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33 results on '"Collaboration, MAGIC"'

1. Broadband Multi-wavelength Properties of M87 during the 2018 EHT Campaign including a Very High Energy Flaring Episode

Author

group, The Event Horizon Telescope - Multi-wavelength science working, Collaboration, The Event Horizon Telescope, Collaboration, The Fermi Large Area Telescope, Collaboration, H. E. S. S., Collaboration, MAGIC, Collaboration, VERITAS, and Collaboration, EAVN

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

The nearby elliptical galaxy M87 contains one of the only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87*, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity. The MWL campaign took place in April 2018, overlapping with the EHT M87* observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high energy (VHE) gamma-rays, as well as details of the individual observations and light curves. We also conduct phenomenological modelling to investigate the basic source properties. We present the first VHE gamma-ray flare from M87 detected since 2010. The flux above 350 GeV has more than doubled within a period of about 36 hours. We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE gamma-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and emphasises the need for combined image and spectral modelling., Comment: 46 pages, 23 figures, submitted to Astronomy & Astrophysics

Published
2024

2. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Balokovic, M., Chandra, S., Cui, Y. -Z., Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y., Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S., Lu, R. -S., Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Collaboration, The Event Horizon Telescope, Collaboration, The Fermi Large Area Telescope, Collaboration, H. E. S. S., Collaboration, MAGIC, Collaboration, VERITAS, and Collaboration, EAVN

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass approximately 6.5 x 10^9 M_solar. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87's spectrum. We can exclude that the simultaneous gamma-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the gamma-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded., Comment: 43 pages, 19 figures, 10 tables; complete author list available in manuscript; The Astrophysical Journal Letters, 2021, 911, L11; publication doi: 3847/2041-8213/abef71, data doi: 10.25739/mhh2-cw46

Published
2021
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3. Observation of a sudden cessation of a very-high-energy gamma-ray flare in PKS 1510-089 with H.E.S.S. and MAGIC in May 2016

Author

Collaboration, H. E. S. S., Abdalla, H., Adam, R., Aharonian, F., Benkhali, F. Ait, Angüner, E. O., Arcaro, C., Arm, C., Armstrong, T., Ashkar, H., Backes, M., Baghmanyan, V., Martins, V. Barbosa, Barnacka, A., Barnard, M., Becherini, Y., Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., de Lavergne, M. de Bony, Bregeon, J., Breuhaus, M., Brun, F., Brun, P., Bryan, M., Büchele, M., Bulik, T., Bylund, T., Caroff, S., Carosi, A., Casanova, S., Ch, T., Ch, S., Chen, A., Cotter, G., Curyło, M., Mbarubucyeye, J. Damascene, Davids, I. D., Davies, J., Deil, C., Devin, J., deWilt, P., Dirson, L., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Dyks, J., Egberts, K., Eichhorn, F., Einecke, S., Emery, G., Ernenwein, J. -P., Feijen, K., Fegan, S., Fiasson, A., de Clairfontaine, G. Fichet, Filipovic, M., Fontaine, G., Funk, S., Füßling, M., Gabici, S., Gallant, Y. A., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Gottschall, D., Grondin, M. -H., Hahn, J., Haupt, M., Hermann, G., Hinton, J. A., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Hörbe, M., Horns, D., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jardin-Blicq, A., Joshi, V., Jung-Richardt, I., Kastendieck, M. A., Katarzyński, K., Katz, U., Khangulyan, D., Khélifi, B., Klepser, S., Kluźniak, W., Komin, Nu., Konno, R., Kosack, K., Kostunin, D., Kreter, M., Lamanna, G., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Levy, C., Lohse, T., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Mar, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Nakashima, K., Nayerhoda, A., de Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O'Brien, P., Odaka, H., Ohm, S., Olivera-Nieto, L., Wilhelmi, E. de Ona, Ostrowski, M., Panter, M., Panny, S., Parsons, R. D., Peron, G., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Noel, A. Priyana, Prokhorov, D. A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ruiz-Velasco, E., Sahakian, V., Sailer, S., Sanchez, D. A., Santangelo, A., Sasaki, M., Scalici, M., Schüssler, F., Schutte, H. M., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Sun, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tavernier, T., Taylor, A. M., Terrier, R., Tiziani, D., Tluczykont, M., Tomankova, L., Trichard, C., Tsirou, M., Tuffs, R., Uchiyama, Y., van der Walt, D. J., van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Yu Wun, Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zorn, J., Zouari, S., Żywucka, N., Collaboration, MAGIC, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Asano, K., Baack, D., Babić, A., Baquero, A., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Bil, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Amico, G., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., neira, E. Do Souto Espi\, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Loporchio, S., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Mir, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., nil, P. Pe\, Perennes, C., Persic, M., Moroni, P. G. Prada, Pr, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., Truzzi, S., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., Jorstad, S. G., Marscher, A. P., Boccardi, B., Casadio, C., Hodgson, J., Kim, J. -Y., Krichbaum, T. P., Lähteenmäki, A., Tornikoski, M., Traianou, E., and Weaver, Z. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behavior, and is one of only a few FSRQs detected at very high energy (VHE, $E>100\,$GeV) $\gamma$-rays. VHE $\gamma$-ray observations with H.E.S.S. and MAGIC during late May and early June 2016 resulted in the detection of an unprecedented flare, which reveals for the first time VHE $\gamma$-ray intranight variability in this source. While a common variability timescale of $1.5\,$hr is found, there is a significant deviation near the end of the flare with a timescale of $\sim 20\,$min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, curvature is detected in the VHE $\gamma$-ray spectrum of PKS 1510-089, which is fully explained through absorption by the extragalactic background light. Optical R-band observations with ATOM reveal a counterpart of the $\gamma$-ray flare, even though the detailed flux evolution differs from the VHE ightcurve. Interestingly, a steep flux decrease is observed at the same time as the cessation of the VHE flare. In the high energy (HE, $E>100\,$MeV) $\gamma$-ray band only a moderate flux increase is observed with Fermi-LAT, while the HE $\gamma$-ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the $\gamma$-ray spectrum indicates that the emission region is located outside of the BLR. Radio VLBI observations reveal a fast moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located $\sim 50\,$pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this correlation is indeed true, VHE $\gamma$ rays have been produced far down the jet where turbulent plasma crosses a standing shock., Comment: 25 pages, 17 figures. Accepted for publication by Astronomy & Astrophysics. Corresponding authors: M. Zacharias, J. Sitarek, D. Sanchez, T. Terzic

Published
2020
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4. MAGIC Highlights

Author

Paredes, Josep M. and Collaboration, MAGIC

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

MAGIC has been exploring the sky at Very High Energy gamma-rays (50 GeV - 50 TeV) since 2004, operating first with a single telescope and from 2009 with two telescopes in stereoscopic mode. MAGIC has carried out a observational program involving fundamental physics and astrophysics topics. In this paper we present some of the most important results obtained by MAGIC, with a special emphasis in the most recent ones., Comment: 11 pages, 5 figures, Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources - XIII - (MULTIF2019), 3-8 June 2019 Mondello (Palermo), Italy

