mazin, Juan Abel Barrio, E. de Oña Wilhelmi, Ievgen Vovk, Aaron Dominguez, Stefano Ansoldi, P. G. Prada Moroni, T. Schweizer, Riccardo Paoletti, Tomislav Terzić, Marina Manganaro, Ana Babić, D. Galindo, B. Banerjee, C. Arcaro, Juri Poutanen, J. Kushida, G. Pedaletti, Thomas Bretz, Jose Luis Contreras, P. Antoranz, P. Cumani, Konstancja Satalecka, Michele Doro, Juan Cortina, Wolfgang Rhode, K. Frantzen, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Arcaro, C., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra GonzÃ¡lez, J., Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carosi, R., Carosi, A., Chatterjee, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De OnÃ£ Wilhelmi, E., DI Pierro, F., Doert, M., Domãnguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., FernÃ¡ndez Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C, Galindo, D., GarciÃ¡ LÃ³pez, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinoviä , N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, Lã³pez, M., LÃ³pez Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martãnez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Noguã©s, L., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribã³, M., Rico, J., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Sillanpaã¤, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Strzys, M., Suriä , T., Takalo, L., Tavecchio, F., Temnikov, P., Terziä , T., Tescaro, D., Teshima, M., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Wu, M. H., and Zanin, R.
Subjects: Individual: SN 2014J [Supernovae], Gamma rays: General, Supernovae: Individual: SN 2014J, Astronomy and Astrophysics, Space and Planetary Science, air, Astrophysics::High Energy Astrophysical Phenomena, Hadron, VHE [gamma ray], FOS: Physical sciences, Astrophysics, Type (model theory), power spectrum, 01 natural sciences, 0103 physical sciences, supernova, MAGIC (telescope), 010303 astronomy & astrophysics, Cherenkov radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, photon, Gamma ray, imaging, General [Gamma rays], Astronomy and Astrophysic, MAGIC, gamma rays: general, supernovae: individual (SN 2014J), flux, Supernova, Cherenkov counter, ddc:520, high [energy], Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract: In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. We probe the possibility of very-high-energy (VHE; $E\geq100$ GeV) gamma rays produced in the early stages of Type Ia supernova explosions. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of $\sim5.5$ hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed. No significant excess was detected from the direction of SN 2014J. Upper limits at 95$\%$ confidence level on the integral flux, assuming a power-law spectrum, d$F/$d$E\propto E^{-\Gamma}$, with a spectral index of $\Gamma=2.6$, for energies higher than 300 GeV and 700 GeV, are established at $1.3\times10^{-12}$ and $4.1\times10^{-13}$ photons~cm$^{-2}$s$^{-1}$, respectively. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first $\sim10$ days after the supernova explosion for energies greater than 300 GeV is limited to $10^{-6}$ of the total available energy budget ($\sim 10^{51}$ erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes., Comment: 5 pages, 2 figures. Accepted for publication in A&A
Published: 2017

16. Open high-level data formats and software for gamma-ray astronomy

Author: P. Eger, Matthew Wood, Regis Terrier, Gernot Maier, Daniela Dorner, Julien Lefaucheur, Saverio Lombardi, Kai Brügge, Jose Luis Contreras, Roland Walter, Tarek M. Hassan, Victor Zabalza, Mathieu Servillat, Bruno Khelifi, Catherine Boisson, Jeremy Perkins, Christoph Deil, A. Ziegler, Karl Kosack, Jürgen Knödlseder, Johannes King, Jaime Rosado, Lars Mohrmann, Michael Mayer, G. Pedaletti, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: Cherenkov Telescope Array, Computer science, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Context (language use), IACT, feedback, Cherenkov counter: atmosphere, 01 natural sciences, programming, Software, Gammaastronomie, Observatory, 0103 physical sciences, Astrophysik, [INFO]Computer Science [cs], ddc:530, Mailing list, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, business.industry, imaging, Gammastrahlung, observatory, Open data, Data model, gamma ray, Física nuclear, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Software engineering, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: [Print] High energy gamma-ray astronomy : 6th International Meeting on High Energy Gamma-Ray Astronomy, Heidelberg, Germany, 11 - 15 July 2016 / Aharonian, Felix A. ; Hofmann, W. ; Rieger, Frank Michael , Melville, NY : AIP Publishing, 2017, 6th International Meeting on High Energy Gamma-Ray Astronomy, Heidelberg, Germany, 11 Jul 2016 - 15 Jul 2016; AIP conference proceedings 1792(1), 070006 (2017). doi:10.1063/1.4969003, n gamma-ray astronomy, a variety of data formats and proprietary software have been traditionally used, often developed for one specific mission or experiment. Especially for ground-based imaging atmospheric Cherenkov telescopes (IACTs), data and software are mostly private to the collaborations operating the telescopes. However, there is a general movement in science towards the use of open data and software. In addition, the next-generation IACT instrument, the Cherenkov Telescope Array (CTA), will be operated as an open observatory.We have created a Github organisation at https://github.com/open-gamma-ray-astro where we are developing high-level data format specifications. A public mailing list was set up at https://lists.nasa.gov/mailman/listinfo/open-gamma-ray-astro and a first face-to-face meeting on the IACT high-level data model and formats took place in April 2016 in Meudon (France). This open multi-mission effort will help to accelerate the development of open data formats and open-source software for gamma-ray astronomy, leading to synergies in the development of analysis codes and eventually better scientific results (reproducible, multi-mission).This write-up presents this effort for the first time, explaining the motivation and context, the available resources and process we use, as well as the status and planned next steps for the data format specifications. We hope that it will stimulate feedback and future contributions from the gamma-ray astronomy community., Published by Inst., Melville, NY
Published: 2017
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17. Observations of IceCube HESE track directions with the MAGIC telescopes

Author: G. Pedaletti, Konstancja Satalecka, Dariusz Gora, Koji Noda, and Elisa Bernardini
Subjects: Physics, Particle physics, Muon, Neutral current, Astrophysics::High Energy Astrophysical Phenomena, Track (disk drive), Hadron, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, High Energy Physics::Experiment, Muon neutrino, MAGIC (telescope), Neutrino
Abstract: The MAGIC telescopes are strongly involved in several multimessenger programs. One of them are follow-up observations of astrophysical neutrino events, to search for hadronic γ-ray emission from the neutrino direction and identify potential neutrino sources. In 2013 the IceCube collaboration reported the first detection of astrophysical neutrinos and up to now 55 events, which interact inside the IceCube detector active volume, dubbed High Energy Starting Events (HESE), have been reported. These include 13 track-like events, caused usually by muon neutrino charge current interactions. The track-like events (as opposed to cascade-like neutral current interactions) are characterised by a very good angular resolution of < 1 deg, which facilitates follow-up observations and potential source identification. The MAGIC telescopes performed follow-up observations of 4 HESE track-like events from the Northern hemisphere: HESE-37, HESE-38, HET (ATel #7856) and the GCN HESE alert from 27/04/2016 (GCN #19363). No sig...
Published: 2017

18. Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes

Author: M. I. Martínez, Sabrina Einecke, G. Pedaletti, S. R. Gozzini, Thomas Bretz, L. Nogués, E. Moretti, J. Becerra González, Giacomo Bonnoli, F. Di Pierro, M. Engelkemeier, E. Prandini, Francesco Longo, I. Snidaric, Stefano Covino, B. De Lotto, Alessio Berti, S. Bonnefoy, A. Sillanpää, Arka Chatterjee, M. Vazquez Acosta, Ana Babić, Wolfgang Rhode, Alexander Hahn, Nikola Godinovic, Gareth Hughes, B. Biasuzzi, U. Barres de Almeida, D. Elsaesser, Juan Abel Barrio, R. Mirzoyan, Damir Lelas, Victoria Moreno, Tomoki Saito, D. Tescaro, Dario Hrupec, L. Perri, A. De Angelis, A. Treves, Vitaly Neustroev, Stefano Ansoldi, P. Da Vela, M. A. Lopez, Kari Nilsson, D. Dominis Prester, Riccardo Paoletti, Daniela Dorner, S. Griffiths, Dorota Sobczyńska, Dariusz Gora, J. Palacio, M. Will, D. Eisenacher Glawion, Abelardo Moralejo, Gaia Vanzo, Marcel Strzys, X. Paredes-Fortuny, Mosè Mariotti, M. Nievas Rosillo, J. M. Paredes, Antonio Stamerra, Yusuke Konno, S. Schroeder, Ivica Puljak, Pierre Colin, M. Gaug, Tomislav Terzić, L. Maraschi, V. Fallah Ramazani, J. Kushida, Martin Makariev, Elina Lindfors, Jose Luis Contreras, Oscar Blanch, Saverio Lombardi, Christian Fruck, Daniel Mazin, B. Banerjee, C. Arcaro, G. Maneva, Juan Cortina, E. de Oña Wilhelmi, S. Paiano, Kazuma Ishio, Karl Mannheim, J. Herrera, M. Doert, E. Colombo, Adrian Biland, M. H. Wu, L. A. Antonelli, J. R. Garcia, Lucas Guillemot, L. O. Takalo, Koji Noda, Aaron Dominguez, F. Borracci, Elisa Bernardini, J. Rico, Pratik Majumdar, M. V. Fonseca, T. Surić, Masahiro Teshima, Tarek M. Hassan, R. J. García López, J. E. Ward, Fabrizio Tavecchio, Ismaël Cognard, Rodolfo Carosi, Ll. Font, Wlodek Bednarek, Alessandro Carosi, D. Kuveždić, N. Torres-Albà, Max Ludwig Ahnen, I. Reichardt, P. Temnikov, P. Giammaria, Massimo Persic, U. Menzel, Diego F. Torres, M. Garczarczyk, Ievgen Vovk, M. Peresano, T. Schweizer, D. Fidalgo, Juri Poutanen, Julian Sitarek, J. Hose, K. Nishijima, Daniela Hadasch, Francesco Dazzi, A. Fernández-Barral, A. Niedzwiecki, P. G. Prada Moroni, David Paneque, M. Hayashida, D. Guberman, D. Zarić, Marina Manganaro, Marc Ribó, D. Galindo, P. Bangale, Hidetoshi Kubo, P. Cumani, Konstancja Satalecka, Michele Doro, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carosi, R., Carosi, A., Chatterjee, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Wilhelmi, E. de Oña, Pierro, F. Di, Doert, M., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Glawion, D. Eisenacher, Elsaesser, D., Engelkemeier, M., Ramazani, V. Fallah, Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Gozzini, S. R., Griffiths, S., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nilsson, K., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Sillanpää, A., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Torres, D. F., Torres Albà, N., Treves, A., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zarić, D., Collaboration), (MAGIC, Cognard, I., Guillemot, L., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Nuclear Physics Division, Bhabha Atomic Research Centre (BARC), Government of India, Department of Atomic Energy-Government of India, Department of Atomic Energy, Politecnico di Milano [Milan] (POLIMI), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Technische Universität Dortmund [Dortmund] (TU), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), IEEC-CSIC, Institut de Física d'Altes Energies, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Università degli Studi di Udine - University of Udine [Italie], Universita degli Studi di Padova, Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Trieste (OAT), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Department of Environment and Energy [Sendai], Tohoku University [Sendai], Optoelectronic Research Centre, University of Southampton, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)
Subjects: non-thermal, pulsars: general, binaries: close, pulsars: individual: B1957+20, gamma-rays: general [radiation mechanisms], Radiation mechanisms: non-thermal, VHE [gamma ray], Astrophysics, spin, 01 natural sciences, 7. Clean energy, star, emission [pulsar], Millisecond pulsar, Pulsars: general, radiation mechanisms: non-thermal, gamma rays: general, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, High Energy Astrophysical Phenomena (astro-ph.HE), acceleration [electron], Physics, radio wave, Superluminal motion, efficiency [acceleration], non-thermal, binaries: close, pulsars: general, pulsars: individual: B1957+20, gamma-rays: general [radiation mechanisms], inverse [Compton scattering], frequency, compact [binary], symbols, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, upper limit, Active galactic nucleus, Pulsars: individual: B1957+20, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Lorentz covariance, GLAST, Binary pulsar, symbols.namesake, Pulsar, Binaries: close, 0103 physical sciences, interaction [pulsar], plasma, radiation mechanisms: non-thermal, binaries: close, pulsars: general, pulsars: individual: B1957+20, gamma-rays: general, Astrophysics::Galaxy Astrophysics, Gamma-rays: general, Planck energy, ta115, 010308 nuclear & particles physics, Crab Pulsar, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], binary [pulsar], Astronomy and Astrophysics, injection [electron], MAGIC, 13. Climate action, Space and Planetary Science, ddc:520, mass
Abstract: B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies., Monthly Notices of the Royal Astronomical Society, 470 (4), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
Published: 2017

19. MAGIC observations of the microquasar V404 Cygni during the 2015 outburst

Author: M. I. Martínez, Sabrina Einecke, Daniela Dorner, Dariusz Gora, A. Sillanpää, R. J. García López, Kazuma Ishio, Gaia Vanzo, A. Loh, Francesco Dazzi, A. Fernández-Barral, A. Niedzwiecki, U. Barres de Almeida, F. Di Pierro, A. De Angelis, Massimo Persic, Damir Lelas, M. Gaug, A. Treves, Vitaly Neustroev, L. Maraschi, Elina Lindfors, B. De Lotto, D. Hadasch, Stefano Ansoldi, David Paneque, Riccardo Paoletti, Dorota Sobczyńska, Daniel Mazin, J. Becerra González, Marcel Strzys, D. Guberman, J. Herrera, M. Vazquez Acosta, Pratik Majumdar, J. Palacio, Marina Manganaro, M. V. Fonseca, Rodolfo Carosi, Jerome Rodriguez, D. Galindo, J. M. Paredes, Christian Fruck, Antonio Stamerra, Giacomo Bonnoli, Koji Noda, B. Biasuzzi, Elisa Bernardini, Stefano Covino, E. Prandini, E. Colombo, Victoria Moreno, P. Cumani, Konstancja Satalecka, Michele Doro, G. Maneva, Tomoki Saito, D. Tescaro, U. Menzel, D. Kuveždić, Alessio Berti, Mosè Mariotti, Adrian Biland, D. Ninci, P. G. Prada Moroni, P. Da Vela, J. Rico, M. Hayashida, S. Schroeder, Ivica Puljak, D. Elsaesser, Diego F. Torres, Juan Abel Barrio, Pierre Colin, Nikola Godinovic, M. Peresano, D. Zarić, M. Garczarczyk, Dario Hrupec, M. Doert, P. Temnikov, Marc Ribó, P. Bangale, M. A. Lopez, Hidetoshi Kubo, Saverio Lombardi, Tomislav Terzić, S. Bonnefoy, Abelardo Moralejo, L. Nogués, M. Engelkemeier, E. Moretti, L. Perri, R. Mirzoyan, Arka Chatterjee, E. de Oña Wilhelmi, S. Griffiths, Ievgen Vovk, D. Fidalgo, J. R. Garcia, Alexander Hahn, Masahiro Teshima, Aaron Dominguez, T. Schweizer, Kyoshi Nishijima, Yusuke Konno, Gareth Hughes, Francesco Longo, D. Eisenacher Glawion, D. Dominis Prester, M. Minev, X. Paredes-Fortuny, Camilla Maggio, M. Nievas Rosillo, I. Reichardt, J. E. Ward, Julian Sitarek, V. Fallah Ramazani, J. Hose, Martin Makariev, Oscar Blanch, Wlodek Bednarek, Alessandro Carosi, S. Paiano, Karl Mannheim, N. Torres-Albà, G. Pedaletti, Wolfgang Rhode, T. Surić, B. Banerjee, C. Arcaro, L. A. Antonelli, Tarek M. Hassan, Fabrizio Tavecchio, Ll. Font, Ana Babić, Max Ludwig Ahnen, J. Kushida, Jose Luis Contreras, P. Giammaria, Juan Cortina, I. Snidaric, L. Takalo, Kari Nilsson, M. Will, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, The German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia \Severo Ochoa' SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia \Mara de Maeztu'MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 2016/22/M/ST9/00382., Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., de Oña Wilhelmi, E., Di Pierro, F., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Griffiths, S., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Minev, M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Sillanpää, A., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Torres, D. F., Torres Albà, N., Treves, A., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Collaboration), (The MAGIC, Loh, A., and Rodriguez, J.
Subjects: Flux, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, general [, gamma-rays], law, Astrophysics::Solar and Stellar Astrophysics, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), radio wave, Gamma-rays: general, Stars: individual: V404 Cygni (V404 Cyg), X-rays: binaries, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, burst, Flare, Radio wave, exceptional, Opacity, gamma-rays: general, stars: individual: V404 Cygni (V404 Cyg), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Compact star, GLAST, VHE, X-ray, 0103 physical sciences, upper limit [flux], quasar, ta115, 010308 nuclear & particles physics, Astronomy, opacity, Astronomy and Astrophysics, Quasar, acceleration, MAGIC, Crab Nebula, 13. Climate action, Space and Planetary Science, gamma ray, [SDU]Sciences of the Universe [physics], ddc:520, binaries [X-rays], individual: V404 Cygni (V404 Cyg) [stars]
Abstract: The microquasar V404 Cygni underwent a series of outbursts in 2015, June 15-31, during which its flux in hard X-rays (20-40 keV) reached about 40 times the Crab Nebula flux. Because of the exceptional interest of the flaring activity from this source, observations at several wavelengths were conducted. The MAGIC telescopes, triggered by the INTEGRAL alerts, followed-up the flaring source for several nights during the period June 18-27, for more than 10 hours. One hour of observation was conducted simultaneously to a giant 22 GHz radio flare and a hint of signal at GeV energies seen by Fermi-LAT. The MAGIC observations did not show significant emission in any of the analysed time intervals. The derived flux upper limit, in the energy range 200--1250 GeV, is 4.8$\times 10^{-12}$ ph cm$^{-2}$ s$^{-1}$. We estimate the gamma-ray opacity during the flaring period, which along with our non-detection, points to an inefficient acceleration in the V404\,Cyg jets if VHE emitter is located further than $1\times 10^{10}$ cm from the compact object., Comment: 7 pages, accepted by MNRAS
Published: 2017

