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51. 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
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52. Multiwavelength observations of the blazar 1ES 1011+496 in Spring 2008

Author: Pierre Colin, E. de Oña Wilhelmi, Kari Nilsson, L. Maraschi, M. Will, Francesco Longo, Tomislav Terzić, Daniela Dorner, C. Pittori, Michael T. Carini, R. Clavero, Louis Antonelli, E. Prandini, Pratik Majumdar, M. V. Fonseca, Mosè Mariotti, K. Kodani, J. Becerra González, W. Bednarek, M. Makariev, M. Palatiello, Ievgen Vovk, Fabrizio Tavecchio, S. N. Shore, M. Gaug, J. Herrera, J. Palacio, J. M. Paredes, Koji Noda, F. Di Pierro, Antonio Stamerra, Thomas Bretz, Elisa Bernardini, Stefano Covino, T. Schweizer, R. Zanin, D. Dominis Prester, A.-K. Overkemping, Adrian Biland, B. Biasuzzi, R. López-Coto, Juri Poutanen, Nikola Godinovic, R. Reinthal, Benito Marcote, Jose Luis Contreras, Saverio Lombardi, S. Rügamer, Marcel Strzys, R. Walters, Junko Kushida, D. Nakajima, Francesco Dazzi, Juan Abel Barrio, A. Niedzwiecki, P. Da Vela, Juan Cortina, Y. Hanabata, S. Bonnefoy, J. Rico, A. González Muñoz, Razmik Mirzoyan, Oscar Blanch, U. Barres de Almeida, P. Antoranz, Tomoki Saito, D. Tescaro, K. Frantzen, P. Temnikov, E. Colombo, Damir Lelas, K. Mallot, David Paneque, J. Sainio, Arka Chatterjee, M. Hayashida, R. J. García López, L. O. Takalo, Kyoshi Nishijima, Wolfgang Rhode, M. H. Wu, D. Guberman, Dorota Sobczyńska, D. Fidalgo, Gareth Hughes, E. Carmona, Markus Garczarczyk, P. G. Prada Moroni, Anne Lähteenmäki, A. De Angelis, Andrei Berdyugin, A. Pease, S. Paiano, Masahiro Teshima, A. Treves, Vitaly Neustroev, D. Garrido Terrats, G. De Caneva, Alba Fernández-Barral, Stefano Ansoldi, Karl Mannheim, Elina Lindfors, M. I. Martínez, Julian Sitarek, Julia Thaele, Riccardo Paoletti, W. Idec, Massimo Persic, C. Schultz, V. Scapin, Yusuke Konno, F. Lucarelli, Daniel Mazin, Marina Manganaro, Marc Ribó, G. Maneva, T. Toyama, S. Vercellone, D. Galindo, Merja Tornikoski, J. E. Ward, Alicia López-Oramas, Ana Babić, Sabrina Einecke, P. Bangale, Reiko Orito, J. Rodriguez Garcia, Christian Fruck, Hidetoshi Kubo, B. De Lotto, A. La Barbera, Konstancja Satalecka, Michele Doro, X. Paredes-Fortuny, J. Hose, D. Elsaesser, M. Nievas Rosillo, H. Takami, B. Banerjee, D. Glawion, Vassil Verguilov, U. Menzel, Diego F. Torres, M. Pasanen, Abelardo Moralejo, A. Sillanpää, T. Steinbring, Ll. Font, I. Snidaric, E. Lorenz, Max Ludwig Ahnen, P. Giammaria, G. Bonnoli, Dario Hrupec, M. A. Lopez, F. Borracci, C. Delgado Mendez, Alessandro Carosi, Jose Miguel Miranda, Ivica Puljak, Glawion, D., 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., Carmona, E., 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 Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., 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., Guberman, D., 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., Lorenz, E., 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., 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., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Rügamer, S., Saito, T., Satalecka, K., Scapin, V., 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., Lucarelli, F., Pittori, C., Vercellone, S., Berdyugin, A., Carini, M. T., Lähteenmäki, A., Pasanen, M., Pease, A., Sainio, J., Tornikoski, M., Walters, R., Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University
Subjects: galaxie [X-rays], galaxie [Gamma-rays], Radiation mechanisms: non-thermal, radiation mechanisms: non-thermal, galaxies: active, gamma-rays, galaxies, X-rays: galaxies, BL-LACERTAE OBJECTS, ACTIVE GALACTIC NUCLEI, LARGE-AREA TELESCOPE, GAMMA-RAY EMISSION, SPECTRAL ENERGY-DISTRIBUTIONS, ALL-SKY SURVEY, LAC, OBJECTS, X-RAY, MAGIC TELESCOPES, SOURCE CATALOG, Astrophysics, Galaxies: active, Gamma-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, 01 natural sciences, Radiació, law.invention, law, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Radiation, Gamma ray, galaxies [Gamma-rays], galaxies [X-rays], Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, BL Lac object, Active galactic nucleus, radiation mechanisms, non-thermal galaxies, active gamma-rays, galaxies X-rays, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 0103 physical sciences, Blazar, ta115, non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysic, Light curve, Galàxies actives, Active galaxies, ddc:520
Abstract: The BL Lac object 1ES 1011+496 was discovered at Very High Energy gamma-rays by MAGIC in spring 2007. Before that the source was little studied in different wavelengths. Therefore a multi-wavelength (MWL) campaign was organized in spring 2008. Along MAGIC, the MWL campaign included the Metsahovi radio observatory, Bell and KVA optical telescopes and the Swift and AGILE satellites. MAGIC observations span from March to May, 2008 for a total of 27.9 hours, of which 19.4 hours remained after quality cuts. The light curve showed no significant variability. The differential VHE spectrum could be described with a power-law function. Both results were similar to those obtained during the discovery. Swift XRT observations revealed an X-ray flare, characterized by a harder when brighter trend, as is typical for high synchrotron peak BL Lac objects (HBL). Strong optical variability was found during the campaign, but no conclusion on the connection between the optical and VHE gamma-ray bands could be drawn. The contemporaneous SED shows a synchrotron dominated source, unlike concluded in previous work based on nonsimultaneous data, and is well described by a standard one zone synchrotron self Compton model. We also performed a study on the source classification. While the optical and X-ray data taken during our campaign show typical characteristics of an HBL, we suggest, based on archival data, that 1ES 1011+496 is actually a borderline case between intermediate and high synchrotron peak frequency BL Lac objects., 13 pages, accepted for publication in MNRAS
Published: 2016
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53. Insights into the emission of the blazar 1ES 1011+496 through unprecedented broadband observations during 2011 and 2012

Author: Daniela Dorner, E. Prandini, Iain A. Steele, Francesco Dazzi, M. Gaug, J. Herrera, A. Fernández-Barral, M. V. Fonseca, Koji Noda, Elisa Bernardini, E. Colombo, F. Di Pierro, S. Bonnefoy, M. Makariev, Talvikki Hovatta, Ivica Puljak, Pierre Colin, L. O. Takalo, D. Garrido Terrats, J. L. Richards, E. de Oña Wilhelmi, Roberta Zanin, Mosè Mariotti, A.-K. Overkemping, D. Eisenacher, E. Carmona, Markus Garczarczyk, J. Krause, B. De Lotto, Natalia Lewandowska, P. Da Vela, D. Nakajima, M. Hayashida, V. Scalzotto, U. Menzel, R. Reinthal, Juan Abel Barrio, Carole Mundell, Razmik Mirzoyan, U. Barres de Almeida, Abelardo Moralejo, Damir Lelas, K. Nishijima, Saverio Lombardi, P. G. Prada Moroni, Michele Palatiello, T. Schweizer, C. Delgado Mendez, T. Steinbring, P. Temnikov, D. Fidalgo, Anthony C. S. Readhead, Hanna Kellermann, M. I. Martínez, P. Bangale, Dorota Sobczyńska, A. De Angelis, A. Treves, Vitaly Neustroev, D. Dominis Prester, Francesco Longo, A. La Barbera, Juri Poutanen, Ana Babić, Stefano Ansoldi, Sabrina Einecke, S. R. Gozzini, Stefano Covino, Riccardo Paoletti, Nikola Godinovic, Benito Marcote, Elizaveta Rastorgueva-Foi, M. Strzys, Yusuke Konno, Y. Hanabata, Marc Ribó, J. Rodriguez Garcia, M. Nievas Rosillo, Jelena Aleksić, Kazuo Saito, J. Kushida, P. Antoranz, M. L. Knoetig, R. López-Coto, Diego F. Torres, G. Maneva, Antonio Stamerra, A. Niedzwiecki, Hidetoshi Kubo, S. N. Shore, X. Paredes-Fortuny, Jose Luis Contreras, Adrian Biland, Alessandro Carosi, W. Idec, David Sánchez, B. Biasuzzi, D. Tescaro, Tuomas Savolainen, David Paneque, P. Munar-Adrover, Julian Sitarek, K. Frantzen, J. Rico, I. Lozano, C. Fruck, T. Toyama, G. De Caneva, Juan Cortina, Anne Lähteenmäki, Oscar Blanch, K. Kodani, Masahiro Teshima, D. Hadasch, V. Kadenius, Elina Lindfors, Merja Tornikoski, Alexander B. Pushkarev, Daniel Mazin, Matthew L. Lister, Julia Thaele, Konstancja Satalecka, Louis Antonelli, Michele Doro, S. Paiano, Joni Tammi, F. D'Ammando, G. Bonnoli, K. Mallot, Karl Mannheim, Jose Miguel Miranda, R. J. García López, J. Hose, Massimo Persic, A. Sillanpää, D. Elsaesser, Takashi Saito, H. Takami, Eckart Lorenz, Alicia López-Oramas, V. Scapin, Reiko Orito, D. Galindo, J. Becerra González, Dario Hrupec, M. A. Lopez, F. Borracci, J. M. Paredes, A. González Mu. noz, Yuri Y. Kovalev, Kari Nilsson, S. Buson, M. Will, C. Arcaro, I. Snidaric, Thomas Bretz, L. Maraschi, Walter Max-Moerbeck, Tomislav Terzić, Wolfgang Rhode, Patrick Vogler, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Aleksic J, Ansoldi S, Antonelli LA, Antoranz P, Arcaro C, Babic A, 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, Carmona E, Carosi A, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi F, De Angelis A, De Caneva G, De Lotto B, Wilhelmi ED, Mendez CD, Di Pierro F, Prester DD, Dorner D, Doro M, Einecke S, Eisenacher D, Elsaesser D, Fernandez-Barral A, Fidalgo D, Fonseca MV, Font L, Frantzen K, Fruck C, Galindo D, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Godinovic N, Munoz AG, Gozzini SR, Hadasch D, Hanabata Y, Hayashida M, Herrera J, Hose J, Hrupec D, Idec W, Kadenius V, Kellermann H, Knoetig ML, Kodani K, Konno Y, Krause J, Kubo H, Kushida J, La Barbera A, Lelas D, Lewandowska N, Lindfors E, Lombardi S, Longo F, Lopez M, Lopez-Coto R, Lopez-Oramas A, Lorenz E, Lozano I, Makariev M, Mallot K, Maneva G, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Miranda JM, Mirzoyan R, Moralejo A, Munar-Adrover P, Nakajima D, Neustroev V, Niedzwiecki A, Rosillo MN, Nilsson K, Nishijima K, Noda K, Orito R, Overkemping A, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Persic M, Poutanen J, Moroni PGP, Prandini E, Puljak I, Reinthal R, Rhode W, Ribo M, Rico J, Garcia JR, Saito T, Saito K, Satalecka K, Scalzotto V, Scapin V, Schweizer T, Shore SN, 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, Vogler P, Will M, Zanin R, Buson S, DAmmando F, Lateenmaki A, Hovatta T, Kovalev YY, Lister ML, Max-Moerbeck W, Mundell C, Pushkarev AB, Rastorgueva-Foi E, Readhead ACS, Richards JL, Tammi J, Sanchez DA, Tornikoski M, Savolainen T, Steele I, Autonomous University of Barcelona, University of Udine, INAF, Osservatorio Astronomico di Roma, University of Siena, University of Padova, University of Rijeka, Max Planck Institute for Physics, Centro Brasileiro de Pesquisas Físicas, Complutense University, University of Maryland, College Park, University of Łódź, Deutsches Elektronen-Synchrotron, Swiss Federal Institute of Technology Zurich, University of Würzburg, CIEMAT, Instituto de Astrofísica de Canarias, Institute of Space Studies of Catalonia, Technische Universität Dortmund, University of Barcelona, Kyoto University, Finnish MAGIC Consortium, Institute for Nuclear Research and Nuclear Energy, Japanese MAGIC Consortium, University of Turku, University of Pisa, Max-Planck-Institut für Physik, ICREA, University of Insubria, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Department of Radio Science and Engineering, California Institute of Technology, Lebedev Physical Institute, Purdue University, National Radio Astronomy Observatory Socorro, University of Liverpool, Crimean Astrophysical Observatory, Max Planck Institute for Radio Astronomy, Metsähovi Radio Observatory, Université Savoie Mont Blanc, Max-Planck-Institut für Radioastronomie, Aalto-yliopisto, Aalto University, Aleksić, J., Ansoldi, S., Antonelli, L. A., Antoranz, P., Arcaro, C, Babic, A., 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., Carmona, E., Carosi, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, 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., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadasch, D., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Kodani, K., Konno, Y., Krause, J., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., 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., Vogler, P., Will, M., Zanin, R., Buson, S., D'Ammando, F., Lähteenmäki, A., Hovatta, T., Kovalev, Y. Y., Lister, M. L., Max Moerbeck, W., Mundell, C., Pushkarev, A. B., Rastorgueva Foi, E., Readhead, A. C. S., Richards, J. L., Tammi, J., Sanchez, D. A., Tornikoski, M., Savolainen, T., Steele, I., 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), and Universitat de Barcelona
Subjects: Photon, jets [galaxies], Astrophysics, 7. Clean energy, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, law, BL Lacertae objects: individual: 1ES 1011+496, galaxies: active, galaxies: jets, gamma rays: galaxies, radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, individual: 1ES 1011+496 [BL Lacertae objects], 010303 astronomy & astrophysics, QC, QB, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Superluminal motion, TEV BLAZARS, Polarization (waves), non-thermal [radiation mechanisms], Cosmology, BL-LACERTAE OBJECTS, ACTIVE GALACTIC NUCLEI, GAMMA-RAY EMISSION, X-RAY, LAC OBJECTS, MAGIC TELESCOPE, CRAB-NEBULA, ENERGY-DISTRIBUTION, active [galaxies], galaxies [gamma rays], Spectral energy distribution, Degree of polarization, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, 0103 physical sciences, galaxie [gamma rays], Blazar, Cosmologia, 010308 nuclear & particles physics, Astronomy and Astrophysic, Position angle, Galaxies, Galàxies, jet [galaxies], ddc:520, BL Lacertae objects: individual: 1ES 1011+496 – galaxies: active – galaxies: jets – radiation mechanisms: non-thermal – gamma rays: galaxies
Abstract: 1ES 1011+496 $(z=0.212)$ was discovered in very high energy (VHE, E >100 GeV) $\gamma$-rays with MAGIC in 2007. The absence of simultaneous data at lower energies led to a rather incomplete characterization of the broadband spectral energy distribution (SED). We study the source properties and the emission mechanisms, probing whether a simple one-zone synchrotron-self-Compton (SSC) scenario is able to explain the observed broadband spectrum. We analyzed VHE to radio data from 2011 and 2012 collected by MAGIC, $Fermi$-LAT, $Swift$, KVA, OVRO, and Mets\"ahovi in addition to optical polarimetry data and radio maps from the Liverpool Telescope and MOJAVE. The VHE spectrum was fit with a simple power law with a photon index of $3.69\pm0.22$ and a flux above 150 GeV of $(1.46\pm0.16)\times10^{-11}$ ph cm$^{-2}$ s$^{-1}$. 1ES 1011+496 was found to be in a generally quiescent state at all observed wavelengths, showing only moderate variability from radio to X-rays. A low degree of polarization of less than 10% was measured in optical, while some bright features polarized up to 60% were observed in the radio jet. A similar trend in the rotation of the electric vector position angle was found in optical and radio. The radio maps indicated a superluminal motion of $1.8\pm0.4\,c$, which is the highest speed statistically significantly measured so far in a high-frequency-peaked BL Lac. For the first time, the high-energy bump in the broadband SED of 1ES 1011+496 could be fully characterized from 0.1 GeV to 1 TeV which permitted a more reliable interpretation within the one-zone SSC scenario. The polarimetry data suggest that at least part of the optical emission has its origin in some of the bright radio features, while the low polarization in optical might be due to the contribution of parts of the radio jet with different orientations of the magnetic field to the optical emission., Comment: 14 pages, 7 figures
Published: 2016
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54. Blue Fermi flat spectrum radio quasars

Author: Tullia Sbarrato, Luigi Foschini, L. Maraschi, Gabriele Ghisellini, Giancarlo Ghirlanda, and Fabrizio Tavecchio
Subjects: Physics, Spectral index, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Luminosity, Space and Planetary Science, Radiative transfer, Emission spectrum, Blazar, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: Many blazars detected by the Fermi satellite, observed spectroscopically in the optical, are line-less, and have been classified as BL Lac objects. Optical-UV photometry of nearly one hundred of them allowed to determine the redshift for a handful of objects and redshift upper limits for the great majority. A few of these are candidates to be "blue quasars", namely flat spectrum radio quasars whose broad emission lines are hidden by an overwhelming synchrotron emission peaking in the UV. This implies that the emitting electrons have high energies. In turn, this requires relatively weak radiative cooling, a condition that can be met if the main radiative dissipation of the jet power occurs outside the broad line region. We confirm this hypothesis by studying and modelling the spectral energy distributions of the 4 "blue quasars" recently discovered. Furthermore, we discuss the distribution of Fermi blazars in the gamma-ray spectral index -- gamma-ray luminosity plane, and argue that "blue quasars" objects are a minority within the blazar populations.
Published: 2012
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55. γ-ray variability of radio-loud narrow-line Seyfert 1 galaxies

Author: Luigi Foschini, L. Maraschi, Fabrizio Tavecchio, R. Decarli, M. Colpi, G. Tagliaferri, Giorgio Calderone, and G. Ghisellini
Subjects: Physics, Jet (fluid), Line-of-sight, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Galaxy, Space and Planetary Science, Blazar, Astrophysics::Galaxy Astrophysics, Line (formation), Fermi Gamma-ray Space Telescope
Abstract: The recent detection of gamma-ray emission from four radio-loud narrow-line Seyfert 1 galaxies suggests that the engine driving the AGN activity of these objects share some similarities with that of blazars, namely the presence of a gamma-ray emitting, variable, jet of plasma closely aligned to the line of sight. In this work we analyze the gamma-ray light curves of the four radio-loud narrow-line Seyfert 1 galaxies for which high-energy gamma-ray emission has been discovered by Fermi/LAT, in order to study their variability. We find significant flux variability in all the sources. This allows us to exclude a starburst origin of the gamma-ray photons and confirms the presence of a relativistic jet. Furthermore we estimate the minimum e-folding variability timescale (3 - 30 days) and infer an upper limit for the size of the emitting region (0.2 - 2 pc, assuming a relativistic Doppler factor delta=10 and a jet aperture of theta=0.1 rad).
Published: 2011
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56. The power of relativistic jets is larger than the luminosity of their accretion disks

Author: Gabriele Ghisellini, Fabrizio Tavecchio, L. Maraschi, A. Celotti, Tullia Sbarrato, Ghisellini, G, Tavecchio, F, Maraschi, L, Celotti, A, and Sbarrato, T
Subjects: Active galactic nucleus, X-ray burster, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, magnetic field, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Article, Settore FIS/05 - Astronomia e Astrofisica, Astrophysical jet, luminescence, Astrophysics::Solar and Stellar Astrophysics, Blazar, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, Supermassive black hole, Multidisciplinary, luminance, field emission, Astronomy, Quasar, simulation, physical parameters, Accretion (astrophysics), astronomy, Rotating black hole, jet stream, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, energy
Abstract: Theoretical models for the production of relativistic jets from active galactic nuclei predict that jet power arises from the spin and mass of the central black hole, as well as the magnetic field near the event horizon. The physical mechanism mechanism underlying the contribution from the magnetic field is the torque exerted on the rotating black hole by the field amplified by the accreting material. If the squared magnetic field is proportional to the accretion rate, then there will be a correlation between jet power and accretion luminosity. There is evidence for such a correlation, but inadequate knowledge of the accretion luminosity of the limited and inhomogeneous used samples prevented a firm conclusion. Here we report an analysis of archival observations of a sample of blazars (quasars whose jets point towards Earth) that overcomes previous limitations. We find a clear correlation between jet power as measured through the gamma-ray luminosity, and accretion luminosity as measured by the broad emission lines, with the jet power dominating over the disk luminosity, in agreement with numerical simulations. This implies that the magnetic field threading the black hole horizon reaches the maximum value sustainable by the accreting matter., 22 pages, 5 figures. Published in Nature, 515, 376
Published: 2014
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57. SWIFTBURST ALERT TELESCOPE,FERMILARGE AREA TELESCOPE, AND THE BLAZAR SEQUENCE

Author: Davide Donato, N. Gehrels, R. M. Sambruna, J. Tueller, R. F. Mushotzky, L. Maraschi, W. H. Baumgartner, C. B. Markwardt, Marco Ajello, G. K. Skinner, and Scott Barthelmy
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Radio spectrum, Luminosity, law.invention, Telescope, Space and Planetary Science, law, Blazar, Fermi Gamma-ray Space Telescope
Abstract: Using public Fermi Large Area Telescope (LAT) and Swift Burst Alert Telescope observations, we constructed the first sample of blazars selected at both hard X-rays and gamma rays. Studying its spectral properties, we find a luminosity dependence of the spectral slopes at both energies. Specifically, luminous blazars, generally classified as flat spectrum radio quasars, have hard continua in the medium-hard X-ray range but soft continua in the LAT gamma-ray range (photon indices GAMMA{sub X} {approx} 2), while lower luminosity blazars, classified as BL Lacs, have opposite behavior, i.e., soft X-ray and hard gamma-ray continua (GAMMA{sub X} {approx}> 2.4 and GAMMA{sub G} < 2). The trends are confirmed by detailed Monte Carlo simulations explicitly taking into account the observational biases of both instruments. Our results support the so-called blazar sequence which was originally based on radio samples of blazars and radio luminosities. We also argue that the X-ray-to-gamma-ray continua of blazars may provide independent insights into the physical conditions around the jet, complementing/superseding the ambiguities of the traditional classification based on optical properties.
Published: 2010
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58. General physical properties of bright Fermi blazars