Published
2020

5. Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period

Author

The VERITAS Collaboration, Abeysekara, A. U., Benbow, W., Bird, R., Brill, A., Brose, R., Buckley, J. H., Chromey, A. J., Daniel, M. K., Falcone, A., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Gillanders, G. H., Hanna, D., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Kaaret, P., Kar, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Pueschel, E., Quinn, J., Ragan, K., Richards, G. T., Roache, E., Sadeh, I., Santander, M., Schlenstedt, S., Sembroski, G. H., Sushch, I., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Williamson, T. J, Zitzer, B., Collaboration, MAGIC, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Busetto, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Espiñera, E. Do Souto, Domínguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nöthe, M., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Will, M., and Zarić, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on observations of the pulsar / Be star binary system PSR J2032+4127 / MT91 213 in the energy range between 100 GeV and 20 TeV with the VERITAS and MAGIC imaging atmospheric Cherenkov telescope arrays. The binary orbit has a period of approximately 50 years, with the most recent periastron occurring on 2017 November 13. Our observations span from 18 months prior to periastron to one month after. A new, point-like, gamma-ray source is detected, coincident with the location of PSR J2032+4127 / MT91 213. The gamma-ray light curve and spectrum are well-characterized over the periastron passage. The flux is variable over at least an order of magnitude, peaking at periastron, thus providing a firm association of the TeV source with the pulsar / Be star system. Observations prior to periastron show a cutoff in the spectrum at an energy around 0.5 TeV. This result adds a new member to the small population of known TeV binaries, and it identifies only the second source of this class in which the nature and properties of the compact object are firmly established. We compare the gamma-ray results with the light curve measured with the X-ray Telescope (XRT) on board the Neil Gehrels \textit{Swift} Observatory and with the predictions of recent theoretical models of the system. We conclude that significant revision of the models is required to explain the details of the emission we have observed, and we discuss the relationship between the binary system and the overlapping steady extended source, TeV J2032+4130., Comment: 12 pages, 3 figures, 1 table. Accepted for publication in ApJL

Published
2018
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6. Discovery of TeV gamma-ray emission from the Pulsar Wind Nebula 3C 58 by MAGIC

Author

Bigas, O. Blanch, Lopez, R., Carmona, E., Collaboration, MAGIC, and Pérez-Torres, M. A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Pulsar Wind Nebula (PWN) 3C 58 is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared to the Crab Nebula due to their morphological similarities. This object was detected by Fermi-LAT with a spectrum extending beyond 100 GeV. We analyzed 81 hours of 3C 58 data taken with the MAGIC telescopes and we detected VHE gamma-ray emission for the first time at TeV energies with a significance of 5.7 sigma and an integral flux of 0.65% C.U. above 1 TeV. The differential energy spectrum between 400 GeV and 10 TeV is well described by a power-law function $d\Phi/dE=f_{o}(E/1TeV)^{-\Gamma}$ with $f_{o}=(2.0\pm0.4stat\pm0.6sys) 10^{-13}cm^{-2}s^{-1}TeV^{-1}$ and $\Gamma=2.4\pm0.2sta\pm0.2sys$. This leads 3C 58 to be the least luminous PWN ever detected at VHE and the one with the lowest flux at VHE to date. According to time-dependent models in which electrons up-scatter photon fields, the best representation favors a distance to the PWN of 2 kpc and FIR comparable to CMB photon fields. If we consider an unexpectedly high FIR density, the data can also be reproduced by models assuming a 3.2 kpc distance. A low magnetic field, far from equipartition, is required to explain the VHE data. Hadronic contribution from the hosting supernova remnant (SNR) requires unrealistic energy budget given the density of the medium, disfavoring cosmic ray acceleration in the SNR as origin of the VHE gamma-ray emission., Comment: 2014 Fermi Symposium proceedings - eConf C14102.1

Published
2015

7. The variability patterns of the TeV blazar PG 1553 + 113 from a decade of MAGIC and multiband observations.

Author

Collaboration:, MAGIC and collaborators:, MWL

Subjects
*BL Lacertae objects, *MAGIC, *RADIO telescopes
Abstract

PG 1553 + 113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m and Medicina radio telescopes, REM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p -value. The complex connection between the low- and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required. [ABSTRACT FROM AUTHOR]

Published
2024
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8. The MAGIC highlights of the gamma ray binary LS I +61 303

Author

Jogler, T., Puchades, N., Bigas, O. Blanch, Bosch-Ramon, V., Cortina, J., Moldón, J., Paredes, J. M., Perez-Torres, M. A., Ribó, M., Rico, J., Torres, D. F., Zabalza, V., and collaboration, MAGIC

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The discovery of emission of TeV gamma rays from X-ray binaries has triggered an intense effort to better understand the particle acceleration, absorption, and emission mechanisms in compact binary systems. Here we present the pioneering effort of the MAGIC collaboration to understand the very high energy emission of the prototype system LS I +61 303. We report on the variable nature of the emission from LS I +61 303 and show that this emission is indeed periodic. The system shows regular outburst at TeV energies in phase phi=0.6-0.7 and detect no signal at periastron (phi~ 0.275). Furthermore we find no indication of spectral variation along the orbit of the compact object and the spectral energy distribution is compatible with a simple power law with index Gamma=2.6+-0.2_(stat)+-0.2_(sys). To answer some of the open questions concerning the emission process of the TeV radiation we conducted a multiwavelength campaign with the MAGIC telescope, XMM-Newton, and Swift in September 2007. We detect a simultaneous outburst at X-ray and TeV energies, with the peak at phase 0.62 and a similar shape at both wavelengths. A linear fit to the strictly simultaneous X-ray/TeV flux pairs provides r=0.81 -0.21 +0.06. Here we present the observations and discuss the implications of the obtained results to the emission processes in the system., Comment: 4 pages, 3 figures, Contribution to the 31st ICRC 2009 Lodz

Published
2009

9. Suzaku and Multi-wavelength Observations of OJ 287 during the Periodic Optical Outburst in 2007

Author

Seta, Hiromi, Isobe, Naoki, Tashiro, Makoto S., Yaji, Yuichi, Arai, Akira, Fukuhara, Masayuki, Kohno, Kotaro, Nakanishi, Koichiro, Sasada, Mahito, Shimajiri, Yoshito, Tosaki, Tomoka, Uemura, Makoto, and collaboration, MAGIC

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Suzaku observations of the blazar OJ 287 were performed in 2007 April 10--13 and November 7--9. They correspond to a quiescent and a flaring state, respectively. The X-ray spectra can be well described with single power-law models in both exposures. The derived X-ray photon index and the flux density at 1 keV were found to be Gamma = 1.65 +- 0.02 and S_{1 keV} = 215 +- 5 nJy, in the quiescent state. In the flaring state, the source exhibited a harder X-ray spectrum (Gamma = 1.50 +- 0.01) with a nearly doubled X-ray flux density S_{1 keV} = 404^{+6}_{-5} nJy. Moreover, significant hard X-ray signals were detected up to ~ 27 keV. In cooperation with the Suzaku, simultaneous radio, optical, and very-high-energy gamma-ray observations were performed with the Nobeyama Millimeter Array, the KANATA telescope, and the MAGIC telescope, respectively. The radio and optical fluxes in the flaring state (3.04 +- 0.46 Jy and 8.93 +- 0.05 mJy at 86.75 Hz and in the V-band, respectively) were found to be higher by a factor of 2--3 than those in the quiescent state (1.73 +- 0.26 Jy and 3.03 +- 0.01 mJy at 86.75 Hz and in the V-band, respectively). No notable gamma-ray events were detected in either observation. The spectral energy distribution indicated that the X-ray spectrum was dominated by inverse Compton radiation in both observations, while synchrotron radiation exhibited a spectral cutoff around the optical frequency. Furthermore, no significant difference in the synchrotron cutoff frequency was found between the quiescent and flaring states. According to a simple synchrotron self-Compton model, the change of the spectral energy distribution is due to an increase in the energy density of electrons with small changes of both the magnetic field strength and the maximum Lorentz factor of electrons., Comment: 22 pages, 8 figures; accepted for publication in PASJ

Published
2009
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10. The June 2008 flare of Markarian 421 from optical to TeV energies

Author

The Agile Collaboration, Collaboration, Gasp-Webt, Collaboration, Magic, Collaboration, Veritas, and Donnarumma, I.

