A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Multi-wavelength study of OT 081: broadband modelling of a transitional blazar
Tekijät: MAGIC Collaboration: Abe, H.; Abe, S.; Acciari, V A; Agudo, I.; Aniello, T.; Ansoldi, S.; Antonelli, L A; Engels, A Arbet; Arcaro, C.; Artero, M.; Asano, K.; Baack, D.; Babić, A.; Baquero, A.; de Almeida, U Barres; Batković, I.; Baxter, J.; Bernardini, E.; Bernardos, M.; Bernete, J.; Berti, A.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, G.; Bošnjak, Ž.; Burelli, I.; Busetto, G.; Campoy-Ordaz, A.; Carosi, A.; Carosi, R.; Carretero-Castrillo, M.; Castro-Tirado, A J; Chai, Y.; Cifuentes, A.; Cikota, S.; 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.; Del Popolo, A.; Delfino, M.; Delgado, J; Mendez, C Delgado; Depaoli, D.; Di Pierro, F.; Di Venere, L.; Prester, D Dominis; Donini, A.; Dorner, D.; Doro, M.; Elsaesser, D.; Emery, G.; Escudero, J.; Fariña, L.; Fattorini, A.; Foffano, L.; Font, L.; Fukami, S.; Fukazawa, Y.; López, R J García; Gasparyan, S.; Gaug, M.; Paiva, J G Giesbrecht; Giglietto, N.; Giordano, F.; Gliwny, P.; Grau, R.; Green, J G; Hadasch, D.; Hahn, A.; Heckmann, L.; Herrera, J.; Hrupec, D.; Hütten, M.; Imazawa, R.; Inada, T.; Iotov, R.; Ishio, K.; Martínez, I Jiménez; Jormanainen, J.; Kerszberg, D.; Kluge, G W; Kobayashi, Y.; Kubo, H.; Kushida, J.; Lezáun, M Láinez; Lamastra, A.; Leone, F.; Lindfors, E.; Linhoff, L.; Lombardi, S.; Longo, F.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; de Oliveira Fraga, B Machado; Majumdar, P.; Makariev, M.; Maneva, G.; Mang, N.; Manganaro, M.; Mangano, S.; Mannheim, K.; Mariotti, M.; Martínez, M.; Mas-Aguilar, A.; Mazin, D.; Menchiari, S.; Mender, S.; Mićanović, S.; Miceli, D.; Miranda, J M; Mirzoyan, R.; Molina, E.; Mondal, H A; Morcuende, D.; Nanci, C.; Neustroev, V.; Nigro, C.; Nishijima, K.; Ekoume, T Njoh; Noda, K.; Nozaki, S.; Ohtani, Y.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J M; Pavletić, L.; Persic, M.; Pihet, M.; Pirola, G.; Podobnik, F.; Moroni, P G Prada; Prandini, E.; Principe, G.; Priyadarshi, C.; Rhode, W; Ribó, M.; Rico, J.; Righi, C.; Sahakyan, N.; Saito, T.; Satalecka, K.; Saturni, F G; Schleicher, B.; Schmidt, K.; Schmuckermaier, F.; Schubert, J L; Schweizer, T.; Sitarek, J.; Spolon, A.; Stamerra, A.; Strišković, J.; Strom, D.; Suda, Y.; Surić, T.; Suutarinen, S.; Tajima, H.; Takahashi, M.; Takeishi, R.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Ubach, S.; van Scherpenberg, J.; Ventura, S.; Verguilov, V.; Viale, I.; Vigorito, C F; Vitale, V.; Walter, R.; Yamamoto, T.; Benkhali, F Ait; Becherini, Y.; Bi, B; Böttcher, M.; Bolmont, J.; Brown, A.; Bulik, T.; Casanova, S.; Chand, T.; Chandra, S.; Chibueze, J.; Chibueze, O.; Egberts, K.; Einecke, S.; Ernenwein, J-P; Fontaine, G.; Gabici, S.; Goswami, P.; Holler, M.; Jamrozy, M.; Joshi, V.; Kasai, E.; Katarzyński, K.; Khatoon, R.; Khélifi, B.; Kluźniak, W.; Kosack, K.; Lang, R G; Le Stum, S.; Lemière, A.; Marx, R.; Moderski, R.; Moghadam, M O; de Naurois, M.; Niemiec, J.; O’Brien, P.; Ostrowski, M.; Peron, G.; Pita, S.; Pühlhofer, G.; Quirrenbach, A.; Rudak, B.; Sahakian, V.; Sanchez, D A; Santangelo, A.; Sasaki, M.; Schutte, H M; Seglar-Arroyo, M.; Shapopi, J N S; Steenkamp, R.; Steppa, C.; Suzuki, H.; Tanaka, T.; Tluczykont, M.; Venter, C.; Wagner, S J; Wierzcholska, A.; Zdziarski, A A; Żywucka, N.; from Fermi-LAT Collaboration: Becerra, J.; Ciprini, S.; Venters, T. M.; MWL collaborators: D’Ammando, F.; Esteban-Gutiérrez, A.; Ramazani, V Fallah; Filippenko, A V; Hovatta, T.; Jermak, H.; Jorstad, S.; Kiehlmann, S.; Lähteenmäki, A.; Larionov, V M; Larionova, E.; Marscher, A P; Morozova, D.; Max-Moerbeck, W.; Readhead, A C S; Reeves, R.; Steele, I A; Tornikoski, M.; Verrecchia, F.; Xiao, H.; Zheng, W.