Author: Gabriele Ghisellini, Annalisa Celotti, L. Maraschi, Fabrizio Tavecchio, Luigi Foschini, and Giancarlo Ghirlanda
Subjects: Physics, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Luminosity, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Satellite, Blazar, Astrophysics::Galaxy Astrophysics, Line (formation), Fermi Gamma-ray Space Telescope
Abstract: We studied all blazars of known redshift detected by the Fermi satellite during its first three months survey. For the majority of them, pointed Swift observations ensures a good multiwavelength coverage, enabling us to to reliably construct their spectral energy distributions (SED). We model the SEDs using a one-zone leptonic model and study the distributions of the derived interesting physical parameters as a function of the observed gamma-ray luminosity. We confirm previous findings concerning the relation of the physical parameters with source luminosity which are at the origin of the blazar sequence. The SEDs allow to estimate the luminosity of the accretion disk for the majority of broad emitting line blazars, while for the line-less BL Lac objects in the sample upper limits can be derived. We find a positive correlation between the jet power and the luminosity of the accretion disk in broad line blazars. In these objects we argue that the jet must be proton-dominated, and that the total jet power is of the same order of (or slightly larger than) the disk luminosity. We discuss two alternative scenarios to explain this result.
Published: 2009
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59. A Kiloparsec‐Scale X‐Ray Jet in the BL Lac Source S5 2007+777

Author: Rita M. Sambruna, L. Maraschi, C. C. Cheung, Fabrizio Tavecchio, and Davide Donato
Subjects: Physics, education.field_of_study, Line-of-sight, Photon, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Population, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Electron, Astrophysics, Magnetic field, Space and Planetary Science, education, Equipartition theorem
Abstract: X-ray jets in AGNs are commonly observed in FR II and FR I radio galaxies, but rarely in BL Lac objects, most probably due to their orientation close to the line of sight and the ensuing foreshortening effects. Only three BL Lac objects are known so far to contain a kpc-scale X-ray jet. In this paper we present the evidence for the existence of a fourth extended X-ray jet in the classical radio-selected source S5 2007+777, which for its hybrid FR I and FR II radio morphology has been classified as a HYMOR (HYbrid MOrphology Radio source). Our Chandra ACIS-S observations of this source revealed an X-ray counterpart to the 19'' long radio jet. Interestingly, the X-ray properties of the kpc-scale jet in S5 2007+777 are very similar to those observed in FR II jets. First, the X-ray morphology closely mirrors the radio one, with the X-rays being concentrated in the discrete radio knots. Second, the X-ray continuum of the jet/brightest knot is described by a very hard power law, with photon index ΓX ~ 1, although the uncertainties are large. Third, the optical upper limit from archival HST data implies a concave radio-to-X-ray SED. If the X-ray emission is attributed to IC/CMB with equipartition, strong beaming (δ = 13) is required, implying a very large scale (Mpc) jet. The beaming requirement can be somewhat relaxed assuming a magnetic field lower than equipartition. Alternatively, synchrotron emission from a second population of very high-energy electrons is viable. Comparison to other HYMOR jets detected with Chandra is discussed, as well as general implications for the origin of the FR I/FR II division.
Published: 2008
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60. TOWARDS A UNITARIAN VIEW OF CHANDRA JETS

Author: L. Maraschi, R. M. Sambruna, and Fabrizio Tavecchio
Subjects: Physics, Jet (fluid), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Blazar, Mathematical Physics
Abstract: In almost a decade of operations, Chandra has observed and discovered the X-ray counterparts of several tens of extragalactic radio jets, with a variety of morphologies and SEDs. Here we take a fresh approach and assume that we do not know their relationship. We then search for phenomenological trends. While admittedly naive, this perspective allow us to start identifying key quantities towards a large-scale jet "unitarian view", just as was previously done for their compact, pc-scale cousins, the blazars. Similarly to the latter, we find that key parameters governing the properties of Chandra jets are their powers and the mass flux, the latter parameterizing the jet interaction with the ambient gas.
Published: 2008
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61. Spectral Energy Distributions of Hard X‐Ray Selected Active Galactic Nuclei in theXMM‐NewtonMedium Deep Survey

Author: O. Garcet, L. Maraschi, D. Maccagni, L. Tresse, David L. Shupe, O. Le Fevre, Helen Smith, Alberto Franceschini, Michael Rowan-Robinson, Marguerite Pierre, Danielle Alloin, Jean Surdej, L. Chiappetti, G. Zamorani, Ginevra Trinchieri, F. Fang, Stefano Andreon, Jason Surace, C. J. Lonsdale, M. Tajer, and M. Polletta
Subjects: Physics, education.field_of_study, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Population, X-ray, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Spectral line, Galaxy, Luminosity, Space and Planetary Science, education, Astrophysics::Galaxy Astrophysics
Abstract: We present the spectral energy distributions (SEDs) of a hard X-ray selected sample. The sample contains 136 sources with F(2-10 keV)>10^-14 erg/cm^2/s and 132 are AGNs. The sources are detected in a 1 square degree area of the XMM-Newton-Medium Deep Survey where optical data from the VVDS, CFHTLS surveys, and infrared data from the SWIRE survey are available. Based on a SED fitting technique we derive photometric redshifts with sigma(1+z)=0.11 and 6% of outliers and identify AGN signatures in 83% of the objects. This fraction is higher than derived when a spectroscopic classification is available. The remaining 17+9-6% of AGNs shows star-forming galaxy SEDs (SF class). The sources with AGN signatures are divided in two classes, AGN1 (33+6-1%) and AGN2 (50+6-11). The AGN1 and AGN2 classes include sources whose SEDs are fitted by type 1 and type 2 AGN templates, respectively. On average, AGN1s show soft X-ray spectra, consistent with being unabsorbed, while AGN2s and SFs show hard X-ray spectra, consistent with being absorbed. The analysis of the average SEDs as a function of X-ray luminosity shows a reddening of the IR SEDs, consistent with a decreasing contribution from the host galaxy at higher luminosities. The AGNs in the SF classes are likely obscured in the mid-infrared, as suggested by their low L(3-20micron)/Lcorr(0.5-10 keV) ratios. We confirm the previously found correlation for AGNs between the radio luminosity and the X-ray and the mid-infrared luminosities. The X-ray-radio correlation can be used to identify heavily absorbed AGNs. However, the estimated radio fluxes for the missing AGN population responsible for the bulk of the background at E>10 keV are too faint to be detected even in the deepest current radio surveys.
Published: 2007
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62. An Infrared Study of the Large-Scale Jet in Quasar PKS 1136-135

Author: Tadayuki Takahashi, L. Maraschi, Yasunobu Uchiyama, Paolo De Coppi, R. M. Sambruna, C. M. Urry, J. Van Duyne, C. C. Cheung, and Fabrizio Tavecchio
Subjects: Physics, Jet (fluid), Photon, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Compton scattering, Synchrotron radiation, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Synchrotron, law.invention, Particle acceleration, Space and Planetary Science, law, Astrophysics::Galaxy Astrophysics
Abstract: We present Spitzer IRAC imaging of the large-scale jet in the quasar PKS 1136-135 at wavelengths of 3.6 and 5.8 um, combined with previous VLA, HST, and Chandra observations. We clearly detect infrared emission from the jet, resulting in the most detailed multifrequency data among the jets in lobe-dominated quasars. The spectral energy distributions of the jet knots have significant variations along the jet, like the archetypal jet in 3C 273. The infrared measurements with IRAC are consistent with the previous idea that the jet has two spectral components, namely (1) the low-energy synchrotron spectrum extending from radio to infrared, and (2) the high-energy component responsible for the X-ray flux. The optical fluxes may be a mixture of the two components. We consider three radiation models for the high-energy component: inverse Compton scattering off CMB photons by radio-emitting electrons in a highly relativistic jet, synchrotron radiation by a second distinct electron population, and synchrotron radiation by ultra high energy protons. Each hypothesis leads to important insights into and constraints on particle acceleration in the jet, as well as the basic physical properties of the jet such as bulk velocity, transporting power, and particle contents., Comment: 9 pages, 5 figures (2 color figures), accepted for publication in ApJ; one typo in Table 1 is corrected
Published: 2007

63. X-Ray/UV/Optical Follow-up of the Blazar PKS 2155-304 after the Giant TeV Flares of 2006 July

Author: Elena Pian, Aldo Treves, M. Villata, Fabrizio Tavecchio, G. Ghisellini, R. M. Sambruna, Giuseppe Malaguti, P. Giommi, L. Maraschi, Luigi Foschini, C. M. Raiteri, G. Di Cocco, G. Tosti, G. Tagliaferri, and Mario Gliozzi
Subjects: PKS 2155-304, Physics, Galaxies: BL Lacertae Objects: General, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Galaxies: BL Lacertae Objects: Individual: Alphanumeric: PKS 2155-304, Synchrotron, law.invention, Wavelength, Space and Planetary Science, law, Spectral energy distribution, Blazar
Abstract: We present all the publicly available data, from optical/UV wavelengths (UVOT) to X-rays (XRT, BAT), obtained from Swift observations of the blazar PKS 2155-304, performed in response to the rapid alert sent out after the strong TeV activity (up to 17 Crab flux level at E > 200 GeV) at the end of July 2006. The X-ray flux increased by a factor of 5 in the 0.3-10 keV energy band and by a factor of 1.5 at optical/UV wavelengths, with roughly one day of delay. The comparison of the spectral energy distribution built with data quasi-simultaneous to the TeV detections shows an increase of the overall normalization with respect to archival data, but only a small shift of the frequency of the synchrotron peak that remains consistent with the values reported in past observations when the TeV activity was much weaker., 13 pages, 3 figures. ApJ Letters, accepted for publication
Published: 2007
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64. Detection of VHE γ-rays from HESS J0632+057 during the 2011 February X-ray outburst with the MAGIC Telescopes

Author: The MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. A. Alvarez(Universidad Complutense, E-28040 Madrid, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Asensio(Universidad Complutense, E-28040 Madrid, Spain), M. Backes(Technische Universität Dortmund, D-44221 Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), D. Bastieri(Università di Padova and INFN, I-35131 Padova, Italy), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Łódź, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Boller(ETH Zurich, CH-8093 Zurich, Switzerland), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, D-80805 München, Germany), V. Bosch-Ramon(Universitat de Barcelona), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), A. Cañellas(Universitat de Barcelona), E. Carmona(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), L. Cossio(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), E. De Cea del Pozo(Institut de Ciències de l'Espai), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), A. Diago Ortega(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(ETH Zurich, CH-8093 Zurich, Switzerland), M. Doro(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), D. Hadasch(Institut de Ciències de l'Espai), D. Häfner(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), B. Huber(ETH Zurich, CH-8093 Zurich, Switzerland), F. Jankowski(Deutsches Elektronen-Synchrotron), T. Jogler(Max-Planck-Institut für Physik, D-80805 München, Germany), V. Kadenius(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Klepser(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), T. Krähenbühl(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), S. Lombardi(Università di Padova and INFN, I-35131 Padova, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), A. Niedzwiecki(University of Łódź, PL-90236 Lodz, Poland), D. Nieto(Universidad Complutense, E-28040 Madrid, Spain), K. Nilsson(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), D. Paneque(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), S. Pardo(Universidad Complutense, E-28040 Madrid, Spain), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. A. Perez-Torres(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), M. Pilia(Università dell'Insubria, Como, I-22100 Como, Italy), J. Pochon(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), I. Puerto Gimenez(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. Reinthal(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, E-08010 Barcelona, Spain)), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Y. Saito(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Łódź, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, I-00136 Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), B. Steinke(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), N. Strah(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), H. Takami(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(ICREA, E-08010 Barcelona, Spain)), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), Q. Weitzel(ETH Zurich, CH-8093 Zurich, Switzerland), V. Zabalza(Universitat de Barcelona), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), now at(EPFL), (EPFL), Ecole polytechnique fédérale de Lausanne(EPFL), Lausanne(EPFL), Switzerland(CIEMAT), supported by INFN Padova(CIEMAT), now at(CIEMAT), (CIEMAT), Centro de Investigaciones Energéticas(CIEMAT), Medioambientales y Tecnológicas(CIEMAT), Madrid(FINCA), Spain(FINCA), now at(FINCA), (FINCA), KIPAC(FINCA), SLAC National Accelerator Laboratory(FINCA), USA(FINCA), Finnish Centre for Astronomy with ESO(FINCA), University of Turku(), and Finland)()
Subjects: High energy, Be star, Astrophysics::High Energy Astrophysical Phenomena, binaries: general, gamma rays: general, stars: individual (MWC 148), X-rays: binaries, X-rays: individual (HESS J0632+057), Astrophysics, Compact star, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, Raigs gamma, 0103 physical sciences, 010303 astronomy & astrophysics, Estels binaris de raigs X, Physics, astro-ph.HE, COUNTERPART, 010308 nuclear & particles physics, Gamma rays, X-ray, Gamma ray, Astronomy and Astrophysics, TEV BINARY, EMISSION, DISCOVERY, VARIABILITY, X-ray binaries, 13. Climate action, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The very high energy (VHE) \gamma-ray source HESS J0632+057 has recently been confirmed to be a \gamma-ray binary. The optical counterpart is the Be star MWC 148, and a compact object of unknown nature orbits it every ~321 d with a high eccentricity of ~0.8. We monitored HESS J0632+057 with the stereoscopic MAGIC telescopes from 2010 October to 2011 March and detected significant VHE \gamma-ray emission during 2011 February, when the system exhibited an X-ray outburst. We find no \gamma-ray signal in the other observation periods when the system did not show increased X-ray flux. Thus HESS J0632+057 exhibits \gamma-ray variability on timescales of the order of one to two months possibly linked to the X-ray outburst that takes place about 100 days after the periastron passage. Furthermore our measurements provide for the first time the \gamma-ray spectrum down to about 140 GeV and indicate no turnover of the spectrum at low energies. We compare the properties of HESS J0632+057 with the similar \gamma-ray binary LS I +61 303, and discuss on the possible origin of the multi-wavelength emission of the source, Comment: 6 pages and 3 figures, submitted, corresponding authors T. Jogler and P. Munar-Adrover
Published: 2015
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65. 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

66. Very high energy gamma-ray observation of the peculiar transient event Swift J1644+57 with the MAGIC telescopes and AGILE

Author: Abelardo Moralejo, Ivica Puljak, Pierre Colin, T. Krähenbühl, L. A. Antonelli, K. Berger, E. Colombo, S. Bonnefoy, Giacomo Bonnoli, R. Mirzoyan, D. Eisenacher, E. Carmona, Markus Garczarczyk, Fabio Zandanel, Ralph Bock, L. O. Takalo, Nina Nowak, Natalia Lewandowska, Mosè Mariotti, M. Doert, Michael Backes, M. Asensio, Takashi Saito, Juan Abel Barrio, K. Mallot, Fabrizio Tavecchio, R. J. García López, Saverio Lombardi, D. Borla Tridon, Ll. Font, F. Jankowski, C. Schultz, V. Scapin, Reiko Orito, S. Partini, Francesco Longo, Julian Sitarek, Kari Nilsson, M. Salvati, R. Reinthal, J. Hose, Dominik Elsaesser, A. Sillanpää, Steven N. Shore, A. La Barbera, Emanuele Paolo Farina, U. Barres de Almeida, Dario Hrupec, Nikola Godinovic, Benito Marcote, Daniela Hadasch, Felix Spanier, P. G. Prada Moroni, J. Moldón, Christian Fruck, T. Toyama, Nijil Mankuzhiyil, W. Idec, Damir Lelas, Patrick Vogler, P. Munar-Adrover, D. Garrido Terrats, Ignasi Reichardt, O. Tibolla, V. Scalzotto, C. Pittori, M. L. Knoetig, Tomislav Terzić, M. Palatiello, Massimo Persic, J. Krause, Dorota Sobczyńska, B. De Lotto, M. A. Lopez, Hajime Takami, Martin Makariev, Oscar Blanch, Riccardo Paoletti, I. Snidaric, Marc Ribó, D. Dominis Prester, Aaron Dominguez, M. V. Fonseca, G. Maneva, Fabrizio Lucarelli, Francesco Dazzi, R. Zanin, A. Saggion, Adrian Biland, J. Kushida, G. De Caneva, S. Klepser, E. Prandini, Jose Luis Contreras, Francisco Prada, Juan Cortina, J. M. Paredes, Antonio Stamerra, S. Spiro, E. Lorenz, A. De Angelis, Victor Stamatescu, Aldo Treves, J. Rico, Thomas Bretz, B. Steinke, J. Masbou, A. Hadamek, J. Storz, Diego F. Torres, M. I. Martínez, Wolfgang Rhode, J. Becerra González, P. Da Vela, A. Boller, L. Cossio, Daniel Ferenc, Mario Meucci, Artemio Herrero, K. Saito, F. Verrecchia, Q. Weitzel, Tihomir Surić, D. Carreto Fidalgo, V. Kadenius, S. Paiano, Karl Mannheim, C. Delgado Mendez, S. R. Gozzini, Gianluca Giavitto, A. González Muñoz, Daniela Dorner, M. Gaug, Elisa Bernardini, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Nakajima, Jose Miguel Miranda, L. Maraschi, Elina Lindfors, Daniel Mazin, Konstancja Satalecka, P. Temnikov, Michele Doro, Shan Sun, Jelena Aleksić, A. Niedzwiecki, David Paneque, Stefano Covino, T. Schweizer, I. Lozano, D. Tescaro, Masahiro Teshima, Robert Wagner, M. Uellenbeck, P. Antoranz, UAM. Departamento de Física Teórica, J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, J., Becerra González, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, E., Farina, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, W., Idec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, and F., Verrecchia
Subjects: Swift Gamma-Ray Burst Mission, active [Galaxies], Radiation mechanisms: non-thermal, TIDAL DISRUPTION, Astrophysics::High Energy Astrophysical Phenomena, radiation mechanisms: non-thermal, galaxies: active, Gamma rays: general, general [Gamma rays], Astrophysics, 01 natural sciences, Tidal disruption event, NEARBY, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Zenith, Physics, gamma rays: general, non-thermal [Radiation mechanisms], STAR, 010308 nuclear & particles physics, Gamma ray, Astronomy, Física, MASSIVE BLACK-HOLE, GALAXIES, BLAZARS, Astronomy and Astrophysics, Galaxies: active, Galaxy, 13. Climate action, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: Astronomy and astrophysics 552(A112 ), 1-6 (2013). doi:10.1051/0004-6361/201321197, Context. On March 28, 2011, the BAT instrument on board the Swift satellite detected a new transient event that in the very beginning was classified as a gamma ray burst (GRB). However, the unusual X-ray flaring activity observed from a few hours up to days after the onset of the event made a different nature seem to be more likely. The long-lasting activity in the X-ray band, followed by a delayed brightening of the source in infrared and radio activity, suggested that it is better interpreted as a tidal disruption event that triggered a dormant black hole in the nucleus of the host galaxy and generated an outflowing jet of relativistic matter. Aims. Detecting a very high energy emission component from such a peculiar object would be enable us to constrain the dynamic of the emission processes and the jet model by providing information on the Doppler factor of the relativistic ejecta. Methods. The MAGIC telescopes observed the peculiar source Swift J1644+57 during the flaring phase, searching for gamma-ray emission at very-high energy (VHE, E > 100 GeV), starting observations nearly 2.5 days after the trigger time. MAGIC collected a total of 28 h of dataduring 12 nights. The source was observed in wobble mode during dark time at a mean zenith angle of 35◦. Data were reduced using a new image-cleaning algorithm, the so-called sum-cleaning, which guarantees a better noise suppression and a lower energy threshold than the standard analysis procedure. Results. No clear evidence for emission above the energy threshold of 100 GeV was found. MAGIC observations permit one to constrain theemission from the source down to 100 GeV, which favors models that explain the observed lower energy variable emission. Data analysis of simultaneous observations from AGILE, Fermi and VERITAS also provide negative detection, which additionally constrain the self-Compton emission component., Published by EDP Sciences, Les Ulis
Published: 2013
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67. The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, Italy), M. Asensio(Universidad Complutense, Spain), M. Backes(Technische Universität Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, München, Germany), J. A. Barrio(Universidad Complutense, Spain), W. Bednarek(University of Łódź, Poland), K. Berger(Inst. de Astrofísica de Canarias, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, Spain), R. K. Bock(Max-Planck-Institut für Physik, München, Germany), A. Boller(ETH Zurich, Switzerland), S. Bonnefoy(Universidad Complutense, Spain), G. Bonnoli(INAF National Institute for Astrophysics, Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, München, Germany), T. Bretz(Universität Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), A. Carosi(INAF National Institute for Astrophysics, Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. L. Contreras(Universidad Complutense, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, Spain), L. Cossio(Università di Udine, and INFN Trieste, Italy), S. Covino(INAF National Institute for Astrophysics, Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, Italy), F. Dazzi(Università di Udine, and INFN Trieste, Italy), A. De Angelis(Università di Udine, and INFN Trieste, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), M. Doert(Technische Universität Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Dorner(Universität Würzburg, Germany), M. Doro(Universitat Autònoma de Barcelona, Spain), D. Eisenacher(Universität Würzburg, Germany), D. Elsaesser(Universität Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), M. V. Fonseca(Universidad Complutense, Spain), L. Font(Universitat Autònoma de Barcelona, Spain), C. Fruck(Max-Planck-Institut für Physik, München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, Spain), M. Gaug(Universitat Autònoma de Barcelona, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. Hose(Max-Planck-Institut für Physik, München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), F. Jankowski(Deutsches Elektronen-Synchrotron), V. Kadenius(Tuorla Observatory, University of Turku, Finland), S. Klepser(IFAE, Edifici Cn., Campus UAB, Spain), M. L. Knoetig(Max-Planck-Institut für Physik, München, Germany), T. Krähenbühl(ETH Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, Italy), N. Lewandowska(Universität Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, Finland), S. Lombardi(INAF National Institute for Astrophysics, Rome, Italy), M. López(Universidad Complutense, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, Spain), E. Lorenz(Max-Planck-Institut für Physik, München, Germany), I. Lozano(Universidad Complutense, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, Italy), K. Mannheim(Universität Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, Spain), J. Masbou(Università di Padova and INFN Padova, Italy), D. Mazin(Max-Planck-Institut für Physik, München, Germany), M. Meucci(Università di Siena, and INFN Pisa, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Max-Planck-Institut für Physik, München, Germany), A. Niedzwiecki(University of Łódź, Poland), D. Nieto(Universidad Complutense, Spain), K. Nilsson(Tuorla Observatory, University of Turku, Finland), N. Nowak(Max-Planck-Institut für Physik, München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, Italy), D. Paneque(Max-Planck-Institut für Physik, München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, Italy), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, Italy), M. Persic(Università di Udine, and INFN Trieste, Italy), M. Pilia(Università dell'Insubria, Como, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, Italy), E. Prandini(Università di Padova and INFN Padova, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, Spain), R. Reinthal(Tuorla Observatory, University of Turku, Finland), W. Rhode(Technische Universität Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, Barcelona, Spain), S. Rügamer(Universität Würzburg, Germany), A. Saggion(Università di Padova and INFN Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), T. Y. Saito(Max-Planck-Institut für Physik, München, Germany), M. Salvati(INAF National Institute for Astrophysics, Rome, Italy), K. Satalecka(Universidad Complutense, Spain), V. Scalzotto(Università di Padova and INFN Padova, Italy), V. Scapin(Universidad Complutense, Spain), C. Schultz(Università di Padova and INFN Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Sobczynska(University of Łódź, Poland), F. Spanier(Universität Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, Spain), A. Stamerra(Università di Siena, and INFN Pisa, Italy), B. Steinke(Max-Planck-Institut für Physik, München, Germany), J. Storz(Universität Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), L. Takalo(Tuorla Observatory, University of Turku, Finland), H. Takami(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), F. Tavecchio(INAF National Institute for Astrophysics, Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, München, Germany), O. Tibolla(Universität Würzburg, Germany), D. F. Torres(ICREA, Barcelona, Spain), T. Toyama(Max-Planck-Institut für Physik, München, Germany), A. Treves(Università dell'Insubria, Como, Italy), M. Uellenbeck(Technische Universität Dortmund, Germany), P. Vogler(ETH Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, München, Germany), Q. Weitzel(ETH Zurich, Switzerland), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), The MAGIC Collaboration(Università di Trieste, and INFN Trieste, Italy), F. Longo(Università di Trieste, and INFN Trieste, Italy), F. Lucarelli(Agenzia Spaziale Italiana), C. Pittori(Agenzia Spaziale Italiana), S. Vercellone(INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy), for the AGILE team(Università di Padova and INFN Padova, Italy), D. Bastieri(Università di Padova and INFN Padova, Italy), C. Sbarra(INFN Padova, Italy), for the Fermi-LAT Collaboration(Max-Planck-Institut für Radioastronomie, Germany), E. Angelakis(Max-Planck-Institut für Radioastronomie, Germany), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Germany), I. Nestoras(Max-Planck-Institut für Radioastronomie, Germany), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Germany), A. Sievers(Instituto de Radio Astronoma Milimétrica, Spain), J. A. Zensus(Max-Planck-Institut für Radioastronomie, Germany), for the F-GAMMA program(Crimean Astrophysical Observatory, Ukraine), K. A. Antonyuk(Crimean Astrophysical Observatory, Ukraine), W. Baumgartner(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), A. Berduygin(Tuorla Observatory, University of Turku, Finland), M. Carini(Department of Physics and Astronomy, Western Kentucky University, USA), K. Cook(Department of Physics and Astronomy, Western Kentucky University, USA), N. Gehrels(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Kadler(Universität Würzburg, Germany), Yu. A. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), Y. Y. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), F. Krauss(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), H. A. Krimm(Universities Space Research Association, Columbia, MD 21044, USA), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory, Finland), M. L. Lister(Department of Physics, Purdue University, USA), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), M. Pasanen(Tuorla Observatory, University of Turku, Finland), A. B. Pushkarev(Pulkovo Observatory, St. Petersburg, Russia), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), J. L. Richards(Department of Physics, Purdue University, USA), J. Sainio(Tuorla Observatory, University of Turku, Finland), D. N. Shakhovskoy(Crimean Astrophysical Observatory, Ukraine), K. V. Sokolovsky(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), M. Tornikoski(Aalto University Metsähovi Radio Observatory, Finland), J. Tueller(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Weidinger(Theoretische Physik IV, Ruhr-Universität Bochum, Germany), J. Wilms(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), 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), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, 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), Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), 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, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), 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), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), 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), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Università degli Studi di Udine - University of Udine [Italie], Universita degli studi di Napoli 'Parthenope' [Napoli], Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Vecteurs - Infections tropicales et méditerranéennes (VITROME), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées (IRBA), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), DAAA, ONERA, Université Paris Saclay (COmUE) [Meudon], ONERA-Université Paris-Saclay, University of Bath [Bath], Waves and Solitons LLC, 918 W. Windsong Dr., Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, E., Leonardo, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, D., Nieto, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, M., Pilia, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, S., Rügamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, S., Vercellone, D., Bastieri, C., Sbarra, E., Angelaki, L., Fuhrmann, I., Nestora, T. P., Krichbaum, A., Siever, J. A., Zensu, K. A., Antonyuk, W., Baumgartner, A., Berduygin, M., Carini, K., Cook, N., Gehrel, M., Kadler, Kovalev, Y. u. A., Y. Y., Kovalev, F., Krau, H. A., Krimm, A., Lähteenmäki, M. L., Lister, W., Max Moerbeck, M., Pasanen, A. B., Pushkarev, A. C. S., Readhead, J. L., Richard, J., Sainio, D. N., Shakhovskoy, K. V., Sokolovsky, M., Tornikoski, J., Tueller, M., Weidinger, J., Wilms, UAM. Departamento de Física Teórica, Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), 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), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-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 Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées [Brétigny-sur-Orge] (IRBA), Universitat Autònoma de Barcelona [Barcelona] (UAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Helmholtz-Gemeinschaft, National Institute for Nuclear Physics (INFN), National Academy of Sciences of Armenia, The Netherlands Institute for Radio Astronomy (ASTRON), 7990-AA Dwingeloo, Netherlands, Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), 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 Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), INAF-OAB, and DAAA, ONERA, Université Paris Saclay [Meudon]
Subjects: galaxies [Gamma rays], Radiation mechanisms: non-thermal, Flux, Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], BL Lacertae objects: individual: 1ES 2344+514, MAGIC (telescope), 010303 astronomy & astrophysics, galaxies: active, BL Lacerae objects: individual: 1ES 2344+514, gamma rays: galaxies, X-rays: individuals: 1ES 2344+514, radiation mechanisms: non-thermal, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, ACTIVE GALACTIC NUCLEI, BL-LACERTAE OBJECTS, GAMMA-RAY EMISSION, SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS, SELF-COMPTON MODEL, X-RAY, LAC OBJECTS, RELATIVISTIC JETS, MARKARIAN 501, Gamma ray, non-thermal [radiation mechanisms], active [galaxies], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxie [gamma rays], 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Light curve, individual: 1ES 2344+514 [BL Lacertae objects], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies [gamma-rays], Space and Planetary Science, ddc:520, individuals: 1ES 2344+514 [X-rays], Fermi Gamma-ray Space Telescope
Abstract: Astronomy and Astrophysics 556 (2013): A67 reproduced with permission from Astronomy and Astrophysics, Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims.We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods.The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign, The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A.Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged
Published: 2013
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68. Very high-energy gamma-ray observations of novae and dwarf novae with the MAGIC telescopes