Subjects
Astrophysics
Abstract

We present optical, X-ray, high energy ($\lessapprox 30$ GeV) and very high energy ($\gtrapprox 100$ GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high energy $\gamma$-ray signal was detected by AGILE with \sqrt{TS}=4.5 on June 9--15, with $F(E>100 \mathrm{MeV})= 42^{+14}_{-12}\times 10^{-8}$ photons cm$^{-2}$ s$^{-1}$. This flaring state is brighter than the average flux observed by EGRET by a factor of $\sim$3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a 5-day flare (June 9-15) peaking at $\sim$ 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 $\times 10^{-9}$ erg cm$^{-2}$ s$^{-1}$ (i.e. > 100 mCrab). A peak synchrotron energy of $\sim$3 keV was derived, higher than typical values of $\sim$0.5-1 keV. VHE observations with MAGIC and VERITAS on June 6-8 show the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a twelve-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. The $\gamma$-ray flare can be interpreted within the framework of the synchrotron self-Compton model in terms of a rapid acceleration of leptons in the jet., Comment: accepted for publication in ApJL, 7 pages, 2 figures, 1 table

Published
2008
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11. Observation of Gamma Rays from the Galactic Center with the MAGIC Telescope

Author

Albert, J. and collaboration, MAGIC

Subjects
Astrophysics
Abstract

Recently, the Galactic Center has been reported to be a source of very high energy (VHE) gamma-rays by the VERITAS, CANGAROO and HESS experiments. The energy spectra as measured by these experiments show substantial differences. In this Letter we present MAGIC observations of the Galactic Center, resulting in the detection of a differential gamma-ray flux consistent with a steady, hard-slope power law, described as dN/(dA dt dE) = (2.9+/-0.6)*10^{-12} (E/TeV)^{-2.2+/-0.2} cm^{-2}s^{-1}TeV^{-1}. The gamma-ray source is centered at (Ra, Dec)=(17h 45m 20s, -29deg 2'. This result confirms the previous measurements by the HESS experiment and indicates a steady source of TeV gamma-rays. We briefly describe the observational technique used, the procedure implemented for the data analysis, and discuss the results in the perspective of different models proposed for the acceleration of the VHE gamma-rays., Comment: ApJL submitted

Published
2005
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12. MAGIC observations of very high energy gamma-rays from HESS J1813-178

Author

Albert, J. and collaboration, MAGIC

Subjects
Astrophysics
Abstract

Recently, the HESS collaboration has reported the detection of gamma-ray emission above a few hundred GeV from eight new sources located close to the Galactic Plane. The source HESS J1813-178 has sparked particular interest, as subsequent radio observations imply an association with SNR G12.82-0.02. Triggered by the detection in VHE gamma-rays, a positionally coincident source has also been found in INTEGRAL and ASCA data. In this Letter we present MAGIC observations of HESS J1813-178, resulting in the detection of a differential gamma-ray flux consistent with a hard-slope power law, described as dN/(dA dt dE) = (3.3+/-0.5)*10^{-12} (E/TeV)^{-2.1+/-0.2} cm^(-2)s^(-1)TeV^(-1). We briefly discuss the observational technique used, the procedure implemented for the data analysis, and put this detection in the perspective of multifrequency observations., Comment: Accepted by ApJ Letters

Published
2005
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14. Unraveling the Complex Behavior of Mrk 421 with Simultaneous X-Ray and VHE Observations during an Extreme Flaring Activity in 2013 April *

