Detection of very high energy gamma-ray emission from the gravitationally lensed blazar QSO B0218+357 with the MAGIC telescopes

Ahnen, M. L.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Arcaro, C.; Babic, A.; Banerjee, B.; Bangale, P.; Barres de Almeida, U.; Barrio, J. A.; Becerra González, J.; Bednarek, W.; Bernardini, E.; Berti, A.; Biasuzzi, B.; Biland, A.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Buson, S.; Carosi, A.; Chatterjee, A.; Clavero, R.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Da Vela, P.; Dazzi, F.; De Angelis, A.; De Lotto, B.; de Oña Wilhelmi, E.; Di Pierro, F.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Einecke, S.; Eisenacher Glawion, D.; Elsaesser, D.; Engelkemeier, M.; Fallah Ramazani, V.; Fernández-Barral, A.; Fidalgo, D.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; Galindo, D.; García López, R. J.; Garczarczyk, M.; Garrido Terrats, D.; Gaug, M.; Giammaria, P.; Godinović, N.; Gora, D.; Guberman, D.; Hadasch, D.; Hahn, A.; Hayashida, M.; Herrera, J.; Hose, J.; Hrupec, D.; Hughes, G.; Idec, W.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; La Barbera, A.; Lelas, D.; Lindfors, E.; Lombardi, S.; Longo, F.; 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.; Paiano, S.; Palacio, J.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Pedaletti, G.; Peresano, M.; Perri, L.; Persic, M.; Poutanen, J.; Prada Moroni, P. G.; Prandini, E.; Puljak, I.; Garcia, J. R.; Reichardt, I.; Rhode, W.; Ribó, M.; Rico, J.; Saito, T.; Satalecka, K.; Schroeder, S.; Schweizer, T.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Snidaric, I.; Sobczynska, D.; Stamerra, A.; Strzys, M.; Surić, T.; Takalo, L.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Torres, D. F.; Toyama, T.; Treves, A.; Vanzo, G.; Verguilov, V.; Vovk, I.; Ward, J. E.; Will, M.; Wu, M. H.; Zanin, R.; Desiante, R.
Detection of very high energy gamma-ray emission from the gravitationally lensed blazar QSO B0218+357 with the MAGIC telescopes

Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Arcaro, C.
Babic, A.
Banerjee, B.
Bangale, P.
Barres de Almeida, U.
Barrio, J. A.
Becerra González, J.
Bednarek, W.
Bernardini, E.
Berti, A.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Buson, S.
Carosi, A.
Chatterjee, A.
Clavero, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
de Oña Wilhelmi, E.
Di Pierro, F.
Doert, M.
Domínguez, A.
Dominis Prester, D.
Dorner, D.
Doro, M.
Einecke, S.
Eisenacher Glawion, D.
Elsaesser, D.
Engelkemeier, M.
Fallah Ramazani, V.
Fernández-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
García López, R. J.
Garczarczyk, M.
Garrido Terrats, D.
Gaug, M.
Giammaria, P.
Godinović, N.
Gora, D.
Guberman, D.
Hadasch, D.
Hahn, A.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
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.
Paiano, S.
Palacio, J.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Pedaletti, G.
Peresano, M.
Perri, L.
Persic, M.
Poutanen, J.
Prada Moroni, P. G.
Prandini, E.
Puljak, I.
Garcia, J. R.
Reichardt, I.
Rhode, W.
Ribó, M.
Rico, J.
Saito, T.
Satalecka, K.
Schroeder, S.
Schweizer, T.
Shore, S. N.
Sillanpää, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Strzys, M.
Surić, T.
Takalo, L.
Tavecchio, F.
Temnikov, P.
Terzić, T.
Tescaro, D.
Teshima, M.
Torres, D. F.
Toyama, T.
Treves, A.
Vanzo, G.
Verguilov, V.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Desiante, R.
Katso/Avaa
Lataukset: 

EDP Science
doi:10.1051/0004-6361/201629461
Näytä kaikki kuvailutiedot
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042716197
Tiivistelmä

Context. QSO B0218+357 is a gravitationally lensed blazar located at a
redshift of 0.944. The gravitational lensing splits the emitted
radiation into two components that are spatially indistinguishable by
gamma-ray instruments, but separated by a 10-12 day delay. In July 2014,
QSO B0218+357 experienced a violent flare observed by the Fermi-LAT and
followed by the MAGIC telescopes.
Aims: The spectral energy
distribution of QSO B0218+357 can give information on the energetics of
z 1 very high energy gamma-ray sources. Moreover the gamma-ray
emission can also be used as a probe of the extragalactic background
light at z 1.
Methods: MAGIC performed observations of QSO
B0218+357 during the expected arrival time of the delayed component of
the emission. The MAGIC and Fermi-LAT observations were accompanied by
quasi-simultaneous optical data from the KVA telescope and X-ray
observations by Swift-XRT. We construct a multiwavelength spectral
energy distribution of QSO B0218+357 and use it to model the source. The
GeV and sub-TeV data obtained by Fermi-LAT and MAGIC are used to set
constraints on the extragalactic background light.
Results: Very
high energy gamma-ray emission was detected from the direction of QSO
B0218+357 by the MAGIC telescopes during the expected time of arrival of
the trailing component of the flare, making it the farthest very high
energy gamma-ray source detected to date. The observed emission spans
the energy range from 65 to 175 GeV. The combined MAGIC and Fermi-LAT
spectral energy distribution of QSO B0218+357 is consistent with current
extragalactic background light models. The broadband emission can be
modeled in the framework of a two-zone external Compton scenario, where
the GeV emission comes from an emission region in the jet, located
outside the broad line region.

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