Acciari, V. A. and Ansoldi, S. and Antonelli, L. A. and Arbet Engels, A. and Artero, M. and Asano, K. and Baack, D. and Babić, A. and Baquero, A. and Barres de Almeida, U. and Barrio, J. A. and Becerra González, J. and Bednarek, W. and Bellizzi, L. and Bernardini, E. and Bernardos, M. and Berti, A. and Besenrieder, J. and Bhattacharyya, W. and Bigongiari, C. and Biland, A. and Blanch, O. and Bonnoli, G. and Bošnjak, Ž. and Busetto, G. and Carosi, R. and Ceribella, G. and Cerruti, M. and Chai, Y. and Chilingarian, A. and Cikota, S. and Colak, S. M. and Colombo, E. and Contreras, J. L. and Cortina, J. and Covino, S. and D'Amico, G. and D'Elia, V. and Da Vela, P. and Dazzi, F. and De Angelis, A. and De Lotto, B. and Delfino, M. and Delgado, J. and Delgado Mendez, C. and Depaoli, D. and Di Pierro, F. and Di Venere, L. and Do Souto Espiñeira, E. and Dominis Prester, D. and Donini, A. and Dorner, D. and Doro, M. and Elsaesser, D. and Fallah Ramazani, V. and Fattorini, A. and Ferrara, G. and Foffano, L. and Fonseca, M. V. and Font, L. and Fruck, C. and Fukami, S. and García López, R. J. and Garczarczyk, M. and Gasparyan, S. and Gaug, M. and Giglietto, N. and Giordano, F. and Gliwny, P. and Godinović, N. and Green, J. G. and Green, D. and Hadasch, D. and Hahn, A. and Heckmann, L. and Herrera, J. and Hoang, J. and Hrupec, D. and Hütten, M. and Inada, T. and Inoue, S. and Ishio, K. and Iwamura, Y. and Jormanainen, J. and Jouvin, L. and Kajiwara, Y. and Karjalainen, M. and Kerszberg, D. and Kobayashi, Y. and Kubo, H. and Kushida, J. and Lamastra, A. and Lelas, D. and Leone, F. and Lindfors, E. and Lombardi, S. and Longo, F. and López-Coto, R. and López-Moya, M. and López-Oramas, A. and Loporchio, S. and Machado de Oliveira Fraga, B. and Maggio, C. and Majumdar, P. and Makariev, M. and Mallamaci, M. and Maneva, G. and Manganaro, M. and Mannheim, K. and Maraschi, L. and Mariotti, M. and Martínez, M. and Mazin, D. and Mender, S. and Mićanović, S. and Miceli, D. and Miener, T. and Minev, M. and Miranda, J. M. and Mirzoyan, R. and Molina, E. and Moralejo, A. and Morcuende, D. and Moreno, V. and Moretti, E. and Neustroev, V. and Nigro, C. and Nilsson, K. and Ninci, D. and Nishijima, K. and Noda, K. and Nozaki, S. and Ohtani, Y. and Oka, T. and Otero-Santos, J. and Paiano, S. and Palatiello, M. and Paneque, D. and Paoletti, R. and Paredes, J. M. and Pavletić, L. and Peñil, P. and Perennes, C. and Persic, M. and Prada Moroni, P. G. and Prandini, E. and Priyadarshi, C. and Puljak, I. and Rhode, W. and Ribó, M. and Rico, J. and Righi, C. and Rugliancich, A. and Saha, L. and Sahakyan, N. and Saito, T. and Sakurai, S. and Satalecka, K. and Saturni, F. G. and Schleicher, B. and Schmidt, K. and Schweizer, T. and Sitarek, J. and Šnidarić, I. and Sobczynska, D. and Spolon, A. and Stamerra, A. and Strom, D. and Strzys, M. and Suda, Y. and Surić, T. and Takahashi, M. and Tavecchio, F. and Temnikov, P. and Terzić, T. and Teshima, M. and Torres-Albà, N. and Tosti, L. and Truzzi, S. and Tutone, A. and van Scherpenberg, J. and Vanzo, G. and Vazquez Acosta, M. and Ventura, S. and Verguilov, V. and Vigorito, C. F. and Vitale, V. and Vovk, I. and Will, M. and Zarić, D. and Angioni, R. and D'Ammando, F. and Ciprini, S. and Cheung, C. C. and Orienti, M. and Pacciani, L. and Prajapati, P. and Kumar, P. and Ganesh, S. and Minev, M. and Kurtenkov, A. and Marchini, A. and Carrasco, L. and Escobedo, G. and Porras, A. and Recillas, E. and Lähteenmäki, A. and Tornikoski, M. and Berton, M. and Tammi, J. and Vera, R. J. C. and Jorstad, S. G. and Marscher, A. P. and Weaver, Z. R. and Hart, M. and Hallum, M. K. and Larionov, V. M. and Borman, G. A. and Grishina, T. S. and Kopatskaya, E. N. and Larionova, E. G. and Nikiforova, A. A. and Morozova, D. A. and Savchenko, S. S. and Troitskaya, Yu. V. and Troitsky, I. S. and Vasilyev, A. A. and Hodges, M. and Hovatta, T. and Kiehlmann, S. and Max-Moerbeck, W. and Readhead, A. C. S. and Reeves, R. and Pearson, T. J. (2021) VHE gamma-ray detection of FSRQ QSO B1420+326 and modeling of its enhanced broadband state in 2020. Astronomy and Astrophysics, 647 . Art. No. A163. ISSN 0004-6361. doi:10.1051/0004-6361/202039687. https://resolver.caltech.edu/CaltechAUTHORS:20210202-095252065
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Abstract