Author

Acciari, V. A., primary, Ansoldi, S., additional, Antonelli, L. A., additional, Engels, A. Arbet, additional, Baack, D., additional, Babić, A., additional, Banerjee, B., additional, de Almeida, U. Barres, additional, Barrio, J. A., additional, González, J. Becerra, additional, Bednarek, W., additional, Bellizzi, L. K., additional, Bernardini, E., additional, Berti, A., additional, Besenrieder, J., additional, Bhattacharyya, W., additional, Bigongiari, C., additional, Biland, A., additional, Blanch, O., additional, Bonnoli, G., additional, Bošnjak, Ž., additional, Busetto, G., additional, Carosi, R., additional, Ceribella, G., additional, Cerruti, M., additional, Chai, Y., additional, Chilingarian, A., additional, Cikota, S., additional, Colak, S. M., additional, Colin, U., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, D’Elia, V., additional, Vela, P. Da, additional, Dazzi, F., additional, Angelis, A. De, additional, Lotto, B. De, additional, Puppo, F. Del, additional, Delfino, M., additional, Delgado, J., additional, Depaoli, D., additional, Pierro, F. Di, additional, Venere, L. Di, additional, Souto Espiñeira, E. Do, additional, Prester, D. Dominis, additional, Donini, A., additional, Dorner, D., additional, Doro, M., additional, Elsaesser, D., additional, Ramazani, V. Fallah, additional, Fattorini, A., additional, Ferrara, G., additional, Foffano, L., additional, Fonseca, M. V., additional, Font, L., additional, Fruck, C., additional, Fukami, S., additional, López, R. J. García, additional, Garczarczyk, M., additional, Gasparyan, S., additional, Gaug, M., additional, Giglietto, N., additional, Giordano, F., additional, Gliwny, P., additional, Godinović, N., additional, Green, D., additional, Hadasch, D., additional, Hahn, A., additional, Hassan, T., additional, Herrera, J., additional, Hoang, J., additional, Hrupec, D., additional, Hütten, M., additional, Inada, T., additional, Inoue, S., additional, Ishio, K., additional, Iwamura, Y., additional, Jouvin, L., additional, Kajiwara, Y., additional, Kerszberg, D., additional, Kobayashi, Y., additional, Kubo, H., additional, Kushida, J., additional, Lamastra, A., additional, Lelas, D., additional, Leone, F., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, López-Coto, R., additional, López-Oramas, A., additional, Loporchio, S., additional, de Oliveira Fraga, B. Machado, additional, Maggio, C., additional, Majumdar, P., additional, Makariev, M., additional, Mallamaci, M., additional, Maneva, G., additional, Manganaro, M., additional, Mannheim, K., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Mender, S., additional, Mićanović, S., additional, Miceli, D., additional, Miener, T., additional, Minev, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Molina, E., additional, Moralejo, A., additional, Morcuende, D., additional, Moreno, V., additional, Moretti, E., additional, Munar-Adrover, P., additional, Neustroev, V., additional, Nigro, C., additional, Nilsson, K., additional, Ninci, D., additional, Nishijima, K., additional, Noda, K., additional, Nogués, L., additional, Nozaki, S., additional, Ohtani, Y., additional, Oka, T., additional, Otero-Santos, J., additional, Palatiello, M., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Pavletić, L., additional, Peñil, P., additional, Peresano, M., additional, Persic, M., additional, Moroni, P. G. Prada, additional, Prandini, E., additional, Puljak, I., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Righi, C., additional, Rugliancich, A., additional, Saha, L., additional, Sahakyan, N., additional, Saito, T., additional, Sakurai, S., additional, Satalecka, K., additional, Schleicher, B., additional, Schmidt, K., additional, Schweizer, T., additional, Sitarek, J., additional, Šnidarić, I., additional, Sobczynska, D., additional, Spolon, A., additional, Stamerra, A., additional, Strom, D., additional, Strzys, M., additional, Suda, Y., additional, Surić, T., additional, Takahashi, M., additional, Tavecchio, F., additional, Temnikov, P., additional, Terzić, T., additional, Teshima, M., additional, Torres-Albà, N., additional, Tosti, L., additional, Scherpenberg, J. van, additional, Vanzo, G., additional, Acosta, M. Vazquez, additional, Ventura, S., additional, Verguilov, V., additional, Vigorito, C. F., additional, Vitale, V., additional, Vovk, I., additional, Will, M., additional, Zarić, D., additional, Collaboration), (MAGIC, additional, Petropoulou, M., additional, Finke, J., additional, D’Ammando, F., additional, Baloković, M., additional, Madejski, G., additional, Mori, K., additional, Puccetti, Simonetta, additional, Leto, C., additional, Perri, M., additional, Verrecchia, F., additional, Villata, M., additional, Raiteri, C. M., additional, Agudo, I., additional, Bachev, R., additional, Berdyugin, A., additional, Blinov, D. A., additional, Chanishvili, R., additional, Chen, W. P., additional, Chigladze, R., additional, Damljanovic, G., additional, Eswaraiah, C., additional, Grishina, T. S., additional, Ibryamov, S., additional, Jordan, B., additional, Jorstad, S. G., additional, Joshi, M., additional, Kopatskaya, E. N., additional, Kurtanidze, O. M., additional, Kurtanidze, S. O., additional, Larionova, E. G., additional, Larionova, L. V., additional, Larionov, V. M., additional, Latev, G., additional, Lin, H. C., additional, Marscher, A. P., additional, Mokrushina, A. A., additional, Morozova, D. A., additional, Nikolashvili, M. G., additional, Semkov, E., additional, Smith, P. S., additional, Strigachev, A., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Vince, O., additional, Barnes, J., additional, Güver, T., additional, Moody, J. W., additional, Sadun, A. C., additional, Hovatta, T., additional, Richards, J. L., additional, Max-Moerbeck, W., additional, Readhead, A. C. S., additional, Lähteenmäki, A., additional, Tornikoski, M., additional, Tammi, J., additional, Ramakrishnan, V., additional, and Reinthal, R., additional

Published
2020
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15. First detection of VHE gamma-ray emission from TXS 1515–273, study of its X-ray variability and spectral energy distribution.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Artero, M, Asano, K, Baack, D, Babić, A, Baquero, A, Barres de Almeida, U, Barrio, J A, Batković, I, Becerra González, J, Bednarek, W, Bellizzi, L, Bernardini, E, Bernardos, M, Berti, A, and Besenrieder, J

Subjects
*SPECTRAL energy distribution, *X-rays, *HARD X-rays, *MAGNETIC flux density, *CRAB Nebula, *SOLAR flares
Abstract

We report here on the first multiwavelength (MWL) campaign on the blazar TXS 1515–273, undertaken in 2019 and extending from radio to very-high-energy gamma-rays (VHE). Up until now, this blazar had not been the subject of any detailed MWL observations. It has a rather hard photon index at GeV energies and was considered a candidate extreme high-synchrotron-peaked source. MAGIC observations resulted in the first-time detection of the source in VHE with a statistical significance of 7.6σ. The average integral VHE flux of the source is 6 ± 1 per cent of the Crab nebula flux above 400 GeV. X-ray coverage was provided by Swift -XRT, XMM–Newton , and NuSTAR. The long continuous X-ray observations were separated by ∼9 h, both showing clear hour scale flares. In the XMM–Newton data, both the rise and decay time-scales are longer in the soft X-ray than in the hard X-ray band, indicating the presence of a particle cooling regime. The X-ray variability time-scales were used to constrain the size of the emission region and the strength of the magnetic field. The data allowed us to determine the synchrotron peak frequency and classify the source as a flaring high, but not extreme synchrotron-peaked object. Considering the constraints and variability patterns from the X-ray data, we model the broad-band spectral energy distribution. We applied a simple one-zone model, which could not reproduce the radio emission and the shape of the optical emission, and a two-component leptonic model with two interacting components, enabling us to reproduce the emission from radio to VHE band. [ABSTRACT FROM AUTHOR]

Published
2021
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16. Studying the nature of the unidentified gamma-ray source HESS J1841−055 with the MAGIC telescopes.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Asano, K, Baack, D, Babić, A, Banerjee, B, Baquero, A, Barres de Almeida, U, Barrio, J A, Becerra González, J, Bednarek, W, Bellizzi, L, Bernardini, E, Bernardos, M, Berti, A, Besenrieder, J, and Bhattacharyya, W

Subjects
*SPECTRAL energy distribution, *TELESCOPES, *GAMMA rays, *MOLECULAR clouds, *HADRONIC atoms
Abstract

We investigate the physical nature and origin of the gamma-ray emission from the extended source HESS J1841−055 observed at TeV and GeV energies. We observed HESS J1841−055 at TeV energies for a total effective time of 43 h with the MAGIC telescopes, in 2012 and 2013. Additionally, we analysed the GeV counterpart making use of about 10 yr of Fermi -LAT data. Using both Fermi -LAT and MAGIC, we study both the spectral and energy-dependent morphology of the source for almost four decades of energy. The origin of the gamma-ray emission from this region is investigated using multiwaveband information on sources present in this region, suggested to be associated with this unidentified gamma-ray source. We find that the extended emission at GeV–TeV energies is best described by more than one source model. We also perform the first energy-dependent analysis of the HESS J1841−055 region at GeV–TeV. We find that the emission at lower energies comes from a diffuse or extended component, while the major contribution of gamma rays above 1 TeV arises from the southern part of the source. Moreover, we find that a significant curvature is present in the combined observed spectrum of MAGIC and Fermi -LAT. The first multiwavelength spectral energy distribution of this unidentified source shows that the emission at GeV–TeV energies can be well explained with both leptonic and hadronic models. For the leptonic scenario, bremsstrahlung is the dominant emission compared to inverse Compton. On the other hand, for the hadronic model, gamma-ray resulting from the decay of neutral pions (π0) can explain the observed spectrum. The presence of dense molecular clouds overlapping with HESS J1841−055 makes both bremsstrahlung and π0-decay processes the dominant emission mechanisms for the source. [ABSTRACT FROM AUTHOR]

