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Monitoring of the radio galaxy M87 during a low emission state from 2012 to 2015 with MAGIC

Collaboration, MAGIC, Acciari, VA, Ansoldi, S, Antonelli, LA, Engels, AA, Arcaro, C, Baack, D, Babić, A, Banerjee, B, Bangale, P, Almeida, UBD, Barrio, JA, González, JB, Bednarek, W, Bellizzi, L, Bernardini, E, Berti, A, Besenrieder, J, Bhattacharyya, W, Bigongiari, C , Biland, A, Blanch, O, Bonnoli, G, Bošnjak, Ž, Busetto, G, Carosi, R, Ceribella, G, Chai, Y, Chilingaryan, A, Cikota, S, Colak, SM, Colin, U, Colombo, E, Contreras, JL, Cortina, J, Covino, S, D'Elia, V, Vela, PD, Dazzi, F, Angelis, AD, Lotto, BD, Delfino, M, Delgado, J, Depaoli, D, Pierro, FD, Venere, LD, Espiñeira, EDS, Prester, DD, Donini, A, Dorner, D, Doro, M, Elsaesser, D, Ramazani, VF, Fattorini, A, Fernández-Barral, A, Ferrara, G, Fidalgo, D, Foffano, L, Fonseca, MV, Font, L, Fruck, C, Fukami, S, López, RJG, Garczarczyk, M, Gasparyan, S, Gaug, M, Giglietto, N, Giordano, F, Godinović, N, Green, D, Guberman, D, Hadasch, D, Hahn, A, Herrera, J, Hoang, J, Hrupec, D, Hütten, M, Inada, T, Inoue, S, Ishio, K, Iwamura, Y, Jouvin, L, Kerszberg, D, 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, BMDO, Maggio, C, Majumdar, P, Makariev, M, Mallamaci, M, Maneva, G, Manganaro, M, Mannheim, K, Maraschi, L, Mariotti, M, Martínez, M, Masuda, S, Mazin, D, Mićanović, S, Miceli, D, Minev, M, Miranda, JM, 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, Nogués, L, Nöthe, M, Nozaki, S, Paiano, S, Palacio, J, Palatiello, M, Paneque, D, Paoletti, R, Paredes, JM, Peñil, P, Peresano, M, Persic, M, Moroni, PGP, Prandini, E, Puljak, I, Rhode, W, Ribó, M, Rico, J, Righi, C, Rugliancich, A, Saha, L, Sahakyan, N, Saito, T, Sakurai, S, Satalecka, K, Schmidt, K, Schweizer, T, Sitarek, J, Šnidarić, I, Sobczynska, D, Somero, 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, Tsujimoto, S, Vagelli, V, Scherpenberg, JV, Vanzo, G, Acosta, MV, Vigorito, CF, Vitale, V, Vovk, I, Will, M, Zarić, D, Collaborators, MWL, Asano, K, Hada, K, Harris, DE, Giroletti, M, Jermak, HE, Madrid, JP, Massaro, F, Richter, S, Spanier, F, Steele, IA and Walker, RC (2020) Monitoring of the radio galaxy M87 during a low emission state from 2012 to 2015 with MAGIC. Monthly Notices of the Royal Astronomical Society, 494 (2). pp. 5354-5365. ISSN 0035-8711

Monitoring of the radio galaxy M87 during a low emission state from 2012 to 2015 with MAGIC.pdf - Published Version

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M87 is one of the closest (z=0.00436) 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 broadband spectral energy distribution (SED) during the low VHE gamma-ray state. The data from M87 collected between 2012 and 2015 as part of a MAGIC monitoring programme are analysed and combined with multi-wavelength data from Fermi-LAT, Chandra, HST, EVN, VLBA and the Liverpool Telescope. The averaged VHE gamma-ray spectrum can be fitted from 100GeV to 10TeV with a simple power law with a photon index of (-2.41 $\pm$ 0.07), while the integral flux above 300GeV is $(1.44 \pm 0.13) \times 10^{-12} cm^{-2} s^{-1}$. During the campaign between 2012 and 2015, M87 is generally found in a low emission state at all observed wavelengths. The VHE gamma-ray flux from the present 2012-2015 M87 campaign is consistent with a constant flux with some hint of variability ($\sim3\sigma$) on a daily timescale in 2013. The low-state gamma-ray emission likely originates from the same region as the flare-state emission. Given the broadband SED, both a leptonic synchrotron self Compton and a hybrid photo-hadronic 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.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: astro-ph.HE; astro-ph.HE
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Related URLs:
Date Deposited: 09 Mar 2020 10:04
Last Modified: 04 Sep 2021 08:06
DOI or ID number: 10.1093/mnras/staa014
URI: https://researchonline.ljmu.ac.uk/id/eprint/12053
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