Author: J. Kushida, Jose Luis Contreras, Juan Cortina, Tomislav Terzić, A. De Angelis, A. Treves, Vitaly Neustroev, M. Hayashida, Marc Ribó, Marina Manganaro, P. Bangale, D. Galindo, Hidetoshi Kubo, B. Biasuzzi, Abelardo Moralejo, H. Takami, Vassil Verguilov, G. Maneva, D. Nakajima, Konstancja Satalecka, Michele Doro, Giacomo Bonnoli, Julia Thaele, M. I. Martínez, R. Zanin, Adrian Biland, Arka Chatterjee, P. G. Prada Moroni, T. Steinbring, D. Fidalgo, K. Mallot, R. J. García López, J. Rico, M. Palatiello, Kyoshi Nishijima, Yusuke Konno, Sabrina Einecke, Pratik Majumdar, R. Reinthal, Francesco Dazzi, Gareth Hughes, M. V. Fonseca, K. Kodani, C. Schultz, V. Scapin, J. Rodriguez Garcia, Dominik Elsaesser, U. Barres de Almeida, R. Desiante, Stefano Covino, R. López-Coto, B. Banerjee, Max Ludwig Ahnen, Stefano Ansoldi, A. Niedzwiecki, Riccardo Paoletti, G. De Caneva, Damir Lelas, Massimo Persic, D. Tescaro, David Paneque, K. Saito, J. Palacio, Ievgen Vovk, D. Guberman, Dorota Sobczyńska, Julian Sitarek, J. M. Paredes, Antonio Stamerra, P. Giammaria, L. Maraschi, Nikola Godinovic, Benito Marcote, E. Hays, Elina Lindfors, J. Hose, Daniel Mazin, T. Toyama, Hanna Kellermann, B. De Lotto, T. Schweizer, D. Dominis Prester, Ivica Puljak, S. Bonnefoy, R. Clavero, P. Temnikov, Pierre Colin, L. A. Antonelli, Kari Nilsson, M. Will, K. Frantzen, Thomas Bretz, F. Di Pierro, R. Mirzoyan, Juri Poutanen, D. Garrido Terrats, P. Da Vela, Wlodek Bednarek, Alessandro Carosi, E. de Oña Wilhelmi, Y. Hanabata, J. A. Barrio, P. Antoranz, E. Carmona, Masahiro Teshima, S. Paiano, Wolfgang Rhode, Karl Mannheim, Jose Miguel Miranda, Fabrizio Tavecchio, Alicia López-Oramas, Ana Babić, F. Borracci, I. Snidaric, Natalia Lewandowska, A. La Barbera, D. Eisenacher Glawion, X. Paredes-Fortuny, M. Nievas Rosillo, E. Lorenz, J. Becerra González, Takashi Saito, Reiko Orito, E. Prandini, U. Menzel, Daniela Dorner, Diego F. Torres, M. Garczarczyk, A. Sillanpää, E. Colombo, M. Gaug, J. Herrera, L. O. Takalo, Francesco Longo, Koji Noda, Elisa Bernardini, Lluis Font, Marcel Strzys, Martin Makariev, Oscar Blanch, Alba Fernández-Barral, W. Idec, Christian Fruck, Mosè Mariotti, A.-K. Overkemping, Dario Hrupec, M. A. Lopez, A. González Muñoz, Saverio Lombardi, C. Delgado Mendez, 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., Carmona, E., 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 Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., 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., Guberman, D., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kellermann, H., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., 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., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Saito, K., Satalecka, K., Scapin, V., 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., Will, M., Zanin, R., Desiante, R., Hays, E., and Universitat de Barcelona
Subjects: Proton, Hadron, Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Raigs gamma, law, Astrophysics::Solar and Stellar Astrophysics, novae, cataclysmic variables, gamma rays: stars, binaries: general, stars: activity, 010303 astronomy & astrophysics, Dwarf nova, Novae, Estels binaris de raigs X, astro-ph.HE, Physics, Novae, cataclysmic variable, cataclysmic variables, Binaries: general, Gamma rays: stars, Novae, cataclysmic variables, Stars: activity, Astronomy and Astrophysics, Space and Planetary Science, Gamma-rays, stars, Binaries, general, Stars, activity, Gamma ray, X-ray binaries, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, activity [Stars], Astrophysics::High Energy Astrophysical Phenomena, Noves (Estels), Telescope, star [Gamma rays], 0103 physical sciences, New stars, general [Binaries], 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysic, 13. Climate action, ddc:520, High Energy Physics::Experiment, Fermi Gamma-ray Space Telescope, Lepton
Abstract: Context. In the last five years the Fermi Large Area Telescope (LAT) instrument detected GeV {\gamma}-ray emission from five novae. The GeV emission can be interpreted in terms of an inverse Compton process of electrons accelerated in a shock. In this case it is expected that protons in the same conditions can be accelerated to much higher energies. Consequently they may produce a second component in the {\gamma}-ray spectrum at TeV energies. Aims. We aim to explore the very-high-energy domain to search for {\gamma}-ray emission above 50 GeV and to shed light on the acceleration process of leptons and hadrons in nova explosions. Methods. We have performed observations with the MAGIC telescopes of the classical nova V339 Del shortly after the 2013 outburst, triggered by optical and subsequent GeV {\gamma}-ray detec- tions. We also briefly report on VHE observations of the symbiotic nova YY Her and the dwarf nova ASASSN-13ax. We complement the TeV MAGIC observations with the analysis of con- temporaneous Fermi-LAT data of the sources. The TeV and GeV observations are compared in order to evaluate the acceleration parameters for leptons and hadrons. Results. No significant TeV emission was found from the studied sources. We computed upper limits on the spectrum and night-by-night flux. The combined GeV and TeV observations of V339 Del limit the ratio of proton to electron luminosities to Lp, Comment: 7 pages, 2 figures, accepted for publication in A&A
Published: 2015
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69. Multiwavelength observations of Mrk 501 in 2008

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(2,*), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), T. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(7,*), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS Collaboration(Deutsches Elektronen-Synchrotron), (Deutsches Elektronen-Synchrotron), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), A. Bouvier(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), C. Duke(Department of Physics, Grinnell College, Grinnell, IA 50112-1690, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(now at GRAPPA Institute, University of Amsterdam, 1098XH), Q. Feng(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), N. Galante(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Gillanders(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), A. S Madhavan(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), G. Maier(Deutsches Elektronen-Synchrotron), P. Majumdar(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), D. Nieto(Physics Department, Columbia University, New York, NY 10027, USA), A. O'Faoláin de Bhróithe(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), G. Ratliff(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), L. C. Reyes(Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Sembroski(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), F. Sheidaei(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), A. W. Smith(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), S. Vincent(Deutsches Elektronen-Synchrotron), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Welsing(Deutsches Elektronen-Synchrotron), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), A. Zajczyk(Department of Physics, Washington University, St. Louis, MO 63130, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External Collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. M. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Ajello(Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA), M. Perri(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), V. M. Larionov(Astron. Inst., St.-Petersburg State Univ., Russia), N. V. Efimova(Astron. Inst., St.-Petersburg State Univ., Russia), T. S. Konstantinova(Astron. Inst., St.-Petersburg State Univ., Russia), E. N. Kopatskaya(Astron. Inst., St.-Petersburg State Univ., Russia), W. P. Chen(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), E. Koptelova(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), H. Y. Hsiao(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), G. N. Kimeridze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), B. Jordan(School of Cosmic Physics, Dublin Institute For Advanced Studies, Ireland), P. Leto(INAF - Osservatorio Astrofisico di Catania, Italy), C. S. Buemi(INAF - Osservatorio Astrofisico di Catania, Italy), C. Trigilio(INAF - Osservatorio Astrofisico di Catania, Italy), G. Umana(INAF - Osservatorio Astrofisico di Catania, Italy), A. Lahtenmaki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), E. Nieppola(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), J. Sainio(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), A. Cesarini(University of Trento, Department of Physics, I38050 Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Yu. A. Kovalev(Astro Space Center of the Lebedev Physical Institute, 117997), Y. Y. Kovalev(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, School services, ELEC, and ~
Subjects: extragalactic background light, Ciencias Físicas, Flux, Electron, Astrophysics, 7. Clean energy, law.invention, purl.org/becyt/ford/1 [https], Raigs gamma, bl lacertae objects, law, individual: Mrk 501 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, Astroparticle physics, BL Lacertae objects: individual: Mrk 501, Gamma rays: general, Astronomy and Astrophysics, Space and Planetary Science, Synchrotron, individual: Mrk 50 [BL Lacertae objects], Homogeneous, astroparticle physics, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, 1171 Geosciences, Astrophysics::High Energy Astrophysical Phenomena, emitting electrons, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, bl lacertae objects: individual: mrk 501, crab-nebula, Blazar, Astrophysics::Galaxy Astrophysics, tev blazars, variability, 221 Nanotechnology, Gamma rays, Individual: Mrk 501, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], gamma rays: general, Galaxies, gamma-ray emission, telescope system, Galàxies, Active Galaxies, blazars, gamma-rays, Mrk 501, Astronomía, Crab Nebula, x-ray, 115 Astronomy and space science, Low emission, 216 Materials engineering, Galàxies actives, active galactic nuclei, Active galaxies, ddc:520, general [gamma rays]
Abstract: Mrk 501 is one of the brightest blazars at TeV energies and has been extensively studied since its first VHE detection in 1996. Our goal is to characterize in detail the source gamma-ray emission, together with the radio-to-X-ray emission, during the non-flaring (low) activity, which is less often studied than the occasional flaring (high) activity. We organized a multiwavelength (MW) campaign on Mrk 501 between March and May 2008. This multi-instrument effort included the most sensitive VHE gamma-ray instruments in the northern hemisphere, namely the imaging atmospheric Cherenkov telescopes MAGIC and VERITAS, as well as Swift, RXTE, the F-GAMMA, GASP-WEBT, and other collaborations and instruments. Mrk 501 was found to be in a low state of activity during the campaign, with a VHE flux in the range of 10%-20% of the Crab nebula flux. Nevertheless, significant flux variations were detected with various instruments, with a trend of increasing variability with energy. The broadband spectral energy distribution during the two different emission states of the campaign can be adequately described within the homogeneous one-zone synchrotron self-Compton model, with the (slightly) higher state described by an increase in the electron number density. This agrees with previous studies of the broadband emission of this source during flaring and non-flaring states. We report for the first time a tentative X-ray-to-VHE correlation during a low VHE activity. Although marginally significant, this positive correlation between X-ray and VHE, which has been reported many times during flaring activity, suggests that the mechanisms that dominate the X-ray/VHE emission during non-flaring-activity are not substantially different from those that are responsible for the emission during flaring activity., Comment: Accepted for publication in A&A
Published: 2015
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70. The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Mu\ noz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Longo(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(6,32,*), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS collaboration(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), (Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. Archambault(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. H. Buckley(Department of Physics, Washington University, St. Louis, MO 63130, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), J. D. Eisch(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(DESY, Platanenallee 6, 15738 Zeuthen, Germany), Q. Feng(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), H. Fleischhack(Deutsches Elektronen-Synchrotron), P. Fortin(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), G. Hughes(Deutsches Elektronen-Synchrotron), T. B. Humensky(Physics Department, Columbia University, New York, NY 10027, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), Y. Khassen(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), F. Krennrich(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), S. Kumar(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), G. Maier(Deutsches Elektronen-Synchrotron), S. McArthur(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), N. Park(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), K. Ragan(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. C. Rovero(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), G. H. Sembroski(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. V. Tucci(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. Weinstein(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), R. Welsing(Deutsches Elektronen-Synchrotron), A. Wilhelm(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), W. P. Chen(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), B. Jordan(School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, 2, Ireland), E. Koptelova(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), B. McBreen(University College Dublin, Belfield, Dublin 4, Ireland), V. M. Larionov(Isaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, Russia), C. S. Lin(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), E. Angelakis(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Capalbi(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), A. Carrami\ nana(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), L. Carrasco(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), P. Cassaro(INAF Istituto di Radioastronomia, Sezione di Noto, Contrada Renna Bassa, 96017 Noto), A. Cesarini(Department of Physics, University of Trento, I38050, Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), T. Hovatta(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), H. A. Krimm(Astro Space Center of the Lebedev Physical Institute, 117997 Moscow, Russia), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. W. Moody(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), G. Maccaferri(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), Y. Mori(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), I. Nestoras(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), A. Orlati(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), C. Pace(Indiana University, Department of Astronomy, Swain Hall West 319, Bloomington, IN 47405-7105, USA), R. Pearson(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), M. Perri(INAF National Institute for Astrophysics, I-00136 Rome, Italy), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. L. Richards(Department of Physics, Purdue University, 525 Northwestern Ave, West Lafayette, IN 47907), A. C. Sadun(Department of Physics, University of Colorado, Denver, CO 80220, USA), T. Sakamoto(Department of Physics and Mathematics, College of Science and 952 Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuoku, Sagamihara-shi Kanagawa 252-5258, Japan), J. Tammi(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), Y. Yatsu(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), A. Zook(Department of Physics and Astronomy, Pomona College, Claremont CA 91711-6312, USA), Aleksić, J, Ansoldi, Stefano, Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Carreto Fidalgo, D., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadamek, A., Hadasch, D., Herrero, A., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Krause, J., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Longo, Francesco, Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Meucci, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nowak, N., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Partini, S., Persic, M., Prada, F., Prada Moroni, P. G., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguezgarcia, J., Rügamer, S., Saggion, A., Saito, K., Salvati, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Wagner, R. M., Zandanel, F., Zanin, R., Archambault, S., Behera, B., Beilicke, M., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Collins Hughes, E., Cui, W., Dumm, J., Eisch, J. D., Falcone, A., Federici, S., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Hanna, D., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krawczynski, H., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Mukherjee, R., Ong, R. A., Otte, A. N., Park, N., Pichel, A., Pohl, M., Popkow, A., Prokoph, H., Quinn, J., Ragan, K., Rajotte, J., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Theiling, M., Tucci, J. V., Tyler, J., Varlotta, A., Wakely, S. P., Weekes, T. C., Weinstein, A., Welsing, R., Wilhelm, A., Williams, D. A., Zitzer, B., Villata, M., Raiteri, C., Aller, H. D., Aller, M. F., Chen, W. P., Jordan, B., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Mcbreen, B., Larionov, V. M., Lin, C. S., Nikolashvili, M. G., Angelakis, E., Capalbi, M., Carramiñana, A., Carrasco, L., Cassaro, P., Cesarini, A., Fuhrmann, L., Giroletti, M., Hovatta, T., Krichbaum, T. P., Krimm, H. A., Max Moerbeck, W., Moody, J. W., Maccaferri, G., Mori, Y., Nestoras, I., Orlati, A., Pace, C., Pearson, R., Perri, M., Readhead, A. C. S., Richards, J. L., Sadun, A. C., Sakamoto, T., Tammi, J., Tornikoski, M., Yatsu, Y., Zook, A., Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Universitat de Barcelona
Subjects: Astrofísica, Brightness, Ciencias Físicas, blazars, Astrophysics, telescope, x-ray variability, 01 natural sciences, Spectral line, BL Lacertae objects, individual, Mrk 421, purl.org/becyt/ford/1 [https], Raigs gamma, emission, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), individual: Mrk 421 [BL Lacertae objects], Galaxies: BL Lacertae objects: individual: Markarian 421, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectra, BL Lacertae object, tev photons, 0103 physical sciences, Nucli galàctic actiu, bl lacertae objects: individual: mrk 421, Blazar, Astronomy and Astrophysics, Space and Planetary Science, Active galactic nuclei, 010308 nuclear & particles physics, light curves, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Light curve, Galaxies, Galàxies, Astronomía, Crab Nebula, optical variability, active galactic nuclei, Galàxies actives, Active galaxies, markarian-421, ddc:520
Abstract: We performed a 4.5-month multi-instrument campaign (from radio to VHE gamma rays) on Mrk421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies., Comment: Accepted for publication in A&A, 18 pages, 14 figures (v2 has a small modification in the acknowledgments, and also corrects a typo in the field "author" in the metadata)
Published: 2015
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71. Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies

Author: V. Braito, J. L. Richards, Bradley M. Peterson, Lars Fuhrmann, L. Maraschi, Emilia Järvelä, P. Romano, Smita Mathur, Stefano Ciroi, S. Vercellone, Alessandro Caccianiga, Luigi C. Gallo, Matthew L. Lister, Mikhail M. Lisakov, G. La Mura, Omar Tibolla, E. Angelakis, Marco Berton, S. Komossa, Joni Tammi, Gianpiero Tagliaferri, S. Kaufmann, Luigi Foschini, Valentina Cracco, Anne Lähteenmäki, Merja Tornikoski, A. Sievers, Dirk Grupe, Yuri Y. Kovalev, Piero Rafanelli, ITA, Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, jets [galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Astrophysical jet, Seyfert [galaxies], 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, general [quasars], 010308 nuclear & particles physics, general [BL Lacertae objects], Astronomy and Astrophysics, Quasar, Galaxy, Accretion (astrophysics), 3. Good health, Space and Planetary Science, Eddington luminosity, symbols, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We have conducted a multiwavelength survey of 42 radio loud narrow-1ine Seyfert 1 galaxies (RLNLS1s), selected by searching among all the known sources of this type and omitting those with steep radio spectra. We analyse data from radio frequencies to X-rays, and supplement these with information available from online catalogs and the literature in order to cover the full electromagnetic spectrum. This is the largest known multiwavelength survey for this type of source. We detected 90% of the sources in X-rays and found 17% at gamma rays. Extreme variability at high energies was also found, down to timescales as short as hours. In some sources, dramatic spectral and flux changes suggest interplay between a relativistic jet and the accretion disk. The estimated masses of the central black holes are in the range $\sim 10^{6-8}M_{\odot}$, smaller than those of blazars, while the accretion luminosities span a range from $\sim 0.01$ to $\sim 0.49$ times the Eddington limit, similar to those of quasars. The distribution of the calculated jet power spans a range from $\sim 10^{42.6}$ to $\sim 10^{45.6}$ erg s$^{-1}$, generally lower than quasars and BL Lac objects, but partially overlapping with the latter. Once normalised by the mass of the central black holes, the jet power of the three types of active galactic nuclei are consistent with each other, indicating the scalability of the jet. Despite the observational differences, the central engine of RLNLS1s is apparently quite similar to that of blazars. The historical difficulties in finding radio-loud narrow-line Seyfert 1 galaxies might be due to their low power and to intermittent jet activity., 35 pages, 13 Figures, 9 Tables. Updated after having found an error in Fig. 2 of Oshlack et al. (2001), which impacted our notes on J2007-4434. See footnote 10 at page 11
Published: 2015

72. The Jet‐Disk Connection in AGNs:ChandraandXMM‐NewtonObservations of Three Powerful Radio‐Loud Quasars

Author: Mario Gliozzi, Luigi Foschini, Fabrizio Tavecchio, R. M. Sambruna, and L. Maraschi
Subjects: Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Power law, Redshift, Galaxy, Space and Planetary Science, Galaxy group, Blazar, Astrophysics::Galaxy Astrophysics
Abstract: The connection between the accretion process that powers AGN and the formation of jets is still poorly understood. Here we tackle this issue using new, deep \chandra and \xmm observations of the cores of three powerful radio loud quasars: 1136--135, 1150+497 (\chandra), and 0723+679 (\xmm), in the redshift range $z$=0.3--0.8. These sources are known from our previous \chandra snapshot survey to have kpc-scale X-ray jets. In 1136--135 and 1150+497, evidence is found for the presence of diffuse thermal X-ray emission around the cores, on scales of 40--50 kpc and with luminosity L$_{0.3-2 keV} \sim 10^{43}$ \lum, suggesting thermal emission from the host galaxy or a galaxy group. The X-ray continua of the cores in the three sources are described by an upward-curved (concave) broken power law, with photon indices $\Gamma_{soft} \sim 1.8-2.1$ and $\Gamma_{hard} \sim 1.7$ below and above $\approx 2$ keV, respectively. There is evidence for an unresolved \feka line with EW $\sim$ 70 eV in the three quasars. The Spectral Energy Distributions of the sources can be well described by a mix of jet and disk emission, with the jet dominating the radio and hard X-rays (via synchrotron and external Compton) and the disk dominating the optical/UV through soft X-rays. The ratio of the jet-to-disk powers is $\sim 1$, consistent with those derived for a number of gamma-ray emitting blazars. This indicates that near equality of accretion and jet power may be common in powerful radio-loud AGN.
Published: 2006
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73. Black hole lightning due to particle acceleration at subhorizon scales

Author: J. Kushida, Jose Luis Contreras, Juan Cortina, J. Hose, R. Reinthal, D. Elsaesser, Michele Palatiello, P. Munar-Adrover, Elina Lindfors, Damir Lelas, Dario Hrupec, R. Zanin, Daniel Mazin, D. Nakajima, Victor Stamatescu, M. A. Lopez, Dorota Sobczyńska, Adrian Biland, K. Nishijima, M. Uellenbeck, D. Garrido Terrats, D. Dominis Prester, J. Rico, V. Scalzotto, Christian Fruck, E. Prandini, Stefano Covino, P. G. Prada Moroni, Francesco Longo, F. Borracci, P. Da Vela, Nikola Godinovic, Benito Marcote, Patrick Vogler, Ana Babić, D. Galindo, Yusuke Konno, O. Tibolla, I. Snidaric, M. Makariev, D. Tescaro, P. Temnikov, Ivica Puljak, M. V. Fonseca, A. Sillanpää, Jörn Wilms, G. Bonnoli, L. Maraschi, Pierre Colin, C. Delgado Mendez, S. R. Gozzini, E. de Oña Wilhelmi, Konstancja Satalecka, Julian Sitarek, Michele Doro, A. Treves, Kari Nilsson, Tomislav Terzić, N. Mankuzhiyil, Daniela Hadasch, Jelena Aleksić, Oscar Blanch, Alessandro Carosi, E. Lorenz, Ruben Lopez-Coto, T. Toyama, A. Niedzwiecki, I. Lozano, G. De Caneva, M. Hayashida, David Paneque, S. Bonnefoy, A. González Muñoz, T. Schweizer, Jose Miguel Miranda, E. Colombo, Francesco Dazzi, Masahiro Teshima, G. Maneva, Felix Spanier, Y. Hanabata, Daniela Dorner, C. Schultz, V. Scapin, Miriam Lucio Martinez, S. Rügamer, Juan Abel Barrio, M. Gaug, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Juri Poutanen, Stefano Ansoldi, J. Herrera, Koji Noda, B. Biasuzzi, U. Bach, Marc Ribó, Riccardo Paoletti, P. Antoranz, Elisa Bernardini, Hajime Takami, P. Bangale, J. M. Paredes, Felicia Krauß, Hidetoshi Kubo, Antonio Stamerra, Julia Thaele, K. Kodani, E. Carmona, L. O. Takalo, Louis Antonelli, J. Storz, A. De Angelis, D. Hildebrand, Mosè Mariotti, A.-K. Overkemping, Sabrina Einecke, Saverio Lombardi, J. Rodriguez Garcia, K. Saito, W. Idec, K. Frantzen, V. Kadenius, S. Paiano, Karl Mannheim, Alicia López-Oramas, Natalia Lewandowska, R. Mirzoyan, A. La Barbera, D. Eisenacher, Markus Garczarczyk, X. Paredes-Fortuny, J. Becerra González, Abelardo Moralejo, T. Steinbring, Hanna Kellermann, U. Menzel, Diego F. Torres, J. Krause, B. De Lotto, Takashi Saito, Reiko Orito, Eduardo Ros, Marcel Strzys, Matthias Kadler, K. Mallot, R. J. García López, Massimo Persic, R. Schulz, Thomas Bretz, S. N. Shore, Wolfgang Rhode, Aleksić, J, Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Biasuzzi, B., Bil, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Mendez, C. Delgado, Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Godinoviæ, N., Muñoz, A. González, Gozzini, S. R., Hadasch, D., Hanabata, Y., Hayashida, M., Herrera, J., Hildebr, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Kodani, K., Konno, Y., Krause, J., Kubo, H., Kushida, J., Barbera, A. La, Lelas, D., Lewowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Mira, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Rügamer, S., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Zanin, R., Kadler, M., Schulz, R., Ros, E., Bach, U., Krauß, F., and Wilms, J.
Subjects: Black Holes, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Very High Energy Gamma Astronomy, Black Holes, Very High Energy Gamma Astronomy, Active Galactic Nuclei, X-shaped radio galaxy, supermassive black hole, jet formation, IC 310, MAGIC telescopes, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Supermassive black hole, ta115, Multidisciplinary, Active Galactic Nuclei, Astronomy and Astrophysics, Galaxy, Intermediate-mass black hole, Stellar black hole, Electrónica, Física nuclear, ddc:500, Spin-flip, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius
Abstract: Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry, but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here, we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC telescopes revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20\% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet., 19 pages, 10 figures, includes Supplementary Materials
Published: 2014
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74. Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010

Author: E. Pueschel, J. Hose, Svetlana G. Jorstad, M. F. Aller, David A. Williams, G. H. Sembroski, D. Nakajima, M. Strzys, R. Welsing, A. Archer, E. Colombo, B. Biasuzzi, F. Borracci, Stefano Ansoldi, Riccardo Paoletti, I. Telezhinsky, Jamie Holder, D. Elsaesser, D. Staszak, Dario Hrupec, L. Ciupik, L. C. Reyes, G. Bonnoli, K. Ragan, M. A. Lopez, N. Galante, Hajime Takami, J. M. Paredes, P. T. Reynolds, Natalia Lewandowska, Hugh D. Aller, L. O. Takalo, G. H. Gillanders, T. Schweizer, Mosè Mariotti, Wystan Benbow, A.-K. Overkemping, D. Hadasch, Victor Stamatescu, J. Biteau, Paul S. Smith, Gordon T. Richards, Wei Cui, A. La Barbera, Sinéad M. Griffin, E. Roache, A. López-Oramas, S. Rügamer, Juan Abel Barrio, J. A. Ros, O. M. Kurtanidze, Alessandro Carosi, Ruben Lopez-Coto, X. Paredes-Fortuny, Mark Gurwell, U. Menzel, Saverio Lombardi, Calvin A. Johnson, P. Kar, M. Villata, K. Mallot, R. J. García López, Felix Spanier, M. Kertzman, A. C. S. Readhead, E. Prandini, D. Galindo, Merja Tornikoski, Yusuke Konno, Diego F. Torres, M. G. Nikolashvili, D. Eisenacher, Antonio Stamerra, K. Kodani, Givi N. Kimeridze, Julian Sitarek, Lorand A. Sigua, K. Nishijima, J. V. Tucci, A. Cesarini, M. Perri, P. Kaaret, J. Storz, D. Dominis Prester, Martin Pohl, C. M. Raiteri, Markus Garczarczyk, C. Fruck, A. Sillanpää, N. Håkansson, M. Makariev, T. Toyama, L. Maraschi, A. Pichel, Jose Miguel Miranda, Matteo Cerruti, Konstancja Satalecka, J. Becerra González, P. Antoranz, Amy Furniss, S. P. Wakely, B. Jordan, Elena G. Larionova, Xuhui Chen, H. C. Lin, Geza Gyuk, Louis Antonelli, Michele Doro, Abelardo Moralejo, Jelena Aleksić, S. McArthur, M. L. Knoetig, P. G. Prada Moroni, P. Munar-Adrover, Ivica Puljak, E. Collins-Hughes, K. Meagher, Nikola Godinovic, Benito Marcote, T. Steinbring, W. Idec, M. V. Fonseca, Pierre Colin, P. Temnikov, M. Hayashida, Patrick Vogler, J. Tyler, A. Niedzwiecki, C. Schultz, V. Scapin, J. H. Buckley, P. Moriarty, Tomislav Terzić, K. Berger, T. Sakamoto, C. Delgado Mendez, S. R. Gozzini, B. McBreen, O. Tibolla, Shan Sun, E. de Oña Wilhelmi, Ivan S. Troitsky, David Paneque, I. Snidaric, Marc Ribó, P. Da Vela, D. Hildebrand, B. Steinke, Steven N. Shore, Q. Feng, K. Frantzen, Massimo Persic, Hidetoshi Kubo, A. Boller, D. A. Morozova, A. Wilhelm, R. Reinthal, Thomas Bretz, Sofia O. Kurtanidze, Kari Nilsson, Elina Lindfors, Justin D. Finke, J. Krause, B. De Lotto, Walter Max-Moerbeck, K. Saito, Razmik Mirzoyan, U. Barres de Almeida, A. González Muñoz, V. Kadenius, Damir Lelas, N. Mankuzhiyil, J. P. Finley, J. S. Perkins, Wen Ping Chen, S. Paiano, E. Lorenz, Karl Mannheim, H. Prokoph, Hanna Kellermann, Daniel Mazin, I. Lozano, Dorota Sobczyńska, J. D. Eisch, Wolfgang Rhode, Daniela Dorner, M. Palatiello, Joseph Moody, Lucy Fortson, M. I. Martínez, M. Gaug, P. Bangale, G. De Caneva, J. Herrera, Matthias Beilicke, Koji Noda, J. Millis, Abraham D. Falcone, Francesco Dazzi, Karlen Shahinyan, Elisa Bernardini, S. Bonnefoy, Sabrina Einecke, J. Rodriguez Garcia, W. Bednarek, Fabrizio Tavecchio, Ll. Font, A. C. Sadun, Anne Lähteenmäki, Stefano Covino, M. J. Lang, A. Varlotta, Masahiro Teshima, A. McCann, Ekaterina Koptelova, A. C. Rovero, J. Kushida, D. Tescaro, Jose Luis Contreras, G. Hughes, M. Uellenbeck, Takashi Saito, Y. Hanabata, A. Popkow, Juan Cortina, V. Bugaev, David Kieda, Reiko Orito, S. Buson, J. L. Richards, Ann E. Wehrle, D. Garrido Terrats, P. Fortin, Oscar Blanch, Ralph Bird, S. Archambault, Valeri M. Larionov, V. Scalzotto, Ana Babić, Julia Thaele, E. Carmona, A. De Angelis, A. Treves, R. A. Ong, G. Maneva, R. Zanin, A. N. Otte, Adrian Biland, J. Rico, Alan P. Marscher, Universitat de Barcelona, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and ~
Subjects: extragalactic background light, Ciencias Físicas, spectral energy-distribution, Flux, Non-thermal / galaxies, Astrophysics, law.invention, Relativistic particle, purl.org/becyt/ford/1 [https], atmospheric cherenkov telescopes, Raigs gamma, bl lacertae objects, law, MAGIC (telescope), Active / BL Lacertae objects, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual: Mrk 421 [BL Lacertae objects], education.field_of_study, gamma-ray outburst, non-thermal [radiation mechanisms], BL Lacertae objects: individual: Mrk 421, Galaxies: active, Gamma rays: galaxies, Radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, Particle acceleration, NON THERMAL RADIATION, large-area telescope, active [galaxies], galaxies [gamma rays], BL LACERTAE OBJECTS, Electrónica, self-compton model, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Flare, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, radiation mechanisms: non-thermal, gamma rays: galaxies, Radiation mechanisms, BL Lacertae objects: individual, simultaneous multiwavelength observations, AGN, education, Blazar, Individual: Mrk 421 / gamma rays, tev blazars, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Galaxies, Astronomía, x-ray, Galàxies actives, Active galaxies, ddc:520
Abstract: A flare from the TeV blazar Mrk 421, occurring in March 2010, was observed for 13 consecutive days from radio to very high energy (VHE, E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, FermiLAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We model the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigate the physical parameters, and evaluate whether the observed broadband SED variability can be associated to variations in the relativistic particle population. Flux variability was remarkable in the X-ray and VHE bands while it was minor or not significant in the other bands. The one-zone SSC model can describe reasonably well the SED of each day for the 13 consecutive days. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission while the other smaller zone, which is spatially separated from the first one, contributes to the daily-variable emission occurring in X-rays and VHE gamma-rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly to the underlying particle population. This shows that the particle acceleration and cooling mechanism producing the radiating particles could be the main one responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by the variation of the parameters related to the emitting region itself ($\delta$, $B$ and $R$), in addition to the parameters related to the particle population., Comment: Published in A&A, 30 pages, 15 figures, 6 tables. Online-data: multi-wavelength light curves (data in Fig. 1) and broadband spectral energy distributions (the data in Figs. 6, and B1-B4) are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A22. Corresponding authors: David Paneque (dpaneque@mpp.mpg.de), Shangyu Sun (sysun@mpp.mpg.de), Hajime Takami (takami@post.kek.jp)
Published: 2014
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75. First broadband characterization and redshift determination of the VHE blazar MAGIC J2001+439

Author: Robert Wagner, Konstancja Satalecka, Michele Doro, K. Nishijima, K. Mallot, R. J. García López, A. Herrero, D. Dominis Prester, M. Uellenbeck, Nina Nowak, J. M. Paredes, A. López-Oramas, J. Kushida, Antonio Stamerra, Jelena Aleksić, Nikola Godinovic, Benito Marcote, Jose Luis Contreras, A. Niedzwiecki, David Paneque, Wlodek Bednarek, Alessandro Carosi, Francisco Prada, J. L. Richards, Juan Cortina, K. Kodani, Ruben Lopez-Coto, Massimo Persic, D. Nakajima, J. Storz, D. Garrido Terrats, Talvikki Hovatta, Patrick Vogler, P. G. Prada Moroni, Valeri M. Larionov, Jose Miguel Miranda, V. Scalzotto, C. Schultz, V. Scapin, Tomislav Terzić, Yusuke Konno, Anthony C. S. Readhead, J. Krause, O. Tibolla, M. Hayashida, B. De Lotto, P. Da Vela, Ana Babić, Hanna Kellermann, L. Maraschi, Elina Lindfors, Kari Nilsson, Daniel Mazin, Marc Ribó, M. V. Fonseca, P. Bangale, Julia Thaele, Hidetoshi Kubo, Stefano Covino, U. Menzel, Emanuele Paolo Farina, A. De Angelis, D. Tescaro, M. Perri, I. Snidaric, Natalia Lewandowska, M. Palatiello, Diego F. Torres, S. Rügamer, Stefano Ansoldi, Juan Abel Barrio, M. I. Martínez, Riccardo Paoletti, Felix Spanier, T. Sakamoto, M. Garczarczyk, E. Lorenz, Hajime Takami, A. La Barbera, L. A. Antonelli, Francesco Dazzi, Sabrina Einecke, P. Antoranz, R. Reinthal, J. Rodriguez Garcia, Dominik Elsaesser, Giacomo Bonnoli, X. Paredes-Fortuny, U. Barres de Almeida, I. Lozano, Fabrizio Tavecchio, Damir Lelas, Ll. Font, Masahiro Teshima, Victor Stamatescu, S. Bonnefoy, R. D. Schwartz, Filippo D'Ammando, Dorota Sobczyńska, R. Mirzoyan, D. Eisenacher, Abelardo Moralejo, P. Temnikov, Fabio Zandanel, Shan Sun, E. Carmona, T. Steinbring, Julian Sitarek, J. Hose, Aaron Dominguez, E. Prandini, Daniela Hadasch, T. Toyama, Aldo Treves, W. Idec, Thomas Bretz, S. N. Shore, Walter Max-Moerbeck, Wolfgang Rhode, K. Frantzen, Ivica Puljak, Tihomir Surić, Pierre Colin, D. Carreto Fidalgo, T. Schweizer, C. Delgado Mendez, S. R. Gozzini, F. Borracci, V. Kadenius, S. Paiano, Karl Mannheim, J. Becerra González, Mario Meucci, F. Verrecchia, E. Colombo, Nijil Mankuzhiyil, P. Munar-Adrover, G. Maneva, Silvia Preziuso, L. O. Takalo, R. Zanin, A. Saggion, Adrian Biland, A. González Muñoz, Mosè Mariotti, A.-K. Overkemping, J. Rico, A. Sillanpää, Daniela Dorner, Takashi Saito, Saverio Lombardi, M. Gaug, Reiko Orito, J. Herrera, Koji Noda, Elisa Bernardini, Christian Fruck, K. Saito, D. Hildebrand, Daniel Ferenc, G. De Caneva, S. Partini, Marcel Strzys, L. C. Reyes, Martin Makariev, Oscar Blanch, M. Doert, Dario Hrupec, M. A. Lopez, Aleksic J, Ansoldi S, Antonelli LA, Antoranz P, Babic A, Bangale P, de Almeida UB, Barrio JA, Gonzalez JB, Bednarek W, Bernardini E, Biland A, Blanch O, Bonnefoy S, Bonnoli G, Borracci F, Bretz T, Carmona E, Carosi A, Fidalgo DC, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi F, De Angelis A, De Caneva G, De Lotto B, Mendez CD, Doert M, Dominguez A, Prester DD, Dorner D, Doro M, Einecke S, Eisenacher D, Elsaesser D, Farina E, Ferenc D, Fonseca MV, Font L, Frantzen K, Fruck C, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Godinovic N, Munoz AG, Gozzini SR, Hadasch D, Hayashida M, Herrera J, Herrero A, Hildebrand D, Hose J, Hrupec D, Idec W, Kadenius V, Kellermann H, Kodani K, Konno Y, Krause J, Kubo H, Kushida J, La Barbera A, Lelas D, Lewandowska N, Lindfors E, Lombardi S, Lopez M, Lopez-Coto R, Lopez-Oramas A, Lorenz E, Lozano I, Makariev M, Mallot K, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Meucci M, Miranda JM, Mirzoyan R, Moralejo A, Munar-Adrover P, Nakajima D, Niedzwiecki A, Nilsson K, Nishijima K, Noda K, Nowak N, Orito R, Overkemping A, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Partini S, Persic M, Prada F, Moroni PGP, Prandini E, Preziuso S, Puljak I, Reinthal R, Rhode W, Riboo M, Rico J, Garcia JR, Rugamer S, Saggion A, Saito T, Saito K, Satalecka K, Scalzotto V, Scapin V, Schultz C, Schweizer T, Shore SN, Sillanpaa A, Sitarek J, Snidaric I, Sobczynska D, Spanier F, Stamatescu V, Stamerra A, Steinbring T, Storz J, Strzys M, Sun S, Suric T, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Thaele J, Tibolla O, Torres DF, Toyama T, Treves A, Uellenbeck M, Vogler P, Wagner RM, Zandanel F, Zanin R, DAmmando F, Hovatta T, Larionov VM, Max-Moerbeck W, Perri M, Readhead ACS, Richards JL, Sakamoto T, Schwartz RD, Verrecchia F, and Reyes LC
Subjects: ACTIVE GALACTIC NUCLEI, BL Lacertae objects: individual: MAGIC J2001+439, Galaxies: active, BL Lac objects: individual (MAGIC J2001+435), gamma rays: observations, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, Nordic Optical Telescope, Spectral line, BL Lacertae objects: individual: MAGIC J2001+435, Gamma rays: galaxies, 0103 physical sciences, GAMMA-RAY SPECTRUM, MAGIC (telescope), 010306 general physics, Blazar, 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), galaxies: active – BL Lacertae objects: individual: MAGIC J2001+435 – BL Lacertae objects: individual: MAGIC J2001+439 – gamma rays: galaxies, FERMI ERA, Astronomy and Astrophysics, PKS 1424+240, BL-LACERTAE OBJECTS, Galaxy, Redshift, EXTRAGALACTIC BACKGROUND LIGHT, LAC OBJECTS, SKY SURVEY, RADIATION, Amplitude, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract: We aim to characterize the broadband emission from 2FGL J2001.1+4352, which has been associated with the unknown-redshift blazar MG4 J200112+4352. Based on its gamma-ray spectral properties, it was identified as a potential very high energy (VHE; E > 100 GeV) gamma-ray emitter. The source was observed with MAGIC first in 2009 and later in 2010 within a multi-instrument observation campaign. The MAGIC observations yielded 14.8 hours of good quality stereoscopic data. The object was monitored at radio, optical and gamma-ray energies during the years 2010 and 2011. The source, named MAGIC J2001+439, is detected for the first time at VHE with MAGIC at a statistical significance of 6.3 {\sigma} (E > 70 GeV) during a 1.3-hour long observation on 2010 July 16. The multi-instrument observations show variability in all energy bands with the highest amplitude of variability in the X-ray and VHE bands. We also organized deep imaging optical observations with the Nordic Optical Telescope in 2013 to determine the source redshift. We determine for the first time the redshift of this BL Lac object through the measurement of its host galaxy during low blazar activity. Using the observational evidence that the luminosities of BL Lac host galaxies are confined to a relatively narrow range, we obtain z = 0.18 +/- 0.04. Additionally, we use the Fermi-LAT and MAGIC gamma-ray spectra to provide an independent redshift estimation, z = 0.17 +/- 0.10. Using the former (more accurate) redshift value, we adequately describe the broadband emission with a one-zone SSC model for different activity states and interpret the few-day timescale variability as produced by changes in the high-energy component of the electron energy distribution., Comment: 17 pages, 15 figures, Accepted for publication in A&A
Published: 2014
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76. A Unified View of Relativistic Jets