Published
2020
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17. Monitoring of the radio galaxy M 87 during a low-emission state from 2012 to 2015 with MAGIC.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Arcaro, C, Baack, D, Babić, A, Banerjee, B, Bangale, P, Barres de Almeida, U, Barrio, J A, Becerra González, J, Bednarek, W, Bellizzi, L, Bernardini, E, Berti, A, Besenrieder, J, Bhattacharyya, W, and Bigongiari, C

Subjects
*COMPTON scattering, *RADIO galaxies, *SPECTRAL energy distribution, *MAGNETIC fields, *HADRONIC atoms, *GAMMA rays
Abstract

M 87 is one of the closest (z  = 0.004 36) extragalactic sources emitting at very high energies (VHE, E > 100 GeV). The aim of this work is to locate the region of the VHE gamma-ray emission and to describe the observed broad-band spectral energy distribution (SED) during the low VHE gamma-ray state. The data from M 87 collected between 2012 and 2015 as part of a MAGIC monitoring programme are analysed and combined with multiwavelength data from Fermi -LAT, Chandra, HST , EVN, VLBA, and the Liverpool Telescope. The averaged VHE gamma-ray spectrum can be fitted from ∼100 GeV to ∼10 TeV with a simple power law with a photon index of (−2.41 ± 0.07), while the integral flux above 300 GeV is |$(1.44\pm 0.13)\times 10^{-12}\, \mathrm{cm}^{-2}\, \mathrm{s}^{-1}$|⁠. During the campaign between 2012 and 2015, M 87 is generally found in a low-emission state at all observed wavelengths. The VHE gamma-ray flux from the present 2012–2015M 87 campaign is consistent with a constant flux with some hint of variability (⁠|$\sim 3\, \sigma$|⁠) on a daily time-scale in 2013. The low-state gamma-ray emission likely originates from the same region as the flare-state emission. Given the broad-band SED, both a leptonic synchrotron self-Compton and a hybrid photohadronic model reproduce the available data well, even if the latter is preferred. We note, however, that the energy stored in the magnetic field in the leptonic scenario is very low, suggesting a matter-dominated emission region. [ABSTRACT FROM AUTHOR]

Published
2020
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18. Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes.

Author

Collaboration:, MAGIC and Collaborators:, External

Subjects
*TELESCOPES, *BL Lacertae objects, *SPECTRAL energy distribution, *GAMMA rays, *HARD X-rays, *HADRONIC atoms, *NEUTRINO detectors
Abstract

Extreme high-energy-peaked BL Lac objects (EHBLs) are an emerging class of blazars. Their typical two-hump-structured spectral energy distribution (SED) peaks at higher energies with respect to conventional blazars. Multiwavelength (MWL) observations constrain their synchrotron peak in the medium to hard X-ray band. Their gamma-ray SED peaks above the GeV band, and in some objects it extends up to several TeV. Up to now, only a few EHBLs have been detected in the TeV gamma-ray range. In this paper, we report the detection of the EHBL 2WHSP J073326.7+515354, observed and detected during 2018 in TeV gamma rays with the MAGIC telescopes. The broad-band SED is studied within an MWL context, including an analysis of the Fermi -LAT data over 10 yr of observation and with simultaneous Swift -XRT, Swift -UVOT, and KVA data. Our analysis results in a set of spectral parameters that confirms the classification of the source as an EHBL. In order to investigate the physical nature of this extreme emission, different theoretical frameworks were tested to model the broad-band SED. The hard TeV spectrum of 2WHSP J073326.7+515354 sets the SED far from the energy equipartition regime in the standard one-zone leptonic scenario of blazar emission. Conversely, more complex models of the jet, represented by either a two-zone spine-layer model or a hadronic emission model, better represent the broad-band SED. [ABSTRACT FROM AUTHOR]

Published
2019
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19. Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes

Author

Ahnen, M. L., primary, Ansoldi, S., additional, Antonelli, L. A., additional, Arcaro, C., additional, Babić, A., additional, Banerjee, B., additional, Bangale, P., additional, de Almeida, U. Barres, additional, Barrio, J. A., additional, González, J. Becerra, additional, Bednarek, W., additional, Bernardini, E., additional, Berti, A., additional, Biasuzzi, B., additional, Biland, A., additional, Blanch, O., additional, Bonnefoy, S., additional, Bonnoli, G., additional, Borracci, F., additional, Bretz, T., additional, Carosi, R., additional, Carosi, A., additional, Chatterjee, A., additional, Colin, P., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, Cumani, P., additional, Da Vela, P., additional, Dazzi, F., additional, De Angelis, A., additional, De Lotto, B., additional, Wilhelmi, E. de Oña, additional, Pierro, F. Di, additional, Doert, M., additional, Domínguez, A., additional, Prester, D. Dominis, additional, Dorner, D., additional, Doro, M., additional, Einecke, S., additional, Glawion, D. Eisenacher, additional, Elsaesser, D., additional, Engelkemeier, M., additional, Ramazani, V. Fallah, additional, Fernández-Barral, A., additional, Fidalgo, D., additional, Fonseca, M. V., additional, Font, L., additional, Fruck, C., additional, Galindo, D., additional, López, R. J. García, additional, Garczarczyk, M., additional, Gaug, M., additional, Giammaria, P., additional, Godinović, N., additional, Gora, D., additional, Gozzini, S. R., additional, Griffiths, S., additional, Guberman, D., additional, Hadasch, D., additional, Hahn, A., additional, Hassan, T., additional, Hayashida, M., additional, Herrera, J., additional, Hose, J., additional, Hrupec, D., additional, Hughes, G., additional, Ishio, K., additional, Konno, Y., additional, Kubo, H., additional, Kushida, J., additional, Kuveždić, D., additional, Lelas, D., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, Majumdar, P., additional, Makariev, M., additional, Maneva, G., additional, Manganaro, M., additional, Mannheim, K., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Menzel, U., additional, Mirzoyan, R., additional, Moralejo, A., additional, Moreno, V., additional, Moretti, E., additional, Neustroev, V., additional, Niedzwiecki, A., additional, Rosillo, M. Nievas, additional, Nilsson, K., additional, Nishijima, K., additional, Noda, K., additional, Nogués, L., additional, Paiano, S., additional, Palacio, J., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Paredes-Fortuny, X., additional, Pedaletti, G., additional, Peresano, M., additional, Perri, L., additional, Persic, M., additional, Poutanen, J., additional, Moroni, P. G. Prada, additional, Prandini, E., additional, Puljak, I., additional, Garcia, J. R., additional, Reichardt, I., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Saito, T., additional, Satalecka, K., additional, Schroeder, S., additional, Schweizer, T., additional, Sillanpää, A., additional, Sitarek, J., additional, Šnidarić, I., additional, Sobczynska, D., additional, Stamerra, A., additional, Strzys, M., additional, Surić, T., additional, Takalo, L., additional, Tavecchio, F., additional, Temnikov, P., additional, Terzić, T., additional, Tescaro, D., additional, Teshima, M., additional, Torres, D. F., additional, Torres-Albà, N., additional, Treves, A., additional, Vanzo, G., additional, Acosta, M. Vazquez, additional, Vovk, I., additional, Ward, J. E., additional, Will, M., additional, Wu, M. H., additional, Zarić, D., additional, Collaboration), (MAGIC, additional, Cognard, I., additional, and Guillemot, L., additional

Published
2017
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20. Discovery of very high Energy $\gamma$ -ray Emission from the Blazar 1ES 0033+595 by the MAGIC Telescopes

Author

Aleksi, J., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., De Almeida, U. B., Barrio, J. A., Gonzalez, J. B., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Fidalgo, D. C., 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., Mendez, C. D., Doert, M., Dominguez, A., Prester, D. D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Lopez, R. J. G., Garczarczyk, M., Terrats, D. G., Gaug, M., Godinovi, N., Munoz, A. G., Gozzini, S. R., 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., Barbera, A. L., 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, J. M., 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, J. M., Paredes-Fortuny, X., Partini, S., Persic, M., Prada, F., Moroni, P. G. P., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribo, M., Rico, J., Garcia, J. R., Rugamer, S., Saggion, A., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpaa, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Suri, T., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzi, 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., Collaboration), (MAGIC, Tronconi, V., Buson, S., and Borghese, A.

