RT Journal Article
T1 Insights into the emission of the blazar 1ES 1011+496 through unprecedented broadband observations during 2011 and 2012
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fonseca González, María Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nievas Rosillo, Mireia
A1 Satalecka, Konstanzja
A1 Scapin, Valeria
AB Context. 1ES 1011+496 (z = 0.212) was discovered in very high-energy (VHE, E >100 GeV) γ rays with MAGIC in 2007. The absence of simultaneous data at lower energies led to an incomplete characterization of the broadband spectral energy distribution (SED).Aims. We study the source properties and the emission mechanisms, probing whether a simple one-zone synchrotron self-Compton (SSC) scenario is able to explain the observed broadband spectrum. Methods. We analyzed data in the range from VHE to radio data from 2011 and 2012 collected by MAGIC, Fermi-LAT, Swift, KVA, OVRO, and Metsähovi in addition to optical polarimetry data and radio maps from the Liverpool Telescope and MOJAVE.Results. The VHE spectrum was fit with a simple power law with a photon index of 3.69 ± 0.22 and a flux above 150 GeV of (1.46±0.16)×10^(−11) ph cm^(−2) s^(−1) . The source 1ES 1011+496 was found to be in a generally quiescent state at all observed wavelengths, showing only moderate variability from radio to X-rays. A low degree of polarization of less than 10% was measured in optical, while some bright features polarized up to 60% were observed in the radio jet. A similar trend in the rotation of the electric vector position angle was found in optical and radio. The radio maps indicated a superluminal motion of 1.8 ± 0.4 c, which is the highest speed statistically significant measured so far in a high-frequency-peaked BL Lac. Conclusions. For the first time, the high-energy bump in the broadband SED of 1ES 1011+496 could be fully characterized from 0.1 GeV to 1 TeV, which permitted a more reliable interpretation within the one-zone SSC scenario. The polarimetry data suggest that at least part of the optical emission has its origin in some of the bright radio features, while the low polarization in optical might be due to the contribution of parts of the radio jet with different orientations of the magnetic field with respect to the optical emission.
PB EDP Sciencies
SN 1432-0746
YR 2016
FD 2016-07
LK https://hdl.handle.net/20.500.14352/24601
UL https://hdl.handle.net/20.500.14352/24601
LA eng
NO © ESO 2016. Artículo firmado por 164 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 (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-HESS-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 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. The Metsähovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST- 1109911. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator (Deller et al. 2011), developed as part of the Australian Major National Research Facilities Programme and operated under licence. The MOJAVE project is supported under NASA-Fermi grants NNX12A087G. Part of this work is based on archival data provided by the ASI ASDC.
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 (France)
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) (Japan)
NO Japan Aerospace Exploration Agency (JAXA)
NO K. A. Wallenberg Foundation
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 NASA-Fermi
DS Docta Complutense
RD 11 abr 2025