20. OUP accepted manuscript

Author: Kazuma Ishio, Rodolfo Carosi, L. Nogués, E. Moretti, Max Ludwig Ahnen, Giacomo Bonnoli, Adrian Biland, M. Peresano, S. Bonnefoy, R. Mirzoyan, Masahiro Teshima, Marcel Strzys, J. Rico, Abelardo Moralejo, E. Prandini, M. Hayashida, Aaron Dominguez, Valentí Bosch-Ramon, S. Paiano, M. Engelkemeier, Karl Mannheim, Wrijupan Bhattacharyya, Dario Hrupec, M. A. Lopez, A. Niedzwiecki, Ana Babić, P. Giammaria, Stefano Covino, Juan Abel Barrio, D. Zarić, J. Kushida, Jose Luis Contreras, R. Zanin, J. Becerra González, Kyoshi Nishijima, Juan Cortina, R. J. García López, J. E. Ward, David Paneque, Camilla Maggio, U. Barres de Almeida, Wlodek Bednarek, Alessandro Carosi, M. Minev, Nikola Godinovic, I. Reichardt, Tomoki Saito, D. Tescaro, Marc Ribó, Damir Lelas, Josep M. Paredes, Alessio Berti, D. Kuveždić, N. Torres-Albà, Arka Chatterjee, D. Guberman, U. Menzel, L. A. Antonelli, S. A. Trushkin, P. Bangale, L. Perri, Kari Nilsson, L. Maraschi, Massimo Persic, Elina Lindfors, Diego F. Torres, Hidetoshi Kubo, Daniela Dorner, A. De Angelis, Dariusz Gora, M. Vazquez Acosta, D. Fidalgo, M. Will, Dorota Sobczyńska, Gaia Vanzo, D. Eisenacher Glawion, X. Paredes-Fortuny, Daniel Mazin, M. Nievas Rosillo, B. Biasuzzi, A. Treves, Vitaly Neustroev, M. Garczarczyk, G. Pedaletti, Victoria Moreno, M. Gaug, Francesco Dazzi, A. Fernández-Barral, Chiara Righi, M. I. Martínez, T. Surić, Yusuke Konno, J. Herrera, B. De Lotto, Koji Noda, Elisa Bernardini, Pratik Majumdar, P. Temnikov, M. V. Fonseca, S. Schroeder, Ivica Puljak, Guy G. Pooley, Pierre Colin, Sabrina Einecke, Christian Fruck, Marina Manganaro, Tarek M. Hassan, G. Maneva, D. Ninci, Wolfgang Rhode, D. Galindo, E. de Oña Wilhelmi, Fabrizio Tavecchio, Ievgen Vovk, Ll. Font, P. Cumani, T. Schweizer, Konstancja Satalecka, Michele Doro, D. Elsaesser, B. Banerjee, I. Snidaric, C. Arcaro, Stefano Ansoldi, P. G. Prada Moroni, Riccardo Paoletti, Tomislav Terzić, J. Palacio, Antonio Stamerra, Julian Sitarek, J. Hose, F. Di Pierro, D. Dominis Prester, P. Da Vela, V. Fallah Ramazani, Alexander Hahn, Mosè Mariotti, Francesco Longo, Saverio Lombardi, E. Colombo, Martin Makariev, L. O. Takalo, Oscar Blanch, D. Hadasch, M. Doert, and J. R. Garcia
Subjects: Physics, Photon, 010308 nuclear & particles physics, Gamma ray, Flux, Astronomy, Astronomy and Astrophysics, Quasar, Context (language use), Astrophysics, 01 natural sciences, Black hole, 13. Climate action, Space and Planetary Science, 0103 physical sciences, MAGIC (telescope), 010303 astronomy & astrophysics, Radio wave
Abstract: The microquasar Cygnus X-1 displays the two typical soft and hard X-ray states of a black hole transient. During the latter, Cygnus X-1 shows a one-sided relativistic radio-jet. Recent detection of the system in the high energy (HE; E greater than or similar to 60 MeV) gamma-ray range with FermiLAT associates this emission with the outflow. Former MAGIC observations revealed a hint of flaring activity in the very high-energy (VHE; E greater than or similar to 100 GeV) regime during this X-ray state. We analyse ~ to 97 h of Cygnus X-1 data taken with the MAGIC telescopes between July 2007 and October 2014. To shed light on the correlation between hard X-ray and VHE gamma rays as previously suggested, we study each main X-ray state separately. We perform an orbital phase-folded analysis to look for variability in the VHE band. Additionally, to place this variability behaviour in a multiwavelength context, we compare our results with Fermi-LAT, AGILE, Swift-BAT, MAXI, RXTE-ASM, AMI and RATAN-600 data. We do not detect Cygnus X-1 in the VHE regime. We establish upper limits for each X-ray state, assuming a power-law distribution with photon index Γ = 3.2. For steady emission in the hard and soft X-ray states, we set integral upper limits at 95 %per cent confidence level for energies above 200 GeV at 2.6 x 10⁻¹² photons cm⁻² s⁻¹ and 1.0 x 10⁻¹¹ photons cm⁻² s ⁻¹, respectively. We rule out steady VHE gamma-ray emission above this energy range, at the level of theMAGIC sensitivity, originating in the interaction between the relativistic jet and the surrounding medium, while the emission above this flux level produced inside the binary still remains a valid possibility.
Published: 2017

21. The first VHE detection of the blazar S4 0954+65 with the MAGIC telescopes during an exceptionally high optical state

Author: G. A. Borman, Talvikki Hovatta, M. Doert, Anne Lähteenmäki, J. Becerra González, Marina Manganaro, Merja Tornikoski, Valeri M. Larionov, J. Finke, Alan P. Marscher, Elina Lindfors, G. Pedaletti, I. S. Troitsky, V. Fallah Ramazani, M. Nievas Rosillo, S. G. Jorstad, Yasuyuki T. Tanaka, and R. Ojha
Subjects: Physics, ta115, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Flux, Astronomy, Astrophysics, Redshift, law.invention, Crab Nebula, law, MAGIC (telescope), Blazar, Flare, Fermi Gamma-ray Space Telescope
Abstract: The blazar S4 0954+65 (at a disputed redshift of z=0.368 or z≥0.45) underwent an exceptionally high state in the optical band during January and February 2015, as revealed by the Tuorla and St. Petersburg University blazar monitoring programs: a brightening of more than 3 magnitudes in the R-band from the average monitored states. Simultaneous data from the Fermi satellite at high energy gamma rays (HE, 100 MeV 100 GeV) emission from S4 0954+65 (ATel #7080). The VHE flux above 150 GeV is estimated to be about 6% of the Crab nebula flux above the same threshold.In this contribution we present a comprehensive multiwavelength picture of this object, including data from mm/optical/X-ray/HE and VHE gamma-ray bands. The high emission state during the flare allows us to compile the simultaneous broadband spectral energy distribu...
Published: 2017

22. Performance of the MAGIC telescopes under moonlight

Author: L. Maraschi, Elina Lindfors, Daniel Mazin, S. Schroeder, Ivica Puljak, U. Menzel, Alexander Hahn, Gareth Hughes, Pierre Colin, M. Doert, M. Vazquez Acosta, E. de Oña Wilhelmi, D. Dominis Prester, Diego F. Torres, J. Palacio, B. Biasuzzi, J. M. Paredes, M. Garczarczyk, Victoria Moreno, V. Fallah Ramazani, S. Paiano, Antonio Stamerra, Stefano Covino, L. Nogués, Karl Mannheim, D. Ninci, A. Niedzwiecki, Kazuma Ishio, A. De Angelis, U. Barres de Almeida, A. Treves, Vitaly Neustroev, R. J. García López, E. Moretti, Damir Lelas, Abelardo Moralejo, Christian Fruck, Dario Hrupec, David Paneque, Dorota Sobczyńska, Francesco Longo, J. Becerra González, Ievgen Vovk, Mosè Mariotti, M. A. Lopez, G. Maneva, Adrian Biland, B. Banerjee, C. Arcaro, G. Pedaletti, T. Surić, J. R. Garcia, E. Prandini, Max Ludwig Ahnen, Louis Antonelli, D. Guberman, Marina Manganaro, Alessio Berti, Aaron Dominguez, M. I. Martínez, Ana Babić, Tomoki Saito, D. Tescaro, J. Kushida, T. Schweizer, P. Temnikov, D. Galindo, J. Rico, Massimo Persic, Arka Chatterjee, M. Minev, I. Reichardt, P. Cumani, Jose Luis Contreras, Konstancja Satalecka, Sabrina Einecke, Michele Doro, Juan Cortina, P. Giammaria, D. Kuveždić, Martin Makariev, J. E. Ward, D. Fidalgo, Giacomo Bonnoli, Julian Sitarek, Rodolfo Carosi, M. Hayashida, Saverio Lombardi, Oscar Blanch, Kyoshi Nishijima, B. De Lotto, L. Perri, J. Hose, Wolfgang Rhode, I. Snidaric, Wrijupan Bhattacharyya, Andrea Rugliancich, Yusuke Konno, D. Zarić, D. Eisenacher Glawion, Marc Ribó, Nikola Godinovic, X. Paredes-Fortuny, D. Elsaesser, Marcel Strzys, M. Nievas Rosillo, P. Bangale, D. Hadasch, Daniela Dorner, F. Di Pierro, Hidetoshi Kubo, Stefano Ansoldi, Riccardo Paoletti, Kari Nilsson, Dariusz Gora, Gaia Vanzo, M. Will, Wlodek Bednarek, Alessandro Carosi, N. Torres-Albà, M. Gaug, P. Da Vela, A. Sillanpää, E. Colombo, J. Herrera, L. O. Takalo, Koji Noda, S. Bonnefoy, Elisa Bernardini, M. Engelkemeier, Tarek M. Hassan, Camilla Maggio, R. Mirzoyan, S. Griffiths, Masahiro Teshima, Fabrizio Tavecchio, Ll. Font, Tomislav Terzić, Juan Abel Barrio, Francesco Dazzi, A. Fernández-Barral, Pratik Majumdar, M. V. Fonseca, M. Peresano, P. G. Prada Moroni, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babiä , A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra GonzÃ¡lez, J., Bednarek, W., Bernardini, E., Berti, Alessio, Bhattacharyya, W., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colin, P, Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., de OÃ±a Wilhelmi, E., Di Pierro, F., Doert, M., Domãnguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., FernÃ¡ndez Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., GarcÃa LÃ³pez, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinoviä , N., Gora, D., Griffiths, S., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveå¾diä , D., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, Lã³pez, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martãnez, M., Mazin, D., Menzel, U., Minev, M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Noguã©s, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribã³, M., Rico, J., Rugliancich, A., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Sillanpã¤ã¤, A., Sitarek, J., Å nidariä , I., Sobczynska, D., Stamerra, A., Strzys, M., Suriä , T., Takalo, L., Tavecchio, F., Temnikov, P., Terziä , T., Tescaro, D., Teshima, M., Torres, D. F., Torres AlbÃ , N., Treves, A., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., and Zariä , D.
Subjects: Moonlight, Photomultiplier, Twilight, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Cherenkov telescopes, 01 natural sciences, Gamma-ray astronomy, Crab Nebula, Optics, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Cherenkov radiation, media_common, Physics, ta115, 010308 nuclear & particles physics, business.industry, Crab nebula, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Cherenkov telescope, Sky, Duty cycle, ddc:540, Electrónica, Física nuclear, Electricidad, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: MAGIC, a system of two imaging atmospheric Cherenkov telescopes, achieves its best performance under dark conditions, i.e. in absence of moonlight or twilight. Since operating the telescopes only during dark time would severely limit the duty cycle, observations are also performed when the Moon is present in the sky. Here we develop a dedicated Moon-adapted analysis to characterize the performance of MAGIC under moonlight. We evaluate energy threshold, angular resolution and sensitivity of MAGIC under different background light levels, based on Crab Nebula observations and tuned Monte Carlo simulations. This study includes observations taken under non-standard hardware configurations, such as reducing the camera photomultiplier tubes gain by a factor ~1.7 (Reduced HV settings) with respect to standard settings (Nominal HV) or using UV-pass filters to strongly reduce the amount of moonlight reaching the cameras of the telescopes. The Crab Nebula spectrum is correctly reconstructed in all the studied illumination levels, that reach up to 30 times brighter than under dark conditions. The main effect of moonlight is an increase in the analysis energy threshold and in the systematic uncertainties on the flux normalization. The sensitivity degradation is constrained to be below 10%, within 15-30% and between 60 and 80% for Nominal HV, Reduced HV and UV-pass filter observations, respectively. No worsening of the angular resolution was found. Thanks to observations during moonlight, the maximal duty cycle of MAGIC can be increased from ~18%, under dark nights only, to up to ~40% in total with only moderate performance degradation., 14 pages, 13 figures, accepted in Astroparticle Physics. Corresponding authors: Daniel Guberman (dguberman@ifae.es) and Pierre Colin (colin@mppmu.mpg.de)
Published: 2017

23. A cut-off in the TeV gamma-ray spectrum of the SNR Cassiopeia A

Author: G. Pedaletti, E. Prandini, Stefano Ansoldi, Riccardo Paoletti, Wolfgang Rhode, A. De Angelis, A. Treves, Vitaly Neustroev, T. Surić, M. I. Martínez, Juan Abel Barrio, M. Engelkemeier, B. De Lotto, S. Bonnefoy, Sabrina Einecke, L. Maraschi, Kazuma Ishio, Elina Lindfors, G. Maneva, J. Kushida, Razmik Mirzoyan, U. Barres de Almeida, Damir Lelas, Rodolfo Carosi, Daniel Mazin, A. Berti, Wlodek Bednarek, Alessandro Carosi, Jose Luis Contreras, Adrian Biland, Chiara Righi, Dorota Sobczyńska, M. Colak, N. Torres-Albà, J. Palacio, M. Hayashida, J. Rico, Camilla Maggio, J. M. Paredes, Antonio Stamerra, B. Banerjee, Daniela Dorner, C. Arcaro, Dariusz Gora, Juan Cortina, Gaia Vanzo, D. Zarić, Arka Chatterjee, S. Schroeder, Marc Ribó, Stefano Covino, Ivica Puljak, Pierre Colin, M. Gaug, Pratik Majumdar, L. Nogués, D. Fidalgo, P. Bangale, M. V. Fonseca, Abelardo Moralejo, E. Moretti, Hidetoshi Kubo, Tomohiro Inada, L. A. Antonelli, J. Herrera, S. N. Shore, E. de Oña Wilhelmi, Martin Will, Petar Temnikov, Koji Noda, Tomoki Saito, D. Tescaro, Marcel Strzys, Elisa Bernardini, Masahiro Teshima, Yusuke Konno, P. G. Prada Moroni, Kyoshi Nishijima, Nikola Godinovic, D. Ninci, D. Kuveždić, Tomislav Terzić, Ievgen Vovk, M. Minev, Tarek M. Hassan, T. Schweizer, I. Reichardt, Fabrizio Tavecchio, A. Niedzwiecki, Ll. Font, I. Snidaric, U. Menzel, M. Peresano, David Paneque, Max Ludwig Ahnen, P. Giammaria, D. Guberman, Marina Manganaro, Ana Babić, D. Galindo, M. Garczarczyk, P. Cumani, Konstancja Satalecka, Michele Doro, Francesco Dazzi, Dario Hrupec, A. Fernández-Barral, M. A. Lopez, R. J. García López, Kari Nilsson, Massimo Persic, F. Di Pierro, D. Dominis Prester, V. Fallah Ramazani, P. Da Vela, Alexander Hahn, Julian Sitarek, J. Hose, M. Vazquez Acosta, B. Biasuzzi, Victoria Moreno, E. Colombo, L. O. Takalo, Aaron Dominguez, D. Hadasch, Francesco Longo, J. E. Ward, Mosè Mariotti, Saverio Lombardi, Martin Makariev, Oscar Blanch, M. Doert, J. R. Garcia, J. Becerra González, Christian Fruck, L. Perri, Giacomo Bonnoli, Wrijupan Bhattacharyya, D. Eisenacher Glawion, D. Elsaesser, M. Nievas Rosillo, S. Paiano, Karl Mannheim, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Berti, A., Bhattacharyya, W., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colak, M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., de Oña Wilhelmi, E., Di Pierro, F., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Inada, T., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Minev, M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Shore, S. N., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Torres-Albà, N., Treves, A., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., and Zarić, D.
Subjects: lepton, Astrophysics, power spectrum, 01 natural sciences, Spectral line, Astrophysics::Solar and Stellar Astrophysics, MAGIC (telescope), 010303 astronomy & astrophysics, acceleration of particle, cosmic ray, energy spectrum [gamma ray], acceleration of particles, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, education.field_of_study, Gamma ray, cosmic rays, gamma rays: general, high [energy], Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::High Energy Astrophysical Phenomena, low [magnetic field], Population, energy spectrum, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, leptonic [model], emission [gamma ray], supernova, 0103 physical sciences, education, Astrophysics::Galaxy Astrophysics, Computer Science::Information Theory, ta115, 010308 nuclear & particles physics, Astronomy, cosmic ray physics, stars: supernovae: individual: Cassiopeia A, supernova remnants, Astronomy and Astrophysics, acceleration, MAGIC, moment, flux, Cassiopeia A, Space and Planetary Science, ddc:520, galaxy [cosmic radiation], spectral, High Energy Physics::Experiment, supernova remnant [ISM], general [gamma rays]
Abstract: It is widely believed that the bulk of the Galactic cosmic rays are accelerated in supernova remnants (SNRs). However, no observational evidence of the presence of particles of PeV energies in SNRs has yet been found. The young historical SNR Cassiopeia A (Cas A) appears as one of the best candidates to study acceleration processes. Between December 2014 and October 2016 we observed Cas A with the MAGIC telescopes, accumulating 158 hours of good-quality data. We derived the spectrum of the source from 100 GeV to 10 TeV. We also analysed $\sim$8 years of $Fermi$-LAT to obtain the spectral shape between 60 MeV and 500 GeV. The spectra measured by the LAT and MAGIC telescopes are compatible within the errors and show a clear turn off (4.6 $\sigma$) at the highest energies, which can be described with an exponential cut-off at $E_c = 3.5\left(^{+1.6}_{-1.0}\right)_{\textit{stat}} \left(^{+0.8}_{-0.9}\right)_{\textit{sys}}$ TeV. The gamma-ray emission from 60 MeV to 10 TeV can be attributed to a population of high-energy protons with spectral index $\sim$2.2 and energy cut-off at $\sim$10 TeV. This result indicates that Cas A is not contributing to the high energy ($\sim$PeV) cosmic-ray sea in a significant manner at the present moment. A one-zone leptonic model fails to reproduce by itself the multi-wavelength spectral energy distribution. Besides, if a non-negligible fraction of the flux seen by MAGIC is produced by leptons, the radiation should be emitted in a region with a low magnetic field (B$\lessapprox$100$\mu$G) like in the reverse shock.), Comment: 8 pages, 3 figures, submitted to MNRAS. Corresponding authors: Daniel Guberman (dguberman@ifae.es), Emma de O\~na Wilhelmi (wilhelmi@ice.csic.es) and Daniel Galindo (dgalindo@am.ub.es)
Published: 2017

24. Erratum: A cut-off in the TeV gamma-ray spectrum of the SNR Cassiopeia A

Author: MAGIC Collaboration: M L Ahnen, S Ansoldi, L A Antonelli, C Arcaro, A Babić, B Banerjee, P Bangale, U Barres de Almeida, J A Barrio, J Becerra González, W Bednarek, E Bernardini, A Berti, W Bhattacharyya, B Biasuzzi, A Biland, O Blanch, S Bonnefoy, G Bonnoli, R Carosi, A Carosi, A Chatterjee, M Colak, P Colin, E Colombo, J L Contreras, J Cortina, S Covino, P Cumani, P Da Vela, F Dazzi, A De Angelis, B De Lotto, E de Oña Wilhelmi, F Di Pierro, M Doert, A Domínguez, D Dominis Prester, D Dorner, M Doro, S Einecke, D Eisenacher Glawion, D Elsaesser, M Engelkemeier, V Fallah Ramazani, A Fernández-Barral, D Fidalgo, M V Fonseca, L Font, C Fruck, D Galindo, R J García López, M Garczarczyk, M Gaug, P Giammaria, N Godinović, D Gora, D Guberman, D Hadasch, A Hahn, T Hassan, M Hayashida, J Herrera, J Hose, D Hrupec, T Inada, K Ishio, Y Konno, H Kubo, J Kushida, D Kuveždić, D Lelas, E Lindfors, S Lombardi, F Longo, M López, C Maggio, P Majumdar, M Makariev, G Maneva, M Manganaro, K Mannheim, L Maraschi, M Mariotti, M Martínez, D Mazin, U Menzel, M Minev, R Mirzoyan, A Moralejo, V Moreno, E Moretti, V Neustroev, A Niedzwiecki, M Nievas Rosillo, K Nilsson, D Ninci, K Nishijima, K Noda, L Nogués, S Paiano, J Palacio, D Paneque, R Paoletti, J M Paredes, G Pedaletti, M Peresano, L Perri, M Persic, P G Prada Moroni, E Prandini, I Puljak, J R Garcia, I Reichardt, W Rhode, M Ribó, J Rico, C Righi, T Saito, K Satalecka, S Schroeder, T Schweizer, S N Shore, J Sitarek, I Šnidarić, D Sobczynska, A Stamerra, M Strzys, T Surić, L Takalo, F Tavecchio, P Temnikov, T Terzić, D Tescaro, M Teshima, D F Torres, N Torres-Albà, A Treves, G Vanzo, M Vazquez Acosta, I Vovk, J E Ward, M Will, and D Zarić
Subjects: Physics, Cassiopeia A, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Gamma ray, ddc:520, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Spectrum (topology)
Published: 2018

