A SEARCH FOR A DARK MATTER ANNIHILATION SIGNAL TOWARD THE CANIS MAJOR OVERDENSITY WITH HESS

被引：37

作者：

Aharonian, F. ^{[1
,29
]}

Akhperjanian, A. G. ^{[2
]}

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

Bazer-Bachi, A. R. ^{[4
]}

Behera, B. ^{[5
]}

Benbow, W. ^{[29
]}

Bernloehr, K. ^{[6
,29
]}

Boisson, C. ^{[7
]}

Bochow, V. ^{[29
]}

Borrel, V. ^{[4
]}

Braun, I. ^{[29
]}

Brion, E. ^{[8
]}

Brucker, J. ^{[9
]}

Brun, P. ^{[8
]}

Buehler, R. ^{[29
]}

Bulik, T. ^{[10
]}

Buesching, I. ^{[11
]}

Boutelier, T. ^{[12
]}

Carrigan, S. ^{[29
]}

Chadwick, P. M. ^{[3
]}

Charbonnier, A. ^{[13
]}

Chaves, R. C. G. ^{[29
]}

Cheesebrough, A. ^{[3
]}

Chounet, L. -M. ^{[14
]}

Clapson, A. C. ^{[29
]}

Coignet, G. ^{[15
]}

Costamante, L. ^{[29
]}

Dalton, M. ^{[6
]}

Degrange, B. ^{[14
]}

Deil, C. ^{[29
]}

Dickinson, H. J. ^{[3
]}

Djannati-Atai, A. ^{[16
,28
]}

Domainko, W. ^{[29
]}

Drury, L. O'C. ^{[1
]}

Dubois, F. ^{[15
]}

Dubus, G. ^{[12
]}

Dyks, J. ^{[10
]}

Dyrda, M. ^{[17
]}

Egberts, K. ^{[29
]}

Emmanoulopoulos, D. ^{[5
]}

Espigat, P. ^{[16
]}

Farnier, C. ^{[18
]}

Feinstein, F. ^{[18
]}

Fiasson, A. ^{[18
]}

Foerster, A. ^{[29
]}

Fontaine, G. ^{[14
]}

Fuessling, M. ^{[6
]}

Gabici, S. ^{[1
]}

Gallant, Y. A. ^{[18
]}

Gerard, L. ^{[16
]}

机构：

[1] Dublin Inst Adv Studies, Dublin 2, Ireland

[2] Yerevan Phys Inst, Yerevan 375036, Armenia

[3] Univ Durham, Dept Phys, Durham DH1 3LE, England

[4] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31029 Toulouse 4, France

[5] Heidelberg Univ, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany

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

[7] Univ Paris Diderot, Observ Paris, CNRS, LUTH, F-92190 Meudon, France

[8] CE Saclay, IRFU DSM CEA, F-91191 Gif Sur Yvette, France

[9] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany

[10] Nicolaus Copernicus Astron Ctr, Warsaw, Poland

[11] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

[12] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, F-38041 Grenoble 9, France

[13] Univ Paris 07, Univ Paris 06, CNRS, IN2P3,LPNHE, F-75252 Paris 5, France

[14] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France

[15] CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France

[16] Univ Paris 07, CNRS, APC, F-75205 Paris 13, France

[17] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland

[18] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor Astroparticules, F-34095 Montpellier, France

[19] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

[20] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[21] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[22] Nicholas Copernicus Univ, Torun Ctr Astron, Torun, Poland

[23] Charles Univ Prague, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic

[24] Uniwersytet Jagiellonski, Obserwatorium Astron, Krakow, Poland

[25] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[26] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany

[27] Univ Namibia, Windhoek, Namibia

[28] Univ Paris 07, CEA, Observ Paris, CNRS,UMR 7164, F-75221 Paris 05, France

[29] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 691卷 / 01期

基金：

新加坡国家研究基金会;

关键词：

dark matter; galaxies: dwarf; gamma rays: observations; DWARF GALAXY; GAMMA-RAYS; MILKY-WAY; PROFILES; EVOLUTION; PARTICLE;

D O I：

10.1088/0004-637X/691/1/175

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A search for a dark matter (DM) annihilation signal into gamma-rays toward the direction of the Canis Major (CMa) overdensity is presented. The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A total of 9.6 hr of high-quality data were collected with the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes, and no evidence for a very high energy gamma-ray signal is found. Upper limits on the CMa dwarf galaxy mass of the order of 10(9) M-circle dot are derived at the 95% confidence level (CL) assuming neutralino masses in the range 500 GeV-10 TeV and relatively large annihilation cross sections. Constraints on the velocity-weighted annihilation cross section <sigma upsilon > are calculated for specific weakly interacting massive-particle scenarios, using a Navarro-Frenk-White model for the DM halo profile and taking advantage of numerical simulations of hierarchical structure formation. Assuming a total halo mass of 3 x 10(8) M-circle dot, 95% CL exclusion limits of the order of 5 x 10(-24) cm(3) s(-1) are reached in the 500 GeV-10 TeV DM particle mass interval.

引用

页码：175 / 181

页数：7

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