RT Journal Article
T1 MAGIC detection of very high energy gamma-ray emission from the low-luminosity blazar 1ES 1741+196
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Domínguez, A.
A1 Fidalgo, D.
A1 Fonseca González, Mª Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nievas Rosillo, Mireia
AB We present the first detection of the nearby (z=0.084) low-luminosity BL Lac object 1ES 1741+196 in the very high energy (VHE: E>100 GeV) band. This object lies in a triplet of interacting galaxies. Early predictions had suggested 1ES 1741+196 to be, along with several other high-frequency BL Lac sources, within the reach of MAGIC detectability. Its detection by MAGIC, later confirmed by VERITAS, helps to expand the small population of known TeV BL Lacs. The source was observed with the MAGIC telescopes between 2010 April and 2011 May, collecting 46 h of good quality data. These observations led to the detection of the source at 6.0 σ confidence level, with a steady flux F(> 100 GeV) = (6.4 ± 1.7_(stat) ± 2.6_(syst)) • 10^(−12) ph cm^(−2) s^( −1) and a differential spectral photon index Γ = 2.4 ± 0.2_(stat) ± 0.2_(syst) in the range of ∼80 GeV - 3 TeV. To study the broad-band spectral energy distribution (SED) simultaneous with MAGIC observations, we use KVA, Swift/UVOT and XRT, and Fermi/LAT data. One-zone synchrotron-self-Compton (SSC) modeling of the SED of 1ES 1741+196 suggests values for the SSC parameters that are quite common among known TeV BL Lacs except for a relatively low Doppler factor and slope of electron energy distribution. A thermal feature seen in the SED is well matched by a giant elliptical’s template. This appears to be the signature of thermal emission from the host galaxy, which is clearly resolved in optical observations.
PB Wiley
SN 0035-8711
YR 2017
FD 2017-06
LK https://hdl.handle.net/20.500.14352/17861
UL https://hdl.handle.net/20.500.14352/17861
LA eng
NO © 2017 The Authors Published by Oxford University Press. Artículo firmado por 159 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 (FPA2015-69818-P, FPA2012-36668, FPA2015-68278-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2013-47447-C3-1-P, AYA2015- 71042-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, 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/NHESS-MAGIC/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 Commissariatà  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 research was supported 572 by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Universities Space Re- 574 search Association through a contract with NASA. F. K. acknowledges funding from the European Unions Horizon 2020 research and innovation programme under grant agreement No 653477.
NO Ministerio de Economía y Competitividad (MINECO)
NO European Unions Horizon 2020
NO German BMBF and MPG
NO Italian INFN and INAF
NO Swiss National Fund SNF
NO Japanese JSPS and MEXT
NO Spanish Centro de Excelencia “Severo Ochoa”
NO Unidad de Excelencia “María de Maeztu”
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 Commissariatà  l’Energie Atomique and the Centre National de la Recherche Scientifique
NO 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)
NO High Energy Accelerator Research Organization (KEK)
NO Japan Aerospace Exploration Agency (JAXA)
NO K. A. Wallenberg Foundation
NO Swedish Research Council
NO Swedish National Space Board
NO Centre National d’Etudes Spatiales in France
NO NASA Postdoctoral Program at the Goddard Space Flight Center
DS Docta Complutense
RD 17 jul 2024