Multimessenger Characterization of Markarian 501 during Historically Low X-Ray and γ-Ray Activity

被引：14

作者：

Abe, H. ^{[1
]}

Abe, S. ^{[1
]}

Acciari, V. A. ^{[2
,3
]}

Agudo, I. ^{[4
]}

Aniello, T. ^{[5
]}

Ansoldi, S. ^{[6
,7
,114
]}

Antonelli, L. A. ^{[5
]}

Arbet-Engels, A. ^{[8
]}

Arcaro, C. ^{[9
,10
]}

Artero, M. ^{[11
]}

Asano, K. ^{[1
]}

Baack, D. ^{[12
]}

Babic, A. ^{[13
]}

Baquero, A. ^{[14
,15
]}

de Almeida, U. Barres ^{[16
]}

Barrio, J. A. ^{[14
,15
]}

Batkovic, I. ^{[9
,10
]}

Baxter, J. ^{[1
]}

Becerra Gonzalez, J. ^{[2
,3
]}

Bednarek, W. ^{[17
]}

Bernardini, E. ^{[9
,10
]}

Bernardos, M. ^{[4
]}

Berti, A. ^{[8
]}

Besenrieder, J. ^{[8
]}

Bhattacharyya, W. ^{[18
]}

Bigongiari, C. ^{[5
]}

Biland, A. ^{[19
]}

Blanch, O. ^{[11
]}

Bonnoli, G. ^{[5
]}

Bosnjak, Z. ^{[13
]}

Burelli, I. ^{[6
,7
]}

Busetto, G. ^{[9
,10
]}

Carosi, R. ^{[20
,21
]}

Carretero-Castrillo, M. ^{[22
]}

Castro-Tirado, A. J. ^{[4
]}

Ceribella, G. ^{[1
]}

Chai, Y. ^{[8
]}

Chilingarian, A. ^{[23
]}

Cikota, S. ^{[13
]}

Colombo, E. ^{[2
,3
]}

Contreras, J. L. ^{[14
,15
]}

Cortina, J. ^{[24
]}

Covino, S. ^{[5
]}

D'Amico, G. ^{[25
]}

D'Elia, V. ^{[5
]}

Da Vela, P. ^{[20
,21
,111
]}

Dazzi, F. ^{[5
]}

De Angelis, A. ^{[9
,10
]}

De Lotto, B. ^{[6
,7
]}

Del Popolo, A. ^{[26
,27
]}

机构：

[1] Univ Tokyo, Inst Cosm Ray Res ICRR, Japanese MAGIC Grp, Kashiwa, Chiba 2778582, Japan

[2] Univ La Laguna, Inst Astrofis Canarias, E-38200 Tenerife, Spain

[3] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain

[4] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain

[5] Natl Inst Astrophys INAF, I-00136 Rome, Italy

[6] Univ Udine, I-33100 Udine, Italy

[7] INFN Trieste, I-33100 Udine, Italy

[8] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[9] Univ Padua, I-35131 Padua, Italy

[10] INFN, I-35131 Padua, Italy

[11] Barcelona Inst Sci & Technol BIST, Inst Fis Altes Energies IFAE, E-08193 Bellaterra, Barcelona, Spain

[12] Tech Univ Dortmund, D-44221 Dortmund, Germany

[13] Univ Zagreb, Fac Elect Engn & Comp FER, Croatian MAGIC Grp, Zagreb 10000, Croatia

[14] Univ Complutense Madrid, IPARCOS Inst, E-28040 Madrid, Spain

[15] Univ Complutense Madrid, EMFTEL Dept, E-28040 Madrid, Spain

[16] URCA, Ctr Brasileiro Pesquisas Fis CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil

[17] Univ Lodz, Fac Phys & Appl Informat, Dept Astrophys, PL-90236 Lodz, Poland

[18] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[19] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland

[20] Univ Pisa, I-56126 Pisa, Italy

[21] INFN, I-56126 Pisa, Italy

[22] Univ Barcelona, ICCUB, IEEC, E-08028 Barcelona, Spain

[23] A Alikhanyan Natl Sci Lab, Armenian MAGIC Grp, Yerevan 0036, Armenia

[24] Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain

[25] Univ Bergen, Dept Phys & Technol, Bergen, Norway

[26] Univ Catania, INFN Sez Catania, INFN MAGIC Grp, I-95123 Catania, Italy

[27] Univ Catania, Dipartimento Fis & Astron, I-95123 Catania, Italy

[28] INFN Sez Torino, INFN MAGIC Grp, I-10125 Turin, Italy

[29] Univ Torino, I-10125 Turin, Italy

[30] INFN Sez Bari, INFN MAGIC Grp, I-70125 Bari, Italy

[31] Univ Bari, Dipartimento Interateneo Fis, I-70125 Bari, Italy

[32] Politecn Bari, I-70125 Bari, Italy

[33] Univ Rijeka, Fac Phys, Croatian MAGIC Grp, Rijeka 51000, Croatia

[34] Univ Wurzburg, D-97074 Wurzburg, Germany

[35] Nat Wissensch Labor Schuler FKG, Hans Haffner Sternwarte Hettstadt, D-97082 Wurzburg, Germany

[36] Friedrich Koenig Gymnasium, D-97082 Wurzburg, Germany

[37] Univ Geneva, Chemin Ecogia 16, CH-1290 Versoix, Switzerland

[38] Univ Turku, Finnish Ctr Astron ESO, Finnish MAGIC Grp, FI-20014 Turku, Finland

[39] Univ Autonoma Barcelona, Dept Fis, E-08193 Bellaterra, Spain

[40] Univ Autonoma Barcelona, CERES, IEEC, E-08193 Bellaterra, Spain

[41] Hiroshima Univ, Grad Sch Adv Sci & Engn, Phys Program, Japanese MAGIC Grp, Hiroshima 7398526, Japan

[42] CRANet Armenia, Armenian MAGIC Grp, Yerevan 0019, Armenia

[43] Univ Split, Fac Elect Engn Mech Engn & Naval Architecture FES, Croatian MAGIC Grp, Split 21000, Croatia

[44] Josip Juraj Strossmayer Univ Osijek, Dept Phys, Croatian MAGIC Grp, Osijek 31000, Croatia

[45] Tokai Univ, Dept Phys, Japanese MAGIC Grp, Hiratsuka, Kanagawa 2591292, Japan

[46] Univ Siena, I-53100 Siena, Italy

[47] INFN Pisa, I-53100 Siena, Italy

[48] A CI Homi Bhabha Natl Inst, Saha Inst Nucl Phys, Kolkata 700064, W Bengal, India

[49] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BG-1784 Sofia, Bulgaria

[50] Yamagata Univ, Dept Phys, Japanese MAGIC Grp, Yamagata 9908560, Japan

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2023年 / 266卷 / 02期

基金：

欧洲研究理事会; 芬兰科学院; 美国国家科学基金会; 美国国家航空航天局;

关键词：

LARGE-AREA TELESCOPE; BL-LAC OBJECTS; SPECTRAL ENERGY-DISTRIBUTION; 23 DAY PERIODICITY; PARSEC-SCALE JETS; MAGIC TELESCOPES; GALACTIC NUCLEI; MRK; 421; MULTIWAVELENGTH VARIABILITY; BACKGROUND-RADIATION;

D O I：

10.3847/1538-4365/acc181

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the broadband emission of Mrk 501 using multiwavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi's Large Area Telescope (LAT), NuSTAR, Swift, GASP-WEBT, and the Owens Valley Radio Observatory. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wave bands, with the highest occurring at X-rays and very-high-energy (VHE) & gamma;-rays. A significant correlation (>3 & sigma;) between X-rays and VHE & gamma;-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between the Swift X-Ray Telescope and Fermi-LAT. We additionally find correlations between high-energy & gamma;-rays and radio, with the radio lagging by more than 100 days, placing the & gamma;-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE & gamma;-rays from mid-2017 to mid-2019 with a stable VHE flux (>0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2 yr long low state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED toward the low state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock.

引用

页数：43

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