RT Journal Article
T1 Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescope
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fidalgo, David Friedrich Carreto
A1 Fonseca González, Mª Victoria
A1 Hoang, Kim Dinh
A1 López Moya, Marcos
A1 Morcuende, D.
A1 Peñil del Campo, Pablo
A1 Saha, Lab
AB 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 J073320,7+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 EIME. In order to investigate the physical nature of this extreme emission, different theoretical frameworks were tested to model the broadband 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-hand SED.
PB Wiley
SN 0035-8711
YR 2019
FD 2019-12
LK https://hdl.handle.net/20.500.14352/6161
UL https://hdl.handle.net/20.500.14352/6161
LA eng
NO © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 175 autores. 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, FPA201782729-C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017-87055C2-2-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 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 a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire 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 performed in part under DOE Contract DE-AC02-76SF00515.; We acknowledge the use of public data from the Swift data archive. This publication uses data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We also acknowledge the use of the Space Science Data Base (SSDC).; 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.
NO Ministerio de Economía y Competitividad (MINECO)/FEDER
NO Centro de Excelencia Severo Ochoa
NO Unidad de Excelencia Maria de Maeztu
NO German BMBF Federal Ministry of Education & Research (BMBF)
NO INAF
NO MPG Max Planck Society
NO Italian INFN Istituto Nazionale di Fisica Nucleare
NO Swiss National Fund SNF Swiss National Science Foundation (SNSF)
NO Indian Department of Atomic Energy
NO Japanese JSPS Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science
NO Bulgarian Ministry of Education and Science, National RI Roadmap Project
NO Academy of FinlandAcademy of Finland
NO Croatian Science Foundation (HrZZ)
NO University of Rijeka Project
NO DFG Collaborative Research Centers German Research Foundation (DFG)
NO Polish National Research Centre
NO Brazilian MCTIC
NO CNPq National Council for Scientific and Technological Development (CNPq)
NO FAPERJ Carlos Chagas Filho Foundation for Research Support of the State of Rio de Janeiro (FAPERJ)
NO DOE United States Department of Energy
NO Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation
DS Docta Complutense
RD 5 may 2024