25. MWL Picture Of The Blazar S5 0716+714 During Its Brightest Outburst

Author: B. Lott, A. Y. Lien, M. Doert, Marina Manganaro, Thomas P. Krichbaum, Ioannis Myserlis, Merja Tornikoski, D. Gasparrini, G. A. Borman, Mark Gurwell, D. J. Thompson, Anne Lähteenmäki, Svetlana G. Jorstad, Fallah Ramazani, Paul Kuin, D. Bastieri, Emmanouil Angelakis, J. A. Zensus, Mireia Nievas, Larionov, Elina Lindfors, Talvikki Hovatta, Ryosuke Itoh, Alexander Kraus, Bindu Rani, and G. Pedaletti
Subjects: Physics, Astronomy, Astrophysics, Blazar, 7. Clean energy, astronomy_astrophysics, BL Lac object
Abstract: S5 0716+714 is a well known BL-Lac object, one of the brightest and most active blazars. The discovery in the Very High Energy band (VHE, E > 100 GeV) by MAGIC happened in 2008. In January 2015 the source went through the brightest optical state ever observed, triggering MAGIC follow-up and a VHE detection with ~ sigma significance (ATel #6999). Rich multi-wavelength coverage of the flare allowed us to construct the broad-band spectral energy distribution of S5 0716+714 during its brightest outburst. In this work we will present the preliminary analysis of MAGIC and Fermi-LAT data of the flaring activity in January and February 2015 for the HE and VHE band, together with radio (Metsahovi, OVRO, VLBA, Effelsberg), sub-millimeter (SMA), optical (Tuorla, Perkins, Steward, AZT-8+ST7, LX-200, Kanata), X-ray and UV (Swift-XRT and UVOT), in the same time-window and discuss the time variability of the MWL light curves during this impressive outburst.
Published: 2016

26. Investigating the peculiar emission from the new VHE gamma-ray source H1722+119

Author: M. Hayashida, M. Makariev, B. Biasuzzi, K. Mallot, R. J. García López, Louis Antonelli, D. Dominis Prester, E. Prandini, M. Doert, M. H. Wu, Massimo Persic, F. D'Ammando, Marc Ribó, G. Bonnoli, Abelardo Moralejo, Juri Poutanen, R. Reinthal, V. Fallah Ramazani, P. Bangale, Y. Hanabata, Razmik Mirzoyan, U. Barres de Almeida, Damir Lelas, T. Steinbring, Marina Manganaro, P. G. Prada Moroni, Stefano Covino, Hidetoshi Kubo, P. Antoranz, D. Galindo, J. Becerra González, G. Pedaletti, Dorota Sobczyńska, D. Nakajima, Thomas Bretz, J. Hose, Andrei Berdyugin, Pratik Majumdar, M. V. Fonseca, S. Bonnefoy, A. Sillanpää, Arka Chatterjee, Francesco Longo, D. Elsaesser, F. Di Pierro, K. Kodani, Alexander Hahn, Konstancja Satalecka, Walter Max-Moerbeck, Tomoki Saito, D. Tescaro, Ivica Puljak, Pierre Colin, H. Takami, L. Nogués, U. Menzel, Michele Doro, M. I. Martínez, Gareth Hughes, Talvikki Hovatta, C. Schultz, E. Moretti, Marcel Strzys, D. Fidalgo, Vassil Verguilov, Aaron Dominguez, Diego F. Torres, Julia Thaele, E. de Oña Wilhelmi, Reiko Orito, F. Verrecchia, Sabrina Einecke, Junko Kushida, P. Da Vela, R. López-Coto, J. Rodriguez Garcia, J. E. Ward, M. Palatiello, Elina Lindfors, A. Niedzwiecki, Kyoshi Nishijima, Ievgen Vovk, Wolfgang Rhode, Daniel Mazin, Oscar Blanch, Julian Sitarek, Juan Abel Barrio, L. Maraschi, Francesco Dazzi, David Paneque, A. Fernández-Barral, Markus Garczarczyk, Yusuke Konno, C. Fruck, B. De Lotto, M. Villata, T. Schweizer, T. Toyama, D. Guberman, Tomislav Terzić, K. Frantzen, J. L. Richards, Mosè Mariotti, A.-K. Overkemping, S. Paiano, Saverio Lombardi, Karl Mannheim, D. Hadasch, L. Perri, A. La Barbera, D. Eisenacher Glawion, X. Paredes-Fortuny, P. Temnikov, M. Nievas Rosillo, W. Idec, A. González Muñoz, E. Colombo, B. Banerjee, S. Buson, L. O. Takalo, Masahiro Teshima, Daniela Dorner, R. Zanin, Dariusz Gora, Adrian Biland, M. Gaug, J. Rico, J. Herrera, Koji Noda, Elisa Bernardini, A. De Angelis, A. Treves, Vitaly Neustroev, Jose Luis Contreras, Juan Cortina, G. Maneva, C. M. Raiteri, Nikola Godinovic, Benito Marcote, Max Ludwig Ahnen, Kari Nilsson, P. Giammaria, M. Will, Dario Hrupec, M. A. Lopez, R. Clavero, D. Garrido Terrats, W. Bednarek, Fabrizio Tavecchio, Ll. Font, I. Snidaric, Ana Babić, Stefano Ansoldi, Riccardo Paoletti, J. Palacio, J. M. Paredes, Antonio Stamerra, Alessandro Carosi, Jose Miguel Miranda, F. Borracci, Anthony C. S. Readhead, Universitat de Barcelona, Aalto-yliopisto, Aalto University, Ahnen ML, Ansoldi S, Antonelli LA, Antoranz P, Babic A, Banerjee B, Bangale P, de Almeida UB, Barrio JA, Gonzalez JB, Bednarek W, Bernardini E, Biasuzzi B, Biland A, Blanch O, Bonnefoy S, Bonnoli G, Borracci F, Bretz T, Buson S, Carosi A, Chatterjee A, Clavero R, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi F, De Angelis A, De Lotto B, Wilhelmi ED, Di Pierro F, Doert M, Dominguez A, Prester DD, Dorner D, Doro M, Einecke S, Glawion DE, Elsaesser D, Ramazani VF, Fernandez-Barral A, Fidalgo D, Fonseca MV, Font L, Frantzen K, Fruck C, Galindo D, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Giammaria P, Godinovic N, Munoz AG, Gora D, Guberman D, Hadasch D, Hahn A, Hanabata Y, Hayashida M, Herrera J, Hose J, Hrupec D, Hughes G, Idec W, Kodani K, Konno Y, Kubo H, Kushida J, La Barbera A, Lelas D, Lindfors E, Lombardi S, Longo F, Lopez M, Lopez-Coto R, Majumdar P, Makariev M, Mallot K, Maneva G, Manganaro M, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Miranda JM, Mirzoyan R, Moralejo A, Moretti E, Nakajima D, Neustroev V, Niedzwiecki A, Rosillo MN, Nilsson K, Nishijima K, Noda K, Nogues L, Orito R, Overkemping A, Paiano S, Palacio J, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Pedaletti G, Perri L, Persic M, Poutanen J, Moroni PGP, Prandini E, Puljak I, Rhode W, Ribo M, Rico J, Garcia JR, Saito T, Satalecka K, Schultz C, Schweizer T, Sillanpaa A, Sitarek J, Snidaric I, Sobczynska D, Stamerra A, Steinbring T, Strzys M, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Thaele J, Torres DF, Toyama T, Treves A, Verguilov V, Vovk I, Ward JE, Will M, Wu MH, Zanin R, DAmmando F, Berdyugin A, Hovatta T, Max-Moerbeck W, Raiteri CM, Readhead ACS, Reinthal R, Richards JL, Verrecchia F, Villata M, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Oña Wilhelmi, E., Di Pierro, F., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Fallah Ramazani, V., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinović, N., González Muñoz, A., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Nogués, L., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Schultz, C., Schweizer, T., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T, Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., D'Ammando, F., Berdyugin, A., Hovatta, T., Max Moerbeck, W., Raiteri, C. M., Readhead, A. C. S., Reinthal, R., Richards, J. L., Verrecchia, F., and Villata, M.
Subjects: galaxie [Gamma-rays], gamma-rays: galaxies, UPGRADE, Astrophysics, DETECTED BLAZARS, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, Raigs gamma, law, galaxies: active, BL Lacertae objects: individual: H1722+119, galaxies, distances and redshifts, BL LACERTAE OBJECTS, ALL-SKY SURVEY, MAGIC, TELESCOPES, LAC OBJECTS, SOURCE CATALOG, MAJOR, HELICAL JETS, CRAB-NEBULA, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), distances and redshift [Galaxies], active BL Lacertae objects, individual, H1722+119 galaxies, distances and redshifts gamma-rays, Galaxies: active, Galaxies: distances and redshifts, Gamma-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, galaxies [Gamma-rays], Extragalactic background light, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Owens Valley Radio Observatory, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, galaxies: active, BL Lacertae objects: individual: H1722+119, galaxies: distances and redshifts, gamma-rays: galaxies, 0103 physical sciences, individual: H1722+119 [BL Lacertae objects], distances and redshifts [Galaxies], ta115, 010308 nuclear & particles physics, Gamma rays, Astronomy, Astronomy and Astrophysic, Redshift, Crab Nebula, 13. Climate action, Galàxies actives, Active galaxies, ddc:520
Abstract: The MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes observed the BL Lac object H1722+119 (redshift unknown) for six consecutive nights between 2013 May 17 and 22, for a total of 12.5 h. The observations were triggered by high activity in the optical band measured by the KVA (Kungliga Vetenskapsakademien) telescope. The source was for the first time detected in the very high energy (VHE, $E > 100$ GeV) $\gamma$-ray band with a statistical significance of 5.9 $\sigma$. The integral flux above 150 GeV is estimated to be $(2.0\pm 0.5)$ per cent of the Crab Nebula flux. We used contemporaneous high energy (HE, 100 MeV $ < E < 100$ GeV) $\gamma$-ray observations from Fermi-LAT (Large Area Telescope) to estimate the redshift of the source. Within the framework of the current extragalactic background light models, we estimate the redshift to be $z = 0.34 \pm 0.15$. Additionally, we used contemporaneous X-ray to radio data collected by the instruments on board the Swift satellite, the KVA, and the OVRO (Owens Valley Radio Observatory) telescope to study multifrequency characteristics of the source. We found no significant temporal variability of the flux in the HE and VHE bands. The flux in the optical and radio wavebands, on the other hand, did vary with different patterns. The spectral energy distribution (SED) of H1722+119 shows surprising behaviour in the $\sim 3\times10^{14} - 10^{18}$ Hz frequency range. It can be modelled using an inhomogeneous helical jet synchrotron self-Compton model., Comment: 12 pages, 5 figures, 2 tables
Published: 2016

27. Observations of Sagittarius A* during the pericenter passage of the G2 object with MAGIC

Author: D. Paneque, D. Garrido Terrats, T. Schweizer, L. Nogués, M. Engelkemeier, M. Makariev, Masahiro Teshima, J. Becerra González, Alessandro Carosi, X. Paredes-Fortuny, F. Di Pierro, A. González Muñoz, A.-K. Overkemping, M. Hayashida, Ruben Lopez-Coto, Elina Lindfors, Laura Maraschi, S. Ansoldi, B. Biasuzzi, Ana Babić, D. Nakajima, J. Rico, M. V. Fonseca, Daniel Mazin, A. Berti, P. Da Vela, Juan Abel Barrio, Jose Miguel Miranda, Arka Chatterjee, Iva Šnidarić, Kyoshi Nishijima, Abelardo Moralejo, A. Treves, Vitaly Neustroev, P. Majumdar, Jose Carlos Herrera, R. J. García López, Benito Marcote, S. Schroeder, T. Steinbring, C. Arcaro, Dariusz Gora, E. Moretti, Pierre Colin, F. Borracci, M. Ribó, Kari Nilsson, K. Frantzen, A. De Angelis, Yusuke Konno, M. Will, Christian Fruck, Stefano Covino, Julian Sitarek, D. Lelas, U. Menzel, I. Puljak, A. Niedzwiecki, Riccardo Paoletti, Julia Thaele, Elisa Prandini, J. Kushida, Dario Hrupec, D. Hadasch, Markus Gaug, D. Galindo, Aaron Dominguez, I. Reichardt, Petar Temnikov, G. Vanzo, R. Zanin, Razmik Mirzoyan, Jose Luis Contreras, Simona Paiano, J. Palacio, M. A. Lopez, Elisa Bernardini, G. Pedaletti, Juan Cortina, A. Biland, Antonio Stamerra, K. Noda, D. Fidalgo, M. Mariotti, J. E. Ward, Juri Poutanen, Dorota Sobczyńska, D. Guberman, Tihomir Surić, Giacomo Bonnoli, J. M. Paredes, S. Bonnefoy, P. Antoranz, G. Maneva, Marina Manganaro, E. de Ona Wilhelmi, M. I. Martínez, W. Idec, P. Bangale, M. Strzys, P. G. Prada Moroni, Diego F. Torres, Konstancja Satalecka, Sabrina Einecke, Michele Doro, A. Sillanpää, K. Kodani, Francesco Longo, V. Fallah Ramazani, Karl Mannheim, Takashi Saito, Max Ludwig Ahnen, Oscar Blanch, M. H. Wu, U. Barres de Almeida, L. Perri, A. La Barbera, Takeshi Toyama, D. Eisenacher Glawion, K. Mallot, M. Nievas Rosillo, J. R. Garcia, Massimo Persic, Leo O. Takalo, Ievgen Vovk, A. Hahn, Hidetoshi Kubo, B. De Lotto, M. Doert, W. Bednarek, V. Verguilov, J. Hose, S. Buson, D. Elsaesser, Markus Garczarczyk, B. Banerjee, Thomas Bretz, S. N. Shore, D. Dominis Prester, S. Lombardi, M. Peresano, Gareth Hughes, Tomislav Terzić, D. Tescaro, N. Godinović, D. Dorner, L. A. Antonelli, R. Clavero, Fabrizio Tavecchio, Eduardo Colombo, Ll. Font, P. Giammaria, M. Palatiello, Francesco Dazzi, A. Fernández-Barral, W. Rhode, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Arcaro, C., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra GonzÃ¡lez, J., Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De OÃ±a Wilhelmi, E., Di Pierro, F., Doert, M., Domãnguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., FernÃ¡ndez Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C, Galindo, D., GarcÃa LÃ³pez, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinoviä , N., GonzÃ¡lez MuÃ±oz, A., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, Lã³pez, M., LÃ³pez Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martãnez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Noguã©s, L., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribã³, M., Rico, J., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Shore, S. N., Sillanpã¤ã¤, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Suriä , T., Takalo, L., Tavecchio, F., Temnikov, P., Terziä , T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., and Zanin, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, black hole physics, general [Gamma rays], Galaxy: center, gamma rays: general, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Black hole physic, 0103 physical sciences, MAGIC (telescope), Black hole physics, Gamma rays: general, Astronomy and Astrophysics, Space and Planetary Science, Supernova remnant, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Galactic Center, center [Galaxy], Astronomy and Astrophysic, Galaxy, Black hole, Sagittarius A, ddc:520, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Astronomy and astrophysics 601, A33 (2017). doi:10.1051/0004-6361/201629355, Context. We present the results of a multi-year monitoring campaign of the Galactic center (GC) with the MAGIC telescopes. These observations were primarily motivated by reports that a putative gas cloud (G2) would be passing in close proximity to the super-massive black hole (SMBH), associated with Sagittarius A*, located at the center of our galaxy. This event was expected to give astronomers a unique chance to study the effect of in-falling matter on the broad-band emission of a SMBH.Aims. We search for potential flaring emission of very-high-energy (VHE; ≥100 GeV) gamma rays from the direction of the SMBH at the GC due to the passage of the G2 object. Using these data we also study the morphology of this complex region.Methods. We observed the GC region with the MAGIC Imaging Atmospheric Cherenkov Telescopes during the period 2012–2015, collecting 67 h of good-quality data. In addition to a search for variability in the flux and spectral shape of the GC gamma-ray source, we use a point-source subtraction technique to remove the known gamma-ray emitters located around the GC in order to reveal the TeV morphology of the extended emission inside that region.Results. No effect of the G2 object on the VHE gamma-ray emission from the GC was detected during the 4 yr observation campaign. We confirm previous measurements of the VHE spectrum of Sagittarius A*, and do not detect any significant variability of the emission from the source. Furthermore, the known VHE gamma-ray emitter at the location of the supernova remnant G0.9+0.1 was detected, as well as the recently discovered VHE source close to the GG radio arc.Key words: Galaxy: center / gamma rays: general / black hole physics, Published by EDP Sciences, Les Ulis
Published: 2016

