Multifrequency studies of the peculiar quasar 4C+21.35 during the 2010 flaring activity
Hewitt JW; McEnery JE; Da Vela P; Lombardi S; Scalzotto V; Nemmen R; Fonseca MV; Vitale V; Horan D; Bretz T; Brigida M; Troja E; Schultz C; Mannheim K; Takami H; Sobczynska D; Satalecka K; Kodani K; Werner M; Tinivella M; Ros E; Nikolashvili MG; Palatiello M; Chiang J; Garczarczyk M; Farina E; Colombo E; Johnson AS; Doro M; Bissaldi E; Takalo L; Bruel P; Reimer O; Sillanpaa A; Frantzen K; Antoranz P; Persic M; Bock RK; Orito R; Krause J; Lopez-Coto R; Puljak I; Fusco P; Lister ML; Gehrels N; Monzani ME; Kubo H; Idec W; Munar-Adrover P; Hadasch D; Contreras JL; Bernardini E; Fukazawa Y; Mazin D; Kopatskaya EN; Wood DL; Vianello G; Schweizer T; Antolini E; Efimova NV; Toyama T; Hughes RE; Drake AJ; Torres DF; Claus R; Thayer JG; Fidalgo DC; Ajello M; Prada F; Longo F; Gonzalez JB; Lindfors E; Miranda JM; Giordano F; Usher TL; Bonamente E; Takahashi T; Chekhtman A; Caraveo PA; Sgro C; Grenier IA; Silva EDE; Paneque D; Angelakis E; Reimer A; Raino S; Djorgovski SG; Vogler P; Hrupec D; Razzano M; Barrio JA; Dermer CD; Nuss E; Rugamer S; Chiaro G; Zandanel F; Savolainen T; Mayer M; Aller MF; Preziuso S; Allafort A; Terrats DG; Larsson S; Paiano S; Elsaesser D; Ansoldi S; Gozzini SR; Font L; Mallot K; Bonnefoy S; Sigua LA; Nilsson K; Bonnoli G; Knoetig ML; Lopez-Oramas A; La Barbera A; Latronico L; Chaves RCG; Kovalev YY; Cortina J; Spanier F; Paredes-Fortuny X; Lozano I; Gaug M; Giroletti M; Bednarek W; Iafrate G; Finke J; Larionov VM; Sanchez DA; Gasparrini D; Antonelli LA; Donato D; Storz J; Cavazzuti E; Thayer JB; Aleksic J; Ackermann M; Spandre G; Blanch O; Knoedlseder J; Cameron RA; Paredes JM; Marcote B; Hose J; Colin P; Moralejo A; Scapin V; Lelas D; Murgia S; Cohen-Tanugi J; Mendez CD; Bregeon J; Martinez M; Lovellette MN; Prandini E; Kadenius V; Menzel U; Berger K; Bastieri D; De Palma F; Teshima M; Nowak N; Loparco F; Vasileiou V; Paoletti R; Tornikoski M; Stamerra A; Porter TA; Blinov DA; De Angelis A; Vandenbroucke J; Ferenc D; Covino S; Dorner D; Wagner RM; Babic A; Overkemping A; Ohsugi T; Carosi A; Buehler R; Garcia JR; Moroni PGP; Einecke S; de Almeida UB; Thaele J; Fruck C; Kushida J; Buson S; Caliandro GA; Homan DC; Hildebrand D; Michelson PF; Bangale P; Shore SN; Kuss M; Favuzzi C; Zanin R; Mariotti M; Konno Y; Takahashi H; Giavitto G; Niedzwiecki A; Mankuzhiyil N; Saito K; Orlando E; Snidaric I; Gurwell MA; Saito T; Stamatescu V; Schulz A; Godfrey G; Tavecchio F; Herrero A; Bellazzini R; Piron F; Pesce-Rollins M; Lubrano P; Lopez RJG; Lopez M; Rico J; Hayashida M; Eisenacher D; Franckowiak A; Lewandowska N; Winer BL; Gargano F; Doert M; Perkins JS; Maneva G; Nakajima D; Lande J; Sitarek J; Tibolla O; Drell PS; Mizuno T; Morselli A; Conrad J; Nishijima K; Maraschi L; Suric T; Temnikov P; Carmona E; Steinbring T; Guiriec S; Meucci M; Moskalenko IV; Partini S; Focke WB; Salvati M; Cutini S; Ciprini S; Reinthal R; D'Ammando F; Prester DD; Lorenz E; Kellermann H; De Lotto B; Barbiellini G; Tosti G; Wood KS; Mazziotta MN; Saggion A; Spinelli P; Ribo M; Dazzi F; Giglietto N; Treves A; Borracci F; Stawarz L; Godinovic N; Sun S; Siskind EJ; Makariev M; Munoz AG; Thompson DJ; De Caneva G; Lahteenmaki A; Tescaro D; Dominguez A; Cecchi C; Terzic T; Pivato G; Orienti M; Nieppola E; Jordan B; Mirzoyan R; Rhode W; Kurtanidze OM; Biland A
https://urn.fi/URN:NBN:fi-fe2021042714510
Tiivistelmä
The discovery of rapidly variable Very High Energy ( VHE; E > 100 GeV). - ray emission from 4C + 21.35 ( PKS 1222+ 216) by MAGIC on 2010 June 17, triggered by the high activity detected by the Fermi Large Area Telescope ( LAT) in high energy ( HE; E > 100 MeV). - rays, poses intriguing questions on the location of the. - ray emitting region in this flat spectrum radio quasar. We present multifrequency data of 4C + 21.35 collected from centimeter to VHE during 2010 to investigate the properties of this source and discuss a possible emission model. The first hint of detection at VHE was observed by MAGIC on 2010 May 3, soon after a gamma- ray flare detected by Fermi-LAT that peaked on April 29. The same emission mechanism may therefore be responsible for both the HE and VHE emission during the 2010 flaring episodes. Two optical peaks were detected on 2010 April 20 and June 30, close in time but not simultaneous with the two gamma- ray peaks, while no clear connection was observed between the X-ray and gamma- ray emission. An increasing flux density was observed in radio and mm bands from the beginning of 2009, in accordance with the increasing gamma- ray activity observed by Fermi-LAT, and peaking on 2011 January 27 in the mm regime ( 230 GHz). We model the spectral energy distributions ( SEDs) of 4C + 21.35 for the two periods of the VHE detection and a quiescent state, using a one-zone model with the emission coming from a very compact region outside the broad line region. The three SEDs can be fit with a combination of synchrotron self-Compton and external Compton emission of seed photons from a dust torus, changing only the electron distribution parameters between the epochs. The fit of the optical/UV part of the spectrum for 2010 April 29 seems to favor an inner disk radius of < six gravitational radii, as one would expect from a prograde-rotating Kerr black hole.
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- Rinnakkaistallenteet [19207]