Detection of persistent VHE gamma-ray emission from PKS 1510-089 by the MAGIC telescopes during low states between 2012 and 2017

被引：26

作者：

Acciari, V. A. ^{[1
]}

Ansoldi, S. ^{[2
,3
,30
,31
,32
,33
]}

Antonelli, L. A. ^{[4
]}

Engels, A. Arbet ^{[5
]}

Arcaro, C. ^{[6
,7
]}

Baack, D. ^{[8
]}

Babic, A. ^{[9
,10
,11
,12
,13
]}

Banerjee, B. ^{[14
]}

Bangale, P. ^{[15
]}

Barres de Almeida, U. ^{[15
,16
]}

Barrio, J. A. ^{[17
]}

Bednarek, W. ^{[18
]}

Bernardini, E. ^{[6
,7
,19
,35
]}

Berti, A. ^{[2
,3
,36
]}

Besenrieder, J. ^{[15
]}

Bhattacharyya, W. ^{[19
]}

Bigongiari, C. ^{[4
]}

Biland, A. ^{[5
]}

Blanch, O. ^{[20
]}

Bonnoli, G. ^{[21
,22
]}

Carosi, R. ^{[22
,23
]}

Ceribella, G. ^{[15
]}

Cikota, S. ^{[9
,10
,11
,12
,13
]}

Colak, S. M. ^{[20
]}

Colin, P. ^{[15
]}

Colombo, E. ^{[1
]}

Contreras, J. L. ^{[17
]}

Cortina, J. ^{[20
]}

Covino, S. ^{[4
]}

D'Elia, V. ^{[4
]}

Da Vela, P. ^{[22
,23
]}

Dazzi, F. ^{[4
]}

De Angelis, A. ^{[6
,7
]}

De Lotto, B. ^{[2
,3
]}

Delfino, M. ^{[20
,37
]}

Delgado, J. ^{[20
,37
]}

Di Pierro, F. ^{[4
]}

Do Souto Espinera, E. ^{[20
]}

Dominguez, A. ^{[17
]}

Prester, D. Dominis ^{[9
,10
,11
,12
,13
]}

Dorner, D. ^{[24
]}

Doro, M. ^{[6
,7
]}

Einecke, S. ^{[8
]}

Elsaesser, D. ^{[8
]}

Ramazani, V. Fallah ^{[25
,26
]}

Fattorini, A. ^{[8
]}

Fernandez-Barral, A. ^{[5
,20
]}

Ferrara, G. ^{[4
]}

Fidalgo, D. ^{[17
]}

Foffano, L. ^{[6
,7
]}

机构：

[1] Univ La Laguna, Inst Astrofis Canarias, E-38206 Tenerife, Spain

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

[3] INFN Trieste, I-34149 Trieste, Italy

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

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

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

[7] INFN Padova, I-35131 Padua, Italy

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

[9] Univ Rijeka, Croatian MAGIC Consortium, Rijeka 51000, Croatia

[10] Univ Split, FESB, Split 21000, Croatia

[11] Univ Zagreb, FER, Zagreb 10000, Croatia

[12] Univ Osijek, Osijek 31000, Croatia

[13] Rudjer Boskovic Inst, Zagreb 10000, Croatia

[14] HBNI, Saha Inst Nucl Phys, 1-AF Bidhannagar,Salt Lake,Sect 1, Kolkata 700064, India

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

[16] URCA, CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil

[17] Univ Complutense, Unidad Particulas & Cosmol UPARCOS, E-28040 Madrid, Spain

[18] Univ Lodz, Dept Astrophys, Lodz, Poland

[19] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany

[20] BIST, IFAE, Barcelona 08193, Spain

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

[22] INFN Pisa, I-56127 Pisa, Italy

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

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

[25] Univ Turku, Tuorla Observ Dept Phys & Astron, Finnish MAGIC Consortium, Turku 20014, Finland

[26] Univ Oulu, Oulu 90014, Finland

[27] Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Spain

[28] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain

[29] Univ Barcelona, ICCUB, IEEC UB, E-08028 Barcelona, Spain

[30] Univ Tokyo, ICRR, Japanese MAGIC Consortium, Chiba 2778582, Japan

[31] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan

[32] Tokai Univ, Kyoto, Kanagawa 2591292, Japan

[33] RIKEN, Saitama 3510198, Japan

[34] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria

[35] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[36] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[37] PIC, Barcelona 08193, Spain

[38] Univ Bologna, INAF Trieste, Bologna, Italy

[39] Univ Bologna, Dept Phys & Astron, Bologna, Italy

[40] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[41] Univ Insubria, Dipartimento Sci & Alta Tecnol, Via Valleggio 11, I-22100 Como, Italy

[42] Osserv Astron Brera, Ist Nazl Astrofis, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy

[43] CALTECH, Owens Valley Radio Observ, Pasadena, CA 91125 USA

[44] Univ Turku, Tuorla Observ, Vaisalantie 20, Piikkio 21500, Finland

[45] Univ Chile, Dept Astron, Camino Observa 1515, Santiago, Chile

[46] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland

[47] Inst Radio Astron Millimetr, Avenida Div Pastora 7,Local 20, Granada 18008, Spain

[48] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[49] Max Planck Inst Radioastron, Auf dem Hugel 69, D-53121 Bonn, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 619卷

关键词：

galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual: PKS 1510-089; LARGE-AREA TELESCOPE; BROAD-LINE REGIONS; MILLIMETER WAVELENGTHS; MAJOR UPGRADE; RADIATION; BLAZARS; ABSORPTION; II; JET; CALIBRATION;

D O I：

10.1051/0004-6361/201833618

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. PKS 1510-089 is a flat spectrum radio quasar strongly variable in the optical and GeV range. To date, very high-energy (VHE, >100 GeV) emission has been observed from this source either during long high states of optical and GeV activity or during short flares. Aims. We search for low-state VHE gamma-ray emission from PKS 1510-089. We characterize and model the source in a broadband context, which would provide a baseline over which high states and flares could be better understood. Methods. PKS 1510-089 has been monitored by the MAGIC telescopes since 2012. We use daily binned Fermi-LAT flux measurements of PKS 1510-089 to characterize the GeV emission and select the observation periods of MAGIC during low state of activity. For the selected times we compute the average radio, IR, optical, UV, X-ray, and gammaray emission to construct a low-state spectral energy distribution of the source. The broadband emission is modeled within an external Compton scenario with a stationary emission region through which plasma and magnetic fields are flowing. We also perform the emissio-model-independent calculations of the maximum absorption in the broad line region (BLR) using two different models. Results. The MAGIC telescopes collected 75 hr of data during times when the Fermi-LAT flux measured above 1 GeV was below 3 x10(-8)cm(-2) s(-1) , which is the threshold adopted for the definition of a low gamma-ray activity state. The data show a strongly significant (9.50-sigma ) VHE gamma-ray emission at the level of (4.27 +/- 0.61(stat)) x 10(-12) cm(-2) s(-1) above 150 GeV, a factor of 80 lower than the highest flare observed so far from this object. Despite the lower flux, the spectral shape is consistent with earlier detections in the VHE band. The broadband emission is compatible with the external Compton scenario assuming a large emission region located beyond the BLR. For the first time the gamma-ray data allow us to place a limit on the location of the emission region during a low gamma ray state of a FSRQ. For the used model of the BLR, the 95% confidence level on the location of the emission region allows us to place it at a distance >74% of the outer radius of the BLR.

引用

页数：11

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