28. Multiband variability studies and novel broadband SED modeling of Mrk 501 in 2009

Author: K. Nishijima, J. L. Richards, Stefano Covino, G. Piner, D. Dominis Prester, U. Menzel, A. Flinders, D. Tescaro, Louis Antonelli, D. Galindo, Aaron Dominguez, S. Schröder, Elena G. Larionova, Kari Nilsson, Paul S. Smith, A. McCann, T. S. Grishina, Wen Ping Chen, M. Will, Pratik Majumdar, J. E. Ward, Daniela Dorner, Dariusz Gora, P. Moriarty, C. Rulten, Soebur Razzaque, D. Garrido Terrats, K. Frantzen, Joseph Moody, Wystan Benbow, G. Hughes, K. Ragan, Ralph Bird, L. Perri, M. Gaug, T. Sakamoto, Valeri M. Larionov, Elina Lindfors, G. H. Sembroski, Daniel Mazin, Ievgen Vovk, A. Hahn, M. Hütten, N. H. Park, Alexander B. Pushkarev, G. Maccaferri, Thomas Bretz, P. Wilcox, P. Kar, D. Nakajima, R. Zanin, J. Herrera, Wei Cui, Amanda Weinstein, J. Palacio, P. G. Prada Moroni, Frank Krennrich, Matthew L. Lister, A. Berti, A. Cesarini, M. Kertzman, A. La Barbera, Walter Max-Moerbeck, E. Colombo, M. Villata, M. P. Connolly, Adrian Biland, D. S. Hanna, Ana Babić, D. Eisenacher Glawion, Juan Abel Barrio, John L. Quinn, M. Capalbi, Koji Noda, Arka Chatterjee, Elisa Bernardini, A. Sillanpää, Adrian Rovero, Antonio Stamerra, J. V. Tucci, M. Nievas Rosillo, M. Palatiello, L. V. Larionova, S. N. Shore, R. Mukherjee, M. J. Lang, Daniel Nieto, M. I. Martínez, S. Bonnefoy, J. Kushida, P. Giammaria, P. Bangale, Wolfgang Rhode, Gernot Maier, G. Pedaletti, L. O. Takalo, Margo F. Aller, Jose Luis Contreras, Andrei Berdyugin, J. A. Zensus, E. Roache, V. Verguilov, D. Fidalgo, C. Pace, Thomas P. Krichbaum, Francesco Dazzi, Juan Cortina, M. Engelkemeier, G. H. Gillanders, A. Carraminyana, S. P. Wakely, Mosè Mariotti, J. Rico, A. Fernández-Barral, R. Clavero, J. Becerra González, A.-K. Overkemping, S. O. Kurtanidze, Sabrina Einecke, Abraham D. Falcone, A. González Muñoz, Evgenia N. Kopatskaya, Lars Fuhrmann, Nikola Godinovic, Benito Marcote, Karlen Shahinyan, Takashi Saito, W. Bednarek, C. Schultz, Marcos Santander, Fabrizio Tavecchio, J. Rodriguez Garcia, E. Pueschel, Ll. Font, A. C. Sadun, A. Popkow, J. Grube, V. Bugaev, Anthony C. S. Readhead, R. Ligustri, A. Archer, I. Snidaric, Yusuke Konno, P. Calcidese, M. Strzys, A. Pichel, Saverio Lombardi, B. De Lotto, Markus Garczarczyk, N. Kelley-Hoskins, J. Tyler, Ann E. Wehrle, B. Banerjee, S. Buson, D. Hadasch, N. Otte, Maria G. Nikolashvili, Gordon T. Richards, L. Nogués, B. Biasuzzi, Juri Poutanen, U. Barres de Almeida, J. P. Finley, K. Mallot, S. Paiano, Marcello Giroletti, I. Nestoras, A. De Angelis, A. Treves, Vitaly Neustroev, X. Paredes-Fortuny, T. B. Humensky, R. A. Ong, Karl Mannheim, J. H. Buckley, Yu. A. Kovalev, R. J. García López, H. Fleischhack, G. N. Kimeridze, I. Sadeh, David A. Williams, Y. Mori, M. V. Fonseca, W. Idec, Matthias Kadler, Yuri Y. Kovalev, Stefano Ansoldi, Riccardo Paoletti, K. Kodani, J. P. Norris, O. M. Kurtanidze, N. V. Efimova, Y. Hanabata, Arkady A. Arkharov, Anne Lähteenmäki, Abelardo Moralejo, G. Maneva, Masahiro Teshima, A. C. Zook, Dario Hrupec, P. Antoranz, B. Zitzer, Hugh Dickinson, R. A. Chigladze, M. Peresano, Ekaterina Koptelova, S. Archambault, M. A. Lopez, T. Steinbring, P. Temnikov, P. Leto, Massimo Persic, J. M. Paredes, Hugh D. Aller, F. Borracci, S. O'Brien, T. Surić, I. Telezhinsky, I. Reichardt, Jamie Holder, G. Vanzo, R. Pearson, Julia Thaele, G. Bonnoli, Mark Gurwell, Eduardo Ros, Andrea Orlati, S. Griffin, L. A. Sigua, Diego F. Torres, Alessandro Carosi, Ruben Lopez-Coto, Maria Krause, Y. Yatsu, A. Wilhelm, Jose Miguel Miranda, Anushka Udara Abeysekara, T. Schweizer, P. Cassaro, Razmik Mirzoyan, E. Moretti, Damir Lelas, Francesco Longo, V. Fallah Ramazani, P. Kaaret, Dorota Sobczyńska, L. Maraschi, Kirill Sokolovsky, Tomislav Terzić, Lucy Fortson, E. de Ona Wilhelmi, Julian Sitarek, C. Fruck, T. Toyama, Ivica Puljak, Max Ludwig Ahnen, David Kieda, F. Di Pierro, Pierre Colin, M. Buchovecky, Oscar Blanch, P. Da Vela, A. Niedzwiecki, Emmanouil Angelakis, M. Doert, M. H. Wu, Ivan S. Troitsky, C. Pagani, David Paneque, Q. Feng, Vladimir A. Hagen-Thorn, E. De la Fuente, E. Prandini, C. M. Raiteri, L. Carrasco, D. Guberman, Jeremy S. Perkins, Martin Pohl, Marina Manganaro, H. A. Krimm, Merja Tornikoski, Konstancja Satalecka, Michele Doro, Dmitry A. Blinov, M. Perri, J. Hose, D. Elsaesser, Daria A. Morozova, P. T. Reynolds, M. Hayashida, Marc Ribó, Hidetoshi Kubo, M. Makariev, Swiss Federal Institute of Technology Zurich, University of Udine, INAF National Institute for Astrophysics, University of Siena, University of Rijeka, Saha Institute of Nuclear Physics, Max Planck Institute for Physics, Complutense University, University of La Laguna, University of Łódź, German Electron Synchrotron, Autonomous University of Barcelona, University of Würzburg, University of Padova, Institute of Space Studies of Catalonia, Dortmund University, Finnish MAGIC Consortium, University of Barcelona, The University of Tokyo, Bulgarian Academy of Sciences, Osservatorio Astronomicodi Roma, University of Pisa, ICREA, University of Maryland, College Park, McGill University, Washington University St. Louis, Harvard University, University College Dublin, University of California Los Angeles, National University of Ireland, Galway, Purdue University, Iowa State University, Pennsylvania State University, University of Utah, University of Minnesota Twin Cities, Adler Planetarium and Astronomy Museum, University of Delaware, Columbia University, University of Iowa, DePauw University, Georgia Institute of Technology, University of Chicago, NASA Goddard Space Flight Center, Universidad de Buenos Aires, Cork Institute of Technology, University of California Santa Cruz, Argonne National Laboratory, University of Johannesburg, University of Michigan, Ann Arbor, St. Petersburg State University, RAS - Pulkovo Astronomical Observatory, Circolo Astrofili Talmassons, Osservatorio Astrofisico della Regione Autonoma Valle d'Aosta, Georgian National Academy of Sciences, National Central University, Aoyama Gakuin University, University of Colorado Denver, Brigham Young University, Tokyo Institute of Technology, Instituto Nacional de Astrofisica Optica y Electronica, Universidad de Guadalajara, University of Denver, University of Arizona, Space Science Institute, Pomona College, University of Leicester, ASI Science Data Center, University of Trento, RAS - P.N. Lebedev Physics Institute, Max Planck Institute for Radio Astronomy, Whittier College, Metsähovi Radio Observatory, INAF Istituto di Radioastronomia, Osservatorio Astrofisico di Catania, California Institute of Technology, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra GonzÃ¡lez, J., Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De OÃ±a Wilhelmi, E., Di Pierro, F., Doert, M., Domãnguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., FernÃ¡ndez Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., GarcÃa LÃ³pez, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinoviä , N., GonzÃ¡lez MuÃ±oz, A., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, Lã³pez, M., LÃ³pez Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martãnez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Noguã©s, L., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reichardt, I., Rhode, W., Ribã³, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Schrã¶der, S., Schultz, C., Schweizer, T., Shore, S. N., Sillanpã¤ã¤, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Suriä , T., Takalo, L., Tavecchio, F., Temnikov, P., Terziä , T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Abeysekara, A. U., Archambault, S., Archer, A., Benbow, W., Bird, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Connolly, M. P., Cui, W., Dickinson, H. J., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Flinders, A., Fortson, L., Gillanders, G. H., Griffin, S., Grube, J., Hã¼tten, M., Hanna, D., Holder, J., Humensky, T. B., Kaaret, P., Kar, P., Kelley Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Maier, G., Mccann, A., Moriarty, P., Mukherjee, R., Nieto, D., O'Brien, S., Ong, R. A., Otte, N., Park, N., Perkins, J., Pichel, A., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Rulten, C., Sadeh, I., Santander, M., Sembroski, G. H., Shahinyan, K., Telezhinsky, I., Tucci, J. V., Tyler, J., Wakely, S. P., Weinstein, A., Wilcox, P., Wilhelm, A., Williams, D. A., Zitzer, B., Razzaque, S., Villata, M., Raiteri, C. M., Aller, H. D., Aller, M. F., Larionov, V. M., Arkharov, A. A., Blinov, D. A., Efimova, N. V., Grishina, T. S., Hagen Thorn, V. A., Kopatskaya, E. N., Larionova, L. V., Larionova, E. G., Morozova, D. A., Troitsky, I. S., Ligustri, R., Calcidese, P., Berdyugin, A., Kurtanidze, O. M., Nikolashvili, M. G., Kimeridze, G. N., Sigua, L. A., Kurtanidze, S. O., Chigladze, R. A., Chen, W. P., Koptelova, E., Sakamoto, T., Sadun, A. C., Moody, J. W., Pace, C., Pearson, R., Yatsu, Y., Mori, Y., Carraminyana, A., Carrasco, L., De La Fuente, E., Norris, J. P., Smith, P. S., Wehrle, A., Gurwell, M. A., Zook, A., Pagani, C., Perri, M., Capalbi, M., Cesarini, A., Krimm, H. A., Kovalev, Y. Y., Kovalev, Y. u. A., Ros, E., Pushkarev, A. B., Lister, M. L., Sokolovsky, K. V., Kadler, M., Piner, G., Lã¤hteenmã¤ki, A., Tornikoski, M., Angelakis, E., Krichbaum, T. P., Nestoras, I., Fuhrmann, L., Zensus, J. A., Cassaro, P., Orlati, A., Maccaferri, G., Leto, P., Giroletti, M., Richards, J. L., Max Moerbeck, W., and Readhead, A. C. S.
Subjects: extragalactic background light, multiwavelength observations, Astrophysics::High Energy Astrophysical Phenomena, bl-lacertae objects, Galaxies: BL Lacertae objects: individual: Markarian 501, Methods: data analysis, observational, Polarization, spectral energy-distribution, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, individual: Markarian 501 [BL Lacertae objects], law, Coincident, 0103 physical sciences, ddc:530, MAGIC (telescope), crab-nebula, Blazar, data analysis [Methods], 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), tev blazars, 010308 nuclear & particles physics, stochastic acceleration, telescope observations, Institut für Physik und Astronomie, Astronomy and Astrophysics, Astronomy and Astrophysic, gamma-ray emission, methods: data analysis, BL Lacertae objects: individual: Markarian 501, Synchrotron, data analysi [Methods], Space and Planetary Science, x-ray, ddc:520, Electrónica, Física nuclear, Electricidad, Degeneracy (mathematics), Astrophysics - High Energy Astrophysical Phenomena, Flare, BL Lac object
Abstract: Astronomy and astrophysics 603, A31 (2017). doi:10.1051/0004-6361/201629540, We present an extensive study of the BL Lac object Mrk 501 based on a data set collected during the multi-instrument campaign spanning from 2009 March 15 to 2009 August 1, which includes, among other instruments, MAGIC, VERITAS, Whipple 10 m, and Fermi-LAT to cover the γ-ray range from 0.1 GeV to 20 TeV; RXTE and Swift to cover wavelengths from UV tohard X-rays; and GASP-WEBT, which provides coverage of radio and optical wavelengths. Optical polarization measurements were provided for a fraction of the campaign by the Steward and St. Petersburg observatories. We evaluate the variability of the source and interband correlations, the γ-ray flaring activity occurring in May 2009, and interpret the results within two synchrotron self-Compton (SSC) scenarios. Aims. The multiband variability observed during the full campaign is addressed in terms of the fractional variability, and the possible correlations are studied by calculating the discrete correlation function for each pair of energy bands where the significance was evaluated with dedicated Monte Carlo simulations. The space of SSC model parameters is probed following a dedicated grid-scan strategy, allowing for a wide range of models to be tested and offering a study of the degeneracy of model-to-data agreement in the individual model parameters, hence providing a less biased interpretation than the “single-curve SSC model adjustment” typically reported in the literature. Methods. We find an increase in the fractional variability with energy, while no significant interband correlations of flux changes are found on the basis of the acquired data set. The SSC model grid-scan shows that the flaring activity around May 22 cannot be modeled adequately with a one-zone SSC scenario (using an electron energy distribution with two breaks), while it can be suitably described within a two (independent) zone SSC scenario. Here, one zone is responsible for the quiescent emission from the averaged 4.5-month observing period, while the other one, which is spatially separated from the first, dominates the flaring emission occurring at X-rays and very-high-energy (>100 GeV, VHE) γ rays. The flaring activity from May 1, which coincides with a rotation of the electric vector polarization angle (EVPA), cannot be satisfactorily reproduced by either a one-zone or a two-independent-zone SSC model, yet this is partially affected by the lack of strictly simultaneous observations and the presence of large flux changes on sub-hour timescales (detected at VHE γ rays). Results. The higher variability in the VHE emission and lack of correlation with the X-ray emission indicate that, at least during the 4.5-month observing campaign in 2009, the highest energy (and most variable) electrons that are responsible for the VHE γ rays do not make a dominant contribution to the ~1 keV emission. Alternatively, there could be a very variable component contributing to the VHE γ-ray emission in addition to that coming from the SSC scenario. The studies with our dedicated SSC grid-scan show that there is some degeneracy in both the one-zone and the two-zone SSC scenarios probed, with several combinations of model parameters yielding a similar model-to-data agreement, and some parameters better constrained than others. The observed γ-ray flaring activity, with the EVPA rotation coincident with the first γ-ray flare, resembles those reported previously for low frequency peaked blazars, hence suggesting that there are many similarities in the flaring mechanisms of blazars with different jet properties., Published by EDP Sciences, Les Ulis
Published: 2016
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29. Super-orbital variability of LS I +61 ° 303 at TeV energies

Author: E. Colombo, K. Mallot, R. J. García López, M. H. Wu, D. Nakajima, L. O. Takalo, H. Takami, Arka Chatterjee, Christian Fruck, Sabrina Einecke, Vassil Verguilov, D. Fidalgo, Ivica Puljak, Pierre Colin, J. Rodriguez Garcia, Daniela Dorner, Dariusz Gora, Massimo Persic, E. de Oña Wilhelmi, Masahiro Teshima, Alexander Hahn, J. Palacio, M. Palatiello, J. M. Paredes, Antonio Stamerra, Francesco Longo, Gareth Hughes, M. Gaug, I. Snidaric, Yusuke Konno, J. Herrera, Stefano Ansoldi, Pratik Majumdar, M. V. Fonseca, A. La Barbera, Lluis Font, Riccardo Paoletti, Julian Sitarek, K. Kodani, Koji Noda, J. Hose, Elisa Bernardini, Francesco Dazzi, Marcel Strzys, D. Dominis Prester, D. Eisenacher Glawion, X. Paredes-Fortuny, M. Nievas Rosillo, A. Herrero, E. Moretti, Nikola Godinovic, Stefano Covino, P. Temnikov, Martin Makariev, Benito Marcote, Oscar Blanch, T. Toyama, G. Pedaletti, Dominik Elsaesser, S. Bonnefoy, Jose Luis Contreras, U. Barres de Almeida, Damir Lelas, Juan Cortina, D. Garrido Terrats, U. Menzel, Diego F. Torres, M. Garczarczyk, F. Di Pierro, Juan Abel Barrio, J. E. Ward, Giacomo Bonnoli, P. G. Prada Moroni, K. Frantzen, S. Paiano, R. López-Coto, A. Niedzwiecki, David Paneque, D. Guberman, Marina Manganaro, M. Hayashida, Thomas Bretz, S. N. Shore, R. Mirzoyan, Tomoki Saito, D. Tescaro, Jorge Casares, Mosè Mariotti, A.-K. Overkemping, A. González Muñoz, Kyoshi Nishijima, Dorota Sobczyńska, E. Prandini, Tomislav Terzić, Marc Ribó, B. De Lotto, C. Schultz, Aaron Dominguez, Karl Mannheim, Alicia López-Oramas, D. Galindo, Saverio Lombardi, P. Bangale, Hidetoshi Kubo, S. Buson, Junko Kushida, P. Da Vela, J. Becerra González, Wolfgang Rhode, D. Hadasch, Max Ludwig Ahnen, C. Delgado Mendez, Reiko Orito, Ana Babić, Konstancja Satalecka, Alba Fernández-Barral, F. Borracci, L. Maraschi, Michele Doro, Elina Lindfors, Dario Hrupec, B. Biasuzzi, Daniel Mazin, M. A. Lopez, Kari Nilsson, A. Sillanpää, M. Will, W. Idec, Abelardo Moralejo, P. Giammaria, T. Steinbring, Wlodek Bednarek, Alessandro Carosi, L. A. Antonelli, B. Banerjee, R. Clavero, Miriam Lucio Martinez, Fabrizio Tavecchio, Jose Miguel Miranda, A. De Angelis, A. Treves, Vitaly Neustroev, Ievgen Vovk, G. Maneva, R. Zanin, Adrian Biland, T. Schweizer, J. Rico, Julia Thaele, Juri Poutanen, Y. Hanabata, P. Antoranz, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinović, N., González Muñoz, A., Gora, D., Guberman, D., Hadasch, D, Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Casares, J., Herrero, A., and Universitat de Barcelona
Subjects: Astrofísica, astroparticle physics, binaries: general, gamma rays: general, stars: individual: LS I +61°303, X-rays: binaries, X-rays: individuals: LS I +61°303, Be star, Astrophysics::High Energy Astrophysical Phenomena, Gamma rays: general, general [Gamma rays], Binary number, FOS: Physical sciences, Astrophysics, 01 natural sciences, Astroparticle physic, Radio spectrum, law.invention, individual: LS I +61°303 [Stars], Telescope, Raigs gamma, law, 0103 physical sciences, Modulation (music), individuals: LS I +61°303 [X-rays], Astroparticle physics, Binaries: general, Stars: individual: LS I +61°303, Astronomy and Astrophysics, Space and Planetary Science, MAGIC (telescope), Spectroscopy, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), general [Binaries], 010308 nuclear & particles physics, binarie [X-rays], Gamma rays, Astronomy and Astrophysic, Orbital period, ddc:520, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Astronomy and astrophysics 591, A76(2016). doi:10.1051/0004-6361/201527964, The gamma-ray binary LS I +61°303 is a well-established source from centimeter radio up to very high energy (VHE;E > 100 GeV).The broadband emission shows a periodicity of $\sim$ 26.5 days, coincident with the orbital period. A longer (super-orbital) period of 1667 $\pm$ 8 dayswas proposed from radio variability and confirmed using optical and high-energy (HE; E > 100 MeV) gamma-ray observations. In this paper, wereport on a four-year campaign performed by MAGIC together with archival data concentrating on a search for a long-timescale signature in the VHE emission from LS I +61°303 Aims.We focus on the search for super-orbital modulation of the VHE emission, similar to that observed at other energies, and on the search forcorrelations between TeV emission and an optical determination of the extension of the circumstellar disk.Methods. A four-year campaign has been carried out using the MAGIC telescopes. The source was observed during the orbital phases when theperiodic VHE outbursts have occurred ($\phi$ = 0:55–0.75, one orbit=26.496 days). Additionally, we included archival MAGIC observations anddata published by the VERITAS collaboration in these studies. For the correlation studies, LS I +61°303 has also been observed during the orbitalphases where sporadic VHE emission had been detected in the past ($\phi$ = 0:75–1.0). These MAGIC observations were simultaneous with opticalspectroscopy from the LIVERPOOL telescope.Results.The TeV flux of the periodical outburst in orbital phases $\phi$ = 0:5–0.75 was found to show yearly variability consistent with the long-term modulation of$\sim$ 4.5 years found in the radio band. This modulation of the TeV flux can be well described by a sine function with a best-fit period of 1610 $\pm$ 58 days. The complete data, including archival observations, span two super-orbital periods. There is no evidence for a correlation betweenthe TeV emission and the mass-loss rate of the Be star, but this may be a ected by the strong, short-timescale (as short as intra-day) variation displayed by the Hfluxes., Published by EDP Sciences, Les Ulis
Published: 2016