Abstract

Monthly notices of the Royal Astronomical Society 446(1), 217 - 225 (2015). doi:10.1093/mnras/stu2024, Published by Oxford Univ. Press, Oxford

Published
2015
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21. Deep observations of the globular cluster M15 with the MAGIC telescopes.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Baack, D, Babić, A, Banerjee, B, Barres de Almeida, U, Barrio, J A, Becerra González, J, Bednarek, W, Bernardini, E, Berti, A, Besenrieder, J, Bhattacharyya, W, Bigongiari, C, Biland, A, Blanch, O, and Bonnoli, G

Subjects
*COMPTON scattering, *GAMMA ray astronomy, *BL Lacertae objects, *GLOBULAR clusters
Abstract

A population of globular clusters (GCs) has been recently established by the Fermi -LAT telescope as a new class of GeV γ-ray sources. Leptons accelerated to TeV energies, in the inner magnetospheres of MSPs or in their wind regions, should produce γ-rays through the inverse Compton scattering in the dense radiation field from the huge population of stars. We have conducted deep observations of the GC M15 with the MAGIC telescopes and used 165 h in order to search for γ-ray emission. A strong upper limit on the TeV γ-ray flux |$\lt 3.2\times 10^{-13}\, \mathrm{cm^{-2}\, s^{-1}}$| above 300 GeV (⁠|$\lt 0.26{{\ \rm per\ cent}}$| of the Crab nebula flux) has been obtained. We interpret this limit as a constraint on the efficiency of the acceleration of leptons in the magnetospheres of the MSPs. We constrain the injection rate of relativistic leptons, ηe, from the MSPs magnetospheres and their surrounding. We conclude that ηe must be lower than expected from the modelling of high-energy processes in MSP inner magnetospheres. For leptons accelerated with the power-law spectrum in the MSP wind regions, ηe is constrained to be much lower than derived for the wind regions around classical pulsars. These constraints are valid for the expected range of magnetic field strengths within the GC and for the range of likely energies of leptons injected from the inner magnetospheres, provided that the leptons are not removed from the GC very efficiently due to advection process. We discuss consequences of these constraints for the models of radiation processes around millisecond pulsars. [ABSTRACT FROM AUTHOR]

Published
2019
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22. Discovery of TeV γ-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Arcaro, C, Baack, D, Babić, A, Banerjee, B, Bangale, P, de Almeida, U Barres, Barrio, J A, Becerra González, J, Bednarek, W, Bernardini, E, Berti, A, Besenrieder, J, Bhattacharyya, W, Bigongiari, C, and Biland, A

Subjects
*SUPERNOVAE, *GALAXIES, *COSMIC rays, *GAMMA rays, *SUPERNOVA remnants
Abstract

SNR G24.7+0.6 is a 9.5 kyrs radio and γ-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL J1834.1–0706e/FGES J1834.1–0706) shows a hard spectral index (Γ ∼ 2) up to 200 GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of SNR G24.7+0.6 with the MAGIC telescopes for a total of 31 h. We detect very high-energy γ-ray emission from an extended source located 0.34° away from the centre of the radio SNR. The new source, named MAGIC J1835–069 is detected up to 5 TeV, and its spectrum is well-represented by a power-law function with spectral index of 2.74 ± 0.08. The complexity of the region makes the identification of the origin of the very high-energy emission difficult; however, the spectral agreement with the LAT source and overlapping position at less than 1.5σ point to a common origin. We analysed 8 yr of Fermi -LAT data to extend the spectrum of the source down to 60 MeV. Fermi -LAT and MAGIC spectra overlap within errors and the global broad-band spectrum is described by a power law with exponential cut-off at 1.9 ± 0.5 TeV. The detected γ-ray emission can be interpreted as the results of proton–proton interaction between the supernova and the CO-rich surrounding. [ABSTRACT FROM AUTHOR]

Published
2019
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23. Constraining very-high-energy and optical emission from FRB 121102 with the MAGIC telescopes.

Author

Collaboration, MAGIC, Acciari, V A, Ansoldi, S, Antonelli, L A, Arbet Engels, A, Arcaro, C, Baack, D, Babić, A, Banerjee, B, and Bangale, P

Subjects
*SOLAR radio bursts, *GAMMA rays, *GALACTIC redshift, *WAVELENGTHS
Abstract

Fast radio bursts (FRBs) are bright flashes observed typically at GHz frequencies with millisecond duration, whose origin is likely extragalactic. Their nature remains mysterious, motivating searches for counterparts at other wavelengths. FRB 121102 is so far the only source known to repeatedly emit FRBs and is associated with a host galaxy at redshift |$z$| ≃ 0.193. We conducted simultaneous observations of FRB 121102 with the Arecibo and MAGIC telescopes during several epochs in 2016–2017. This allowed searches for millisecond time-scale burst emission in very-high-energy (VHE) gamma-rays as well as the optical band. While a total of five FRBs were detected during these observations, no VHE emission was detected, neither of a persistent nature nor burst-like associated with the FRBs. The average integral flux upper limits above 100 GeV at 95 per cent confidence level are 6.6 × 10−12photons cm−2s−1(corresponding to luminosity L VHE≲ 1045erg s−1) over the entire observation period, and 1.2 × 10−7photons cm−2s−1(L VHE≲ 1049erg s−1) over the total duration of the five FRBs. We constrain the optical U -band flux to be below 8.6 mJy at 5σ level for 1-ms intervals around the FRB arrival times. A bright burst with U -band flux 29 mJy and duration ∼12 ms was detected 4.3 s before the arrival of one FRB. However, the probability of spuriously detecting such a signal within the sampled time space is 1.5 per cent (2.2, post-trial), i.e. consistent with the expected background. We discuss the implications of the obtained upper limits for constraining FRB models. [ABSTRACT FROM AUTHOR]

Published
2018
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24. The broad-band properties of the intermediate synchrotron peaked BL Lac S2 0109+22 from radio to VHE gamma-rays.