Author: L. Maraschi
Subjects: Physics, Jet (fluid), Accretion disc, Astrophysical jet, Space and Planetary Science, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Blazar, Cosmology
Abstract: I summarize here recent work on the physical conditions in blazar jets including the comparison between emission regions at subparsec scales (1016−17 cm) and at very large scales (1022−24 cm) recently detected in X-rays by Chandra. The jet properties at both scales together with those of the presumed associated accretion disk (1014−15 cm) suggest the possibility of a unified scenario for the origin and propagation of jets in strong radio sources.
Published: 2004
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77. A Survey of Extended Radio Jets withChandraand theHubble Space Telescope

Author: C. C. Cheung, Fabrizio Tavecchio, R. M. Sambruna, J. K. Gambill, G. Chartas, L. Maraschi, C. M. Urry, and R. Cerutti
Subjects: Physics, Jet (fluid), Scattering, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Plasma, Synchrotron, law.invention, Luminosity, Wavelength, Space and Planetary Science, law
Abstract: We present the results from an X-ray and optical survey of a sample of 17 radio jets in AGN performed with Chandra and HST. The sample was selected from the radio and is unbiased toward detection at shorter wavelengths, but preferentially it includes beamed sources. We find that X-ray emission is common on kpc-scales, with over half radio jets exhibiting at least one X-ray knot on the Chandra images. The distributions of the radio-to-X-ray and radio-to-optical spectral indices for the detected jets are similar to the limits for the non-detections,suggesting all bright radio jets have X-ray counterparts which will be visible in longer observations. Comparing the radio and X-ray morphologies shows that the majority of the X-ray jets have structures that closely map the radio. Analysis of the SED of the jet knots suggest the knots in which the X-ray and radio morphologies track each other produce X-rays by IC scattering of the Cosmic Microwave Background. The remaining knots produce X-rays by the synchrotron process. Spectral changes are detected along the jets, with the ratio of the X-ray-to-radio and optical-to-radio flux densities decreasing from the inner to the outer regions. This suggests the presence of an additional contribution to the X-ray flux in the jet's inner part, either from synchrotron or IC of the stellar light. Alternatively, in a pure IC/CMB scenario, the plasma decelerates as it flows from the inner to the outer regions. Finally, the X-ray spectral indices for the brightest knots are flat, indicating that the bulk of the luminosity of the jets is emitted at GeV energies, and raising the interesting possibility of future detections with GLAST.
Published: 2004
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78. GAMMA-RAY EXCESS FROM A STACKED SAMPLE OF HIGH- AND INTERMEDIATE-FREQUENCY PEAKED BLAZARS OBSERVED WITH THE MAGIC TELESCOPE

Author: Daniel Ferenc, M. Camara, Jose Luis Contreras, H. Vankov, Ilana M. Braun, Daniel Nieto, D. Bose, Dominik Elsaesser, Juan Cortina, Diego F. Torres, M. Pasanen, Pratik Majumdar, A. Sillanpää, M. V. Fonseca, Dorota Sobczyńska, J. M. Paredes, Antonio Stamerra, M. Rissi, Daniela Dorner, Abelardo Moralejo, Javier Moldon, Stefano Covino, J. C. Struebig, S. Spiro, E. Lorenz, Ivica Puljak, Pierre Colin, Dario Hrupec, Thomas Bretz, S. N. Shore, Roberta Zanin, B. Steinke, M. López, J. Rico, D. Dominis Prester, A. De Angelis, R. K. Bock, Petar Temnikov, D. Tescaro, A. La Barbera, Elisa Bernardini, B. De Lotto, S. Klepser, D. Hildebrand, L. Peruzzo, Mariano Moles, E. Prandini, Kari Nilsson, Marc Ribó, Valentí Bosch-Ramon, Francisco Prada, L. A. Antonelli, S. Rügamer, Juan Abel Barrio, M. T. Costado, Ignasi Reichardt, M. I. Martínez, A. Herrero, V. Scapin, D. Borla Tridon, A. Laille, O. Tibolla, R. J. García López, Denis Bastieri, Q. Weitzel, Riccardo Paoletti, Tihomir Surić, Giacomo Bonnoli, Igor Oya, Fabrizio Tavecchio, F. De Sabata, Daniel Kranich, L. Maraschi, Ll. Font, V. Scalzotto, Elina Lindfors, Andrei Berdyugin, T. Jogler, Pol Bordas, K. Berger, G. Maneva, Daniel Mazin, D. Pascoli, Agnieszka Sierpowska-Bartosik, A. Saggion, S. Paiano, R. G. Pegna, Karl Mannheim, Masahiro Teshima, Adrian Biland, Markus Gaug, C. Delgado Mendez, L. O. Takalo, R. de los Reyes, R. Mirzoyan, C. Schultz, Manel Errando, J. Becerra González, Felix Spanier, Wolfgang Rhode, Jelena Ninkovic, Miguel A. Pérez-Torres, E. Carmona, Markus Garczarczyk, Mosè Mariotti, Mario Meucci, Francesco Dazzi, Fabio Zandanel, Takashi Saito, Massimo Persic, C. C. Hsu, E. Leonardo, D. Britzger, Nikola Godinovic, Tomislav Terzić, Reiko Orito, M. Sánchez-Conde, M. De Maria, Aaron Dominguez, Felicitas Pauss, Saverio Lombardi, Victor Zabalza, T. Schweizer, N. Puchades, T. Krähenbühl, M. Salvati, M. Shayduk, E. De Cea del Pozo, P. Antoranz, Nijil Mankuzhiyil, S. Partini, Francesco Longo, D. Höhne-Mönch, Oscar Blanch, Robert Wagner, M. Doert, Michael Backes, Konstancja Satalecka, Michele Doro, Hiroko Miyamoto, Jelena Aleksić, C. Baixeras, Julian Sitarek, J. Hose, Daniela Hadasch, S. Commichau, Wlodek Bednarek, Alessandro Carosi, Jose Miguel Miranda, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, J. A., Barrio, D., Bastieri, Gonzalez, J., W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, G., Bonnoli, P., Borda, Tridon, D., V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, Angelis, A., Cea, E., Los, R., Lotto, B., Maria, M., Sabata, F., Mendez, C., M., Doert, A., Dom\inguez, Prester, D., D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J., Garc\ia, M., Garczarczyk, M., Gaug, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., H\ohne M\onch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, T., Kr\ahenb\uhl, D., Kranich, Barbera, A., A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Mart\inez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, S., Paiano, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., R\ugamer, A., Saggion, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanp\a\a, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, and R., Zanin
Subjects: CHERENKOV TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Standard deviation, BL-LAC OBJECTS, HESS, gamma rays: galaxies, 0103 physical sciences, BL lacertae objects, Blazar, 010303 astronomy & astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), BL Lacertae objects: general, 010308 nuclear & particles physics, general [BL Lacertae objects], Gamma ray, CONSTRAINTS, Astronomy and Astrophysics, Redshift, CRAB-NEBULA, MODEL, Crab Nebula, gamma rays: observations, Intermediate frequency, Space and Planetary Science, JET, DISCOVERY, galaxies [gamma rays], RADIATION, Electrónica, Física nuclear, EMISSION, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: 14 páginas, 6 figuras, 4 tablas.-- El Pdf del artículo es la versión pre-print: arXiv:1002.2951v3.-- MAGIC Collaboration: et al., Between 2004 and 2009, a sample of 28 X-ray selected high- and intermediate-frequency peaked blazars with an X-ray flux larger than 2 μJy at 1 keV in the redshift range from 0.018 to 0.361 was observed with the MAGIC telescope at energies above 100 GeV. Seven among them were detected and the results of these observations are discussed elsewhere. Here we concentrate on the remaining 21 blazars which were not detected during this observation campaign and present the 3σ (99.7%) confidence upper limits on their flux. The individual flux upper limits lie between 1.6% and 13.6% of the integral flux from the Crab Nebula. Applying a stacking method to the sample of non-detections with a total of 394.1 hr exposure time, we find evidence for an excess with a cumulative significance of 4.9 standard deviations. It is not dominated by individual objects or flares, but increases linearly with the observation time as for a constant source with an integral flux level of ~1.5% of that observed from the Crab Nebula above 150 GeV., The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Polish MNiSzW Grant N N203 390834, by the YIP of the Helmholtz Gemeinschaft, and by grant DO02-353 of the the Bulgarian National Science Fund.
Published: 2011
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79. The Brightest Gamma-Ray Flaring Blazar in the Sky: AGILE and Multi-wavelength Observations of 3C 454.3 During 2010 November

Author: Sofia O. Kurtanidze, Valeri M. Larionov, M. F. Aller, Lorand A. Sigua, M. Trifoglio, V. Strelnitski, S. G. Sergeev, Fulvio Gianotti, J. L. Gomez, M. Cardillo, Pietro Ubertini, I. M. McHardy, Angela Bazzano, Fabrizio Lucarelli, Kirill Sokolovsky, C. M. Raiteri, A. Trois, T. Krajci, F. Lazzarotto, Mark Gurwell, I. Donnarumma, A. C. Sadun, Y. Evangelista, G. Walker, Manasvita Joshi, P. Santolamazza, M. Pasanen, D. A. Morozova, R. Reinthal, Elena Pian, M. G. Nikolashvili, M. Tavani, G. A. Borman, P. W. Cattaneo, A. Sillanpää, A. A. Arkharov, L. Maraschi, N. V. Efimova, Givi N. Kimeridze, E. Del Monte, F. Longo, G. Pucella, C. Pittori, K. Nilsson, A. Pellizzoni, E. Striani, V. Vittorini, Marc Türler, V. Bianchin, M. Rapisarda, A. Giuliani, Carlo Ferrigno, P. Soffitta, S. V. Nazarov, Hugh D. Aller, G. Barbiellini, R. A. Chigladze, E. Lindfors, Arnaud Ferrari, F. Verrecchia, S. Sabatini, M. Pilia, M. Villata, M. Giusti, F. Fuschino, Andrei Berdyugin, Uwe Bach, I. Agudo, L. O. Takalo, A. W. Chen, Brian W. Taylor, P. Giommi, Omar M. Kurtanidze, S. N. Molina, J. A. Ros, G. Piano, Stephanie Sallum, M. Feroci, Andrea Bulgarelli, T. Sakamoto, Yu. S. Efimov, P. Romano, S. Vercellone, L. Pacciani, Mariateresa Fiocchi, A. Rappoldi, R. D. Schwartz, S., Vercellone, E., Striani, V., Vittorini, I., Donnarumma, L., Pacciani, G., Pucella, M., Tavani, C. M., Raiteri, M., Villata, P., Romano, M., Fiocchi, A., Bazzano, V., Bianchin, C., Ferrigno, L., Maraschi, E., Pian, M., T\urler, P., Ubertini, A., Bulgarelli, A. W., Chen, A., Giuliani, Longo, Francesco, G., Barbiellini, M., Cardillo, P. W., Cattaneo, Monte, E., Y., Evangelista, M., Feroci, A., Ferrari, F., Fuschino, F., Gianotti, M., Giusti, F., Lazzarotto, A., Pellizzoni, G., Piano, M., Pilia, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, M., Trifoglio, A., Troi, P., Giommi, F., Lucarelli, C., Pittori, P., Santolamazza, F., Verrecchia, I., Agudo, H. D., Aller, M. F., Aller, A. A., Arkharov, U., Bach, A., Berdyugin, G. A., Borman, R., Chigladze, Y. S., Efimov, N. V., Efimova, J. L., Gomez, M. A., Gurwell, I. M., Mchardy, M., Joshi, G. N., Kimeridze, T., Krajci, O. M., Kurtanidze, S. O., Kurtanidze, V. M., Larionov, E., Lindfor, S. N., Molina, D. A., Morozova, S. V., Nazarov, M. G., Nikolashvili, K., Nilsson, M., Pasanen, R., Reinthal, J. A., Ro, A. C., Sadun, T., Sakamoto, S., Sallum, S. G., Sergeev, R. D., Schwartz, L. A., Sigua, A., Sillanp\a\a, K. V., Sokolovsky, V., Strelnitski, L., Takalo, B., Taylor, and G., Walker
Subjects: galaxies: active, galaxies: jets, radiation mechanisms: non-thermal, quasars: general, quasars: individual: 3C 454.3, Photon, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, 01 natural sciences, law.invention, Pulsar, law, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), general [quasars], 010308 nuclear & particles physics, individual: 3C 454.3 [quasars], Gamma ray, Astronomy and Astrophysics, non-thermal [radiation mechanisms], jet [galaxies], Space and Planetary Science, Sky, active [galaxies], Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract: Since 2005, the blazar 3C 454.3 has shown remarkable flaring activity at all frequencies, and during the last four years it has exhibited more than one gamma-ray flare per year, becoming the most active gamma-ray blazar in the sky. We present for the first time the multi-wavelength AGILE, SWIFT, INTEGRAL, and GASP-WEBT data collected in order to explain the extraordinary gamma-ray flare of 3C 454.3 which occurred in November 2010. On 2010 November 20 (MJD 55520), 3C 454.3 reached a peak flux (E>100 MeV) of F_gamma(p) = (6.8+-1.0)E-5 ph/cm2/s on a time scale of about 12 hours, more than a factor of 6 higher than the flux of the brightest steady gamma-ray source, the Vela pulsar, and more than a factor of 3 brighter than its previous super-flare on 2009 December 2-3. The multi-wavelength data make a thorough study of the present event possible: the comparison with the previous outbursts indicates a close similarity to the one that occurred in 2009. By comparing the broadband emission before, during, and after the gamma-ray flare, we find that the radio, optical and X-ray emission varies within a factor 2-3, whereas the gamma-ray flux by a factor of 10. This remarkable behavior is modeled by an external Compton component driven by a substantial local enhancement of soft seed photons., Accepted for publication in ApJ Letters. 18 Pages, 4 Figures, 1 Table
Published: 2011

80. The BL Lacertae objects OQ 530 and S5 0716+714

Author: Annalisa Celotti, G. Tagliaferri, Hugh D. Aller, M. Ravasio, L. Maraschi, Anna Wolter, G. Ghisellini, M. F. Aller, Enrico Massaro, Fabrizio Tavecchio, P. Giommi, G. Tosti, and Roberto Nesci
Subjects: Physics, Photon, X-rays : galaxies, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), BL lacertae objects : general, FOS: Physical sciences, S5 0716+714, Inverse, Astronomy and Astrophysics, Astrophysics, External source, Spectral line, Synchrotron, Flattening, law.invention, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, law, Homogeneous, BL Lacertae objects : individual : OQ 530, BL Lacertae objects : individual : OQ 530, S5 0716+714, Blazar
Abstract: We present the results of the BeppoSAX observations of two BL Lacs, OQ 530 and S5 0716+714, as part of a ToO program for the simultaneous observation at radio, optical, X-ray and TeV energies. Both sources are detected in the LECS and MECS, with S5 0716+714 visible also in the PDS band, up to about 60 keV. The X-ray spectra of both sources are better fitted by a double power-law model, with a steep soft X-ray component flattening at harder energies, with breaks at 0.3 and 1.5 keV, respectively. The concave shape of the spectra in both objects is consistent with soft X-rays being produced by the synchrotron and harder X-rays by the inverse Compton processes. Also the X-ray variability properties confirm this scenario, in particular for S5 0716+714 our observation shows variations by about a factor 3 over one hour below 3 keV and no variability above. Their simultaneous broad band energy spectral distributions can be successfully interpreted within the frame of a homogeneous synchrotron and inverse Compton model, including a possible contribution from an external source of seed photons with the different spectral states of S5 0716+714 being reproduced by changing the injected power. The resulting parameters are fully consistent with the two sources being intermediate objects within the "sequence" scenario proposed for blazars., Comment: 10 pages, 8 figures, accepted by A&A
Published: 2003
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81. The X‐Ray Spectrum of the Seyfert I Galaxy Markarian 766: Dusty Warm Absorber or Relativistic Emission Lines?

Author: E. M. Puchnarewicz, William C. Priedhorsky, I. M. McHardy, Shane W. Davis, F. A. Cordova, L. Maraschi, Ehud Behar, T. P. Sasseen, Keith O. Mason, P. M. Ogle, Graziella Branduardi-Raymont, P. T. O'Brien, and M. J. Page
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Continuum (design consultancy), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Space and Planetary Science, Ionization, Magnitude (astronomy), Reflection (physics), Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: Competing models for broad spectral features in the soft X-ray spectrum of the Seyfert I galaxy Mrk766 are tested against data from a 130 ks XMM-Newton observation. A model including relativistically broadened Ly-alpha emission lines of OVIII, NVII and CVI is a better fit to 0.3-2 keV XMM RGS data than a dusty warm absorber. Moreover, the measured depth of neutral iron absorption lines in the spectrum is inconsistent with the magnitude of the iron edge required to produce the continuum break at 17-18Angstroms in the dusty warm absorber model. The relativistic emission line model can reproduce the broad-band (0.1-12 keV) XMM-EPIC data with the addition of a fourth line to represent emission from ionized iron at 6.7 keV and an excess due to reflection at energies above the iron line. The profile of the 6.7 keV iron line is consistent with that measured for the low energy lines. There is evidence in the RGS data at the 3sigma level for spectral features that vary with source flux. The covering fraction of warm absorber gas is estimated to be ~12%. Iron in the warm absorber is found to be overabundant with respect to CNO compared to solar values., Accepted for publication in ApJ Letters
Published: 2003
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82. MAGIC upper limits for two milagro-detected bright Fermi sources in the region of SNR G65.1+0.6

Author: M. Camara, R. Reinthal, Mosè Mariotti, Pratik Majumdar, M. V. Fonseca, Dominik Elsaesser, Thomas Bretz, M. Rissi, Saverio Lombardi, J. Pochon, Denis Bastieri, Tihomir Surić, S. N. Shore, Stefano Covino, L. O. Takalo, B. Steinke, J. Krause, B. De Lotto, M. Salvati, Aaron Dominguez, Felicitas Pauss, T. Krähenbühl, M. Lopez, Dorota Sobczyńska, S. Partini, D. Höhne-Mönch, D. Tescaro, R. Mirzoyan, Wolfgang Rhode, N. Strah, S. Klepser, Victor Zabalza, Karl Mannheim, K. Nilsson, D. Dominis Prester, S. Rügamer, E. Carmona, Juan Abel Barrio, S. Spiro, E. Lorenz, E. Lindfors, M. I. Martínez, Giacomo Bonnoli, E. De Cea del Pozo, Julian Sitarek, D. Borla Tridon, R. J. García López, Francisco Prada, Jose Luis Contreras, P. G. Prada Moroni, D. Bose, E. Prandini, J. Hose, C. DelgadoMendez, Juan Cortina, Agnieszka Sierpowska-Bartosik, Nikola Godinovic, M. De Maria, A. La Barbera, K. Berger, Daniela Hadasch, L. Maraschi, Massimo Persic, P. Bordas, C. Schultz, Igor Oya, Fabrizio Tavecchio, Felix Spanier, Oscar Blanch, J. C. Struebig, J. Moldón, J. Becerra González, Ll. Font, J. M. Paredes, Diego F. Torres, F. Longo, M. Pasanen, V. Scalzotto, Andrei Berdyugin, Antonio Stamerra, Roberta Zanin, D. Hildebrand, L. Peruzzo, Mario Meucci, Masahiro Teshima, R. G. Pegna, A. Boller, K. Saito, M. Doert, Michael Backes, A. Carosi, R. K. Bock, M. Garczarczyk, V. Scapin, J. Storz, Manel Errando, Abelardo Moralejo, Francesco Dazzi, F. De Sabata, N. Puchades, R. Paoletti, Fabio Zandanel, Miguel A. Sánchez-Conde, Miguel A. Pérez-Torres, E. Leonardo, T. Saito, Daniel Ferenc, H. Vankov, Ilana M. Braun, Marc Ribó, Tomislav Terzić, Reiko Orito, A. Saggion, Adrian Biland, I. Puljak, N. Mankuzhiyil, J. Rico, A. De Angelis, L. A. Antonelli, T. Jogler, D. Kranich, Ignasi Reichardt, Wlodek Bednarek, M. Shayduk, A. Herrero, Quirin Weitzel, Daniel Nieto, Jose Miguel Miranda, G. Maneva, Dario Hrupec, Valentí Bosch-Ramon, Gianluca Giavitto, P. Colin, D. Mazin, A. Sillanpää, Daniela Dorner, M. Gaug, Petar Temnikov, Elisa Bernardini, P. Antoranz, Konstancja Satalecka, Michele Doro, Hiroko Miyamoto, T. Schweizer, Jelena Aleksić, A. Diago Ortega, Robert Wagner, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, J. A., Barrio, D., Bastieri, Gonzalez, J., W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, Tridon, D., V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, M., Camara, E., Carmona, A., Carosi, P., Colin, J. L., Contrera, J., Cortina, S., Covino, F., Dazzi, Angelis, A., Cea, E., Lotto, B., Maria, M., Sabata, F., Mendez, C., Ortega, A., M., Doert, A., Dom\inguez, Prester, D., D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J., Garc\ia, M., Garczarczyk, M., Gaug, G., Giavitto, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., H\ohne M\onch, J., Hose, D., Hrupec, T., Jogler, S., Klepser, T., Kr\ahenb\uhl, D., Kranich, J., Krause, Barbera, A., E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Mart\inez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, A., Moralejo, D., Nieto, K., Nilsson, R., Orito, I., Oya, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, J., Pochon, F., Prada, P. G., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., R\ugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, A., Sierpowska Bartosik, A., Sillanp\a\a, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J., Storz, N., Strah, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, and R., Zanin
Subjects: Photon, GAMMA-RAY PULSARS, TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, SOURCE LIST, CATALOG, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Telescope, Pulsar, law, Observatory, ISM: supernova remnants, pulsars: individual: PSR J1957+2831 LAT PSR J1954+2836 LAT PSR J1958+2846, pulsars: individual(PSR J1957+2831, LAT PSR J1954+2836, LAT PSR J1958+2846), 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Pulsars, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Supernoves, Astronomy and Astrophysics, individual: PSR J1957+2831 LAT PSR J1954+2836 LAT PSR J1958+2846 [pulsars], Púlsars, Crab Nebula, Supernovae, 13. Climate action, Space and Planetary Science, Milagro, supernova remnant [ISM], Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We report on the observation of the region around supernova remnant G65.1+0.6 with the stand-alone MAGIC-I telescope. This region hosts the two bright GeV gamma-ray sources 1FGL J1954.3+2836 and 1FGL J1958.6+2845. They are identified as GeV pulsars and both have a possible counterpart detected at about 35 TeV by the Milagro observatory. MAGIC collected 25.5 hours of good quality data, and found no significant emission in the range around 1 TeV. We therefore report differential flux upper limits, assuming the emission to be point-like (, 8 pages, 3 figures, 1 table
Published: 2010
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83. Detection of very high energy γ-ray emission from the Perseus cluster Head-Tail Galaxy IC 310 by the MAGIC telescopes