30. Long-term multi-wavelength variability and correlation study of Markarian 421 from 2007 to 2009

Author: E. Moretti, Alessandro Carosi, D. Nakajima, Kyoshi Nishijima, Arka Chatterjee, C. M. Raiteri, Nikola Godinovic, Benito Marcote, D. Fidalgo, Jose Miguel Miranda, D. Dominis Prester, Yusuke Konno, B. Jordan, Aaron Dominguez, L. Perri, Elena G. Larionova, Marina Manganaro, Kari Nilsson, Pratik Majumdar, M. V. Fonseca, Wen Ping Chen, M. Will, A. La Barbera, D. Galindo, R. Zanin, Merja Tornikoski, Mosè Mariotti, Dario Hrupec, K. Kodani, S. N. Shore, Louis Antonelli, D. Eisenacher Glawion, Max Ludwig Ahnen, X. Paredes-Fortuny, M. Nievas Rosillo, J. E. Ward, A. González Muñoz, Adrian Biland, A.-K. Overkemping, Razmik Mirzoyan, U. Barres de Almeida, J. Palacio, Dmitry A. Blinov, G. Pedaletti, M. A. Lopez, Juri Poutanen, Konstancja Satalecka, Sofia O. Kurtanidze, Michele Doro, U. Menzel, J. M. Paredes, S. Bonnefoy, Givi N. Kimeridze, Thomas Bretz, E. N. Kopatskaya, M. H. Wu, Antonio Stamerra, K. Frantzen, J. Rico, M. Villata, P. Giammaria, Damir Lelas, Alexander Hahn, Y. Hanabata, E. Forné, F. Di Pierro, Jose Luis Contreras, H. C. Lin, R. López-Coto, I. Snidaric, Daniela Dorner, Dariusz Gora, A. Niedzwiecki, F. Borracci, Gareth Hughes, P. Antoranz, Juan Abel Barrio, Juan Cortina, Saverio Lombardi, L. V. Larionova, Ivan S. Troitsky, David Paneque, Dorota Sobczyńska, P. Temnikov, S. Paiano, Karl Mannheim, B. Biasuzzi, M. Gaug, J. Herrera, Talvikki Hovatta, Junko Kushida, Diego F. Torres, Wolfgang Rhode, D. Guberman, Koji Noda, Elisa Bernardini, M. G. Nikolashvili, P. Da Vela, Francesco Longo, J. Hose, D. Garrido Terrats, J. Becerra González, E. Prandini, A. De Angelis, A. Treves, D. Elsaesser, Vitaly Neustroev, D. Hadasch, Julia Thaele, P. G. Prada Moroni, R. Clavero, Markus Garczarczyk, Valeri M. Larionov, R. Ligustri, H. Takami, W. Bednarek, Julian Sitarek, Fabrizio Tavecchio, J. A. Ros, Abelardo Moralejo, M. Palatiello, Stefano Ansoldi, A. C. Sadun, C. Schultz, Vassil Verguilov, G. Maneva, B. Banerjee, S. Buson, Riccardo Paoletti, T. Steinbring, C. Fruck, Lorand A. Sigua, W. Idec, Ivica Puljak, Francesco Dazzi, A. Fernández-Barral, Pierre Colin, Oscar Blanch, T. S. Grishina, Ana Babić, E. de Oña Wilhelmi, E. Colombo, T. Toyama, O. M. Kurtanidze, G. Bonnoli, Elina Lindfors, Anne Lähteenmäki, M. Hayashida, D. A. Morozova, L. O. Takalo, Masahiro Teshima, Ekaterina Koptelova, A. Sillanpää, B. De Lotto, Ievgen Vovk, L. Maraschi, Tomislav Terzić, T. Schweizer, Reiko Orito, Daniel Mazin, Marc Ribó, P. Bangale, Hidetoshi Kubo, Stefano Covino, Tomoki Saito, D. Tescaro, M. Makariev, B. McBreen, M. I. Martínez, Sabrina Einecke, J. Rodriguez Garcia, K. Mallot, R. J. García López, Massimo Persic, Lluis Font, Marcel Strzys, N. V. Efimova, L. Nogués, Universitat de Barcelona, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Oña Wilhelmi, E., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinović, N., González Muñoz, A., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Nogués, L., Orito, R., Overkemping, A, Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Blinov, D. A., Chen, W. P., Efimova, N. V., Forné, E., Grishina, T. S., Hovatta, T., Jordan, B., Kimeridze, G. N., Kopatskaya, E. N., Koptelova, E., Kurtanidze, O. M., Kurtanidze, S. O., Lähteenmäki, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Ligustri, R., Lin, H. C., Mcbreen, B., Morozova, D. A., Nikolashvili, M. G., Raiteri, C. M., Ros, J. A., Sadun, A. C., Sigua, L. A., Tornikoski, M., Troitsky, I. S., Villata, M., Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University
Subjects: Astrofísica, Astroparticle physics, BL Lacertae objects: individual: Markarian 421, Radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Astroparticle physic, individual: Markarian 421 [BL Lacertae objects], 01 natural sciences, Radiació, law.invention, Telescope, law, 0103 physical sciences, MAGIC (telescope), Blazar, 010303 astronomy & astrophysics, Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, non-thermal [Radiation mechanisms], Radiation, 010308 nuclear & particles physics, Compton scattering, Astronomy and Astrophysic, Light curve, Astrophysics - Astrophysics of Galaxies, astroparticle physics / BL Lacertae objects: individual: Markarian 421 / radiation mechanisms: non-thermal, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We study the multi-band variability and correlations of the TeV blazar Mrk 421 on year time scales, which can bring additional insight on the processes responsible for its broadband emission. We observed Mrk 421 in the very high energy (VHE) gamma-ray range with the Cherenkov telescope MAGIC-I from March 2007 to June 2009 for a total of 96 hours of effective time after quality cuts. The VHE flux variability is quantified with several methods, including the Bayesian Block algorithm, which is applied to data from Cherenkov telescopes for the first time. The 2.3 year long MAGIC light curve is complemented with data from the Swift/BAT and RXTE/ASM satellites and the KVA, GASP-WEBT, OVRO, and Mets\"ahovi telescopes from February 2007 to July 2009, allowing for an excellent characterisation of the multi-band variability and correlations over year time scales. Mrk 421 was found in different gamma-ray emission states during the 2.3 year long observation period. Flares and different levels of variability in the gamma-ray light curve could be identified with the Bayesian Block algorithm. The same behaviour of a quiet and active emission was found in the X-ray light curves measured by Swift/BAT and the RXTE/ASM, with a direct correlation in time. The behaviour of the optical light curve of GASP-WEBT and the radio light curves by OVRO and Mets\"ahovi are different as they show no coincident features with the higher energetic light curves and a less variable emission. The fractional variability is overall increasing with energy. The comparable variability in the X-ray and VHE bands and their direct correlation during both high- and low-activity periods spanning many months show that the electron populations radiating the X-ray and gamma-ray photons are either the same, as expected in the Synchrotron-Self-Compton mechanism, or at least strongly correlated, as expected in electromagnetic cascades., Comment: Corresponding authors: Ann-Kristin Overkemping (ann-kristin.overkemping@tu-dortmund.de), Marina Manganaro (manganaro@iac.es), Diego Tescaro (diego.tescaro@gmail.com), To be published in Astronomy&Astrophysics (A&A), 12 pages, 9 figures
Published: 2016

31. The high-energy gamma-ray detection of G73.9+0.9, a supernova remnant interacting with a molecular cloud

Author: Denys Malyshev, G. Pedaletti, M. López-Caniego, Joanna Mikolajewska, Andrzej A. Zdziarski, Rupal Basak, Maria Chernyakova, Ruizhi Yang, Emma de Ona Wilhelmi, and Ministerio de Economía y Competitividad (España)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Electron, 01 natural sciences, symbols.namesake, 0103 physical sciences, Planck, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Molecular cloud, X-ray, Bremsstrahlung, Astronomy, Astronomy and Astrophysics, Magnetic field, Supernova, Space and Planetary Science, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We have analysed the Fermi Large Area Telescope (LAT) data on the SNR G73.9+0.9. We have confirmed a previous detection of high-energy γ-rays from this source at a high significance of ≃12σ. The observed spectrum shows a significant curvature, peaking in EFE at ∼1 GeV. We have also calculated the flux upper limits in the mm-wavelength and X-ray ranges from Planck and XMM–Newton, respectively. We have inspected the intensity of the CO (1→0) emission line and found a large peak at a velocity range corresponding to the previously estimated source distance of ∼4 kpc, which may indicate an association between a molecular cloud and the supernova remnant (SNR). The γ-ray emission appears due to interaction of accelerated particles within the SNR with the matter of the cloud. The most likely radiative process responsible for the γ-ray emission is decay of neutral pions produced in ion–ion collisions. While a dominant leptonic origin of this emission can be ruled out, the relativistic electron population related to the observed radio flux will necessarily lead to a certain level of bremsstrahlung γ-ray emission. Based on this broad-band modelling, we have developed a method to estimate the magnetic field, yielding B ≳ 80 μG at our best estimate of the molecular cloud density (or less at a lower density). G73.9+0.9 appears similar, though somewhat weaker, to other SNRs interacting with a local dense medium detected by the LAT., This research has been supported in part by the grants AYA2012-39303, SGR2009-811 and iLINK2011-0303. AAZ, JM and RB have been supported in part by the Polish NCN grants 2012/04/M/ST9/00780 and 2013/10/M/ST9/00729.
Published: 2016

32. Molecular environment, reverberation, and radiation from the pulsar wind nebula in CTA 1

Author: Diego F. Torres, J. M. Martin, and G. Pedaletti
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Reverberation, Field (physics), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radiation, 01 natural sciences, Pulsar wind nebula, Shock (mechanics), symbols.namesake, Acceleration, Space and Planetary Science, 0103 physical sciences, symbols, ddc:520, Planck, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We estimate the molecular mass around CTA 1 using data from Planck and the Harvard CO survey. We observe that the molecular mass in the vicinity of the complex is not enough to explain the TeV emission observed by VERITAS, even under favorable assumptions for the cosmic-ray acceleration properties of the supernova remnant. This supports the idea that the TeV emission comes from the PWN. Here, we model the spectrum of the PWN at possible different stages of its evolution, including both the dynamics of the PWN and the SNR and their interaction via the reverse shock. We have included in the model the energy lost via radiation by particles and the particles escape when computing the pressure produced by the gas. This leads to an evolving energy partition, since for the same instantaneous sharing of the injection of energy provided by the rotational power, the field and the particles are affected differently by radiation and losses. We present the model, and study in detail how the spectrum of a canonical isolated PWN is affected during compression and re-expansion and how this may impact on the CTA 1 case. By exploring the phase-space of parameters that lead to radii in agreement with those observed, we then analyze different situations that might represent the current stage of the CTA 1 PWN, and discuss caveats and requirements of each one., Comment: 13 pages, 8 figures, accepted for publication in MNRAS
Published: 2016
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33. Very high energy γ-ray observations of the binary PSR B1259–63/SS2883 around the 2007 Periastron

Author: A. A. Zdziarski, M. K. Daniel, Gavin Rowell, L. Venter, A. C. Clapson, M. C. Medina, T. J. L. McComb, Gilles Henri, Marek Sikora, W. Domainko, P. H. Tam, S. Rosier-Lees, P. Espigat, S. Schwemmer, Cameron B Rulten, Andrea Santangelo, Michal Dyrda, K. Katarzyński, M. Kerschhaggl, Michael Punch, Felix Aharonian, Guillaume Dubus, Jacek Niemiec, B. C. Raubenheimer, B. Giebels, A. R. Bazer-Bachi, F. Brun, O. Tibolla, A. Shalchi, D. Gerbig, M. Panter, J. L. Skilton, O. C. de Jager, S. Schwarzburg, D. Nedbal, M. Vivier, Karl Kosack, Christian Farnier, C. Stegmann, I. Jung, Stefan Wagner, Gisela Anton, Dieter Horns, Pierre Brun, Łukasz Stawarz, B. Rudak, Kathrin Egberts, G. Lamanna, B. Degrange, A. Cheesebrough, J. Dyks, Heinrich J. Völk, P. Vincent, I. D. Davids, Frank M. Rieger, D. Göring, David Maurin, S. Pita, V. Borrel, M. Tluczykont, Y. A. Gallant, Stefan Ohm, G. Coignet, J-F. Olive, Martin Ward, B. Behera, L. Rob, V. Sahakian, G. Vasileiadis, Rolf Bühler, Andreas Quirrenbach, J.-P. Tavernet, A. Hoffmann, J. F. Glicenstein, R. Kossakowski, F. M. Schöck, M. Paz Arribas, G. Heinzelmann, J. Bolmont, Ullrich Schwanke, M. Dalton, A. G. Akhperjanian, R. Steenkamp, G. Pedaletti, J.-P. Lenain, P. M. Chadwick, Francesca Volpe, B. Nicholas, Anna Szostek, F. Dubois, Konrad Bernlöhr, G. Superina, G. Pühlhofer, A. Fiasson, Timothé Boutelier, Emmanuel Moulin, Reinhard Schlickeiser, Hugh Dickinson, V. Marandon, Christo Venter, C. Jahn, U. F. Katz, A. Zech, A. Djannati-Ataï, M. Hauser, C. van Eldik, M. Holleran, M. Renaud, D. Hauser, D. Klochkov, Catherine Boisson, Rafal Moderski, Dimitrios Emmanoulopoulos, H. Sol, R. C. G. Chaves, S. M. Rayner, J. P. Vialle, P. Goret, Guy Pelletier, A. Förster, Martin Raue, S. Hoppe, A. Charbonnier, S. Heinz, L. O'c. Drury, M. Füßling, E. de Oña Wilhelmi, Sarah Kaufmann, L. Gérard, B. Glück, Nu. Komin, T. Bulik, Christoph Deil, T. Kneiske, I. Büsching, P.-O. Petrucci, L.-M. Chounet, Yvonne Becherini, D. Nekrassov, W. Kluźniak, A. Jacholkowska, G. Fontaine, S. J. Nolan, Jim Hinton, Dmitry Khangulyan, Thomas Lohse, Michał Ostrowski, K. J. Orford, J. Ripken, D. Keogh, Werner Hofmann, U. Barres de Almeida, F. Feinstein, Julien Masbou, Stefano Gabici, M. de Naurois, Alexandre Marcowith, O. Martineau-Huynh, B. Khélifi, G. Hermann, Regis Terrier, J. Ruppel, J. Brucker, D. Spangler, M. Naumann-Godo, F. Stinzing, A. Bochow, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Astrophysique des Hautes Energies (APC - AHE), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], observational [methods], Flux, Astrophysics, 01 natural sciences, Spectral line, neutron [stars], Pulsar, 0103 physical sciences, Binary star, 010303 astronomy & astrophysics, Astroparticle physics, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], binaries: general [stars], Gamma ray, observations [gamma rays], Astronomy, telescopes, Astronomy and Astrophysics, non-thermal [radiation mechanisms], Light curve, Neutron star, 13. Climate action, Space and Planetary Science
Abstract: Aims. This article presents very-high-energy (VHE; E > 100 GeV) data from the $\gamma$-ray binary PSR B1259-63 as taken during the years 2005, 2006 and before as well as shortly after the 2007 periastron passage. These data extend the knowledge of the lightcurve of this object to all phases of the 3.4 year binary orbit. The lightcurve constrains physical mechanisms present in this TeV source. Methods. Observations of VHE $\gamma$-rays with the HESS telescope array using the Imaging Atmospheric Cherenkov Technique were performed. The HESS instrument features an angular resolution of < 0.1° and an energy resolution of < 20%. Gamma-ray events in an energy range of 0.5-70 TeV were recorded. From these data, energy spectra and lightcurve with a monthly time sampling were extracted. Results. VHE $\gamma$-ray emission from PSR B1259-63 was detected with an overall significance of 9.5 standard deviations using 55h of exposure, obtained from April to August 2007. The monthly flux of $\gamma$-rays during the observation period was measured, yielding VHE lightcurve data for the early pre-periastron phase of the system for the first time. No spectral variability was found on timescales of months. The spectrum is described by a power law with a photon index of $\Gamma$ = 2.8 $\pm$ 0.2stat $\pm$ 0.2sys and flux normalisation $\Phi_{0}$ = (1.1 $\pm$ 0.1stat $\pm$ 0.2sys) $\times$ 10-12 TeV-1 cm-2 s-1. PSR B1259-63 was also monitored in 2005 and 2006, far from periastron passage, comprising 8.9 h and 7.5 h of exposure, respectively. No significant excess of $\gamma$-rays is seen in those observations. Conclusions. PSR B1259-63 has been re-confirmed as a variable TeV $\gamma$-ray emitter. The firm detection of VHE photons emitted at a true anomaly $\theta$$\approx$-0.35 of the pulsar orbit, i.e. already ~50 days prior to the periastron passage, disfavors the stellar disc target scenario as a primary emission mechanism, based on current knowledge about the companion star's disc inclination, extension, and density profile. Results. VHE $\gamma$-ray emission from PSR B1259-63 was detected with an overall significance of 9.5 standard deviations using 55h of exposure, obtained from April to August 2007. The monthly flux of $\gamma$-rays during the observation period was measured, yielding VHE lightcurve data for the early pre-periastron phase of the system for the first time. No spectral variability was found on timescales of months. The spectrum is described by a power law with a photon index of $\Gamma$ = 2.8 $\pm$ 0.2stat $\pm$ 0.2sys and flux normalisation $\Phi_{0}$ = (1.1 $\pm$ 0.1stat $\pm$ 0.2sys) $\times$ 10-12 TeV-1 cm-2 s-1. PSR B1259-63 was also monitored in 2005 and 2006, far from periastron passage, comprising 8.9 h and 7.5 h of exposure, respectively. No significant excess of $\gamma$-rays is seen in those observations. Conclusions. PSR B1259-63 has been re-confirmed as a variable TeV $\gamma$-ray emitter. The firm detection of VHE photons emitted at a true anomaly $\theta$$\approx$-0.35 of the pulsar orbit, i.e. already ~50 days prior to the periastron passage, disfavors the stellar disc target scenario as a primary emission mechanism, based on current knowledge about the companion star's disc inclination, extension, and density profile.
Published: 2009

34. Simultaneous HESS and Chandra observations of Sagitarius A$^{\star}$ during an X-ray flare

Author: F. Aharonian, A. G. Akhperjanian, U. Barres de Almeida, A. R. Bazer-Bachi, Y. Becherini, B. Behera, W. Benbow, K. Bernlöhr, C. Boisson, A. Bochow, V. Borrel, I. Braun, E. Brion, J. Brucker, P. Brun, R. Bühler, T. Bulik, I. Büsching, T. Boutelier, S. Carrigan, P. M. Chadwick, A. Charbonnier, R. C. G. Chaves, A. Cheesebrough, L.-M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C. Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, C. Hadjichristidis, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. de Jager, I. Jung, K. Katarzyński, S. Kaufmann, E. Kendziorra, M. Kerschhaggl, D. Khangulyan, B. Khélifi, D. Keogh, Nu. Komin, K. Kosack, G. Lamanna, J.-P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J. L. McComb, M. C. Medina, R. Moderski, E. Moulin, M. Naumann-Godo, M. de Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J.-F. Olive, E. de Oña Wilhelmi, K. J. Orford, J. L. Osborne, M. Ostrowski, M. Panter, G. Pedaletti, G. Pelletier, P.-O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, J. L. Skilton, H. Sol, D. Spangler, Ł. Stawarz, R. Steenkamp, C. Stegmann, G. Superina, P. H. Tam, J.-P. Tavernet, R. Terrier, O. Tibolla, C. van Eldik, G. Vasileiadis, C. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 10859748 - Holleran, Mathew, 12006653 - Venter, Christo, 10179240 - Raubenheimer, Barend Christoffel, 13235176 - Büsching, Ingo, 10065857 - De Jager, Ocker Cornelis, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Event horizon, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Flux, Astrophysics, gamma-rays:observations, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Coincident, law, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, individuals: Sgr A* [X-rays], Supermassive black hole, education.field_of_study, 010308 nuclear & particles physics, Astrophysics (astro-ph), observations [gamma rays], Astronomy and Astrophysics, X-rays:individual sources:Sgr A, Particle acceleration, Sagittarius A, Space and Planetary Science, individuals: Sgr $A^{\star }$ [X-rays], Flare
Abstract: The rapidly varying (~10 minute timescale) non-thermal X-ray emission observed from Sgr A* implies that particle acceleration is occuring close to the event horizon of the supermassive black hole. The TeV gamma-ray source HESS J1745-290 is coincident with Sgr A* and may be closely related to its X-ray emission. Simultaneous X-ray and TeV observations are required to elucidate the relationship between these objects. We report on joint H.E.S.S./Chandra observations performed in July 2005, during which an X-ray flare was detected. Despite a factor of 9 increase in the X-ray flux of Sgr A*, no evidence is found for an increase in the TeV gamma-ray flux from this region. We find that an increase in the gamma-ray flux of a factor of 2 or greater can be excluded at a confidence level of 99%. This finding disfavours scenarios in which the keV and TeV emission are associated with the same population of accelerated particles and in which the bulk of the gamma-ray emission is produced within ~10^{14} cm (~100 R_S) of the supermassive black hole., 5 pages, 2 figures
Published: 2008