Author

Collaboration, MAGIC, Ansoldi, S, Antonelli, L A, Arcaro, C, Baack, D, Babić, A, Banerjee, B, Bangale, P, Barres de Almeida, U, and Barrio, J A

Subjects
*GAMMA rays, *SYNCHROTRONS, *BL Lacertae objects, *ATMOSPHERIC radiation, *SPECTRAL energy distribution
Abstract

The Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes observed S2 0109+22 in 2015 July during its flaring activity in high-energy gamma-rays observed by Fermi -Large Area Telescope. We analyse the MAGIC data to characterize the very high energy (VHE) gamma-ray emission of S2 0109+22, which belongs to the subclass of intermediate synchrotron peak (ISP) BL Lacertae (BL Lac) objects. We study the multifrequency emission in order to investigate the source classification. Finally, we compare the source long-term behaviour to other VHE gamma-ray emitting (TeV) blazars. We performed a temporal and spectral analysis of the data centred around the MAGIC interval of observation (MJD 57225–57231). Long-term radio and optical data have also been investigated using the discrete correlation function. The redshift of the source is estimated through optical host-galaxy imaging and also using the amount of VHE gamma-ray absorption. The quasi-simultaneous multifrequency spectral energy distribution (SED) is modelled with the conventional one-zone synchrotron self-Compton (SSC) model. MAGIC observations resulted in the detection of the source at a significance level of 5.3σ. The VHE gamma-ray emission of S2 0109+22 is variable on a daily time scale. VHE gamma-ray luminosity of the source is lower than the average of TeV BL Lacs. The optical polarization and long-term optical/radio behaviour of the source are different from the general population of TeV blazars. All these findings agree with the classification of the source as an ISP BL Lac object. We estimate the source redshift as $$z$$ = 0.36 ± 0.07. The SSC parameters describing the SED are rather typical for blazars. [ABSTRACT FROM AUTHOR]

Published
2018
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25. Discovery of very high energy γ-ray emission from the blazar 1ES 0033+595 by the MAGIC telescopes

Author

Aleksić, J., primary, Ansoldi, S., additional, Antonelli, L. A., additional, Antoranz, P., additional, Babic, A., additional, Bangale, P., additional, de Almeida, U. Barres, additional, Barrio, J. A., additional, González, J. Becerra, additional, Bednarek, W., additional, Berger, K., additional, Bernardini, E., additional, Biland, A., additional, Blanch, O., additional, Bonnefoy, S., additional, Bonnoli, G., additional, Borracci, F., additional, Bretz, T., additional, Carmona, E., additional, Carosi, A., additional, Fidalgo, D. Carreto, additional, Colin, P., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, Da Vela, P., additional, Dazzi, F., additional, De Angelis, A., additional, De Caneva, G., additional, De Lotto, B., additional, Mendez, C. Delgado, additional, Doert, M., additional, Domínguez, A., additional, Prester, D. Dominis, additional, Dorner, D., additional, Doro, M., additional, Einecke, S., additional, Eisenacher, D., additional, Elsaesser, D., additional, Farina, E., additional, Ferenc, D., additional, Fonseca, M. V., additional, Font, L., additional, Frantzen, K., additional, Fruck, C., additional, López, R. J. García, additional, Garczarczyk, M., additional, Terrats, D. Garrido, additional, Gaug, M., additional, Godinović, N., additional, Muñoz, A. González, additional, Gozzini, S. R., additional, Hadasch, D., additional, Hayashida, M., additional, Herrera, J., additional, Herrero, A., additional, Hildebrand, D., additional, Hose, J., additional, Hrupec, D., additional, Idec, W., additional, Kadenius, V., additional, Kellermann, H., additional, Kodani, K., additional, Konno, Y., additional, Krause, J., additional, Kubo, H., additional, Kushida, J., additional, Barbera, A. La, additional, Lelas, D., additional, Lewandowska, N., additional, Lindfors, E., additional, Lombardi, S., additional, López, M., additional, López-Coto, R., additional, López-Oramas, A., additional, Lorenz, E., additional, Lozano, I., additional, Makariev, M., additional, Mallot, K., additional, Maneva, G., additional, Mankuzhiyil, N., additional, Mannheim, K., additional, Maraschi, L., additional, Marcote, B., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Menzel, U., additional, Meucci, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Moralejo, A., additional, Munar-Adrover, P., additional, Nakajima, D., additional, Niedzwiecki, A., additional, Nilsson, K., additional, Nishijima, K., additional, Noda, K., additional, Nowak, N., additional, Orito, R., additional, Overkemping, A., additional, Paiano, S., additional, Palatiello, M., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Paredes-Fortuny, X., additional, Partini, S., additional, Persic, M., additional, Prada, F., additional, Moroni, P. G. Prada, additional, Prandini, E., additional, Preziuso, S., additional, Puljak, I., additional, Reinthal, R., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Garcia, J. Rodriguez, additional, Rügamer, S., additional, Saggion, A., additional, Saito, T., additional, Saito, K., additional, Satalecka, K., additional, Scalzotto, V., additional, Scapin, V., additional, Schultz, C., additional, Schweizer, T., additional, Shore, S. N., additional, Sillanpää, A., additional, Sitarek, J., additional, Snidaric, I., additional, Sobczynska, D., additional, Spanier, F., additional, Stamatescu, V., additional, Stamerra, A., additional, Steinbring, T., additional, Storz, J., additional, Sun, S., additional, Surić, T., additional, Takalo, L., additional, Takami, H., additional, Tavecchio, F., additional, Temnikov, P., additional, Terzić, T., additional, Tescaro, D., additional, Teshima, M., additional, Thaele, J., additional, Tibolla, O., additional, Torres, D. F., additional, Toyama, T., additional, Treves, A., additional, Uellenbeck, M., additional, Vogler, P., additional, Wagner, R. M., additional, Zandanel, F., additional, Zanin, R., additional, collaboration), (MAGIC, additional, Tronconi, V., additional, Buson, S., additional, and Borghese, A., additional

Published
2014
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26. A first joint M87 campaign in 2008 from radio to TeV gamma-rays

Author

Wagner, R. M., Collaboration, MAGIC, Collaboration, VERITAS, team, the VLBA 43 GHz M87 monitoring, Beilicke, M., Davies, F., Krawczynski, H., Mazin, D., Raue, M., Wagner, S., Walker, R. C., and Collaboration, for the H. E. S. S.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

M87, the central galaxy of the Virgo cluster, is the first radio galaxy detected in the TeV regime. The structure of its jet, which is not pointing toward the line of sight, is spatially resolved in X-ray (by Chandra), in optical and in radio observations. Time correlation between the TeV flux and emission at other wavelengths provides a unique opportunity to localize the very high energy gamma-ray emission process occurring in AGN. For 10 years, M87 has been monitored in the TeV band by atmospheric Cherenkov telescopes. In 2008, the three main atmospheric Cherenkov telescope observatories (H.E.S.S., MAGIC and VERITAS) coordinated their observations in a joint campaign from January to May with a total observation time of approx. 120 hours. The campaign largely overlapped with an intensive VLBA project monitoring the core of M87 at 43 GHz every 5 days. In February, high TeV activities with rapid flares have been detected. Contemporaneously, M87 was observed with high spatial resolution instruments in X-rays (Chandra). We discuss the results of the joint observation campaign in 2008.

Published
2009

32. Observation of the gamma-ray binary HESS J0632+057 with the HESS, MAGIC, and VERITAS telescopes

Author

Adams, CB, Benbow, W, Brill, A, Cotter, G, Spencer, S, Collaboration, VERITAS, collaboration, MAGIC, and Collaboration, H.E.S.S.

