M. L. Ahnen et al. (2017) First multi-wavelength campaign on the gamma-ray-loud active galaxy IC 310. A&A 603, A25. https://doi.org/10.1051/0004-6361/201630347
First multi-wavelength campaign on the gamma-ray-loud active galaxy IC 310
|Author:||Ahnen, M. L.1; Ansoldi, S.2,3,4; Antonelli, L. A.5;|
1Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
2Univ Udine, I-33100 Udine, Italy.
3INFN Trieste, I-33100 Udine, Italy.
4Kyoto Univ, Dept Phys, Kyoto 6068501, Japan.
5INAF, Natl Inst Astrophys, I-00136 Rome, Italy.
6Univ Padua, I-35131 Padua, Italy.
7INFN, I-35131 Padua, Italy.
8Univ Osijek, Univ Zagreb FER, Univ Split FESB, Univ Rijeka,Rudjer Boskovic Inst,Croatian MAGIC C, Osijek, Croatia.
9Saha Inst Nucl Phys, 1 Bidhannagar,Salt Lake,Sector 1, Kolkata 700064, India.
10Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
11MCTI, CBPF, R Dr Xavier Sigaud,150 Urca, BR-22290180 Rio De Janeiro, RJ, Brazil.
12Univ Complutense, Madrid 28040, Spain.
13Inst Astrofis Canarias, San Cristobal la Laguna 38200, Spain.
14Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain.
15NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
16Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
17Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
18Univ Lodz, PL-90236 Lodz, Poland.
19Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany.
20Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany.
21Univ Trieste, I-34127 Trieste, Italy.
22Barcelona Inst Sci & Technol, IFAE, Campus UAB, Barcelona 08193, Spain.
23Univ Siena, I-53100 Siena, Italy.
24INFN Pisa, I-53100 Siena, Italy.
25Univ Wurzburg, D-97074 Wurzburg, Germany.
26Ecole Polytech Fed Lausanne, CH-1085 Lausanne, Switzerland.
27CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain.
28Dortmund Univ Technol, D-44221 Dortmund, Germany.
29Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany.
30Univ Turku, Finnish MAGIC Consortium Tuorla Observ, Turku, Finland.
31Univ Turku, Astron Div, Oulu 90014, Finland.
32Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain.
33Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
34Univ Barcelona, ICC, IEEC UB, Barcelona 08028, Spain.
35Univ Tokyo, ICRR, Dept Phys, Japanese MAGIC Consortium, Tokyo, Japan.
36Univ Tokushima, Tokai Univ, Kyoto Univ, Hakubi Ctr, Tokushima, Japan.
37Inst Nucl Energy Res, Sofia 1784, Bulgaria.
38Finnish Ctr Astron ESO FINCA, Turku 21500, Finland.
39INAF Trieste, Trieste, Italy.
40Univ Bologna, Dept Phys & Astron, I-40126 Bologna, Italy.
41Univ Pisa, I-56126 Pisa, Italy.
42INFN Pisa, I-56126 Pisa, Italy.
43ICREA, Barcelona 08193, Spain.
44Univ Amsterdam, GRAPPA & Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
45Netherlands Inst Radio Astron, ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands.
46Univ Erlangen Numberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany.
47Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany.
48Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, Valencia 46100, Spain.
49Univ Valencia, Observ Astron, C Catedratico Jose Beltran 2, Valencia 46980, Spain.
50Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
51ESA ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
52Aalto Univ Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland.
53Aalto Univ, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland.
|Online Access:||PDF Full Text (PDF, 0.8 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe2019093030645
|Publish Date:|| 2019-09-30
Context: The extragalactic very-high-energy gamma-ray sky is rich in blazars. These are jetted active galactic nuclei that are viewed at a small angle to the line-of-sight. Only a handful of objects viewed at a larger angle are so far known to emit above 100 GeV. Multi-wavelength studies of such objects up to the highest energies provide new insights into the particle and radiation processes of active galactic nuclei.
Aims: We aim to report the results from the first multi-wavelength campaign observing the TeV detected nucleus of the active galaxy IC 310, whose jet is observed at a moderate viewing angle of 10°−20°.
Methods: The multi-instrument campaign was conducted between 2012 November and 2013 January, and involved observations with MAGIC, Fermi, INTEGRAL, Swift, OVRO, MOJAVE and EVN. These observations were complemented with archival data from the AllWISE and 2MASS catalogs. A one-zone synchrotron self-Compton model was applied to describe the broadband spectral energy distribution.
Results: IC 310 showed an extraordinary TeV flare at the beginning of the campaign, followed by a low, but still detectable TeV flux. Compared to previous measurements in this energy range, the spectral shape was found to be steeper during the low emission state. Simultaneous observations in the soft X-ray band showed an enhanced energy flux state and a harder-when-brighter spectral shape behavior. No strong correlated flux variability was found in other frequency regimes. The broadband spectral energy distribution obtained from these observations supports the hypothesis of a double-hump structure.
Conclusions: The harder-when-brighter trend in the X-ray and VHE emission, observed for the first time during this campaign, is consistent with the behavior expected from a synchrotron self-Compton scenario. The contemporaneous broadband spectral energy distribution is well described with a one-zone synchrotron self-Compton model using parameters that are comparable to those found for other gamma-ray-emitting misaligned blazars.
Astronomy and astrophysics
|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 he 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 188.8.131.52.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and bythe Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.
|Academy of Finland Grant Number:||
268740 (Academy of Finland Funding decision)
© ESO, 2017.