35. Teraelectronvolt pulsed emission from the Crab pulsar detected by MAGIC

Author: MAGIC Collaboration, M. L. Ahnen, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, B. Banerjee, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, S. Buson, E. Carmona, A. Carosi, A. Chatterjee, R. Clavero, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, E. de Oña Wilhelmi, C. Delgado Mendez, F. Di Pierro, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher Glawion, D. Elsaesser, A. Fernández-Barral, D. Fidalgo, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. García López, M. Garczarczyk, D. Garrido Terrats, M. Gaug, P. Giammaria, N. Godinović, A. González Muñoz, D. Gora, D. Guberman, D. Hadasch, A. Hahn, Y. Hanabata, M. Hayashida, J. Herrera, J. Hose, D. Hrupec, G. Hughes, W. Idec, K. Kodani, Y. Konno, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, E. Lindfors, S. Lombardi, F. Longo, M. López, R. López-Coto, E. Lorenz, P. Majumdar, M. Makariev, K. Mallot, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martínez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, E. Moretti, D. Nakajima, V. Neustroev, A. Niedzwiecki, M. Nievas Rosillo, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, J. Palacio, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, G. Pedaletti, M. Persic, J. Poutanen, P. G. Prada Moroni, E. Prandini, I. Puljak, W. Rhode, M. Ribó, J. Rico, J. Rodriguez Garcia, T. Saito, K. Satalecka, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpää, J. Sitarek, I. Snidaric, D. Sobczynska, A. Stamerra, T. Steinbring, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzić, D. Tescaro, M. Teshima, J. Thaele, D. F. Torres, T. Toyama, A. Treves, V. Verguilov, I. Vovk, J. E. Ward, M. Will, M. H. Wu, and R. Zanin
Subjects: Astrophysics::High Energy Astrophysical Phenomena
Abstract: Aims: To investigate the extension of the very-high-energy spectral tail of the Crab pulsar at energies above 400 GeV. Methods: We analyzed $\sim$320 hours of good quality data of Crab with the MAGIC telescope, obtained from February 2007 until April 2014. Results: We report the most energetic pulsed emission ever detected from the Crab pulsar reaching up to 1.5 TeV. The pulse profile shows two narrow peaks synchronized with the ones measured in the GeV energy range. The spectra of the two peaks follow two different power-law functions from 70 GeV up to 1.5 TeV and connect smoothly with the spectra measured above 10 GeV by the Large Area Telescope (LAT) on board of the Fermi satellite. When making a joint fit of the LAT and MAGIC data, above 10 GeV, the photon indices of the spectra differ by 0.5$\pm$0.1. Conclusions: We measured with the MAGIC telescopes the most energetic pulsed photons from a pulsar to date. Such TeV pulsed photons require a parent population of electrons with a Lorentz factor of at least $5\times 10^6$. These results strongly suggest IC scattering off low energy photons as the emission mechanism and a gamma-ray production region in the vicinity of the light cylinder.
Published: 2015

36. Prospects for observations of pulsars and pulsar wind nebulae with CTA

Author: E. d. Ona Wilhelmi, B. Rudak, J. A. Barrio, J. L. Contreras, Y. Gallant, D. Hadasch, T. Hassan, M. Lopez, D. Mazin, N. Mirabal, G. Pedaletti, M. Renaud, R. d. los, D. F. Torres, CTA Consortium, Acharya B. S., Actis M., Aghajani T., BISSALDI, ELISABETTA, E. d., Ona Wilhelmi, B., Rudak, J. A., Barrio, J. L., Contrera, Y., Gallant, D., Hadasch, T., Hassan, M., Lopez, D., Mazin, N., Mirabal, G., Pedaletti, M., Renaud, R. d., Lo, D. F., Torre, Cta, Consortium, Acharya, B. S., Actis, M., Aghajani, T., and Bissaldi, Elisabetta
Subjects: Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Pulsars, Pulsar Wind Nebulae, Cherenkov telescopes, Astrophysics, Pulsar wind nebula, Binary pulsar, law.invention, Telescope, Pulsar, law, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Cherenkov Telescope Array, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The last few years have seen a revolution in very-high gamma-ray astronomy (VHE; E>100 GeV) driven largely by a new generation of Cherenkov telescopes (namely the H.E.S.S. telescope array, the MAGIC and MAGIC-II large telescopes and the VERITAS telescope array). The Cherenkov Telescope Array (CTA) project foresees a factor of 5 to 10 improvement in sensitivity above 0.1 TeV, extending the accessible energy range to higher energies up to 100 TeV, in the Galactic cut-off regime, and down to a few tens GeV, covering the VHE photon spectrum with good energy and angular resolution. As a result of the fast development of the VHE field, the number of pulsar wind nebulae (PWNe) detected has increased from one PWN in the early '90s to more than two dozen firm candidates today. Also, the low energy threshold achieved and good sensitivity at TeV energies has resulted in the detection of pulsed emission from the Crab Pulsar (or its close environment) opening new and exiting expectations about the pulsed spectra of the high energy pulsars powering PWNe. Here we discuss the physics goals we aim to achieve with CTA on pulsar and PWNe physics evaluating the response of the instrument for different configurations., accepted for publication in Astroparticle Physics
Published: 2013

37. Detailed Investigation of the Gamma-Ray Emission in the Vicinity of SNR W28 with FERMI-LAT

Author: Ryo Yamazaki, Jean Ballet, Takahiro Hayakawa, Diego F. Torres, Yasuo Fukui, G. Pedaletti, John W. Hewitt, Hideaki Katagiri, Yasushi Fukazawa, Marianne Lemoine-Goumard, Y. Hanabata, Andrew W. Strong, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), FERMI, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), IEEC-CSIC, Universitat Autònoma de Barcelona (UAB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Universitat Autònoma de Barcelona [Barcelona] (UAB)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Spectral line, law.invention, Telescope, gamma rays: ISM, Spitzer Space Telescope, cosmic rays, law, cceleration of particles, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Molecular cloud, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], diffusion, Gamma ray, Astronomy and Astrophysics, ISM: supernova remnants Online-only material: color figures, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We present a detailed investigation of the $\gamma$-ray emission in the vicinity of the supernova remnant (SNR) W28 (G6.4$-$0.1) observed by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. We detected significant $\gamma$-ray emission spatially coincident with TeV sources HESS J1800$-$240A, B, and C, located outside the radio boundary of the SNR. Their spectra in the 2-100 GeV band are consistent with the extrapolation of the power-law spectra of the TeV sources. We also identified a new source of GeV emission, dubbed Source W, which lies outside the boundary of TeV sources and coincides with radio emission from the western part of W28. All of the GeV $\gamma$-ray sources overlap with molecular clouds in the velocity range from 0 to 20 km s$^{-1}$. Under the assumption that the $\gamma$-ray emission towards HESS J1800-240A, B, and C comes from $\pi^0$ decay due to the interaction between the molecular clouds and cosmic rays (CRs) escaping from W28, they can be naturally explained by a single model in which the CR diffusion coefficient is smaller than the theoretical expectation in the interstellar space. The total energy of the CRs escaping from W28 is constrained through the same modeling to be larger than $\sim$ 2 $\times$ 10$^{49}$ erg. The emission from Source W can also be explained with the same CR escape scenario., Comment: 21 pages, 3 figures, accepted for publication in ApJ
Published: 2014

38. On the possible correlation of Galactic VHE source locations and enhancements of the surface density in the Galactic plane

Author: G. Pedaletti, E. de Oña Wilhelmi, and Diego F. Torres
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), Population, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Planck, education, Astrophysics::Galaxy Astrophysics, media_common, Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), symbols, Astrophysics - High Energy Astrophysical Phenomena, Energy source
Abstract: The association of very-high energy sources with regions of the sky rich in dust and gas has been noticed in the study of individual VHE sources. However, the statistical significance of such correlation for the whole population of TeV detections has not been assessed yet. Here we present a study of the association of VHE sources in the central Galactic region with positions of enhanced material content. We obtain estimates of the material content through two classical tracers: dust emission and intensity of the $^\textrm{12}$CO(1$\rightarrow$0) line. We make use of the recently released all-sky maps of astrophysical foregrounds of the Planck Collaboration and of the extensive existing CO mapping of the Galactic sky. In order to test the correlation, we construct randomized samples of VHE source positions starting from the inner Galactic plane survey sources detected by the H.E.S.S. array. We find hints of a positive correlation between positions of VHE sources and regions rich in molecular material, which in the best of cases reaches the 3.9sigma level. The latter confidence is however decreased if variations in the selection criteria are considered, what lead us to conclude that a positive correlation cannot be firmly established yet. Forthcoming VHE facilities will be needed in order to firmly establish the correlation., Comment: 6 pages, 5 figures, 1 table. Accepted for publication in A&A
Published: 2014
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39. On the potential of the Cherenkov Telescope Array for the study of cosmic-ray diffusion in molecular clouds

Author: G. Pedaletti, Diego F. Torres, Stefano Gabici, Daniel Mazin, E. de Oña Wilhelmi, Victor Stamatescu, IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] (UAB), APC - Astrophysique des Hautes Energies (APC - AHE), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Cosmic ray, Astrophysics, Parameter space, 01 natural sciences, ISM: clouds, Acceleration, gamma rays: ISM, cosmic rays, Observatory, 0103 physical sciences, Diffusion (business), education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Molecular cloud, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, radiation mechanisms: non-thermal, Cherenkov Telescope Array, Space and Planetary Science, astroparticle physics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Molecular clouds act as primary targets for cosmic-ray interactions and are expected to shine in gamma-rays as a by-product of these interactions. Indeed several detected gamma-ray sources both in HE and VHE gamma-rays (HE: 100 MeV < E < 100 GeV; VHE: E > 100 GeV) have been directly or indirectly associated with molecular clouds. Information on the local diffusion coefficient and the cosmic-ray population can be inferred from the observed gamma-ray signals. In this work we explore the capability of the forthcoming Cherenkov Telescope Array Observatory (CTA) to provide such measurements. We investigate the expected emission from clouds hosting an accelerator, surveying the parameter space for different modes of acceleration, age of the source, cloud density profile, and cosmic-ray diffusion coefficient. We present some of the most interesting cases for CTA regarding this science topic. The simulated gamma-ray fluxes depend strongly on the input parameters. In several cases, we find that it will be possible to constrain both the properties of the accelerator and the propagation mode of cosmic rays in the cloud from CTA data alone., 10 pages, 10 figures, 1 table, accepted for publication in A&A
Published: 2013

40. Search for VHE gamma-ray emission from Geminga pulsar and nebula with the MAGIC telescopes

Author: J. Palacio, S. Bonnefoy, R. Mirzoyan, Dario Hrupec, Daniela Dorner, Dariusz Gora, Gaia Vanzo, A. De Angelis, Marina Manganaro, Jose Luis Contreras, Vitaly Neustroev, J. E. Ward, Giacomo Bonnoli, F. Di Pierro, D. Fidalgo, Ignasi Reichardt, M. Gaug, D. Dominis Prester, K. Frantzen, G. Pedaletti, Thomas Bretz, E. Moretti, B. De Lotto, Miriam Lucio Martinez, Juan Cortina, J. M. Paredes, Antonio Stamerra, R. Clavero, D. Galindo, D. Nakajima, Stefano Covino, Juri Poutanen, Tihomir Surić, J. Herrera, Sara Buson, D. Eisenacher Glawion, Arka Chatterjee, P. G. Prada Moroni, Pratik Majumdar, M. V. Fonseca, Y. Hanabata, Fabrizio Tavecchio, Nikola Godinovic, Tomoki Saito, D. Tescaro, Benito Marcote, Junko Kushida, P. Da Vela, Koji Noda, G. Maneva, Ll. Font, P. Antoranz, S. Paiano, M. Lopez, Wolfgang Rhode, G. Hughes, Elisa Bernardini, Adrian Biland, S. N. Shore, Marcel Strzys, I. Snidaric, Karl Mannheim, M. Garczarczy, Tomislav Terzić, Martin Makariev, V. Fallah Ramazani, Konstancja Satalecka, Michele Doro, Martin Will, M. Peresano, Julian Sitarek, Oscar Blanch, L. Maraschi, J. Rico, R. López-Coto, J. Hose, F. Borracci, Daniel Mazin, K. Nishijima, Daniela Hadasch, C. Fruck, F. Longo, Yusuke Konno, A. Niedzwiecki, P. Colin, Ievgen Vovk, T. Toyama, Masahiro Teshima, L. Nogués, A. González Muñoz, K. Mallot, R. J. García López, B. Biasuzzi, David Paneque, C. Schultz, T. Schweizer, A. Sillanpää, M. Doert, M. H. Wu, Alexander Hahn, D. Guberman, E. Lindfors, U. Menzel, W. Idec, Mosè Mariotti, A.-K. Overkemping, A. La Barbera, Michele Palatiello, Wlodek Bednarek, P. Temnikov, Max Ludwig Ahnen, Juan Abel Barrio, X. Paredes-Fortuny, D. Garrido Terrats, Diego F. Torres, Francesco Dazzi, A. Fernández-Barral, Julia Thaele, Saverio Lombardi, Massimo Persic, Aaron Dominguez, K. Nilsson, Jose Miguel Miranda, M. Nievas Rosillo, Stefano Ansoldi, P. Giammaria, E. Colombo, Abelardo Moralejo, L. O. Takalo, Ana Babić, R. Paoletti, T. Steinbring, J. Becerra González, Alessio Berti, L. A. Antonelli, K. Kodani, Ivica Puljak, E. de Oña Wilhelmi, L. M. Perri, Roberta Zanin, Sabrina Einecke, J. Rodriguez Garcia, A. Carosi, Dominik Elsaesser, U. Barres de Almeida, Damir Lelas, Dorota Sobczyńska, E. Prandini, Aldo Treves, M. Hayashida, Marc Ribó, P. Bangale, Hidetoshi Kubo, Vassil Verguilov, B. Banerjee, Universitat de Barcelona, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., De Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S, Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Oña Wilhelmi, E., Di Pierro, F., Doert, M., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Glawion, D. Eisenacher, Elsaesser, D., Ramazani, V. Fallah, Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Giammaria, P., Godinović, N., Muñoz, A. González, Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nilsson, K., Nishijima, K., Noda, K., Nogués, L., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Saito, T., Satalecka, K., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., and Zanin, R.
Subjects: CRAB PULSAR, Astrophysics, 01 natural sciences, Power law, Pulsar wind nebula, neutron stars, LARGE-AREA TELESCOPE, Spectral line, MAJOR UPGRADE, Raigs gamma, astroparticle physics, stars: neutron, pulsars: general, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Nebula, CURVATURE-RADIATION, Gamma ray, CATALOG, astroparticle physics, neutron stars , pulsars, Geminga, Geminga, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Current generation, Astrophysics::High Energy Astrophysical Phenomena, general [Pulsars], FOS: Physical sciences, Astroparticle physic, Nebulae, HIGH-ENERGY EMISSION, RAPIDLY SPINNING PULSARS, 1E 0630+178, SLOT GAPS, MODEL, Pulsar, 0103 physical sciences, Cherenkov radiation, Telescopis, 010308 nuclear & particles physics, Gamma rays, neutron [Stars], Astronomy and Astrophysics, Astronomy and Astrophysic, Astroparticle physics, Pulsars: general, Stars: neutron, Space and Planetary Science, pulsars, ddc:520, Nebuloses, Telescopes
Abstract: Astronomy and astrophysics 591, A138(2016). doi:10.1051/0004-6361/201527722, The Geminga pulsar, one of the brighest gamma-ray sources, is a promising candidate for emission of very-high-energy (VHE > 100 GeV) pulsed gamma rays. Also, detection of a large nebula has been claimed by water Cherenkov instruments. We performed deep observations of Geminga with the MAGIC telescopes, yielding 63 h of good-quality data, and searched for emission from the pulsar and pulsar wind nebula. We did not find any significant detection, and derived 95% confidence level upper limits. The resulting upper limits of 5.3 × 10$^{-13}$ TeV cm$^{-2}$ s$^{-1}$ for the Geminga pulsar and 3.5 × 10$^{-12}$ TeV cm$^{-2} s$^{-1}$ for the surrounding nebula at 50 GeV are the mostconstraining ones obtained so far at VHE. To complement the VHE observations, we also analyzed 5 yr of Fermi-LAT data from Geminga, finding that the sub-exponential cut-off is preferred over the exponential cut-off that has been typically used in the literature. We also find that, above 10 GeV, the gamma-ray spectra from Geminga can be described with a power law with index softer than 5. The extrapolation of the power-law Fermi-LAT pulsed spectra to VHE goes well below the MAGIC upper limits, indicating that the detection of pulsed emission from Geminga with the current generation of Cherenkov telescopes is very difficult., Published by EDP Sciences, Les Ulis
Published: 2016

41. CTA and cosmic-ray diffusion in molecular clouds

Author: G. Pedaletti, Stefano Gabici, Daniel Mazin, E. de Oña Wilhelmi, Diego F. Torres, and Victor Stamatescu
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Molecular cloud, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Cosmic ray, Astrophysics, Parameter space, Cherenkov Telescope Array, Acceleration, Observatory, CTA - Abteilung Hofmann, Diffusion (business), education, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Molecular clouds act as primary targets for cosmic-ray interactions and are expected to shine in gamma-rays as a by-product of these interactions. Indeed several detected gamma-ray sources both in HE and VHE gamma-rays (HE: 100 MeV < E < 100 GeV; VHE: E > 100 GeV) have been directly or indirectly associated with molecular clouds. Information on the local diffusion coefficient and the local cosmic-ray population can be deduced from the observed gamma-ray signals. In this work we concentrate on the capability of the forthcoming Cherenkov Telescope Array Observatory (CTA) to provide such measurements. We investigate the expected emission from clouds hosting an accelerator, exploring the parameter space for different modes of acceleration, age of the source, cloud density profile, and cosmic ray diffusion coefficient. We present some of the most interesting cases for CTA regarding this science topic. The simulated gamma-ray fluxes depend strongly on the input parameters. In some cases, from CTA data it will be possible to constrain both the properties of the accelerator and the propagation mode of cosmic rays in the cloud., In Proceedings of the 2012 Heidelberg Symposium on High Energy Gamma-Ray Astronomy. All CTA contributions at arXiv:1211.1840
Published: 2012