Author: D. Bose, T. Krähenbühl, J. Becerra González, Diego F. Torres, M. Pasanen, Mario Meucci, M. Doert, Michael Backes, Abelardo Moralejo, E. De Cea del Pozo, N. Strah, M. Shayduk, Stefano Covino, Marc Ribó, Riccardo Paoletti, A. Pinzke, Aaron Dominguez, Nijil Mankuzhiyil, K. Berger, Felicitas Pauss, Victor Zabalza, Manel Errando, D. Tescaro, J. M. Paredes, Antonio Stamerra, Fabio Zandanel, K. Saito, A. La Barbera, T. Schweizer, S. Rügamer, R. J. García López, Agnieszka Sierpowska-Bartosik, Juan Abel Barrio, D. Borla Tridon, Jose Luis Contreras, J. Krause, B. De Lotto, Massimo Persic, Juan Cortina, A. De Angelis, S. Partini, Felix Spanier, Giacomo Bonnoli, J. Storz, Takashi Saito, A. Cañellas, Francesco Longo, D. Höhne-Mönch, Christoph Pfrommer, Reiko Orito, L. Maraschi, Elina Lindfors, Ignasi Reichardt, A. Boller, S. Klepser, D.V. Semikoz, M. Camara, Pierre Colin, L. Cossio, N. Puchades, Masahiro Teshima, Andrei Berdyugin, L. A. Antonelli, A. Diago Ortega, Robert Wagner, Daniel Mazin, T. Jogler, Pratik Majumdar, M. V. Fonseca, M. Salvati, Hiroko Miyamoto, Jelena Aleksić, R. G. Pegna, C. Schultz, Thomas Bretz, S. N. Shore, F. De Sabata, Mosè Mariotti, G. Maneva, A. Sillanpää, Artemio Herrero, Nikola Godinovic, Igor Oya, Fabrizio Tavecchio, Daniel Kranich, Ll. Font, D. Dominis Prester, A. Saggion, Denis Bastieri, Q. Weitzel, Adrian Biland, Tihomir Surić, Daniel Nieto, M. De Maria, B. Steinke, Kari Nilsson, Saverio Lombardi, Pol Bordas, Wolfgang Rhode, Tomislav Terzić, Javier Moldon, Francisco Prada, J. Pochon, Julian Sitarek, S. Spiro, E. Lorenz, Daniel Ferenc, Andrii Neronov, Martin Makariev, Oscar Blanch, Karl Mannheim, J. Hose, Daniela Hadasch, H. Vankov, Ilana M. Braun, V. Scalzotto, E. Colombo, Wlodek Bednarek, Alessandro Carosi, Konstancja Satalecka, Michele Doro, Jose Miguel Miranda, Ralph Bock, P. Antoranz, L. O. Takalo, Dario Hrupec, M. A. Lopez, E. Prandini, R. Reinthal, Dominik Elsaesser, Dorota Sobczyńska, R. Mirzoyan, E. Carmona, Markus Garczarczyk, Valentí Bosch-Ramon, V. Scapin, Gianluca Giavitto, Daniela Dorner, J. C. Struebig, Petar Temnikov, Roberta Zanin, Elisa Bernardini, Miguel A. Pérez-Torres, C. Delgado Mendez, Francesco Dazzi, J. Rico, Miguel A. Sánchez-Conde, E. Leonardo, D. Hildebrand, L. Peruzzo, M. I. Martínez, P. G. Prada Moroni, I. Puljak, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, J. A., Barrio, D., Bastieri, J. B., Gonzalez, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, M., Camara, A., Canella, E., Carmona, A., Carosi, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, F., Dazzi, A. D., Angeli, E. D., del Pozo, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A. D., Ortega, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J. G., Lopez, M., Garczarczyk, G., Giavitto, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, T., Jogler, S., Klepser, T., Krahenbuhl, D., Kranich, J., Krause, A. L., Barbera, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, M., Makariev, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, A., Moralejo, D., Nieto, K., Nilsson, R., Orito, I., Oya, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, J., Pochon, F., Prada, P. G. P., Moroni, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, S., Rugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J., Storz, N., Strah, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, R., Zanin, A., Neronov, C., Pfrommer, A., Pinzke, D. V., Semikoz, APC - THEORIE, 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)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), MAGIC, 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)-Institut für theoretische Physik, 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, gamma rays: galaxies, galaxies: individual: IC310, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Raigs gamma, Very High Energy Gamma-ray Astronomy, MAGIC telescope, Active Galactic Nuclei, Galaxies, galaxies: individual: IC 310, 0103 physical sciences, MAGIC (telescope), Cosmic rays, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Spectral index, 010308 nuclear & particles physics, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma rays, Astronomy and Astrophysics, gamma rays: galaxies — galaxies: active — galaxies: individual (IC 310), Galaxy, Galàxies, Crab Nebula, Space and Planetary Science, ddc:520, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We report on the detection with the MAGIC telescopes of very high energy gamma-rays from IC 310, a head-tail radio galaxy in the Perseus galaxy cluster, observed during the interval November 2008 to February 2010. The Fermi satellite has also detected this galaxy. The source is detected by MAGIC at a high statistical significance of 7.6sigma in 20.6 hr of stereo data. The observed spectral energy distribution is flat with a differential spectral index of -2.00 \pm 0.14. The mean flux above 300 GeV, between October 2009 and February 2010, (3.1 \pm 0.5)x10^{-12} cm^{-2} s^{-1}, corresponds to (2.5 \pm 0.4)% of Crab Nebula units. Only an upper limit, of 1.9% of Crab Nebula units above 300 GeV, was obtained with the 2008 data. This, together with strong hints (>3sigma) of flares in the middle of October and November 2009, implies that the emission is variable. The MAGIC results favour a scenario with the very high energy emission originating from the inner jet close to the central engine. More complicated models than a simple one-zone SSC scenario, e.g. multi-zone SSC, external Compton or hadronic, may be required to explain the very flat spectrum and its extension over more than three orders of magnitude in energy., 6 pages, 5 figures, submitted to ApJL
Published: 2010
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84. [ITAL]XMM-Newton[/ITAL] Observations of a Possible Light Echo in the Seyfert 1 Nucleus of NGC 4051

Author: T. P. Sasseen, I. M. McHardy, L. Maraschi, Philip Uttley, William C. Priedhorsky, Keith O. Mason, E. M. Puchnarewicz, F. A. Cordova, and M. J. Page
Subjects: Physics, Astronomy, Flux, Astronomy and Astrophysics, Radius, Astrophysics, medicine.disease_cause, Light curve, Galaxy, Luminosity, Amplitude, Space and Planetary Science, Light echo, medicine, Ultraviolet
Abstract: We discuss a 1.5 day long observation of the bright variable Seyfert 1 galaxy NGC 4051 that was obtained with the X-ray and ultraviolet telescopes on XMM-Newton and extended in the X-ray band using the Rossi X-Ray Timing Explorer. The ultraviolet (2900 A) and X-ray (2-10 keV) light curves varied with peak-to-peak amplitudes of 5% and a factor of ~4, respectively. A simple interband cross-correlation function shows three broad features: a positive correlation with coefficient rM = +0.63 at a lag (Topt - TX-ray) τ ~ +0.2 days, an anticorrelation with rM = -0.65 at τ ~ +0.7 days, and a broad but slightly weaker feature with rM ≥ 0.53 over τ = 1.2-1.4 days. Because of the asymmetric sampling of the optical and X-ray data, only positive lags could be probed. Monte Carlo simulations based on synthetic uncorrelated light curves derived from the power spectrum of the real data give an ~85% confidence in features at this level. If the X-ray and UV light curves are indeed correlated, the lag is highly significant (i.e., not consistent with zero), which is suggestive of a scenario in which X-rays are being reprocessed into UV light at a distance from the X-ray source. A simple model in which the reprocessor is an inclined optically thick ring at a radius of 0.14 lt-days from the X-ray source reproduces the UV data well. A comparison of the modulated fractions in the ultraviolet and X-ray bands suggests that 5% of the 2900 A flux is produced in this way. The reprocessing site is close enough to the X-ray emitter for X-ray heating from a source with the luminosity of NGC 4051 to produce a brightening in the UV band, and the amount of UV flux emitted suggests that the covering fraction of the reprocessor is about 6%. We briefly discuss the possible physical nature of the reprocessing ring structure.
Published: 2002
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85. Long‐Term Spectral Variability of Seyfert Galaxies fromRossi X‐Ray Timing ExplorerColor‐Flux Diagrams

Author: I. M. McHardy, Francesco Haardt, Philip Uttley, L. Maraschi, P.-O. Petrucci, and I. E. Papadakis
Subjects: Physics, Space and Planetary Science, Spectral slope, Reflection (physics), Flux, Astronomy and Astrophysics, Astrophysics, Power law, Monitoring program, Equivalent width, Spectral line, Line (formation)
Abstract: We present results from RXTE data obtained during a systematic monitoring program of four Seyfert galaxies (NGC5548, NGC5506, MCG-6-30-15 and NGC4051). We studied the variability of three hardness ratios derived from the light curves in four energy bands. All the objects show similar spectral variations in all ratios. In order to interpret the results we computed the hardness ratios corresponding to a simple spectral model of a power law plus iron line plus reflection component, considering two possibilities: a)variations with constant line equivalent width and reflection parameter R and b) variations with constant line and reflection flux. The overall, mean observed trends can be explained by spectral slope variations and a constant flux Fe line and reflection component, although the existence of a line component which is variable on short time scales cannot be excluded. Finally, we find that the data are not consistent with an increase of R with flux for individual sources, indicating that, as a single source varies, softer spectra do not correspond to larger R values.
Published: 2002
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86. Four Years of Monitoring Blazar PKS 2155−304 withBeppoSAX: Probing the Dynamics of the Jet

Author: You-Hong Zhang, Annalisa Celotti, Giovanni Fossati, Elena Pian, G. Tagliaferri, L. Maraschi, Aldo Treves, L. Chiappetti, G. Ghisellini, and Fabrizio Tavecchio
Subjects: Physics, PKS 2155-304, Jet (fluid), X-rays : galaxies, galaxies : active, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), BL lacertae objects : general, FOS: Physical sciences, methods : data analysis, Astronomy and Astrophysics, Context (language use), Astrophysics, BL lacertae objects : individual (PKS 2155-304), law.invention, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, law, Spectral analysis, Blazar, Phenomenology (particle physics), Flare, Physical quantity
Abstract: PKS 2155--304 is one of the brightest blazars in the X-ray band. It was repeatedly monitored with BeppoSax during three long campaigns of about 2 days each in November of 1996, 1997 and 1999. The source underwent different states of intensity and was clearly variable with successive flares detected. This paper presents temporal and spectral analysis to study the X-ray variability trends for a blazar. The rich phenomenology is interpreted in the context of a model where relativistic electrons are accelerated through internal shocks taking place in the jets. The most important parameter turns out to be the initial time interval between the two shells ejected from the central engine to produce the flare, which may determine the structure of the shock and in turn the physical quantities of the emitting region to reproduce the observed trends of the X-ray variability (abridged)., 51 pages, 11 figures, ApJ in press, Scheduled for the v572 no2, June 20, 2002 issue
Published: 2002
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87. X-rays from radio-galaxies: BeppoSAX observations

Author: Paola Grandi, L. Maraschi, and C. M. Urry
Subjects: Physics, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Solid angle, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Jet (particle physics), Radiation, Astrophysics, Galaxy, Spectral line, Space and Planetary Science, Reflection (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: We briefly review BeppoSAX observations of X-ray bright radio-galaxies. Their X-ray spectra are quite varied, and perhaps surprisingly, any similarity between radio-loud AGN and Seyfert galaxies is the exception rather than the rule. When detected, reprocessing features (iron line and reflection) are generally weak, suggesting two possible scenarios: either: (1) non-thermal (jet?) radiation dilutes the X-ray emission from the disk in radio-loud objects, or (2) the solid angle subtended by the X-ray reprocessing material is smaller in radio-loud than in radio-quiet AGN due to different characteristics of the accretion disk itself., Comment: 6 pages, to appear in `Life Cycles of Radio Galaxies', ed. J. Biretta et al., New Astronomy Reviews
Published: 2002
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88. Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies (Corrigendum)

Author: Smita Mathur, Anne Lähteenmäki, Sarah Kaufmann, Stefano Ciroi, Mikhail M. Lisakov, V. Braito, Valentina Cracco, O. Tibolla, S. Komossa, Alessandro Caccianiga, J. L. Richards, Merja Tornikoski, A. Sievers, G. Tagliaferri, Bradley M. Peterson, Lars Fuhrmann, Dirk Grupe, L. Maraschi, P. Romano, Matthew L. Lister, Marco Berton, S. Vercellone, Joni Tammi, Luigi C. Gallo, G. La Mura, Luigi Foschini, Emilia Järvelä, Emmanouil Angelakis, Yuri Y. Kovalev, Piero Rafanelli, and ITA
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectrum (topology), Galaxy, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract: We have conducted a multiwavelength survey of 42 radio loud narrow-1ine Seyfert 1 galaxies (RLNLS1s), selected by searching among all the known sources of this type and omitting those with steep radio spectra. We analyse data from radio frequencies to X-rays, and supplement these with information available from online catalogs and the literature in order to cover the full electromagnetic spectrum. This is the largest known multiwavelength survey for this type of source. We detected 90% of the sources in X-rays and found 17% at gamma rays. Extreme variability at high energies was also found, down to timescales as short as hours. In some sources, dramatic spectral and flux changes suggest interplay between a relativistic jet and the accretion disk. The estimated masses of the central black holes are in the range $\sim 10^{6-8}M_{\odot}$, smaller than those of blazars, while the accretion luminosities span a range from $\sim 0.01$ to $\sim 0.49$ times the Eddington limit, similar to those of quasars. The distribution of the calculated jet power spans a range from $\sim 10^{42.6}$ to $\sim 10^{45.6}$ erg s$^{-1}$, generally lower than quasars and BL Lac objects, but partially overlapping with the latter. Once normalised by the mass of the central black holes, the jet power of the three types of active galactic nuclei are consistent with each other, indicating the scalability of the jet. Despite the observational differences, the central engine of RLNLS1s is apparently quite similar to that of blazars. The historical difficulties in finding radio-loud narrow-line Seyfert 1 galaxies might be due to their low power and to intermittent jet activity.
Published: 2017
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89. MAGIC Gamma-ray Telescope Observation of the Perseus Cluster of Galaxies: implications for cosmic rays, dark matter, and NGC1275

Author: J. Moldón, Lluis Font, Daniel Nieto, T. Krähenbühl, Stefano Covino, Takashi Saito, S. Commichau, Susumu Inoue, C. C. Hsu, Reiko Orito, Wlodek Bednarek, Alessandro Carosi, R. Mirzoyan, A. De Angelis, Jelena Ninkovic, Nikola Godinovic, N. Puchades, M. Doert, Riccardo Paoletti, Michael Backes, Dominik Elsaesser, Christoph Pfrommer, M. De Maria, Masahiro Teshima, D. Bose, Francesco Dazzi, Miguel A. Pérez-Torres, Ignasi Reichardt, E. Carmona, Markus Garczarczyk, J. Zapatero, E. Leonardo, C. Baixeras, D. Tescaro, J. M. Paredes, Diego F. Torres, Antonio Stamerra, A. La Barbera, Dorota Sobczyńska, Thomas Bretz, F. De Sabata, M. Pasanen, R. J. García López, A. Domínguez, Giacomo Bonnoli, Mariano Moles, Nicola Galante, Pol Bordas, M. Salvati, R. K. Bock, Dario Hrupec, Marc Ribó, S. Rügamer, A. Sillanpää, Agnieszka Sierpowska-Bartosik, M. T. Costado, Abelardo Moralejo, Ivica Puljak, Gabriele Ghisellini, Torsten A. Enßlin, M. Shayduk, D. Borla Tridon, L. Maraschi, Elina Lindfors, M. Sánchez-Conde, Wolfgang Rhode, S. Partini, Francesco Longo, G. Maneva, D. Höhne-Mönch, J. C. Struebig, Felicitas Pauss, Nijil Mankuzhiyil, V. Scalzotto, Roberta Zanin, Victor Zabalza, Manel Errando, Massimo Persic, J. Becerra González, E. De Cea del Pozo, R. G. Pegna, B. De Lotto, P. Temnikov, A. Saggion, L. A. Antonelli, Fabio Zandanel, Julian Sitarek, S. Klepser, Mario Meucci, E. Prandini, J. A. Barrio, Adrian Biland, M. Camara, Tomislav Terzić, A. Laille, Andrei Berdyugin, Pratik Majumdar, M. V. Fonseca, M. Rissi, Igor Oya, Markus Gaug, Denis Bastieri, R. de los Reyes, S. N. Shore, Tihomir Surić, C. Schultz, Jose Luis Contreras, Fabrizio Tavecchio, Daniel Kranich, S. Paiano, Karl Mannheim, B. Steinke, M. López, Juan Cortina, M. I. Martínez, S. Spiro, E. Lorenz, Kari Nilsson, A. Herrero, D. Pascoli, J. Rico, T. Jogler, D. Hildebrand, L. Peruzzo, Daniel Ferenc, H. Vankov, Ilana M. Braun, P. Antoranz, Daniela Dorner, A. Pinzke, D. Britzger, Konstancja Satalecka, Michele Doro, Hiroko Miyamoto, Elisa Bernardini, Jelena Aleksić, T. Schweizer, C. Delgado Mendez, Valentí Bosch-Ramon, V. Scapin, P. Colin, Robert Wagner, D. Dominis Prester, Francisco Prada, K. Berger, Mosè Mariotti, Felix Spanier, J. Hose, Daniela Hadasch, Saverio Lombardi, S. Balestra, Jose Miguel Miranda, L. O. Takalo, D. Mazin, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, D., Bastieri, J. B., Gonzalez, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, A. D., Angeli, E. D., del Pozo, R. D., Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, T., Krahenbuhl, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, S., Paiano, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., Rugamer, A., Saggion, T. Y., Saito, M., Salvati, M. A., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, V., Zabalza, F., Zandanel, R., Zanin, J., Zapatero, C., Pfrommer, A., Pinzke, T. A., Enlin, S., Inoue, and G., Ghisellini
Subjects: Radio galaxy, Astrophysics, 01 natural sciences, Raigs gamma, Dark Matter, MAGIC (telescope), Very High Energy Gamma-ray Astronomy, MAGIC telescope, Galaxy Cluster, 010303 astronomy & astrophysics, gamma-rays: observations, galaxies: clusters: individual (Perseus), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Clusters of galaxies, FLUX-LIMITED SAMPLE, COSMOLOGICAL SIMULATIONS, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, HARD X-RAY, Cúmuls de galàxies, ACTIVE GALACTIC NUCLEI, PARTICLE HYDRODYNAMICS SIMULATIONS, COMA CLUSTER, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Cooling flow, MAGNETIC-FIELDS, RADIO HALOS, 0103 physical sciences, Cosmic rays, Galaxy cluster, Astrophysics::Galaxy Astrophysics, HESS OBSERVATIONS, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Galaxy, gamma ray astronomy, INTERGALACTIC MEDIUM, Space and Planetary Science, Fermi Gamma-ray Space Telescope
Abstract: The Perseus galaxy cluster was observed by the MAGIC Cherenkov telescope for a total effective time of 24.4 hr during 2008 November and December. The resulting upper limits on the gamma-ray emission above 100 GeV are in the range of 4.6 to 7.5 x 10^{-12} cm^{-2} s^{-1} for spectral indices from -1.5 to -2.5, thereby constraining the emission produced by cosmic rays, dark matter annihilations, and the central radio galaxy NGC1275. Results are compatible with cosmological cluster simulations for the cosmic-ray-induced gamma-ray emission, constraining the average cosmic ray-to-thermal pressure to, 15 pages, 5 figures; accepted for publication in ApJ; updated to match the journal final version
Published: 2009
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90. DISCOVERY OF VERY HIGH ENERGY gamma-RAYS FROM THE BLAZAR S5 0716+714