Abstract

The results of gamma-ray observations of the binary system HESS J0632 + 057 collected during 450 hr over 15 yr, between 2004 and 2019, are presented. Data taken with the atmospheric Cherenkov telescopes H.E.S.S., MAGIC, and VERITAS at energies above 350 GeV were used together with observations at X-ray energies obtained with Swift-XRT, Chandra, XMM-Newton, NuSTAR, and Suzaku. Some of these observations were accompanied by measurements of the Hα emission line. A significant detection of the modulation of the very high-energy gamma-ray fluxes with a period of 316.7 ± 4.4 days is reported, consistent with the period of 317.3 ± 0.7 days obtained with a refined analysis of X-ray data. The analysis of data from four orbital cycles with dense observational coverage reveals short-timescale variability, with flux-decay timescales of less than 20 days at very high energies. Flux variations observed over a timescale of several years indicate orbit-to-orbit variability. The analysis confirms the previously reported correlation of X-ray and gamma-ray emission from the system at very high significance, but cannot find any correlation of optical Hα parameters with fluxes at X-ray or gamma-ray energies in simultaneous observations. The key finding is that the emission of HESS J0632 + 057 in the X-ray and gamma-ray energy bands is highly variable on different timescales. The ratio of gamma-ray to X-ray flux shows the equality or even dominance of the gamma-ray energy range. This wealth of new data is interpreted taking into account the insufficient knowledge of the ephemeris of the system, and discussed in the context of results reported on other gamma-ray binary systems.

Published
2022

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

Author

M. I. Martínez, Sabrina Einecke, G. Pedaletti, S. R. Gozzini, Thomas Bretz, L. Nogués, E. Moretti, J. Becerra González, Giacomo Bonnoli, F. Di Pierro, M. Engelkemeier, E. Prandini, Francesco Longo, I. Snidaric, Stefano Covino, B. De Lotto, Alessio Berti, S. Bonnefoy, A. Sillanpää, Arka Chatterjee, M. Vazquez Acosta, Ana Babić, Wolfgang Rhode, Alexander Hahn, Nikola Godinovic, Gareth Hughes, B. Biasuzzi, U. Barres de Almeida, D. Elsaesser, Juan Abel Barrio, R. Mirzoyan, Damir Lelas, Victoria Moreno, Tomoki Saito, D. Tescaro, Dario Hrupec, L. Perri, A. De Angelis, A. Treves, Vitaly Neustroev, Stefano Ansoldi, P. Da Vela, M. A. Lopez, Kari Nilsson, D. Dominis Prester, Riccardo Paoletti, Daniela Dorner, S. Griffiths, Dorota Sobczyńska, Dariusz Gora, J. Palacio, M. Will, D. Eisenacher Glawion, Abelardo Moralejo, Gaia Vanzo, Marcel Strzys, X. Paredes-Fortuny, Mosè Mariotti, M. Nievas Rosillo, J. M. Paredes, Antonio Stamerra, Yusuke Konno, S. Schroeder, Ivica Puljak, Pierre Colin, M. Gaug, Tomislav Terzić, L. Maraschi, V. Fallah Ramazani, J. Kushida, Martin Makariev, Elina Lindfors, Jose Luis Contreras, Oscar Blanch, Saverio Lombardi, Christian Fruck, Daniel Mazin, B. Banerjee, C. Arcaro, G. Maneva, Juan Cortina, E. de Oña Wilhelmi, S. Paiano, Kazuma Ishio, Karl Mannheim, J. Herrera, M. Doert, E. Colombo, Adrian Biland, M. H. Wu, L. A. Antonelli, J. R. Garcia, Lucas Guillemot, L. O. Takalo, Koji Noda, Aaron Dominguez, F. Borracci, Elisa Bernardini, J. Rico, Pratik Majumdar, M. V. Fonseca, T. Surić, Masahiro Teshima, Tarek M. Hassan, R. J. García López, J. E. Ward, Fabrizio Tavecchio, Ismaël Cognard, Rodolfo Carosi, Ll. Font, Wlodek Bednarek, Alessandro Carosi, D. Kuveždić, N. Torres-Albà, Max Ludwig Ahnen, I. Reichardt, P. Temnikov, P. Giammaria, Massimo Persic, U. Menzel, Diego F. Torres, M. Garczarczyk, Ievgen Vovk, M. Peresano, T. Schweizer, D. Fidalgo, Juri Poutanen, Julian Sitarek, J. Hose, K. Nishijima, Daniela Hadasch, Francesco Dazzi, A. Fernández-Barral, A. Niedzwiecki, P. G. Prada Moroni, David Paneque, M. Hayashida, D. Guberman, D. Zarić, Marina Manganaro, Marc Ribó, D. Galindo, P. Bangale, Hidetoshi Kubo, P. Cumani, Konstancja Satalecka, Michele Doro, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carosi, R., Carosi, A., Chatterjee, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Wilhelmi, E. de Oña, Pierro, F. Di, Doert, M., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Glawion, D. Eisenacher, Elsaesser, D., Engelkemeier, M., Ramazani, V. Fallah, Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Gozzini, S. R., Griffiths, S., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nilsson, K., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Sillanpää, A., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Torres, D. F., Torres Albà, N., Treves, A., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zarić, D., Collaboration), (MAGIC, Cognard, I., Guillemot, L., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Nuclear Physics Division, Bhabha Atomic Research Centre (BARC), Government of India, Department of Atomic Energy-Government of India, Department of Atomic Energy, Politecnico di Milano [Milan] (POLIMI), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Technische Universität Dortmund [Dortmund] (TU), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), IEEC-CSIC, Institut de Física d'Altes Energies, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Università degli Studi di Udine - University of Udine [Italie], Universita degli Studi di Padova, Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Trieste (OAT), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Department of Environment and Energy [Sendai], Tohoku University [Sendai], Optoelectronic Research Centre, University of Southampton, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
non-thermal, pulsars: general, binaries: close, pulsars: individual: B1957+20, gamma-rays: general [radiation mechanisms], Radiation mechanisms: non-thermal, VHE [gamma ray], Astrophysics, spin, 01 natural sciences, 7. Clean energy, star, emission [pulsar], Millisecond pulsar, Pulsars: general, radiation mechanisms: non-thermal, gamma rays: general, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, High Energy Astrophysical Phenomena (astro-ph.HE), acceleration [electron], Physics, radio wave, Superluminal motion, efficiency [acceleration], non-thermal, binaries: close, pulsars: general, pulsars: individual: B1957+20, gamma-rays: general [radiation mechanisms], inverse [Compton scattering], frequency, compact [binary], symbols, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, upper limit, Active galactic nucleus, Pulsars: individual: B1957+20, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Lorentz covariance, GLAST, Binary pulsar, symbols.namesake, Pulsar, Binaries: close, 0103 physical sciences, interaction [pulsar], plasma, radiation mechanisms: non-thermal, binaries: close, pulsars: general, pulsars: individual: B1957+20, gamma-rays: general, Astrophysics::Galaxy Astrophysics, Gamma-rays: general, Planck energy, ta115, 010308 nuclear & particles physics, Crab Pulsar, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], binary [pulsar], Astronomy and Astrophysics, injection [electron], MAGIC, 13. Climate action, Space and Planetary Science, ddc:520, mass
Abstract

B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies., Monthly Notices of the Royal Astronomical Society, 470 (4), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2017

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