42. H.E.S.S. constraints on Dark Matter annihilations towards the Sculptor and Carina Dwarf Galaxies

Author: J. Dyks, Michael Punch, Reinhard Schlickeiser, A. Hoffmann, M. Kerschhaggl, A. Jacholkowska, M. de Naurois, R. C. G. Chaves, S. Kaufmann, C. L. Naumann, D. Nedbal, Christian Farnier, Dieter Horns, J. Mehault, A. Djannati-Ataï, P. Espigat, H. J. Dickinson, Michał Ostrowski, Dirk Lennarz, Gilles Henri, F. M. Schöck, M. Paz Arribas, J. K. Becker, D. Klochkov, Jacek Niemiec, Olaf Reimer, Omar Tibolla, A. A. Zdziarski, Ullrich Schwanke, J. Conrad, G. Pelletier, J. D. Hague, U. Barres de Almeida, Felix Ryde, J. Bolmont, P. Hofverberg, D. Khangulyan, W. Kluźniak, G. Lamanna, R. Steenkamp, Martin Ward, O. C. de Jager, N. Maxted, R. Kossakowski, Cameron B Rulten, M. Sikora, M. Dalton, S. Schwemmer, Anna Barnacka, Andrea Santangelo, M. Panter, Serguei Vorobiov, A. Shalchi, Martin Raue, G. Heinzelmann, L. O'c. Drury, A. Lopatin, David Maurin, Svenja Carrigan, B. Degrange, J. L. Skilton, A. C. Clapson, H. Gast, H.-S. Zechlin, M. Vivier, Stefan Wagner, Gisela Anton, A. Fiasson, S. Schwarzburg, D. Göring, J.-P. Tavernet, K. Kosack, Franky Dubois, Felix Aharonian, M. Vorster, Y. A. Gallant, D. Keogh, F. Stinzing, P. Brun, Francois Brun, Thomas Lohse, H. Laffon, M. Naumann-Godo, Matteo Cerruti, G. Spengler, M. V. Fernandes, Emmanuel Moulin, Guillaume Dubus, Łukasz Stawarz, Christo Venter, Marek Jamrozy, Anna Zajczyk, Pascal Vincent, K. Valerius, M. K. Daniel, M. Dyrda, Stefan Ohm, C. Jahn, S. Pita, B. Opitz, Heinrich J. Völk, U. F. Katz, Werner Hofmann, Helene Sol, Julien Masbou, J. F. Glicenstein, R. Moderski, Yvonne Becherini, Iurii Sushch, V. Borrel, A. Zech, Regis Terrier, L. Fallon, Francesca Volpe, B. Nicholas, A. Viana, S. J. Nolan, S. Rosier-Lees, Gavin Rowell, Jim Hinton, G. Fontaine, D. Hampf, R. de los Reyes, A. Schönwald, A. Frster, G. Pedaletti, K. Katarzyński, K. Egberts, V. Sahakian, J. Ruppel, Tomasz Bulik, Nu. Komin, Joachim Ripken, L.-M. Chounet, M. C. Medina, I. D. Davids, F. Feinstein, W. Domainko, P. Goret, J. Brucker, B. Giebels, G. Coignet, A. Marcowith, D. Gerbig, P. M. Chadwick, P.-O. Petrucci, Catherine Boisson, A. Bochow, M. Füßling, B. Khélifi, J-F. Olive, M. A. Kastendieck, E. de Oña Wilhelmi, V. Marandon, D. Nekrassov, L. Gérard, B. Glück, S. Fegan, P. Eger, Andreas Quirrenbach, T. J. L. McComb, M. Tluczykont, Christoph Deil, Anna Szostek, S. M. Rayner, J. P. Vialle, Konrad Bernlöhr, T. Kneiske, A. R. Bazer-Bachi, A. Charbonnier, S. Heinz, G. Pühlhofer, G. Hermann, A. Reimer, B. Behera, Fabio Acero, L. Rob, A. Wierzcholska, G. Vasileiadis, C. Stegmann, I. Jung, B. Rudak, A. G. Akhperjanian, N. Nguyen, M. Hauser, C. van Eldik, A. Abramowski, Sabrina Casanova, Frank M. Rieger, M. Renaud, P. Bordas, Chia-Chun Lu, I. Büsching, A. Cheesebrough, Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), HESS, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: internal Bremsstrahlung, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Dwarf galaxy problem, Scalar field dark matter, FOS: Physical sciences, Carina, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, 0103 physical sciences, 010303 astronomy & astrophysics, Light dark matter, observations - dwarf spheroidal galaxy [gamma-rays], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Sommerfeld enhancement, 010308 nuclear & particles physics, Hot dark matter, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astronomy and Astrophysics, Dwarf spheroidal galaxy, Dark matter halo, Cuspy halo problem, Dark galaxy, Astrophysics - High Energy Astrophysical Phenomena, Sculptor
Abstract: The Sculptor and Carina Dwarf spheroidal galaxies were observed with the H.E.S.S. Cherenkov telescope array between January 2008 and December 2009. The data sets consist of a total of 11.8 and 14.8 hours of high quality data, respectively. No gamma-ray signal was detected at the nominal positions of these galaxies above 220 GeV and 320 GeV, respectively. Upper limits on the gamma-ray fluxes at 95% C.L. assuming two forms for the spectral energy distribution (a power law shape and one derived from dark matter annihilation) are obtained at the level of 10^-13 to 10^-12 cm^-2s^-1 in the TeV range. Constraints on the velocity weighted dark matter particle annihilation cross section for both Sculptor and Carina dwarf galaxies range from ~ 10^-21 cm^3s^-1 down to ~ 10^-22 cm^3s^-1 depending on the dark matter halo model used. Possible enhancements of the gamma-ray flux are studied: the Sommerfeld effect, which is found to exclude some dark matter particle masses, the internal Bremsstrahlung and clumps in the dark-matter halo distributions., Comment: Accepted for publication on Astroparticle Physics, 25 pages, 12 figures
Published: 2011

43. Search for Lorentz Invariance breaking with a likelihood fit of the PKS 2155-304 Flare Data Taken on MJD 53944

Author: Sabrina Casanova, Michael Punch, G. Hermann, B. Behera, V. Sahakian, A. Shalchi, Felix Ryde, C. Stegmann, O. C. de Jager, L. Rob, Svenja Carrigan, Frank M. Rieger, I. Jung, B. Rudak, P. Bordas, Christo Venter, M. A. Kastendieck, Gilles Henri, C. Jahn, U. F. Katz, R. C. G. Chaves, R. Moderski, Christian Farnier, A. Zech, Dirk Lennarz, S. Schwarzburg, M. Kerschhaggl, M. Vivier, Cameron B Rulten, G. Vasileiadis, Dieter Horns, M. Sikora, M. C. Medina, B. Giebels, A. Lopatin, L.-M. Chounet, I. D. Davids, Francois Brun, B. Degrange, A. A. Zdziarski, Rolf Bühler, M. de Naurois, P. Brun, Serguei Vorobiov, A. C. Clapson, Stefan Wagner, Gisela Anton, A. Marcowith, Andreas Quirrenbach, H. J. Dickinson, Emmanuel Moulin, Guillaume Dubus, Joachim Ripken, V. Marandon, J. Ruppel, Reinhard Schlickeiser, K. Kosack, Marek Jamrozy, A. Cheesebrough, Franky Dubois, D. Göring, P. Hofverberg, Christoph Deil, D. Keogh, T. Kneiske, Felix Aharonian, Helene Sol, M. Naumann-Godo, A. Jacholkowska, L. O'c. Drury, H. Laffon, D. Khangulyan, W. Kluźniak, Matteo Cerruti, G. Spengler, Julien Masbou, M. Tluczykont, A. Hoffmann, Gavin Rowell, G. Pelletier, L. Fallon, R. de los Reyes, M. Dalton, Stefan Ohm, J. K. Becker, P. Eger, S. Pita, J. Bolmont, M. Dyrda, R. Kossakowski, Konrad Bernlöhr, F. Feinstein, K. Valerius, M. K. Daniel, Anna Szostek, D. Nedbal, A. Schönwald, H. Gast, F. M. Schöck, Thomas Lohse, H.-S. Zechlin, M. Paz Arribas, V. Borrel, G. Lamanna, G. Pühlhofer, U. Barres de Almeida, Werner Hofmann, Regis Terrier, J. Brucker, A. Fiasson, A. Reimer, David Maurin, A. Djannati-Ataï, Pascal Vincent, S. Kaufmann, T. J. L. McComb, Fabio Acero, A. Viana, Ullrich Schwanke, A. R. Bazer-Bachi, Michał Ostrowski, S. Schwemmer, Anna Barnacka, Andrea Santangelo, A. Charbonnier, F. Stinzing, J.-P. Tavernet, S. Heinz, D. Klochkov, J. L. Skilton, D. Hampf, Alicja Wierzcholska, R. Steenkamp, J. F. Glicenstein, Iurii Sushch, M. V. Fernandes, Martin Ward, S. Rosier-Lees, M. Panter, Y. A. Gallant, G. Pedaletti, J. Dyks, Łukasz Stawarz, G. Coignet, J. D. Hague, Catherine Boisson, A. Bochow, K. Katarzyński, Heinrich J. Völk, P. Goret, M. Vorster, W. Domainko, N. Maxted, Francesca Volpe, B. Khélifi, J-F. Olive, B. Nicholas, C. L. Naumann, Yvonne Becherini, Martin Raue, G. Heinzelmann, J. Mehault, M. Füßling, E. de Oña Wilhelmi, G. Fontaine, K. Egberts, Nu. Komin, Anna Zajczyk, D. Gerbig, L. Gérard, B. Glück, B. Opitz, Jim Hinton, A. G. Akhperjanian, N. Nguyen, M. Hauser, C. van Eldik, A. Abramowski, P.-O. Petrucci, M. Renaud, Chia-Chun Lu, D. Nekrassov, I. Büsching, A. Frster, Tomasz Bulik, S. J. Nolan, P. M. Chadwick, S. Fegan, P. Espigat, Jacek Niemiec, Olaf Reimer, Omar Tibolla, J. Conrad, S. M. Rayner, J. P. Vialle, Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: Quantum Gravity, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Lorentz covariance, PKS 2155-304, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, High Energy Stereoscopic System, Sensitivity (control systems), Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Lorentz Invariance breaking, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], active galaxies, Astronomy and Astrophysics, H.E.S.S, Active galaxies, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Energy (signal processing)
Abstract: Several models of Quantum Gravity predict Lorentz Symmetry breaking at energy scales approaching the Planck scale (10^{19} GeV). With present photon data from the observations of distant astrophysical sources, it is possible to constrain the Lorentz Symmetry breaking linear term in the standard photon dispersion relations. Gamma-ray Bursts (GRB) and flaring Active Galactic Nuclei (AGN) are complementary to each other for this purpose, since they are observed at different distances in different energy ranges and with different levels of variability. Following a previous publication of the High Energy Stereoscopic System (H.E.S.S.) collaboration, a more sensitive event-by-event method consisting of a likelihood fit is applied to PKS 2155-304 flare data of MJD 53944 (July 28, 2006) as used in the previous publication. The previous limit on the linear term is improved by a factor of ~3 up to M^{l}_{QG} > 2.1x10^{18} GeV and is currently the best result obtained with blazars. The sensitivity to the quadratic term is lower and provides a limit of M^{q}_{QG} > 6.4x10^10 GeV, which is the best value obtained so far with an AGN and similar to the best limits obtained with GRB., 24 pages, 9 figures. Accepted for publication in Astropart. Phys. Rev1 is the final accepted version (typo corrections)
Published: 2011

44. Discovery of VHE γ-rays from the BL Lacertae object PKS 0548-322

Author: Yvonne Becherini, A. Cheesebrough, S. M. Rayner, J. P. Vialle, G. Pedaletti, Joachim Ripken, A. Hoffmann, A. Förster, Martin Raue, J. F. Glicenstein, P.-O. Petrucci, B. Behera, L. Rob, Stefan Wagner, J. L. Skilton, G. Vasileiadis, D. Nekrassov, Michael Punch, J. Ruppel, M. K. Daniel, Christoph Deil, T. Kneiske, M. Kerschhagg, K. Egberts, Anna Szostek, Gilles Henri, L.-M. Chounet, P. M. Chadwick, G. Pelletier, L. Venter, A. C. Clapson, W. Domainko, P. H. Tam, Gerard Fontaine, A. Djannati-Ataï, A. Marcowith, Christo Venter, C. Jahn, Thomas Lohse, Guillaume Dubus, M. de Naurois, J. Brucker, G. Lamanna, F. Volp, M. Panter, U. Katz, E. Moulin, Tomasz Bulik, R. Moderski, M. Füssling, A. Zech, D. Hauser, Frank M. Rieger, T. J. L. McComb, F. Stinzing, A. Shalchi, A. Jacholkowska, B. Giebels, A. R. Bazer-Bachi, S. Schwemmer, S. Rosier-Lees, A. Charbonnier, F. Feinstein, D. Spangler, S. Heinz, Andrea Santangelo, R. C. G. Chaves, O. C. de Jager, J. M. Martin, P. Espigat, D. Khangulyan, W. Kluźniak, B. C. Raubenheimer, U. Barres de Almeida, S. Hoppe, A. Bochow, S. Schwarzburg, S. J. Nolan, D. Keogh, Jacek Niemiec, Jim Hinton, David Maurin, M. Vivier, L. O'c. Drury, C. Boisson, J-F. Olive, Dieter Horns, A. A. Zdziarski, Christian Stegmann, Stefan Ohm, Gavin Rowell, D. Gerbig, J.-P. Tavernet, Gisela Anton, S. Pita, C. B. Rulten, Francois Brun, C. van Eldik, Michal Ostrowski, J. Dyks, J.-P. Lenain, Stefano Gabici, D. Emmanoulopoulos, C. Farnier, Werner Hofmann, D. Nedbal, E. de Oña Wilhelm, G. Heinzelmann, Isak Delberth Davids, Regis Terrier, K. Kosack, Konrad Bernlöhr, A. Fiasson, B. Khélifi, G. Superina, Helene Sol, G. Hermann, G. Pühlhofer, Lukasz Stawarz, Michal Dyrda, K. J. Orford, M. Naumann-Godo, J. Bolmont, Rolf Bühler, Andreas Quirrenbach, B. Nicholas, V. Sahakian, Martin Ward, M. Sikora, Franky Dubois, Felix Aharonian, Reinhard Schlickeiser, F. M. Schöck, Riaan Steenkamp, M. Paz Arribas, Hugh Dickinson, Ullrich Schwanke, M. Dalton, Julien Masbou, M. C. Medina, A. G. Akhperjanian, Eckhard Kendziorra, V. Marandon, M. Hauser, M. Holleran, Heinrich J. Völk, M. Renaud, I. Jung, B. Rudak, Olivier Martineau-Huynh, B. Degrange, I. Büsching, Timothé Boutelier, Nu. Komin, P. Goret, Y. A. Gallant, Sarah Kaufmann, Pascal Vincent, L. Gérard, B. Glück, O. Tibolla, Wystan Benbow, Pierre Brun, D. Göring, V. Borrel, M. Tluczykont, R. Schröder, G. Coignet, Krzysztof Katarzynski, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris
Subjects: BL Lacertae objects: individual: PKS 0548-322, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Swift Gamma-Ray Burst Mission, Photon, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Flux, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, law, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, Astronomy, observations [gamma rays], Astronomy and Astrophysics, Synchrotron, individual: PKS 0548-322 [BL Lacertae objects], Crab Nebula, Space and Planetary Science, active [galaxies], Spectral energy distribution, gamma rays: observations, BL Lac object
Abstract: 6 pages, 3 figures; PKS 0548-322 (z=0.069) is a "high-frequency-peaked'' BL Lac object and a candidate very high energy (VHE, E>100 GeV) gamma-ray emitter, due to its high X-ray and radio flux. Observations at the VHE band provide insights into the origin of very energetic particles present in this source and the radiation processes at work. We report observations made between October 2004 and January 2008 with the H.E.S.S. array, a four imaging atmospheric-Cherenkov telescopes. Contemporaneous UV and X-ray observations with the Swift satellite in November 2006 are also reported. PKS 0548-322 is detected for the first time in the VHE band with H.E.S.S. We measure an excess of 216 gamma-rays corresponding to a significance of 5.6 standard deviations. The photon spectrum of the source is described by a power-law, with a photon index of Gamma=2.86 +/- 0.34 (stat) +/- 0.10 (sys). The integral flux above 200 GeV is 1.3 % of the flux of the Crab Nebula, and is consistent with being constant in time. Contemporaneous Swift/XRT observations reveal an X-ray flux between 2 and 10 keV of F_{2-10 keV}=2.3 +/- 0.2 x 10^{-11} erg.cm^{-2}. s^{-1}, an intermediate intensity state with respect to previous observations. The spectral energy distribution can be reproduced using a simple one-zone synchrotron self Compton model, with parameters similar those observed for other sources of this type.
Published: 2010

45. Detection of Gamma Rays From a Starburst Galaxy

Author: S. Schwarzburg, J. Dyks, O. C. de Jager, Jim Hinton, U. Schwanke, Dmitry Khangulyan, Frank M. Rieger, M. K. Daniel, W. Kluźniak, M. Kerschhaggl, R. C. G. Chaves, J-F. Olive, K. J. Orford, S. Hoppe, M. Vivier, B. Behera, Stefan Ohm, Anna Szostek, F. Dubois, Petter Hofverberg, Dimitrios Emmanoulopoulos, L. Rob, Nu. Komin, Stefan Wagner, M. de Naurois, Gisela Anton, S. Schwemmer, P. Espigat, Alexandre Marcowith, Y. A. Gallant, P. Goret, J. Mehault, Andrea Santangelo, A. A. Zdziarski, M. Naumann-Godo, S. Rosier-Lees, Emmanuel Moulin, A. Charbonnier, F. Stinzing, G. Pedaletti, J.-P. Lenain, S. Heinz, J. Ripken, Francesca Volpe, M. Panter, B. Nicholas, Jacek Niemiec, M. Füßling, E. de Oña Wilhelmi, G. Fontaine, Olaf Reimer, J.F. Glicenstein, Sarah Kaufmann, U. Barres de Almeida, A. C. Clapson, F. Brun, L. Gérard, B. Glück, A. Djannati-Ataï, Tomasz Bulik, J. Ruppel, L.-M. Chounet, D. Klochkov, G. Vasileiadis, Guillaume Dubus, A. Jacholkowska, Michael Punch, J. Brucker, F. Feinstein, D. Göring, Olivier Martineau-Huynh, D. Keogh, A. Bochow, W. Domainko, P. H. Tam, Gavin Rowell, David Maurin, A. Fiasson, Julien Masbou, Thomas Lohse, V. Borrel, V. Sahakian, Michal Dyrda, Timothé Boutelier, Stefano Gabici, P.-O. Petrucci, Yvonne Becherini, S. J. Nolan, Rolf Bühler, Andreas Quirrenbach, G. Lamanna, Christian Farnier, B. C. Raubenheimer, M. Renaud, J. P. Tavernet, M. C. Medina, Dieter Horns, Konrad Bernlöhr, G. Superina, G. Pühlhofer, D. Nekrassov, Werner Hofmann, Michał Ostrowski, Fabio Acero, K. Katarzyński, A. R. Bazer-Bachi, B. Khélifi, German Hermann, Regis Terrier, Catherine Boisson, Christoph Deil, T. Kneiske, D. Gerbig, Gilles Henri, Pierre Brun, D. Nedbal, S. Pita, M. Tluczykont, P. Vincent, Martin Ward, Cameron B Rulten, M. Sikora, Felix Aharonian, Stephen Fegan, T. J. L. McComb, A. Hoffmann, K. Kosack, J. L. Skilton, Łukasz Stawarz, Heinrich J. Völk, C. van Eldik, L. Venter, G. Coignet, M. Hauser, D. Hauser, I. Büsching, A. Cheesebrough, R. Kossakowski, O. Tibolla, L. O'c. Drury, C. Stegmann, I. Jung, R. Steenkamp, B. Rudak, Kathrin Egberts, B. Degrange, G. Heinzelmann, J. Bolmont, Christo Venter, C. Jahn, U. F. Katz, R. Moderski, A. Zech, Reinhard Schlickeiser, Hugh Dickinson, V. Marandon, I. D. Davids, P. M. Chadwick, M. Raue, S. M. Rayner, J. P. Vialle, Guy Pelletier, B. Giebels, A. Förster, Helene Sol, F. M. Schöck, M. Paz Arribas, M. Dalton, A. G. Akhperjanian, A. Shalchi, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), HESS, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Multidisciplinary, 010308 nuclear & particles physics, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, FOS: Physical sciences, Astronomy, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Electromagnetic radiation, Galaxy, 3. Good health, Supernova, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics
Abstract: Starburst galaxies exhibit in their central regions a highly increased rate of supernovae, the remnants of which are thought to accelerate energetic cosmic rays up to energies of ~ 10^15 eV. We report the detection of gamma rays -- tracers of such cosmic rays -- from the starburst galaxy NGC 253 using the H.E.S.S. array of imaging atmospheric Cherenkov telescopes. The gamma-ray flux above 220 GeV is F = (5.5 +/- 1.0stat +/- 2.8sys) x 10^-13 ph. s-1 cm-2, implying a cosmic-ray density about three orders of magnitude larger than that in the center of the Milky Way. The fraction of cosmic-ray energy channeled into gamma rays in this starburst environment is 5 times larger than that in our Galaxy., 24 pages, 8 figures, published in Science Express, see: http://www.sciencemag.org/cgi/content/abstract/1178826
Published: 2009

