MAGIC search for VHE γ-ray emission from AE Aquarii in a multiwavelength context

被引：8

作者：

Aleksie, J. ^{[1
]}

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

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

Antoranz, P. ^{[5
,6
]}

Babie, A. ^{[7
,8
]}

Bangale, P. ^{[9
]}

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

Becerra Gonzalez, J. ^{[11
]}

Bedriarek, W. ^{[12
]}

Bernardini, E. ^{[13
]}

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

Biland, A. ^{[14
]}

Blanch, O. ^{[1
]}

Bonnefoy, S. ^{[10
]}

Bonnoli, G. ^{[4
]}

Borracci, E. ^{[9
]}

Bretz, T. ^{[15
]}

Carmona, E. ^{[16
]}

Carosi, A. ^{[4
]}

Colin, P. ^{[9
]}

Colombo, E. ^{[11
]}

Contreras, J. L. ^{[10
]}

Cortina, J. ^{[1
]}

Covino, S. ^{[4
]}

Da Vela, P. ^{[5
,6
]}

Dazzio, F. ^{[9
]}

De Angelis, A. ^{[2
,3
]}

De Caneva, G. ^{[13
]}

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

Wilhelmi, E. de Ona ^{[17
]}

Delgado Mendez, C. ^{[16
]}

Doert, M. ^{[18
]}

Presters, D. Dominis ^{[7
,8
]}

Dorner, D. ^{[15
]}

Doro, M. ^{[19
,20
]}

Einecke, S. ^{[18
]}

Eisenacher, D. ^{[15
]}

Elsaesser, D. ^{[15
]}

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

Font, L. ^{[21
,22
]}

Frantzen, K. ^{[18
]}

Fruck, C. ^{[9
]}

Galindo, D.

Garcia Lopez, R. J. ^{[11
]}

Garczarczyk, M. ^{[13
]}

Terrats, D. Garrido ^{[21
,22
]}

Gaug, M. ^{[21
,22
]}

Godinovie, N. ^{[7
,8
]}

Gonzalez Munoz, A. ^{[1
]}

Gozzini, S. R. ^{[13
]}

机构：

[1] IFAE, Bellaterra 08193, Spain

[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 Siena, I-53100 Siena, Italy

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

[7] Univ Rijeka, Croatian MAG Consortium, Rudjer Boskov Inst, Zagreb 10000, Croatia

[8] Univ Split, Zagreb 10000, Croatia

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

[10] Univ Complutense, E-28040 Madrid, Spain

[11] Inst Astrofis Canarias, Tenerife 38200, Spain

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

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

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

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

[16] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain

[17] Inst Space Sci, Barcelona 08193, Spain

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

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

[20] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[21] Univ Autonoma Barcelona, Unitat Fis Radiac, Dept Fis, Bellaterra 08193, Spain

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

[23] Kyoto Univ, Div Phys & Astron, Japanese MAG Consortium, Kyoto 6068501, Japan

[24] Univ Turku, Finnish MAG Consortium, Tuorla Observ, Oulu 900147, Finland

[25] Univ Oulu, Dept Phys, Oulu 900147, Finland

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

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

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

[29] ICREA, Barcelona 08193, Spain

[30] Inst Space Sci, Barcelona 08193, Spain

[31] Univ Insubria, I-22100 Como, Italy

[32] INFN Milano Bicocca, I-22100 Como, Italy

[33] INAF Trieste, I-34131 Trieste, Italy

[34] Astron Observ Belgrade, Belgrade 11060, Serbia

[35] Sultan Qaboos Univ, Coll Sci, Dept Phys, PC-123 Muscat, Oman

[36] Lawrence Livermore Natl Lab, Livermore, CA 95125 USA

[37] Univ Crete, Dept Phys, Iraklion 71003, Greece

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

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 568卷

关键词：

accretion; accretion disks; radiation mechanisms: non-thermal; novae; cataclysmic variables; gamma rays: stars; MAGNETIZED WHITE-DWARF; PULSATIONS; TELESCOPE; DISCOVERY; PROPELLER; FLARES; STARS; BURST; AQR;

D O I：

10.1051/0004-6361/201424072

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. It has been claimed that the nova-like cataclysmic variable AE Aquarii (AE Aqr) is a very-high-energy (VHE, E > 100 GeV) source both on observational and theoretical grounds. Aims. We search for VHE gamma-ray emission from AE Aqr during different states of the source at several wavelengths to confirm or rule out previous claims of detection of gamma-ray emission from this object. Methods. We report on observations of AE Aqr performed by MAGIC. The source was observed during 12 h as part of a multiwavelength campaign carried out between May and June 2012 covering the optical, X-ray, and gamma-ray ranges. Besides MAGIC, the other facilities involved were the KVA, Skinakas, and Vidojevica telescopes in the optical and Swift in X-rays. We calculated integral upper limits coincident with different states of the source in the optical. We computed upper limits to the pulsed emission limiting the signal region to 30% of the phaseogram and we also searched for pulsed emission at different frequencies applying the Rayleigh test. Results. AE Aqr was not detected at VHEs during the multiwavelength campaign. We establish integral upper limits at the 95% confidence level for the steady emission assuming the differential flux proportional to a power-law function d phi/dE proportional to E-r, with a Crab-like photon spectral index of Gamma = 2.6. The upper limit above 200 GeV is 6.4 x 10(-12) cm(-2) s(-1) and above 1 TeV is 7.4 x 10(-13) cm(-2) s(-1). We obtained an upper limit for the pulsed emission of 2.6 x 10(-12) cm(-2) s(-1) for energies above 200 GeV. Applying the Rayleigh test for pulsed emission at different frequencies we did not find any significant signal. Conclusions. Our results indicate that AE Aqr is not a VHE gamma-ray emitter at the level of emission previously claimed. We have established the most constraining upper limits for the VHE gamma-ray emission of AE Aqr.

引用

页数：8

共 46 条

[31] The white dwarf in AE Aqr brakes harder [J].