Kustantaja: Oxford University Press (OUP)
Julkaisuvuosi: 2025
Journal: Monthly Notices of the Royal Astronomical Society
Tietokannassa oleva lehden nimi: Monthly Notices of the Royal Astronomical Society
Vuosikerta: 540
Numero: 1
Aloitussivu: 364
Lopetussivu: 384
ISSN: 0035-8711
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/stae2469
Verkko-osoite: https://doi.org/10.1093/mnras/stae2469
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/484826177
OT 081 is a well-known, luminous blazar that is remarkably variable in many energy bands. We present the first broadband study of the source which includes very-high-energy (VHE, E >100 GeV) γ-ray data taken by the MAGIC and H.E.S.S. imaging Cherenkov telescopes. The discovery of VHE γ-ray emission happened during a high state of γ-ray activity in July 2016, observed by many instruments from radio to VHE γ-rays. We identify four states of activity of the source, one of which includes VHE γ-ray emission. Variability in the VHE domain is found on daily timescales. The intrinsic VHE spectrum can be described by a power-law with index 3.27 ± 0.44stat ± 0.15sys (MAGIC) and 3.39 ± 0.58stat ± 0.64sys (H.E.S.S.) in the energy range of 55–300 GeV and 120–500 GeV, respectively. The broadband emission cannot be sucessfully reproduced by a simple one-zone synchrotron self-Compton model. Instead, an additional external Compton component is required. We test a lepto-hadronic model that reproduces the dataset well and a proton-synchrotron dominated model that requires an extreme proton luminosity. Emission models that are able to successfully represent the data place the emitting region well outside of the Broad Line Region (BLR) to a location at which the radiative environment is dominated by the infrared thermal radiation field of the dusty torus. In the scenario described by this flaring activity, the source appears to be an FSRQ, in contrast with past categorizations. This suggests that the source can be considered to be a transitional blazar, intermediate between BL Lac and FSRQ objects.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
This work was supported in part by the Croatian Science Foundation under the project number IP-2022-10-4595.
MS-A was supported by the grant FJC2020-044895-I funded by MCIN/AEI/10.13039/501100011033 and by the European Union NextGenerationEU/PRTR.
HBX acknowledges the support from the National Natural Science Foundation of China (NSFC 12203034), the Shanghai Science and Technology Fund (22YF1431500), and the science research grants from the China Manned Space Project. 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, MPG, and HGF, the Italian INFN and INAF, the Swiss National Fund SNF, the grants PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31, PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, and PID2019-107988GB-C22 funded by MCIN/AEI 10.13039/501100011033, 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 DO1-400/18.12.2020, and the Academy of Finland grant no. 320045 is gratefully acknowledged. This work was also been supported by Centros de Excelencia ‘Severo Ochoa’ y Unidades ‘María de Maeztu’ program of the MCIN/AEI 10.13039/501100011033 (SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S, CEX2019-000918-M, and MDM-2015-0509-18-2) and by the CERCA institution of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2022-10-4595 and the University of Rijeka Project uniri-prirod-18-48; by the Deutsche Forschungsgemeinschaft (SFB1491 and SFB876); by the Polish Ministry Of Education and Science grant no. 2021/WK/08; and by the Brazilian MCTIC, CNPq, and FAPERJ.
The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland grant no. 2016/22/M/ST9/00382, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science & Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science, the University of Amsterdam, and the Science Committee of Armenia grant 21AG-1C085. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen, and in Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation.
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’Études Spatiales in France. This work was performed in part under DOE Contract DE-AC02-76SF00515.
Part of this work is based on archival data, software, or online services provided by the Space Science Data Center ASI under contract ASI-INFN 2021-43-HH.0.
This research has made use of data from the OVRO 40-m monitoring program (Richards et al. 2011), supported by private funding from the California Institute of Technology and the Max Planck Institute for Radio Astronomy, and by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911.
SK acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreement no. 771282. WM-M gratefully acknowledges support by the ANID BASAL project FB210003 and FONDECYT 11190853. RR was supported by ANID BASAL grant FB210003. SC acknowledges support by the Italian Space Agency (Agenzia Spaziale Italiana, ASI) through contract ASI-OHBI-2017-12-I.0, with agreement ASI-INFN 2021-43-HH.0, and its Space Science Data Center (SSDC). This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by the Aalto University. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00856.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research has made use of the TeVCat online source catalogue (http://tevcat.uchicago.edu). The research at Boston University was supported by NASA Fermi Guest Investigator grants 80NSSC17K0649 and 80NSSC20K1567. 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. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, NNX12AO93G, and NNX15AU81G. AVF and WZ received financial assistance from the Christopher R. Redlich Fund, as well as donations from Gary and Cynthia Bengier, Clark and Sharon Winslow, Alan Eustace (WZ is a Bengier–Winslow–Eustace Specialist in Astronomy), and numerous other donors. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the U.S. National Science Foundation, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. The authors wish to thank Matteo Cerruti (APC – Université Paris Cité and ICC – Universitat de Barcelona) for providing the numerical results for the hadronic and lepto-hadronic models used in this work.
