MAGIC Collaboration:, External Collaborators:, Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes, Monthly Notices of the Royal Astronomical Society, Volume 490, Issue 2, December 2019, Pages 2284–2299, https://doi.org/10.1093/mnras/stz2725
Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes
|Author:||Acciari, V. A.1,2; Ansoldi, S.3,4,5,6,7,8; Antonelli, L. A.9;|
1Inst Astrofis Canarias, E-38200 Tenerife, Spain.
2Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
3Univ Udine, I-33100 Udine, Italy.
4INFN Trieste, I-33100 Udine, Italy.
5Univ Tokyo, ICRR, Chiba 2778582, Japan.
6Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
7Tokai Univ, Dept Phys, Hiratsuka, Kanagawa 2591292, Japan.
8RIKEN, Saitama 3510198, Japan.
9Natl Inst Astrophys INAF, I-00136 Rome, Italy.
10Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
11Tech Univ Dortmund, Dept Phys, D-44221 Dortmund, Germany.
12Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
13Univ Split FESB, Dept Phys, Split 21000, Croatia.
14Univ Zagreb FER, Dept Phys, Zagreb 10000, Croatia.
15Univ Osijek, Dept Phys, Osijek 31000, Croatia.
16Rudjer Boskovic Inst, Dept Phys, Zagreb 10000, Croatia.
17HBNI, Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
18CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil.
19Univ Complutense Madrid, IPARCOS Inst, E-28040 Madrid, Spain.
20Univ Complutense Madrid, EMFTEL Dept, E-28040 Madrid, Spain.
21Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
22Univ Siena, Dept Phys, I-53100 Siena, Italy.
23INFN Pisa, I-53100 Siena, Italy.
24Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
25Univ Padua, Dept Phys, I-35131 Padua, Italy.
26INFN, I-35131 Padua, Italy.
27INFN, I-00044 Rome, Italy.
28Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
29BIST, IFAE, E-08193 Bellaterra, Barcelona, Spain.
30Univ Pisa, Dept Phys, I-56126 Pisa, Italy.
31INFN Pisa, I-56126 Pisa, Italy.
32UB, IEEC, ICCUB, E-08028 Barcelona, Spain.
33NAS RA, ICRANet Armenia, Yerevan 0019, Armenia.
34Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
35PIC, E-08193 Bellaterra, Barcelona, Spain.
36Univ Wurzburg, Dept Phys, D-97074 Wurzburg, Germany.
37Univ Turku, Finnish Ctr Astron ESO FINCA, FI-20014 Turku, Finland.
38Univ Oulu, Astron Res Unit, FI-90014 Oulu, Finland.
39Univ Autonoma Barcelona, Dept Fis, E-08193 Bellaterra, Spain.
40Univ Autonoma Barcelona, CERES, IEEC, E-08193 Bellaterra, Spain.
41Univ Trieste, Dept Fis, I-34127 Trieste, Italy.
42Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BG-1784 Sofia, Bulgaria.
43INAF Trieste, Trieste, Italy.
44Univ Bologna, Dept Phys & Astron, Bologna, Italy.
45INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
|Online Access:||PDF Full Text (PDF, 2.1 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe202003097665
Oxford University Press,
|Publish Date:|| 2020-03-09
Extreme high-energy-peaked BL Lac objects (EHBLs) are an emerging class of blazars. Their typical two-hump-structured spectral energy distribution (SED) peaks at higher energies with respect to conventional blazars. Multiwavelength (MWL) observations constrain their synchrotron peak in the medium to hard X-ray band. Their gamma-ray SED peaks above the GeV band, and in some objects it extends up to several TeV. Up to now, only a few EHBLs have been detected in the TeV gamma-ray range. In this paper, we report the detection of the EHBL 2WHSP J073326.7+515354, observed and detected during 2018 in TeV gamma rays with the MAGIC telescopes. The broad-band SED is studied within an MWL context, including an analysis of the Fermi-LAT data over 10 yr of observation and with simultaneous Swift-XRT, Swift-UVOT, and KVA data. Our analysis results in a set of spectral parameters that confirms the classification of the source as an EHBL. In order to investigate the physical nature of this extreme emission, different theoretical frameworks were tested to model the broad-band SED. The hard TeV spectrum of 2WHSP J073326.7+515354 sets the SED far from the energy equipartition regime in the standard one-zone leptonic scenario of blazar emission. Conversely, more complex models of the jet, represented by either a two-zone spine-layer model or a hadronic emission model, better represent the broad-band SED.
Monthly notices of the Royal Astronomical Society
|Pages:||2284 - 2299|
|Type of Publication:||
A1 Journal article – refereed
|Field of Science:||
115 Astronomy and space science
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 JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 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, and Unidad de Excelencia ‘María de Maeztu’ MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 220.127.116.11.02, 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’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.
JBG acknowledges the support of the Viera y Clavijo program funded by ACIISI and ULL. MC has received financial support through the Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation, grant no. LCF/BQ/LI18/11630012.
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).