RT Journal Article
T1 Investigating the peculiar emission from the new VHE gamma-ray source H1722+119
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Bonnefoy, Simon Francois Albert
A1 Contreras González, José Luis
A1 Fonseca González, Mª Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nievas Rosillo, Mireia
A1 otros, ...
AB The MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes observed the BL Lac object H1722+119 (redshift unknown) for six consecutive nights between 2013 May 17 and 22, for a total of 12.5 h. The observations were triggered by high activity in the optical band measured by the KVA (Kungliga Vetenskapsakademien) telescope. The source was for the first time detected in the very high energy (VHE, E > 100 GeV) γ-ray band with a statistical significance of 5.9 σ. The integral flux above 150 GeV is estimated to be (2.0 ± 0.5) per cent of the Crab Nebula flux. We used contemporaneous high energy (HE, 100MeV < E < 100 GeV) γ-ray observations from Fermi-LAT (Large Area Telescope) to estimate the redshift of the source. Within the framework of the current extragalactic background light models, we estimate the redshift to be z = 0.34±0.15. Additionally, we used contemporaneous X-ray to radio data collected by the instruments on board the Swift satellite, the KVA, and the OVRO (Owens Valley Radio Observatory) telescope to study multifrequency characteristics of the source. We found no significant temporal variability of the flux in the HE and VHE bands. The flux in the optical and radio wavebands, on the other hand, did vary with different patterns. The spectral energy distribution (SED) of H1722+119 shows surprising behaviour in the ∼ 3×1014 −1018 Hz frequency range. It can be modelled using an inhomogeneous helical jet synchrotron self-Compton model.
PB Wiley
SN 0035-8711
YR 2016
FD 2016-07-01
LK https://hdl.handle.net/20.500.14352/24629
UL https://hdl.handle.net/20.500.14352/24629
LA eng
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NO © 2016 The Authors. Artículo firmado por 160 autores. We are grateful to Marco Landoni for help with adopting data from Landoni et al. (2014).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 (FPA2012-39502), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESSMAGIC/2010/0.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 from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911.Antonio Stamerra acknowledges financial support in the frame of the INAF Senior Scientist program of ASDC and by the Italian Ministry for Research and Scuola Normale Superiore.Elisa Prandini gratefully acknowledges the financial support of the Marie Heim-Vogtlin grant of the Swiss National Science Foundation.
NO Ministerio de Economía y Competitividad (MINECO)
NO German BMBF and MPG
NO Italian INFN and INAF
NO Swiss National Fund SNF
NO Japanese JSPS and MEXT
NO Centro de Excelencia Severo Ochoa
NO Spanish Consolider Ingenio 2010 programme
NO Academy of Finland
NO Croatian Science Foundation (HrZZ)
NO University of Rijeka
NO DFG Collaborative Research Centers
NO Polish MNiSzW
NO National Aeronautics and Space Administration and the Department of Energy in the United States
NO 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
NO Agenzia Spaziale Italiana
NO Istituto Nazionale di Fisica Nucleare in Italy
NO Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan
NO High Energy Accelerator Research Organization (KEK) in Japan
NO Japan Aerospace Exploration Agency (JAXA)
NO K. A. Wallenberg Foundation in Sweden
NO Swedish Research Council
NO Swedish National Space Board
NO Istituto Nazionale di Astrofisica in Italy
NO Centre National d’Études Spatiales in France
NO NASA
NO NSF
NO INAF Senior Scientist program of ASDC
NO Italian Ministry for Research
NO Scuola Normale Superiore in Italy
NO Swiss National Science Foundation
DS Docta Complutense
RD 18 jul 2024