Context. QSO B1420+326 is a blazar classified as a flat-spectrum radio quasar (FSRQ). At the beginning of the year 2020, it was found to be in an enhanced flux state and an extensive multiwavelength campaign allowed us to trace the evolution of the flare. Aims. We search for very high-energy (VHE) gamma-ray emission from QSO B1420+326 during this flaring state. We aim to characterize and model the broadband emission of the source over different phases of the flare. Methods. The source was observed with a number of instruments in radio, near-infrared, optical (including polarimetry and spectroscopy), ultraviolet, X-ray, and gamma-ray bands. We use dedicated optical spectroscopy results to estimate the accretion disk and the dust torus luminosity. We performed spectral energy distribution modeling in the framework of combined synchrotron-self-Compton and external Compton scenario in which the electron energy distribution is partially determined from acceleration and cooling processes. Results. During the enhanced state, the flux of both SED components of QSO B1420+326 drastically increased and the peaks were shifted to higher energies. Follow-up observations with the MAGIC telescopes led to the detection of VHE gamma-ray emission from this source, making it one of only a handful of FSRQs known in this energy range. Modeling allows us to constrain the evolution of the magnetic field and electron energy distribution in the emission region. The gamma-ray flare was accompanied by a rotation of the optical polarization vector during a low -polarization state. Also, a new superluminal radio knot contemporaneously appeared in the radio image of the jet. The optical spectroscopy shows a prominent FeII bump with flux evolving together with the continuum emission and a MgII line with varying equivalent width.
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| Additional Information: | © 2021 ESO. Received: 15 October 2020; Accepted: 18 December 2020; Published online 29 March 2021. We would like to dedicate this paper to the memory of our friend and colleague, Dr. Valeri Larionov (1950−2020), who enthusiastically contributed to this and many other projects aimed at understanding blazars. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish MINECO (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729-C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017-87055-C2-2-P, FPA2017-90566-REDC); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-268/16.12.2019 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588 and SEV-2015-0548, the Unidad de Excelencia “María de Maeztu” MDM-2014-0369 and the “la Caixa” Foundation (fellowship LCF/BQ/PI18/11630012), by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Etudes Spatiales in France. This work was performed in part under DOE Contract DE-AC02-76SF00515. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the OVRO 40 m monitoring program Richards et al. (2011) which is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. This study was based in part on observations conducted using the 1.8 m Perkins Telescope Observatory (PTO) in Arizona, which is owned and operated by Boston University. The research at Boston University was supported in part by NASA Fermi GI program grants 80NSSC17K0649, 80NSSC19K1504, and 80NSSC19K1505. We thank the ASAS-SN team for making their data publicly available. The VLBA is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. This work made use of the Lowell Discovery Telescope (formerly Discovery Channel Telescope) at Lowell Observatory. Lowell is a private, nonprofit institution dedicated to astrophysical research and public appreciation of astronomy and operates the LDT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. We acknowledge support by Bulgarian National Science Fund under grant DN18-10/2017 and National RI Roadmap Projects DO1-277/16.12.2019 and DO1-268/16.12.2019 of the Ministry of Education and Science of the Republic of Bulgaria. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | gamma rays: galaxies – galaxies: jets – radiation mechanisms: non-thermal – quasars: individual: QSO B1420+326 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202039687 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20210202-095252065 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Official Citation: | VHE gamma-ray detection of FSRQ QSO B1420+326 and modeling of its enhanced broadband state in 2020 MAGIC Collaboration, V. A. Acciari, et. al. A&A, 647 (2021) A163; DOI: https://doi.org/10.1051/0004-6361/202039687 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| ID Code: | 107862 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 03 Feb 2021 19:05 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 31 Mar 2021 14:29 |
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