New hard-TeV extreme blazars detected with the MAGIC telescopes
|Author:||Acciari, V. A.1,2; Ansoldi, S.3,4,5,6,7,8,9; Antonelli, L. A.9;|
1Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
2Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
3Univ Udine, I-33100 Udine, Italy.
4INFN Trieste, I-33100 Udine, Italy.
5Univ Tokyo, Japanese Mag Consortium ICRR, Chiba 2778582, Japan.
6Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
7Tokai Univ, Hiratsuka, Kanagawa 2591292, Japan.
8RIKEN, Saitama 3510198, Japan.
9Natl Inst Astrophys INAF, I-100136 Rome, Italy.
10Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
11Tech Univ Dortmund, D-44221 Dortmund, Germany.
12Croatian Consortium Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
13Univ Split, FESB, Split 21000, Croatia.
14Univ Zagreb, FER, Zagreb 10000, Croatia.
15Univ Osijek, Osijek 31000, Croatia.
16Rudjer Boskovic Inst, Zagreb 10000, Croatia.
17HBNI, Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
18URCA, CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil.
19Univ Complutense Madrid, IPARCOS Inst, E-28040 Madrid, Spain.
20Univ Complutense Madrid, EMFTEL Dept, E-28040 Madrid, Spain.
21Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
22Univ Siena, I-53100 Siena, Italy.
23INFN Pisa, I-53100 Siena, Italy.
24DESY, D-15738 Zeuthen, Germany.
25Univ Padua, I-35131 Padua, Italy.
26Ist Nazl Fis Nucl, I-35131 Padua, Italy.
27Ist Nazl Fis Nucl, I-00044 Rome, Italy.
28Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
29Barcelona Inst Sci & Technol, IFAE, E-08193 Bellaterra, Barcelona, Spain.
30Univ Pisa, I-56126 Pisa, Italy.
31INFN Pisa, I-56126 Pisa, Italy.
32Univ Barcelona, ICCUB, IEEC UB, E-08028 Barcelona, Spain.
33A Alikhanyan Natl Lab, Armenian Consortium ICRANet Armenia NAS RA, Yerevan, Armenia.
34Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
35PIC, E-08193 Bellaterra, Barcelona, Spain.
36Univ Wurzburg, D-97074 Wurzburg, Germany.
37Univ Turku, FINNISH MAG Consortium, Finnish Ctr Astron ESO FINCA, FI-20014 Turku, Finland.
38Univ Oulu, Astron Res Unit, FI-90014 Oulu, Finland.
39Univ Autonoma Barcelona, Dept Fis, E-08193 Bellaterra, Spain.
40Univ Autonoma Barcelona, CERES IEEC, E-08193 Bellaterra, Spain.
41Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
42Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BG-1784 Sofia, Bulgaria.
43INAF Trieste, Trieste, Italy.
44Univ Bologna, Dept Phys & Astron, Bologna, Italy.
45North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
46Univ Savoie Mt Blanc, Univ Grenoble Alpes, LAPP, CNRS, F-74000 Annecy, France.
47Ist Radioastron, Bologna, Italy.
48Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy.
49Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
50NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
51INAF Astron Observ Rome, Via Frascati 33, I-00044 Rome, Italy.
52Montana State Univ, Dept Phys, POB 173840, Bozeman, MT 59717 USA.
|Online Access:||PDF Full Text (PDF, 8.9 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe2020061845030
|Publish Date:|| 2020-06-18
Extreme high-frequency-peaked BL Lac objects (EHBLs) are blazars that exhibit extremely energetic synchrotron emission. They also feature nonthermal gamma-ray emission whose peak lies in the very high-energy (VHE, E > 100 GeV) range, and in some sources exceeds 1 TeV: this is the case for hard-TeV EHBLs such as 1ES 0229+200. With the aim of increasing the EHBL population, 10 targets were observed with the MAGIC telescopes from 2010 to 2017, for a total of 265 hr of good-quality data. The data were complemented by coordinated Swift observations. The X-ray data analysis confirms that all but two sources are EHBLs. The sources show only a modest variability and a harder-when-brighter behavior, typical for this class of objects. At VHE gamma-rays, three new sources were detected and a hint of a signal was found for another new source. In each case, the intrinsic spectrum is compatible with the hypothesis of a hard-TeV nature of these EHBLs. The broadband spectral energy distributions (SEDs) of all sources are built and modeled in the framework of a single-zone, purely leptonic model. The VHE gamma-ray-detected sources were also interpreted with a spine–layer model and a proton synchrotron model. The three models provide a good description of the SEDs. However, the resulting parameters differ substantially in the three scenarios, in particular the magnetization parameter. This work presents the first mini catalog of VHE gamma-ray and multiwavelength observations of EHBLs.
Astrophysical journal. Supplement series
|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 ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2017-82729-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-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 18.104.22.168.02, 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. E.P. has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska–Curie grant agreement No. 664931. M.C. has received financial support through the Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation, grant No. LCF/BQ/LI18/11630012.
The authors are grateful to Luigi Costamante for providing the data previously published. Part of this work is based on archival data, software, or online services provided by the Space Science Data Center—ASI. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory.
© 2020. The American Astronomical Society.