Constraints on particle acceleration in SS433/W50 from MAGIC and HESS observations

被引：18

作者：

Ahnen, M. L. ^{[1
]}

Ansoldi, S. ^{[2
,3
,29
]}

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

Arcaro, C. ^{[5
,6
]}

Babie, A. ^{[7
]}

Banerjee, B. ^{[8
]}

Bangale, P. ^{[9
]}

de Almeida, U. Barres ^{[2
,3
,9
,30
]}

Barrio, J. A. ^{[10
]}

Gonzalez, J. Becerra ^{[11
,12
,31
]}

Bednarek, W. ^{[13
]}

Bernardini, E. ^{[14
,32
]}

Berti, A. ^{[2
,3
,33
]}

Biasuzzi, B. ^{[2
,3
]}

Biland, A. ^{[1
]}

Blanch, O. ^{[15
]}

Bonnefoy, S. ^{[10
]}

Bonnoli, G. ^{[16
,17
]}

Borracci, F. ^{[9
]}

Carosi, R. ^{[16
,17
]}

Carosi, A. ^{[4
]}

Chatterjee, A. ^{[8
]}

Colin, P.

Colombo, E. ^{[9
]}

Contreras, J. L. ^{[11
,12
]}

Cortina, J. ^{[10
]}

Covino, S. ^{[15
]}

Cumani, P. ^{[4
]}

Da Vela, P. ^{[16
,17
]}

Dazzi, F. ^{[4
]}

De Angelis, A. ^{[5
,6
,7
]}

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

Wilhelmi, E. de Ona ^{[18
]}

Di Pierro, F. ^{[4
]}

Doert, M. ^{[19
]}

Dominguez, A. ^{[10
]}

Prester, D. Dominis ^{[7
]}

Dorner, D. ^{[20
,21
]}

Doro, M. ^{[5
,6
]}

Einecke, S. ^{[19
]}

Glawion, D. Eisenacher ^{[20
,21
]}

Elsaesser, D. ^{[19
]}

Engelkemeier, M. ^{[19
]}

Ramazani, V. Fallah ^{[22
]}

Fernandez-Barra, A. ^{[15
]}

Fidalgo, D. ^{[10
]}

Fonseca, M. V. ^{[10
]}

Font, L. ^{[23
]}

Fruck, C. ^{[9
]}

Galindo, D. ^{[24
]}

机构：

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

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

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

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

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

[6] INFN, I-35131 Padua, Italy

[7] Univ Osijek, Univ Zagreb FER, Univ Split FESB, Croatian MAGIC Consortium,Rudjer Boskov Inst Univ, Zagreb 10000, Croatia

[8] Saha Inst Nucl Phys, 1-AF Bidhannagar, Kolkata 700064, India

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

[10] Univ Complutense, Madrid 28040, Spain

[11] Inst Astrofis Canarias, San Cristobal la Laguna 38200, Spain

[12] Univ La Laguna, Dpto Astrofis, Tenerife, Spain

[13] Univ Lodz, PL-90236 Lodz, Poland

[14] Deutsch Elektr Synchrotron DESY, D-15738 Zeuthen, Germany

[15] Barcelona Inst Sci & Technol, IFAE, Campus UAB, Bellaterra 08193, Spain

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

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

[18] Inst Space Sci CSIC IEEC, Barcelona 08193, Spain

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

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

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

[22] Univ Oulu, Astron Div, Oulu 90014, Finland

[23] Univ Autenoma Barcelona, Unitat Fis Radiat, Dept Fis, Bellaterra 08193, Spain

[24] Univ Barcelona, IEEC UB, ICC, Barcelona 08028, Spain

[25] Univ Tokyo, ICRR, Japanese MAGIC Consortium, Dept Phys, Tokushima 7708501, Japan

[26] Univ Tokushima, Tokai Univ, Kyoto Univ, Hakubi Ctr, Tokushima 7708501, Japan

[27] Inst Nucl Energy Res, Sofia 1784, Bulgaria

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

[29] INFN Pisa, I-56126 Pisa, Italy

[30] ICREA & Inst Space Sci CSIC IEEC, Barcelona 08193, Spain

[31] Kyoto Univ, Dept Phys, Kyoto 6068501, Japan

[32] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[33] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[34] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[35] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany

[36] Univ Trieste, Trieste, Italy

[37] FINCA, Turku, Finland

[38] Univ Bologna, INAF Trieste, I-40126 Bologna, Italy

[39] Univ Bologna, Dept Phys & Astron, I-40126 Bologna, Italy

[40] CEA Saclay, WuServ Astrophys, Univ Paris Diderot, Lab AIM,UMR 7158 CEA DSM CNRS, F-91191 Gif Sur Yvette, France

[41] INAF IAPS Roma, I-00133 Rome, Italy

[42] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa

[43] Univ Hamburg, Inst Experimentalphys, D-22761 Hamburg, Germany

[44] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany

[45] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[46] Natl Acad Sci Republ Armenia, Marshall Baghramian Ave 24, Yerevan 0019, Armenia

[47] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia

[48] Humboldt Univ, Inst Phys, Newtonstr. 15, D-12489 Berlin, Germany

[49] Univ Namibia, Dept Phys, 13301 Private Bag, Windhoek, Namibia

[50] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 612卷

基金：

英国科学技术设施理事会; 新加坡国家研究基金会;

关键词：

gamma rays: general; stars: black holes; X-rays: binaries; ISM: jets and outflows; X-RAY-SPECTRUM; GAMMA-RAYS; GALACTIC PLANE; CRAB-NEBULA; SS; 433; JETS; EMISSION; SS-433; MICROQUASARS; SYSTEM;

D O I：

10.1051/0004-6361/201731169

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system. Aims. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (P-orb similar to 13.1 days) and precession of the circumstellar disk (P-pre similar to 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations. Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to similar to 40-80 h, depending on the region, was employed. Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be less than or similar to 10(-12)-10(-13) TeV-1 cm(-2) s(-1) in an energy interval ranging from similar to few x 100 GeV to similar to few TeV. Integral flux limits down to similar to 10(-12)-10(-13) ph cm(-2) s(-1) and similar to 10(-13)-10(-14) ph cm(-2) s(-1) are obtained at 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jet regions and on the physics of the jet/medium interactions. Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, q(p) <= 2.5 x 10(-5), to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields greater than or similar to 10 mu G is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with E-e up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.

引用

页数：8

共 34 条

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