46. HESS upper limits on very high energy gamma-ray emission from the microquasar GRS 1915+105

Author: O. C. de Jager, S. Vorobiov, M. Vivier, Jim Hinton, G. Fontaine, Michael Punch, Joachim Ripken, Dmitry Khangulyan, M. Kerschhaggl, V. Sahakian, D. Keogh, Michał Ostrowski, Werner Hofmann, Stefan Wagner, Gisela Anton, M. Hauser, G. Pedaletti, J.-P. Lenain, M. K. Daniel, K. J. Orford, Francesca Volpe, A. Hoffmann, B. Nicholas, C. van Eldik, R. C. G. Chaves, Pierre Brun, M. Holleran, S. Hoppe, A. Shalchi, J. F. Glicenstein, A. C. Clapson, Guillaume Dubus, S. J. Nolan, Christian Farnier, D. Göring, Dieter Horns, P. M. Chadwick, Andreas Quirrenbach, S. Schwemmer, Gilles Henri, Frank M. Rieger, I. Büsching, S. Pita, S. Schwarzburg, Andrea Santangelo, A. A. Zdziarski, A. Djannati-Ataï, M. Tluczykont, L.-M. Chounet, M. Panter, D. Klochkov, Reinhard Schlickeiser, Rafal Moderski, Christoph Deil, Y. A. Gallant, T. Kneiske, Nu. Komin, B. Giebels, J. Dyks, A. Cheesebrough, Hugh Dickinson, W. Kluźniak, B. Behera, P. Goret, Jan Conrad, V. Marandon, L. Rob, P.-O. Petrucci, I. D. Davids, B. Khélifi, D. Nekrassov, Yvonne Becherini, G. Hermann, J. L. Skilton, Regis Terrier, W. Domainko, P. H. Tam, L. Fallon, A. Jacholkowska, Anna Szostek, F. Dubois, Christo Venter, D. Nedbal, Marek Sikora, M. Füßling, Petter Hofverberg, E. de Oña Wilhelmi, F. M. Schöck, G. Lamanna, C. Jahn, M. Paz Arribas, Sarah Kaufmann, U. F. Katz, G. Vasileiadis, V. Borrel, A. Zech, Ullrich Schwanke, S. M. Rayner, M. Dalton, L. Gérard, A. Charbonnier, Michal Dyrda, B. Glück, J. P. Vialle, Łukasz Stawarz, H. Sol, Cameron B Rulten, S. Heinz, P. Espigat, Tomasz Bulik, A. G. Akhperjanian, B. C. Raubenheimer, Guy Pelletier, R. Steenkamp, A. Förster, Martin Raue, O. Tibolla, M. Renaud, A. Fiasson, Thomas Lohse, Timothé Boutelier, A. R. Bazer-Bachi, Jacek Niemiec, Heinrich J. Völk, L. O'c. Drury, Olaf Reimer, G. Heinzelmann, Gavin Rowell, J. Bolmont, D. Gerbig, Felix Aharonian, J. Ruppel, Catherine Boisson, Peter Eger, Stephen Fegan, R. de los Reyes, J. Brucker, Emmanuel Moulin, M. Naumann-Godo, F. Stinzing, P. Vincent, C. Stegmann, Martin Ward, Felix Ryde, Iurii Sushch, R. Kossakowski, I. Jung, B. Rudak, Kathrin Egberts, B. Degrange, A. Bochow, S. Rosier-Lees, K. Kosack, Konrad Bernlöhr, G. Superina, G. Pühlhofer, Fabio Acero, Stefan Ohm, J-F. Olive, G. Coignet, K. Katarzyński, M. de Naurois, Alexandre Marcowith, J. Mehault, David Maurin, L. Venter, J.-P. Tavernet, T. J. L. McComb, F. Feinstein, F. Brun, Julien Masbou, Stefano Gabici, U. Barres de Almeida, A. Schönwald, M. C. Medina, Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), HESS, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Context (language use), Astrophysics, 01 natural sciences, Luminosity, law.invention, Telescope, X-rays: binaries, Astrophysical jet, law, individuals: GRS 1915+105 [X-rays], 0103 physical sciences, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, X-rays: individuals: GRS 1915+105, Astroparticle physics, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, Astronomy, observations [gamma rays], Astronomy and Astrophysics, Particle acceleration, Space and Planetary Science, binaries [X-rays], gamma rays: observations
Abstract: Context. High energy particles reside in the relativistic jets of microquasars, making them possible sources of very high energy radiation (VHE, >100 GeV). Detecting this emission would provide a new handle on jet physics. Aims. Observations of the microquasar GRS 1915+105 with the HESS telescope array were undertaken in 2004-2008 to search for VHE emission. Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays. Results. There is no evidence for a VHE gamma-ray signal either from the direction of the microquasar or its vicinity. An upper limit of $6.1\times 10^$ ph cm-2 s-1 (99.9% confidence level) is set on the photon flux above 410 GeV, equivalent to a VHE luminosity of ${\sim} 10^$ erg s-1 at 11 kpc. Conclusions. The VHE to X-ray luminosity ratio in GRS 1915+105 is at least four orders of magnitude lower than the ratio observed in gamma-ray binaries. The VHE radiative efficiency of the compact jet is less than 0.01% based on its estimated total power of 1038 erg s-1. Particle acceleration in GRS 1915+105 is not efficient at high energies and/or the magnetic field is too strong. It is also possible that VHE gamma-rays are produced by GRS 1915+105, but the emission is highly time-dependent.
Published: 2009

47. HESS observations of $\gamma$-ray bursts in 2003-2007

Author: F. Aharonian, A. G. Akhperjanian, U. Barres de Almeida, A. R. Bazer-Bachi, B. Behera, W. Benbow, K. Bernlöhr, C. Boisson, A. Bochow, V. Borrel, I. Braun, E. Brion, J. Brucker, P. Brun, R. Bühler, T. Bulik, I. Büsching, T. Boutelier, S. Carrigan, P. M. Chadwick, A. Charbonnier, R. C. G. Chaves, A. Cheesebrough, L.-M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C. Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, C. Hadjichristidis, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. de Jager, I. Jung, K. Katarzyński, S. Kaufmann, E. Kendziorra, M. Kerschhaggl, D. Khangulyan, B. Khélifi, D. Keogh, Nu. Komin, K. Kosack, G. Lamanna, J.-P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J. L. McComb, M. C. Medina, R. Moderski, E. Moulin, M. Naumann-Godo, M. de Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J.-F. Olive, E. de Oña Wilhelmi, K. J. Orford, J. L. Osborne, M. Ostrowski, M. Panter, G. Pedaletti, G. Pelletier, P.-O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, J. L. Skilton, H. Sol, D. Spangler, Ł. Stawarz, R. Steenkamp, C. Stegmann, G. Superina, P. H. Tam, J.-P. Tavernet, R. Terrier, O. Tibolla, C. van Eldik, G. Vasileiadis, C. Venter, L. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, and A. Zech
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, bursts [gamma rays], observations [gamma rays], Astronomy and Astrophysics, Astrophysics, Photon energy, 01 natural sciences, Redshift, Space and Planetary Science, 0103 physical sciences, Background light, Gamma-ray burst, 010303 astronomy & astrophysics, Cherenkov radiation
Abstract: Very-high-energy (VHE; >~100 GeV) gamma-rays are expected from gamma-ray bursts (GRBs) in some scenarios. Exploring this photon energy regime is necessary for understanding the energetics and properties of GRBs. GRBs have been one of the prime targets for the H.E.S.S. experiment, which makes use of four Imaging Atmospheric Cherenkov Telescopes (IACTs) to detect VHE gamma-rays. Dedicated observations of 32 GRB positions were made in the years 2003-2007 and a search for VHE gamma-ray counterparts of these GRBs was made. Depending on the visibility and observing conditions, the observations mostly start minutes to hours after the burst and typically last two hours. Results from observations of 22 GRB positions are presented and evidence of a VHE signal was found neither in observations of any individual GRBs, nor from stacking data from subsets of GRBs with higher expected VHE flux according to a model-independent ranking scheme. Upper limits for the VHE gamma-ray flux from the GRB positions were derived. For those GRBs with measured redshifts, differential upper limits at the energy threshold after correcting for absorption due to extra-galactic background light are also presented.
Published: 2009

48. Very high energy gamma-ray observations of the galaxy clusters Abell 496 and Abell 85 with H.E.S.S

Author: F. Aharonian, A. G. Akhperjanian, G. Anton, U. Barres de Almeida, A. R. Bazer-Bachi, Y. Becherini, B. Behera, K. Bernlöhr, C. Boisson, A. Bochow, V. Borrel, I. Braun, E. Brion, J. Brucker, P. Brun, R. Bühler, T. Bulik, I. Büsching, T. Boutelier, P. M. Chadwick, A. Charbonnier, R. C. G. Chaves, A. Cheesebrough, L.-M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, M. K. Daniel, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C. Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. de Jager, I. Jung, K. Katarzyński, U. Katz, S. Kaufmann, E. Kendziorra, M. Kerschhaggl, D. Khangulyan, B. Khélifi, D. Keogh, Nu. Komin, K. Kosack, G. Lamanna, J.-P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J. L. McComb, M. C. Medina, R. Moderski, E. Moulin, M. Naumann-Godo, M. de Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J.-F. Olive, E. de Oña Wilhelmi, K. J. Orford, M. Ostrowski, M. Panter, M. Paz Arribas, G. Pedaletti, G. Pelletier, P.-O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, J. L. Skilton, H. Sol, D. Spangler, Ł. Stawarz, R. Steenkamp, C. Stegmann, G. Superina, A. Szostek, P. H. Tam, J.-P. Tavernet, R. Terrier, O. Tibolla, C. van Eldik, G. Vasileiadis, C. Venter, L. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), HESS, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, IACT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma rays: observations, 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, Abell 85, Physics, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma ray, observations [gamma rays], Astronomy and Astrophysics, Galaxy, Space and Planetary Science, clusters: individual: Abell 496 [galaxies], Galaxies: clusters: individual: Abell 496, clusters: individual: Abell 85 [galaxies]
Abstract: Aims: The nearby galaxy clusters Abell 496 and Abell 85 are studied in the very high energy (VHE, E > 100 GeV) band to investigate VHE cosmic rays (CRs) in this class of objects which are the largest gravitationally bound systems in the Universe. Methods: H.E.S.S., an array of four Imaging Atmospheric Cherenkov Telescopes (IACT), is used to observe the targets in the range of VHE gamma rays. Results: No significant gamma-ray signal is found at the respective position of the two clusters with several different source size assumptions for each target. In particular, emission regions corresponding to the high density core, to the extension of the entire X-ray emission in these clusters, and to the very extended region where the accretion shock is expected, are investigated. Upper limits are derived for the gamma-ray flux at energies E>570 GeV for Abell 496 and E>460 GeV for Abell 85. Conclusions: From the non-detection in VHE gamma rays, upper limits on the total energy of hadronic CRs in the clusters are calculated. If the cosmic-ray energy density follows the large scale gas density profile, the limit on the fraction of energy in these non-thermal particles with respect to the total thermal energy of the intra-cluster medium (ICM) is 51% for Abell 496 and only 8% for Abell 85 due to its larger mass and higher gas density. These upper limits are compared with theoretical estimates. They predict about ~10% of the thermal energy of the ICM in non-thermal particles. The observations presented here can constrain these predictions especially for the case of the Abell 85 cluster., 11 pages, 4 figures, accepted for publication in A&A
Published: 2009

49. Simultaneous multiwavelength observations of the second exceptional $\gamma$-ray flare of PKS 2155–304 in July 2006

Author: F. Aharonian, A. G. Akhperjanian, G. Anton, U. Barres de Almeida, A. R. Bazer-Bachi, Y. Becherini, B. Behera, W. Benbow, K. Bernlöhr, C. Boisson, A. Bochow, V. Borrel, E. Brion, J. Brucker, P. Brun, R. Bühler, T. Bulik, I. Büsching, T. Boutelier, P. M. Chadwick, A. Charbonnier, R. C. G. Chaves, A. Cheesebrough, L.-M. Chounet, A. C. Clapson, G. Coignet, L. Costamante, M. Dalton, M. K. Daniel, I. D. Davids, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C. Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, D. Göhring, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. de Jager, C. Jahn, I. Jung, K. Katarzyński, U. Katz, S. Kaufmann, E. Kendziorra, M. Kerschhaggl, D. Khangulyan, B. Khélifi, D. Keogh, W. Kluźniak, T. Kneiske, Nu. Komin, K. Kosack, G. Lamanna, J.-P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J. L. McComb, M. C. Medina, R. Moderski, L. A. G. Monard, E. Moulin, M. Naumann-Godo, M. de Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J.-F. Olive, E. de Oña Wilhelmi, K. J. Orford, M. Ostrowski, M. Panter, M. Paz Arribas, G. Pedaletti, G. Pelletier, P.-O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, M. Sikora, J. L. Skilton, H. Sol, D. Spangler, Ł. Stawarz, R. Steenkamp, C. Stegmann, G. Superina, A. Szostek, P. H. Tam, J.-P. Tavernet, R. Terrier, O. Tibolla, M. Tluczykont, C. van Eldik, G. Vasileiadis, C. Venter, L. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Flux (metallurgy), law, 0103 physical sciences, 010303 astronomy & astrophysics, PKS 2155-304, Physics, 010308 nuclear & particles physics, Gamma ray, observations [gamma rays], Astronomy and Astrophysics, Light curve, galaxies [X-rays], Space and Planetary Science, active [galaxies], BL Lacertae objects: individual: PKS 2155–304 [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, Flare, BL Lac object
Abstract: Simultaneous HESS/CHANDRA/optical observations were performed on the BL Lac object PKS 2155-304 in the night of July 29-30 2006, when the source underwent its second major gamma-ray outburst in Summer 2006. This event took place about 44 hours after the July 28 outburst, known for its ultrafast variability. An unprecedented 6 to 8 hours of uninterrupted coverage was achieved, with spectra and light curves measured down to 7 and 2-minute timescales, respectively. The gamma-ray flux reached a maximum of 11x the Crab flux (>400 GeV), with rise/decay timescales of ~1 hour, plus a few smaller-amplitude flares superimposed on the decaying phase. The emission in the X-ray and VHE bands is strongly correlated, both in flux and spectrum, with no evidence of lags. The VHE spectrum shows a curvature that is variable with time and stronger at higher fluxes. The huge VHE variations (22x) are only accompanied by small-amplitude X-ray and optical variations (factor 2 and 15% respectively). The source has shown for the first time in an HBL a large Compton dominance (L_C/L_S ~10) -- rapidly evolving -- and a cubic relation between VHE and X-ray flux variations, during a decaying phase. These results challenge the common scenarios for the TeV-blazar emission., 22 pages, 16 figures, accepted for publication in A&A
Published: 2009

50. Discovery of very high energy $\gamma$-ray emission from Centaurus A with H.E.S.S

Author: F. Aharonian, A. G. Akhperjanian, G. Anton, U. Barres de Almeida, A. R. Bazer-Bachi, Y. Becherini, B. Behera, W. Benbow, K. Bernlöhr, C. Boisson, A. Bochow, V. Borrel, E. Brion, J. Brucker, P. Brun, R. Bühler, T. Bulik, I. Büsching, T. Boutelier, P. M. Chadwick, A. Charbonnier, R. C. G. Chaves, A. Cheesebrough, L.-M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, M. K. Daniel, I. D. Davids, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C. Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J.-F. Glicenstein, B. Glück, P. Goret, D. Göhring, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. de Jager, C. Jahn, I. Jung, K. Katarzyński, U. Katz, S. Kaufmann, E. Kendziorra, M. Kerschhaggl, D. Khangulyan, B. Khélifi, D. Keogh, W. Kluźniak, T. Kneiske, Nu. Komin, K. Kosack, G. Lamanna, I. J. Latham, J.-P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J. L. McComb, M. C. Medina, R. Moderski, E. Moulin, M. Naumann-Godo, M. de Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J.-F. Olive, E. de Oña Wilhelmi, K. J. Orford, M. Ostrowski, M. Panter, M. Paz Arribas, G. Pedaletti, G. Pelletier, P.-O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, M. Sikora, J. L. Skilton, H. Sol, D. Spangler, Ł. Stawarz, R. Steenkamp, C. Stegmann, G. Superina, A. Szostek, P. H. Tam, J.-P. Tavernet, R. Terrier, O. Tibolla, M. Tluczykont, C. van Eldik, G. Vasileiadis, C. Venter, L. Venter, J. P. Vialle, P. Vincent, J. Vink, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Centaurus A, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], individual (Cen A) [galaxies], 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Gamma ray, observations [gamma rays], Astronomy and Astrophysics, Cherenkov Telescope Array, Particle acceleration, Crab Nebula, Space and Planetary Science, active [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the discovery of faint very high energy (VHE, E>100 GeV) gamma-ray emission from the radio galaxy Centaurus A in observations performed with the H.E.S.S. experiment, an imaging atmospheric Cherenkov telescope array consisting of four telescopes located in Namibia. Centaurus A has been observed for more than 120 h. A signal with a statistical significance of 5.0 sigma is detected from the region including the radio core and the inner kpc jets. The integral flux above an energy threshold of ~250 GeV is measured to be ~0.8 % of the flux of the Crab Nebula (apparent luminosity: L(>250 GeV)~2.6x10^39 erg s^-1, adopting a distance of 3.8 Mpc. The spectrum can be described by a power law with a photon index of 2.7 +/- 0.5_stat +/- 0.2_sys. No significant flux variability is detected in the data set. However, the low flux only allows detection of variability on the timescale of days to flux increments above a factor of ~15-20 (3 sigma and 4 sigma, respectively). The discovery of VHE gamma-ray emission from Centaurus A reveals particle acceleration in the source to >TeV energies and, together with M 87, establishes radio galaxies as a class of VHE emitters., 5 pages, 4 figures, accepted for publication in ApJ Letters
Published: 2009

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