Author: H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, D. Bastieri, J. Becerra González, J. K. Becker, W. Bednarek, A. Berdyugin, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla Tridon, V. Bosch-Ramon, D. Bose, I. Braun, T. Bretz, D. Britzger, M. Camara, E. Carmona, A. Carosi, P. Colin, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, F. Dazzi, A. De Angelis, E. de Cea del Pozo, R. De los Reyes, B. De Lotto, M. De Maria, F. De Sabata, C. Delgado Mendez, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E. Fernández, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. García López, M. Garczarczyk, M. Gaug, N. Godinovic, F. Goebel, D. Hadasch, A. Herrero, D. Hildebrand, D. Höhne-Mönch, J. Hose, D. Hrupec, C. C. Hsu, T. Jogler, S. Klepser, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S. Lombardi, F. Longo, M. López, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, J. M. Miranda, R. Mirzoyan, H. Miyamoto, J. Moldón, M. Moles, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, R. Orito, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G. Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, I. Puljak, I. Reichardt, W. Rhode, M. Ribó, J. Rico, M. Rissi, A. Robert, S. Rügamer, A. Saggion, J. Sainio, T. Y. Saito, M. Salvati, M. Sánchez-Conde, K. Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M. Shayduk, S. N. Shore, A. Sierpowska-Bartosik, A. Sillanpää, J. Sitarek, D. Sobczynska, F. Spanier, S. Spiro, A. Stamerra, L. S. Stark, T. Suric, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, D. F. Torres, N. Turini, H. Vankov, R. M. Wagner, C. Villforth, V. Zabalza, F. Zandanel, R. Zanin, J. Zapatero, H., Anderhub, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, D., Bastieri, J. B., Gonzalez, J. K., Becker, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, A. D., Angeli, E. D., Del Pozo, R. D., Los Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, E., Fernandez, R., Firpo, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, N., Godinovic, F., Goebel, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, J., Sainio, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, L. S., Stark, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, D. F., Torre, N., Turini, H., Vankov, R. M., Wagner, C., Villforth, V., Zabalza, F., Zandanel, R., Zanin, J., Zapatero, and Universitat de Barcelona
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Raigs gamma, law, Observacions astronòmiques, 0103 physical sciences, MAGIC (telescope), Blazar, Cosmic rays, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Very High Energy Gamma-ray Astronomy, MAGIC telescope, Active Galactic Nuclei, Gamma rays, Gamma ray, Astronomy and Astrophysics, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, Crab Nebula, Space and Planetary Science, BL Lacertae objects: individual: S5 0716+714, gamma rays: observations, Spectral energy distribution, ddc:520, High Energy Physics::Experiment, Electrónica, Física nuclear, Electricidad, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract: The MAGIC collaboration reports the detection of the blazar S5 0716+714 z=0.31+-0.08 in very high energy gamma-rays. The observations were performed in November 2007 and in April 2008, and were triggered by the KVA telescope due to the high optical state of the object. An overall significance of the signal accounts to S =5.8sigma for 13.1 hours of data. Most of the signal S = 6.9sigma comes from the April 2008 data sample during a higher optical state of the object suggesting a possible correlation between the VHE gamma-ray and optical emissions. The differential energy spectrum of the 2008 data sample follows a power law with a photon index of Gamma = 3.45+-0.54_(stat)+-0.2_(syst), and the integral flux above 400GeV is at the level of 7.5+-2.2_(stat)+-2.3_(syst)*10^-12 cm^-2 s^-1 corresponding to a 9% Crab Nebula flux. Modeling of the broad band spectral energy distribution indicates that a structured jet model appears to be more promising in describing the available data than a simple one zone synchrotron self-Compton model., accepted to ApJL
Published: 2009
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91. Upper Limits on the VHE Gamma-Ray Emission from the Willman 1 Satellite Galaxy with the Magic Telescope

Author: E. Aliu, H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, H. Bartko, D. Bastieri, J. Becerra González, J. K. Becker, W. Bednarek, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla Tridon, V. Bosch-Ramon, D. Bose, T. Bretz, I. Britvitch, M. Camara, E. Carmona, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, V. Curtef, F. Dazzi, A. De Angelis, E. De Cea del Pozo, R. de los Reyes, B. De Lotto, M. De Maria, F. De Sabata, C. Delgado Mendez, A. Dominguez, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E. Fernández, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. García López, M. Garczarczyk, M. Gaug, F. Goebel, D. Hadasch, M. Hayashida, A. Herrero, D. Höhne-Mönch, J. Hose, C. C. Hsu, S. Huber, T. Jogler, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S. Lombardi, F. Longo, M. López, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, J. Moldón, M. Moles, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, N. Otte, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G. Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, W. Rhode, M. Ribó, J. Rico, M. Rissi, A. Robert, S. Rügamer, A. Saggion, T. Y. Saito, M. Salvati, M. Sanchez-Conde, K. Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M. Shayduk, K. Shinozaki, S. N. Shore, N. Sidro, A. Sierpowska-Bartosik, A. Sillanpää, J. Sitarek, D. Sobczynska, F. Spanier, A. Stamerra, L. S. Stark, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, M. Tluczykont, D. F. Torres, N. Turini, H. Vankov, R. M. Wagner, W. Wittek, V. Zabalza, F. Zandanel, R. Zanin, J. Zapatero, E., Aliu, H., Anderhub, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, H., Bartko, D., Bastieri, J. B., Gonzalez, J. K., Becker, W., Bednarek, K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, T., Bretz, I., Britvitch, M., Camara, E., Carmona, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, V., Curtef, F., Dazzi, A. D., Angeli, E. D., del Pozo, R. d., los Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A., Dominguez, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, E., Fernandez, R., Firpo, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, F., Goebel, D., Hadasch, M., Hayashida, A., Herrero, D., Hohne Monch, J., Hose, C. C., Hsu, S., Huber, T., Jogler, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, M., Meyer, J. M., Miranda, R., Mirzoyan, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, N., Otte, I., Oya, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, T., Schweizer, M., Shayduk, K., Shinozaki, S. N., Shore, N., Sidro, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, A., Stamerra, L. S., Stark, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, M., Tluczykont, D. F., Torre, N., Turini, H., Vankov, R. M., Wagner, W., Wittek, V., Zabalza, F., Zandanel, R., Zanin, and J., Zapatero
Subjects: SUBSTRUCTURE, Astrophysics::High Energy Astrophysical Phenomena, DARK-MATTER ANNIHILATION, Dark matter, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, MILKY-WAY, DWARF GALAXY, GALACTIC SATELLITES, URSA-MAJOR, SEARCH, SIGNAL, HALOS, SUPERSYMMETRY, Very High Energy Gamma-ray Astronomy, MAGIC telescope, Dark Matter, Cosmology:dark matter, Raigs gamma, 0103 physical sciences, Satellite galaxy, 010303 astronomy & astrophysics, Cosmic rays, Dwarf galaxy, Physics, Annihilation, 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma rays, Gamma ray, Bremsstrahlung, Astronomy and Astrophysics, Galaxies, IMAGING CHERENKOV DETECTOR, Galàxies, Space and Planetary Science, gamma ray astronomy, Dark matter (Astronomy), Neutralino, Electrónica, Física nuclear, Matèria fosca (Astronomia), Electricidad
Abstract: We present the result of the observation of the ultrafaint dwarf galaxy Willman 1 performed with the 17 m MAGIC telescope during 15.5 hr between March and May 2008. No significant $\gamma$-ray emission was found. We derived upper limits of the order of $10^{-12}$ ph cm$^{-2}$ s$^{-1}$ on the integral flux above 100 GeV, which we compare with predictions from several of the established neutralino benchmark models in the mSUGRA parameter space. The neutralino annihilation spectra are defined after including the recently quantified contribution of internal bremsstrahlung from the virtual sparticles that mediate the annihilation. Flux boost factors of three orders of magnitude are required even in the most optimistic scenario to match our upper limits. However, uncertainties in the dark matter intrinsic and extrinsic properties (e.g., presence of substructures, Sommerfeld effect) may significantly reduce this gap., Comment: (6 pages, updated to match journal version and reference, Fig. 2 corrected)
Published: 2009
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92. Black hole physics. Black hole lightning due to particle acceleration at subhorizon scales

Author: J, Aleksić, S, Ansoldi, L A, Antonelli, P, Antoranz, A, Babic, P, Bangale, J A, Barrio, J, Becerra González, W, Bednarek, E, Bernardini, B, Biasuzzi, A, Biland, O, Blanch, S, Bonnefoy, G, Bonnoli, F, Borracci, T, Bretz, E, Carmona, A, Carosi, P, Colin, E, Colombo, J L, Contreras, J, Cortina, S, Covino, P, Da Vela, F, Dazzi, A, De Angelis, G, De Caneva, B, De Lotto, E, de Oña Wilhelmi, C, Delgado Mendez, D, Dominis Prester, D, Dorner, M, Doro, S, Einecke, D, Eisenacher, D, Elsaesser, M V, Fonseca, L, Font, K, Frantzen, C, Fruck, D, Galindo, R J, García López, M, Garczarczyk, D, Garrido Terrats, M, Gaug, N, Godinović, A, González Muñoz, S R, Gozzini, D, Hadasch, Y, Hanabata, M, Hayashida, J, Herrera, D, Hildebrand, J, Hose, D, Hrupec, W, Idec, V, Kadenius, H, Kellermann, K, Kodani, Y, Konno, J, Krause, H, Kubo, J, Kushida, A, La Barbera, D, Lelas, N, Lewandowska, E, Lindfors, S, Lombardi, F, Longo, M, López, R, López-Coto, A, López-Oramas, E, Lorenz, I, Lozano, M, Makariev, K, Mallot, G, Maneva, N, Mankuzhiyil, K, Mannheim, L, Maraschi, B, Marcote, M, Mariotti, M, Martínez, D, Mazin, U, Menzel, J M, Miranda, R, Mirzoyan, A, Moralejo, P, Munar-Adrover, D, Nakajima, A, Niedzwiecki, K, Nilsson, K, Nishijima, K, Noda, R, Orito, A, Overkemping, S, Paiano, M, Palatiello, D, Paneque, R, Paoletti, J M, Paredes, X, Paredes-Fortuny, M, Persic, J, Poutanen, P G, Prada Moroni, E, Prandini, I, Puljak, R, Reinthal, W, Rhode, M, Ribó, J, Rico, J, Rodriguez Garcia, S, Rügamer, T, Saito, K, Saito, K, Satalecka, V, Scalzotto, V, Scapin, C, Schultz, T, Schweizer, S N, Shore, A, Sillanpää, J, Sitarek, I, Snidaric, D, Sobczynska, F, Spanier, V, Stamatescu, A, Stamerra, T, Steinbring, J, Storz, M, Strzys, L, Takalo, H, Takami, F, Tavecchio, P, Temnikov, T, Terzić, D, Tescaro, M, Teshima, J, Thaele, O, Tibolla, D F, Torres, T, Toyama, A, Treves, M, Uellenbeck, P, Vogler, R, Zanin, M, Kadler, R, Schulz, E, Ros, U, Bach, F, Krauß, and J, Wilms
Abstract: Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.
Published: 2014

93. Discovery of very high energy gamma-ray emission from the blazar 1ES 0033+595 by the MAGIC telescopes

Author: T. Steinbring, A. González Muñoz, Natalia Lewandowska, D. Hildebrand, A. La Barbera, Daniela Dorner, X. Paredes-Fortuny, A. De Angelis, F. Borracci, M. Uellenbeck, Konstancja Satalecka, Michele Doro, S. Partini, S. Buson, Aaron Dominguez, Dario Hrupec, M. A. Lopez, K. Saito, U. Menzel, M. Gaug, J. Becerra González, Mario Meucci, Jelena Aleksić, R. López-Coto, Julian Sitarek, J. Hose, Daniela Hadasch, K. Nishijima, Takashi Saito, A. Niedzwiecki, J. Herrera, T. Toyama, Koji Noda, Giacomo Bonnoli, D. Dominis Prester, Reiko Orito, Diego F. Torres, Thomas Bretz, K. Frantzen, David Paneque, Elisa Bernardini, S. N. Shore, D. Nakajima, G. Maneva, Nikola Godinovic, Benito Marcote, R. Zanin, A. Saggion, P. G. Prada Moroni, M. Garczarczyk, Tihomir Surić, D. Carreto Fidalgo, Martin Makariev, M. I. Martínez, A. Borghese, E. Prandini, Oscar Blanch, O. Tibolla, V. Kadenius, P. Temnikov, Adrian Biland, Francisco Prada, S. Paiano, Lluis Font, Karl Mannheim, M. Hayashida, Victor Stamatescu, J. Krause, A. Herrero, B. De Lotto, J. Rico, Alicia López-Oramas, Stefano Covino, A. Sillanpää, K. Berger, M. Doert, C. Delgado Mendez, V. Tronconi, Hajime Takami, I. Lozano, Nijil Mankuzhiyil, G. De Caneva, S. Bonnefoy, Wolfgang Rhode, Aldo Treves, Sabrina Einecke, S. R. Gozzini, Robert Wagner, J. Rodriguez Garcia, Felix Spanier, W. Idec, P. Munar-Adrover, M. Palatiello, Francesco Dazzi, Masahiro Teshima, S. Sun, Christian Fruck, Daniel Ferenc, D. Tescaro, Yusuke Konno, Silvia Preziuso, Mosè Mariotti, A.-K. Overkemping, P. Da Vela, C. Schultz, V. Scapin, Ivica Puljak, Pierre Colin, Saverio Lombardi, Wlodek Bednarek, Alessandro Carosi, L. Maraschi, Elina Lindfors, E. Colombo, Julia Thaele, Daniel Mazin, Fabio Zandanel, Marc Ribó, L. O. Takalo, P. Bangale, Jose Miguel Miranda, R. Reinthal, Dominik Elsaesser, Hidetoshi Kubo, U. Barres de Almeida, Damir Lelas, R. Mirzoyan, M. V. Fonseca, P. Antoranz, Dorota Sobczyńska, D. Eisenacher, L. A. Antonelli, J. A. Barrio, E. Carmona, Fabrizio Tavecchio, Emanuele Paolo Farina, Nina Nowak, T. Schweizer, S. Rügamer, Tomislav Terzić, Patrick Vogler, I. Snidaric, Hanna Kellermann, K. Mallot, R. J. García López, E. Lorenz, Massimo Persic, J. M. Paredes, Antonio Stamerra, K. Kodani, J. Storz, Stefano Ansoldi, Riccardo Paoletti, J. Kushida, Jose Luis Contreras, Juan Cortina, D. Garrido Terrats, V. Scalzotto, Ana Babić, Kari Nilsson, and Abelardo Moralejo
Subjects: BL Lacertae objects: individual: (1ES 0033+595), Gamma-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.HE, astro-ph.CO, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, individual: (1ES 0033 595), gamma-rays: galaxies [BL Lacertae objects], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, BL Lacertae objects: individual: (1ES 0033 595), 01 natural sciences, Luminosity, 0103 physical sciences, MAGIC (telescope), education, Blazar, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, ta115, 010308 nuclear & particles physics, galaxies: BL Lacertae objects: individual (1ES 0033+595), gamma rays: galaxies, Compton scattering, Astronomy, Astrophysics - Astrophysics of Galaxies, Extragalactic background light, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Monthly Notices of the Royal Astronomical Society, 446 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
Published: 2014
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94. An active state of the BL Lac Object Markarian 421 detected by INTEGRAL in April 2013

Author: A. Stamerra, A. Bazzano, Aldo Treves, P. Romano, M. Villata, Simona Soldi, L. Maraschi, Carlo Ferrigno, S. Vercellone, M. Fiocchi, T. Pursimo, Gianluca Castignani, Filippo D'Ammando, Elena Pian, René Hudec, C. M. Raiteri, Fabrizio Tavecchio, P. Ubertini, Luigi Foschini, Volker Beckmann, R. Walter, Giuseppe Malaguti, R. Boissay, V. Bianchin, Marc Türler, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Brera (OAB), 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), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Pian E, Turler M, Fiocchi M, Boissay R, Bazzano A, Foschini L, Tavecchio F, Bianchin V, Castignani G, Ferrigno C, Raiteri CM, Villata M, Beckmann V, DAmmando F, Hudec R, Malaguti G, Maraschi L, Pursimo T, Romano P, Soldi S, Stamerra A, Treves A, Ubertini P, Vercellone S, Walter R, Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), 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), INAF-OAB, 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, FOS: Physical sciences, Synchrotron radiation, Astrophysics, law.invention, Apparent magnitude, law, gamma rays: galaxies, education, Blazar, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, education.field_of_study, Astronomy and Astrophysics, radiation mechanisms: non-thermal, Light curve, X-rays: galaxies, Space and Planetary Science, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: active / X-rays: galaxies / radiation mechanisms: non-thermal / gamma rays: galaxies, Fermi Gamma-ray Space Telescope, BL Lac object, Flare
Abstract: Multiwavelength variability of blazars offers indirect insight into their powerful engines and on the mechanisms through which energy is propagated from the centre down the jet. The BL Lac object Mkn 421 is a TeV emitter, a bright blazar at all wavelengths, and therefore an excellent target for variability studies. Mkn 421 was observed by INTEGRAL and Fermi-LAT in an active state on 16-21 April 2013. Well sampled optical, soft, and hard X-ray light curves show the presence of two flares. The average flux in the 20-100 keV range is 9.1e-11 erg/s/cm2 (~4.5 mCrab) and the nuclear average apparent magnitude, corrected for Galactic extinction, is V ~12.2. In the time-resolved X-ray spectra (3.5-60 keV), which are described by broken power laws and, marginally better, by log-parabolic laws, we see a hardening that correlates with flux increase, as expected in refreshed energy injections in a population of electrons that later cool via synchrotron radiation. The hardness ratios between the JEM-X fluxes in two different bands and between the JEM-X and IBIS/ISGRI fluxes confirm this trend. During the observation, the variability level increases monotonically from the optical to the hard X-rays, while the large LAT errors do not allow a significant assessment of the MeV-GeV variability. The cross-correlation analysis during the onset of the most prominent flare suggests a monotonically increasing delay of the lower frequency emission with respect to that at higher frequency, with a maximum time-lag of about 70 minutes, that is however not well constrained. The spectral energy distributions from the optical to the TeV domain are satisfactorily described by homogeneous models of blazar emission based on synchrotron radiation and synchrotron self-Compton scattering, except in the state corresponding to the LAT softest spectrum and highest flux., Comment: 11 pages, 6 figures, in press in A&A
Published: 2014
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95. Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes

Author: Nina Nowak, Abelardo Moralejo, D. Häfner, L. A. Antonelli, W. Idec, J. Masbou, M. I. Martínez, J. M. Paredes, Antonio Stamerra, M. Salvati, Dario Hrupec, Thomas Bretz, V. Kadenius, S. Rügamer, Mosè Mariotti, Marc Ribó, M. A. Lopez, Fabrizio Tavecchio, S. N. Shore, Juan Abel Barrio, D. Borla Tridon, Dominik Elsaesser, U. Barres de Almeida, S. Bonnefoy, K. Berger, Ll. Font, A. Hadamek, M. Doert, Emanuele Paolo Farina, Aaron Dominguez, J. Storz, G. De Caneva, Damir Lelas, R. Mirzoyan, Michael Backes, A. De Angelis, Christian Fruck, D. Eisenacher, J. Becerra González, Saverio Lombardi, T. Krähenbühl, M. L. Knoetig, Ignasi Reichardt, P. G. Prada Moroni, E. Carmona, I. Snidaric, Markus Garczarczyk, Nijil Mankuzhiyil, P. Munar-Adrover, Wolfgang Rhode, O. Tibolla, Dorota Sobczyńska, Kari Nilsson, M. V. Fonseca, Mario Meucci, Felix Spanier, M. Palatiello, E. Colombo, G. Maneva, Daniel Ferenc, A. Boller, L. Cossio, R. Zanin, A. Saggion, Ralph Bock, Nikola Godinovic, Benito Marcote, K. Mallot, R. J. García López, S. Spiro, E. Lorenz, Adrian Biland, Francesco Dazzi, L. O. Takalo, B. Steinke, Riccardo Paoletti, S. Partini, D. Dominis Prester, Artemio Herrero, J. Rico, K. Saito, J. Kushida, Jose Luis Contreras, Tomislav Terzić, J. Moldón, Francisco Prada, Juan Cortina, Hajime Takami, Ivica Puljak, Massimo Persic, Pierre Colin, R. Reinthal, Giacomo Bonnoli, Patrick Vogler, J. Krause, B. De Lotto, Martin Makariev, M. Asensio, Oscar Blanch, D. Garrido Terrats, A. Sillanpää, V. Scalzotto, Takashi Saito, Q. Weitzel, Tihomir Surić, Reiko Orito, C. Schultz, V. Scapin, D. Carreto Fidalgo, E. Prandini, Aldo Treves, S. Klepser, S. Paiano, C. Delgado Mendez, S. R. Gozzini, Karl Mannheim, Gianluca Giavitto, A. González Muñoz, Daniela Dorner, M. Gaug, Diego F. Torres, Elisa Bernardini, Natalia Lewandowska, F. Jankowski, F. Borracci, A. La Barbera, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Nakajima, Jose Miguel Miranda, P. Antoranz, L. Maraschi, M. Uellenbeck, Elina Lindfors, Konstancja Satalecka, Daniel Mazin, Michele Doro, P. Temnikov, Fabio Zandanel, Shan Sun, Jelena Aleksić, I. Lozano, D. Hadasch, Masahiro Teshima, A. Niedzwiecki, T. Schweizer, Stefano Covino, David Paneque, D. Tescaro, Robert Wagner, Victor Stamatescu, Julian Sitarek, J. Hose, T. Toyama, P. Da Vela, and Universitat de Barcelona
Subjects: Astrofísica, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Telescope, Raigs gamma, law, 0103 physical sciences, MAGIC (telescope), Nucli galàctic actiu, Blazar, 010303 astronomy & astrophysics, BL Lac objects: individual(1ES 1727+502), galaxies: active, gamma rays, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Active galactic nuclei, Telescopis, 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Galaxies: active, Space and Planetary Science, Galaxies, Galàxies, Crab Nebula, 13. Climate action, ddc:520, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Telescopes
Abstract: Motivated by the Costamante & Ghisellini (2002) predictions we investigated if the blazar 1ES 1727+502 (z=0.055) is emitting very high energy (VHE, E>100 GeV) gamma rays. We observed the BL Lac object 1ES 1727+502 in stereoscopic mode with the two MAGIC telescopes during 14 nights between May 6th and June 10th 2011, for a total effective observing time of 12.6 hours. For the study of the multiwavelength spectral energy distribution (SED) we use simultaneous optical R-band data from the KVA telescope, archival UV/optical and X-ray observations by instruments UVOT and XRT on board of the Swift satellite and high energy (HE, 0.1 GeV - 100 GeV) gamma-ray data from the Fermi-LAT instrument. We detect, for the first time, VHE gamma-ray emission from 1ES 1727+502 at a statistical significance of 5.5 sigma. The integral flux above 150 GeV is estimated to be (2.1\pm0.4)% of the Crab Nebula flux and the de-absorbed VHE spectrum has a photon index of (2.7\pm0.5). No significant short-term variability was found in any of the wavebands presented here. We model the SED using a one-zone synchrotron self-Compton model obtaining parameters typical for this class of sources., 7 pages, 5 figures, 2 tables, submitted to A&A
Published: 2014
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96. Optimized dark matter searches in deep observations of Segue 1 with MAGIC

