Optimized dark matter searches in deep observations of Segue 1 with MAGIC

被引：119

作者：

Aleksic, J. ^{[1
]}

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

Antonelli, L. A. ^{[9
]}

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

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

Bangale, P. ^{[9
]}

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

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

Becerra Gonzalez, J. ^{[11
]}

Bednarek, W. ^{[12
]}

Berger, K. ^{[11
]}

Bernardini, E. ^{[13
]}

Biland, A. ^{[14
]}

Blanch, O. ^{[1
]}

Bock, R. K. ^{[9
]}

Bonnefoy, S. ^{[10
]}

Bonnoli, G. ^{[4
]}

Borracci, F. ^{[9
]}

Bretz, T. ^{[15
]}

Carmona, E. ^{[16
]}

Carosi, A. ^{[4
]}

Fidalgo, D. Carreto ^{[15
]}

Colin, P. ^{[9
]}

Colombo, E. ^{[11
]}

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

Cortina, J. ^{[1
]}

Covino, S. ^{[4
]}

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

Dazzi, F. ^{[9
]}

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

De Caneva, G. ^{[13
]}

De Lotto, B. ^{[17
]}

Delgado Mendez, C. ^{[16
]}

Doert, M. ^{[17
]}

Dominguez, A. ^{[18
]}

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

Dorner, D. ^{[15
]}

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

Einecke, S. ^{[17
]}

Eisenacher, D. ^{[15
]}

Elsaesser, D. ^{[15
]}

Farina, E. ^{[21
]}

Ferenc, D. ^{[7
,8
]}

Fonseca, M. V. ^{[5
,6
]}

Font, L. ^{[22
,23
]}

Frantzen, K. ^{[17
]}

Fruck, C. ^{[9
]}

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

Garczarczyk, M. ^{[13
]}

Garrido Terrats, D. ^{[22
,23
]}

机构：

[1] IFAE, E-08193 Bellaterra, 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, Rudjer Boskov Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia

[8] Univ Split, HR-10000 Zagreb, Croatia

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

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

[11] Inst Astrofis Canarias, E-38200 Tenerife, Spain

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

[13] DESY, D-15738 Zeuthen, Germany

[14] ETH, CH-8093 Zurich, Switzerland

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

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

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

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

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

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

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

[22] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, E-08193 Bellaterra, Spain

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

[24] CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Spain

[25] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan

[26] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland

[27] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland

[28] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria

[29] Univ Barcelona, ICC, IEEC, E-08028 Barcelona, Spain

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

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

[32] INAF Trieste, Trieste, Italy

[33] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

[34] Tech Univ Munich, D-85748 Garching, Germany

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2014年 / 02期

基金：

芬兰科学院;

关键词：

dark matter experiments; gamma ray experiments; dwarfs galaxies; GAMMA-RAY EMISSION; GALAXY; LIMITS; CONSTRAINTS; SIGNALS;

D O I：

10.1088/1475-7516/2014/02/008

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a similar to 500 GeV dark matter particle annihilating into tau(+)tau(-), and is of order <sigma(ann)v > similar or equal to 1.2x10(-24) cm(3) s(-1) - a factor similar to 40 above the <sigma(ann)v > similar or equal to thermal value.

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页数：36

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