Author: M. V. Fonseca, L. Maraschi, M. Palatiello, Daniel Ferenc, Antonio Stamerra, Christian Fruck, Juan Abel Barrio, I. Puljak, J. Kushida, K. Kodani, Mosè Mariotti, Abelardo Moralejo, A.-K. Overkemping, Stefano Covino, Jose Luis Contreras, Oscar Blanch, Tomislav Terzić, Francesco Dazzi, Daniela Dorner, Juan Cortina, T. Steinbring, J. Storz, R. J. García López, Fabio Zandanel, G. Bonnoli, Shan Sun, Nikola Godinovic, Benito Marcote, R. Zanin, P. Da Vela, Robert Wagner, D. Hadasch, A. Saggion, Tihomir Surić, D. Carreto Fidalgo, Jelena Aleksić, D. Tescaro, A. Niedzwiecki, Adrian Biland, David Paneque, B. De Lotto, Saverio Lombardi, D. Garrido Terrats, K. Frantzen, Nijil Mankuzhiyil, X. Paredes-Fortuny, D. Dominis Prester, Damir Lelas, D. Nakajima, Louis Antonelli, Elina Lindfors, Karl Mannheim, P. Munar-Adrover, P. G. Prada Moroni, Daniel Mazin, A. De Angelis, V. Scalzotto, Stefano Ansoldi, Konstancja Satalecka, Silvia Preziuso, Riccardo Paoletti, Markus Gaug, S. Rügamer, Michele Doro, C. Schultz, V. Scapin, Dario Hrupec, Aaron Dominguez, Marc Ribó, A. López-Oramas, M. Uellenbeck, Dorothee Hildebrand, Ana Babić, G. De Caneva, R. Reinthal, Alessandro Carosi, P. Antoranz, Hidetoshi Kubo, S. Bonnefoy, Ruben Lopez-Coto, J. Becerra González, Petar Temnikov, J. M. Paredes, J. Hose, Diego F. Torres, Jose Miguel Miranda, Kari Nilsson, M. López, Dorota Sobczyńska, Elisa Bernardini, D. Elsaesser, T. Schweizer, H. Kellermann, Yusuke Konno, O. Tibolla, U. Barres de Almeida, Mario Meucci, K. Berger, I. Lozano, M. Salvati, F. Borracci, W. Idec, R. K. Bock, Emanuele Paolo Farina, A. Sillanpää, M. Doert, Takashi Saito, Masahiro Teshima, Alejandro Ibarra, E. Colombo, Hajime Takami, Reiko Orito, G. Maneva, C. Delgado Mendez, Felix Spanier, Natalia Lewandowska, K. Saito, Julian Sitarek, Pierre Colin, Julia Thaele, Aldo Treves, L. O. Takalo, A. La Barbera, E. Carmona, M. I. Martínez, Kazuyoshi Nishijima, M. Hayashida, P. Bangale, Gianluca Giavitto, A. González Muñoz, V. Kadenius, Sabrina Einecke, S. R. Gozzini, Francisco Prada, J. Rodriguez Garcia, M. Makariev, J. Rico, Victor Stamatescu, U. Menzel, Simona Paiano, Thomas Bretz, R. Mirzoyan, Wolfgang Rhode, J. Krause, K. Mallot, Massimo Persic, Takeshi Toyama, I. Snidaric, D. Eisenacher, Markus Garczarczyk, Nina Nowak, E. Lorenz, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Elisa Prandini, Patrick Vogler, A. Herrero, S. Partini, Universitat de Barcelona, and SCOAP
Subjects: Astrofísica, Particle physics, Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, dark matter, indirect searches, gamma-ray experiments, Imaging Air Cherenkov Telescopes, dwarf spheroidal galaxies, Segue 1, Gamma ray experiments, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Gamma ray astronomy, Satellite galaxy, Astronomia de raigs gamma, ddc:530, 010306 general physics, Dwarf galaxies, Dwarf galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, Telescopis, 010308 nuclear & particles physics, Bremsstrahlung, Astronomy and Astrophysics, Segue, Galaxies, dwarfs galaxies, Galàxies, High Energy Physics - Phenomenology, Dark matter experiments, Dark matter (Astronomy), dark matter experiments, gamma ray experiments, Monochromatic color, Matèria fosca (Astronomia), Astrophysics - High Energy Astrophysical Phenomena, Telescopes
Abstract: Aleksic, J. et al., We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ~ 500 GeV dark matter particle annihilating into τ+τ−, and is of order langleσannvrangle simeq 1.2 × 10−24 cm3 s−1 — a factor ~ 40 above the langleσannvrangle simeq thermal value., The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider- Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the Croatian Science Foundation Project 09/176, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.
Published: 2014
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97. MAGIC long-term study of the distant TeV blazar PKS 1424+240 in a multiwavelength context

Author: Aaron Dominguez, Mosè Mariotti, A.-K. Overkemping, P. G. Prada Moroni, C. Schultz, V. Scapin, Anthony C. S. Readhead, A. González Muñoz, Hajime Takami, O. Tibolla, A. De Angelis, A. Treves, Saverio Lombardi, Daniela Dorner, Daniel Ferenc, S. Rügamer, Juan Abel Barrio, M. Gaug, J. Herrera, Koji Noda, Hanna Kellermann, Elisa Bernardini, G. Maneva, R. Zanin, A. Saggion, S. Partini, Antonio Stamerra, S. N. Shore, K. Kodani, Adrian Biland, Victor Stamatescu, C. Delgado Mendez, J. Rico, P. Temnikov, Stefano Covino, J. Storz, Nina Nowak, Fabio Zandanel, Nikola Godinovic, Benito Marcote, S. Sun, Jari Kotilainen, Julian Sitarek, S. Bonnefoy, D. Tescaro, C. Fruck, T. Toyama, M. Palatiello, Dario Gasparrini, D. Eisenacher, T. Schweizer, Stefano Ansoldi, M. Uellenbeck, Francesco Dazzi, Riccardo Paoletti, E. Carmona, Markus Garczarczyk, A. K. Furniss, Oscar Blanch, J. L. Richards, Elina Lindfors, K. Mallot, Daniel Mazin, R. J. García López, Matthew L. Lister, Konstancja Satalecka, E. Prandini, Michele Doro, Talvikki Hovatta, G. De Caneva, G. Bonnoli, M. Doert, Massimo Persic, P. Da Vela, Ivica Puljak, Pierre Colin, M. Makariev, D. Nakajima, Robert Wagner, R. Reinthal, Razmik Mirzoyan, U. Barres de Almeida, U. Menzel, Jelena Aleksić, Damir Lelas, I. Lozano, D. Hildebrand, W. Idec, M. V. Fonseca, A. Niedzwiecki, Vasiliki Pavlidou, Dorota Sobczyńska, David Paneque, Anne Lähteenmäki, A. Sillanpää, Masahiro Teshima, K. Nishijima, K. Saito, Tuomas Kangas, Takashi Saito, Dario Hrupec, D. Dominis Prester, D. Hadasch, M. I. Martínez, P. Bangale, Francisco Prada, Reiko Orito, Sabrina Einecke, S. R. Gozzini, J. Rodriguez Garcia, E. Colombo, Louis Antonelli, Felix Spanier, L. O. Takalo, Nijil Mankuzhiyil, X. Paredes-Fortuny, P. Munar-Adrover, Silvia Preziuso, M. A. Lopez, P. Antoranz, Natalia Lewandowska, A. La Barbera, Yusuke Konno, Julia Thaele, J. Becerra González, Mario Meucci, K. Frantzen, Tihomir Surić, D. Carreto Fidalgo, J. M. Paredes, V. Kadenius, S. Paiano, Karl Mannheim, M. Hayashida, Alicia López-Oramas, J. Krause, B. De Lotto, Marc Ribó, Diego F. Torres, Hidetoshi Kubo, Abelardo Moralejo, J. Hose, T. Steinbring, D. Elsaesser, A. Herrero, Emanuele Paolo Farina, S. Cutini, Kari Nilsson, Thomas Bretz, J. Kushida, Jose Luis Contreras, Juan Cortina, F. Borracci, D. Garrido Terrats, V. Scalzotto, Ana Babić, Walter Max-Moerbeck, Wolfgang Rhode, Alessandro Carosi, Ruben Lopez-Coto, Jose Miguel Miranda, W. Bednarek, Fabrizio Tavecchio, Ll. Font, I. Snidaric, E. Lorenz, Patrick Vogler, Erkki Kankare, L. Maraschi, Tomislav Terzić, Universitat de Barcelona, Metsähovi Radio Observatory, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Anne Lähteenmäki Group
Subjects: Astrofísica, PARTICLE-ACCELERATION, Astrophysics, 7. Clean energy, LARGE-AREA TELESCOPE, Spectral line, Raigs gamma, Gamma rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, MAGIC (telescope), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, BL-LACERTAE OBJECTS, EXTRAGALACTIC BACKGROUND LIGHT, GAMMA-RAY EMISSION, SPECTRAL ENERGY-DISTRIBUTION, ACTIVE GALACTIC NUCLEI, LAC OBJECTS, X-RAY, FERMI OBSERVATIONS, Gamma ray, Extragalactic background light, galaxies [gamma rays], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, 1171 Geosciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma rays: observations, blazar, BL Lac: AGNs: individual (PKS 1424+240), 114 Physical sciences, Nucli galàctic actiu, Blazar, Active galactic nuclei, Telescopis, 221 Nanotechnology, Gamma rays, Light curve, Redshift, individual: PKS 1424+240 [BL Lacertae objects], 115 Astronomy and space science, 216 Materials engineering, ddc:520, Telescopes
Abstract: We present a study of the very high energy (VHE; E > 100 GeV) gamma-ray emission of the blazar PKS 1424+240 observed with the MAGIC telescopes. The primary aim of this paper is the multiwavelength spectral characterization and modeling of this blazar, which is made particularly interesting by the recent discovery of a lower limit of its redshift of z > 0.6 and makes it a promising candidate to be the most distant VHE source. The source has been observed with the MAGIC telescopes in VHE gamma rays for a total observation time of ~33.6 h from 2009 to 2011. The source was marginally detected in VHE gamma rays during 2009 and 2010, and later, the detection was confirmed during an optical outburst in 2011. The combined significance of the stacked sample is ~7.2 sigma. The differential spectra measured during the different campaigns can be described by steep power laws with the indices ranging from 3.5 +/- 1.2 to 5.0 +/- 1.7. The MAGIC spectra corrected for the absorption due to the extragalactic background light connect smoothly, within systematic errors, with the mean spectrum in 2009-2011 observed at lower energies by the Fermi-LAT. The absorption-corrected MAGIC spectrum is flat with no apparent turn down up to 400 GeV. The multiwavelength light curve shows increasing flux in radio and optical bands that could point to a common origin from the same region of the jet. The large separation between the two peaks of the constructed non-simultaneous spectral energy distribution also requires an extremely high Doppler factor if an one zone synchrotron self-Compton model is applied. We find that a two-component synchrotron self-Compton model describes the spectral energy distribution of the source well, if the source is located at z~0.6., 15 pages, 8 figures. A&A accepted for publication
Published: 2014
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98. Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

Author: P. G. Prada Moroni, W. Bednarek, Pierre Colin, Diego F. Torres, D. Nakajima, Fabrizio Tavecchio, Stefano Covino, Ll. Font, Konstancja Satalecka, Michele Doro, Kouichi Hirotani, Nijil Mankuzhiyil, X. Paredes-Fortuny, Dario Hrupec, R. Zanin, A. Saggion, Adrian Biland, Kazuo Saito, P. Munar-Adrover, A. Treves, R. Reinthal, Shan Sun, A. Sillanpää, Antonio Stamerra, Silvia Preziuso, M. A. Lopez, Marc Ribó, Thomas Bretz, S. N. Shore, G. Maneva, Jelena Aleksić, Takashi Saito, A. Niedzwiecki, Abelardo Moralejo, J. Kushida, Jose Luis Contreras, J. M. Paredes, Hidetoshi Kubo, Reiko Orito, Natalia Lewandowska, U. Barres de Almeida, T. Steinbring, M. Makariev, A. Herrero, I. Puljak, M. V. Fonseca, E. Lorenz, M. Uellenbeck, D. Hadasch, J. Storz, Juan Cortina, D. Paneque, G. De Caneva, A. La Barbera, J. Rico, Christian Fruck, Elina Lindfors, S. Partini, Yusuke Konno, Emanuele Paolo Farina, U. Menzel, S. Bonnefoy, M. Doert, Daniel Mazin, Simona Paiano, B. Biasuzzi, Patrick Vogler, Daniel Ferenc, Elisa Prandini, P. Da Vela, T. Schweizer, Razmik Mirzoyan, S. Rügamer, B. De Lotto, L. Maraschi, Robert Wagner, J. Krause, I. Lozano, J. Becerra González, S. Ansoldi, Damir Lelas, M. I. Martínez, P. Bangale, V. Kadenius, Tomislav Terzić, D. Tescaro, G. Bonnoli, Hajime Takami, C. Delgado Mendez, Dorota Sobczyńska, Sabrina Einecke, Oscar Blanch, M. Hayashida, S. R. Gozzini, R. J. García López, N. Nowak, Kari Nilsson, Masahiro Teshima, Juan Abel Barrio, J. Rodriguez Garcia, Riccardo Paoletti, Markus Gaug, Nikola Godinovic, Benito Marcote, J. Hose, D. Garrido Terrats, Daniela Dorner, Takeshi Toyama, K. Mallot, W. Rhode, V. Scalzotto, D. Eisenacher, I. Šnidarić, K. Frantzen, M. Palatiello, Markus Garczarczyk, D. Elsaesser, Massimo Persic, Ana Babić, Petar Temnikov, Koji Noda, Elisa Bernardini, H. Kellermann, A. González Muñoz, C. Schultz, V. Scapin, Jose Carlos Herrera, Francesco Dazzi, A. López-Oramas, Karl Mannheim, Alessandro Carosi, Ruben Lopez-Coto, Jose Miguel Miranda, F. Borracci, T. Surić, Julia Thaele, E. Carmona, D. Fidalgo, Dorothee Hildebrand, P. Antoranz, M. Strzys, Julian Sitarek, Victor Stamatescu, Felix Spanier, K. Nishijima, D. Dominis Prester, Omar Tibolla, Louis Antonelli, A. De Angelis, K. Kodani, W. Idec, Mosè Mariotti, A.-K. Overkemping, Saverio Lombardi, E. Colombo, L. O. Takalo, and Universitat de Barcelona
Subjects: Astrofísica, Spectral shape analysis, Astrophysics::High Energy Astrophysical Phenomena, Theoretical models, FOS: Physical sciences, Gamma rays: stars, Pulsars: individual: Crab pulsar, Stars: neutron, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Spectral line, Raigs gamma, MAGIC (telescope), Connection (algebraic framework), pulsars: individual: Crab pulsar, gamma rays: stars, Pulsars, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Telescopis, Crab Pulsar, Gamma rays, Light curve, Stars, Púlsars, Estels, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Telescopes, Fermi Gamma-ray Space Telescope
Abstract: The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E>100GeV) gamma-rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. In order to test the new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. We analyzed 135 hours of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 4.6 years of {\it Fermi}-LAT data were also analyzed. The known two pulses per period were detected with a significance of $8.0 \sigma$ and $12.6 \sigma$. In addition, significant emission was found between the two pulses with $6.2 \sigma$. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models., Comment: 5 pages, 4 figures
Published: 2014
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99. Contemporaneous observations of the radio galaxy NGC 1275 from radio to very high energy gamma-rays

Author: M. Palatiello, A. La Barbera, R. Zanin, X. Paredes-Fortuny, A. Saggion, Adrian Biland, Francesco Dazzi, Abelardo Moralejo, K. Berger, M. Uellenbeck, D. Garrido Terrats, T. Schweizer, M. Salvati, A. Herrero, T. Steinbring, V. Scalzotto, J. Rico, C. Delgado Mendez, S. R. Gozzini, S. Rügamer, S. Bonnefoy, K. Frantzen, F. Borracci, Felix Spanier, Tihomir Surić, D. Carreto Fidalgo, P. Temnikov, P. Da Vela, D. Dominis Prester, D. Hildebrand, Nijil Mankuzhiyil, Dominik Elsaesser, R. Mirzoyan, Fabio Zandanel, U. Barres de Almeida, Shan Sun, P. Munar-Adrover, R. Reinthal, L. A. Antonelli, Silvia Preziuso, D. Eisenacher, W. Idec, Ana Babić, Daniela Dorner, Damir Lelas, S. Paiano, Francisco Prada, Karl Mannheim, E. Carmona, J. Kushida, K. Mallot, R. J. García López, Jose Luis Contreras, Julian Sitarek, M. Gaug, Stefano Covino, I. Lozano, E. Colombo, K. Saito, J. Hose, Dorota Sobczyńska, Juan Cortina, Daniela Hadasch, J. Krause, B. De Lotto, M. Doert, J. A. Barrio, A. De Angelis, A. López-Oramas, Thomas Bretz, Alessandro Carosi, Ralph Bock, Daniel Ferenc, Barbara Balmaverde, M. V. Fonseca, S. N. Shore, L. O. Takalo, D. Nakajima, T. Toyama, Masahiro Teshima, J. Becerra González, L. Font, Massimo Persic, Mosè Mariotti, A.-K. Overkemping, Ruben Lopez-Coto, Nikola Godinovic, A. Sillanpää, Benito Marcote, Elisa Bernardini, Fabrizio Tavecchio, Mario Meucci, Wolfgang Rhode, D. Tescaro, P. G. Prada Moroni, M. I. Martínez, G. Maneva, Hanna Kellermann, Giacomo Bonnoli, U. Menzel, Jose Miguel Miranda, I. Snidaric, Saverio Lombardi, Ivica Puljak, Pierre Colin, Diego F. Torres, V. Kadenius, O. Tibolla, R. Rekola, L. Maraschi, Sabrina Einecke, Kari Nilsson, Tomislav Terzić, Gianluca Giavitto, Reiko Orito, A. González Muñoz, M. Garczarczyk, Elina Lindfors, Daniel Mazin, J. Rodriguez Garcia, S. Partini, Nina Nowak, E. Lorenz, G. De Caneva, Martin Makariev, Oscar Blanch, Patrick Vogler, Aaron Dominguez, Christian Fruck, Dario Hrupec, W. Bednarek, M. A. Lopez, E. Prandini, Aldo Treves, C. Schultz, V. Scapin, P. Antoranz, M. L. Knoetig, Julia Thaele, Stefano Ansoldi, Riccardo Paoletti, J. M. Paredes, Jun Kataoka, Antonio Stamerra, A. Hadamek, Emanuele Paolo Farina, J. Storz, Robert Wagner, Y. Takahashi, Konstancja Satalecka, Michele Doro, Marc Ribó, Jelena Aleksić, P. Bangale, A. Niedzwiecki, David Paneque, Victor Stamatescu, Natalia Lewandowska, and Universitat de Barcelona
Subjects: Astrofísica, PARTICLE-ACCELERATION, Radio galaxy, Flux, Astrophysics, 01 natural sciences, Spectral line, LARGE-AREA TELESCOPE, MAGIC TELESCOPES, Raigs gamma, Jets (Astrofísica), Galaxies: active, Galaxies: individual: NGC 1275, Galaxies: jets, Gamma rays: galaxies, MAGIC (telescope), 010303 astronomy & astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, COSMIC-RAYS, galaxies: active, galaxies: jets, galaxies: individual (NGC1275/3C 84), gamma rays: galaxies, ACTIVE GALACTIC NUCLEI, PERSEUS CLUSTER, TEV EMISSION, 3C 84, CHANDRA VIEW, LAC OBJECTS, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, 010308 nuclear & particles physics, Gamma rays, Física atmosférica, Light curve, Galaxies, Galaxy, Galàxies, Astrophysical jets, Galàxies actives, Active galaxies, ddc:520
Abstract: The radio galaxy NGC 1275, recently identified as a very high energy (VHE, >100 GeV) gamma-ray emitter by MAGIC, is one of the few non-blazar AGN detected in the VHE regime. In order to better understand the origin of the gamma-ray emission and locate it within the galaxy, we studied contemporaneous multi-frequency observations of NGC 1275 and modeled the overall spectral energy distribution (SED). We analyzed unpublished MAGIC observations carried out between Oct. 2009 and Feb. 2010, and the previously published ones taken between Aug. 2010 and Feb. 2011. We studied the multi-band variability and correlations by analyzing data of Fermi-LAT (0.1-100 GeV), as well as Chandra (X-ray), KVA (optical) and MOJAVE (radio) data taken during the same period. Using customized Monte Carlo simulations corresponding to early MAGIC stereo data, we detect NGC 1275 also in the earlier campaign. The flux level and energy spectra are similar to the results of the second campaign. The monthly light curve >100 GeV shows a hint of variability at the 3.6 sigma level. In the Fermi-LAT band, both flux and spectral shape variabilities are reported. The optical light curve is variable and shows a clear correlation with the gamma-ray flux >100 MeV. In radio, 3 compact components are resolved in the innermost part of the jet. One of them shows a similar trend as the LAT and KVA light curves. The 0.1-650 GeV spectra measured simultaneously with MAGIC and Fermi-LAT can be well fitted either by a log-parabola or by a power-law with a sub-exponential cutoff for both campaigns. A single-zone synchrotron-self-Compton model, with an electron spectrum following a power-law with an exponential cutoff, can explain the broadband SED and the multi-band behavior of the source. However, this model suggests an untypical low bulk-Lorentz factor or a velocity alignment closer to the line of sight than the pc-scale radio jet., 14 pages, 11 figures, accepted for publication in A&A
Published: 2014
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100. Theoretical Implications from the Spectral Evolution of Markarian 501 Observed withBeppoSAX

Author: Elena Pian, C. M. Raiteri, Aldo Treves, M. Villata, A. Djannati-Ataï, Rita M. Sambruna, Annalisa Celotti, L. Maraschi, C. M. Urry, Eliana Palazzi, L. Chiappetti, Giovanni Fossati, G. Ghisellini, and Fabrizio Tavecchio
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Flux, Astronomy and Astrophysics, Astrophysics, Synchrotron, Spectral line, law.invention, Luminosity, Synchrotron emission, Spectral evolution, Space and Planetary Science, Homogeneous, law, Blazar
Abstract: We present new BeppoSAX observations of the TeV-emitting blazar Mrk 501 performed in 1999 June and a homogeneous reanalysis of all the BeppoSAX observations during the period from 1997 April to 1999 June. Recently published TeV spectra by the Cerenko Array at Themis, which are quasi-simultaneous with the 1997 BeppoSAX pointings, are used to constrain further the physical parameters of the jet in 1997 April with detailed models of the X-ray and TeV components. During the 1997-1999 period, the peak frequency of the synchrotron emission moved from about 100 keV in 1997 April to 0.5 keV in 1999 June. The shift in the peak frequency appears to be correlated with the long-term luminosity decrease. We interpret the results in the framework of a homogeneous synchrotron self-Compton model, discussing the evolution of the physical parameters of the emitting region under simple assumptions for the variability model. We also compute the expected variations of the TeV flux under the same assumptions.
Published: 2001
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