OBSERVATIONS OF MILKY WAY DWARF SPHEROIDAL GALAXIES WITH THE FERMI-LARGE AREA TELESCOPE DETECTOR AND CONSTRAINTS ON DARK MATTER MODELS

被引：259

作者：

Abdo, A. A. ^{[1
,2
]}

Ackermann, M. ^{[3
,4
]}

Ajello, M. ^{[3
,4
]}

Atwood, W. B. ^{[5
,6
]}

Baldini, L. ^{[7
]}

Ballet, J. ^{[8
]}

Barbiellini, G. ^{[9
,10
]}

Bastieri, D. ^{[11
,12
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[7
]}

Berenji, B. ^{[3
,4
]}

Bloom, E. D. ^{[3
,4
]}

Bonamente, E. ^{[13
,14
]}

Borgland, A. W. ^{[3
,4
]}

Bregeon, J. ^{[7
]}

Brez, A. ^{[7
]}

Brigida, M. ^{[15
,16
]}

Bruel, P. ^{[17
]}

Burnett, T. H. ^{[18
]}

Buson, S. ^{[12
]}

Caliandro, G. A. ^{[15
,16
]}

Cameron, R. A. ^{[3
,4
]}

Caraveo, P. A. ^{[19
]}

Casandjian, J. M. ^{[8
]}

Cecchi, C. ^{[13
,14
]}

Chekhtman, A. ^{[1
,20
]}

Cheung, C. C. ^{[1
,2
,38
]}

Chiang, J. ^{[3
,4
]}

Ciprini, S. ^{[13
,14
]}

Claus, R. ^{[3
,4
]}

Cohen-Tanugi, J. ^{[21
]}

Conrad, J. ^{[22
,23
]}

de Angelis, A. ^{[24
,25
]}

de Palma, F. ^{[15
,16
]}

Digel, S. W. ^{[3
,4
]}

do Couto e Silva, E. ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Drlica-Wagner, A. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Dumora, D. ^{[26
,27
]}

Farnier, C. ^{[21
]}

Favuzzi, C. ^{[15
,16
]}

Fegan, S. J. ^{[17
]}

Focke, W. B. ^{[3
,4
]}

Fortin, P. ^{[17
]}

Frailis, M. ^{[24
,25
]}

Fukazawa, Y. ^{[28
]}

Fusco, P. ^{[15
,16
]}

Gargano, F. ^{[16
]}

Gehrels, N. ^{[29
,38
]}

机构：

[1] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

[2] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA

[3] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[5] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[7] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[8] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France

[9] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[10] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[11] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[12] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[13] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[14] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[15] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[16] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

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

[18] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[19] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy

[20] George Mason Univ, Fairfax, VA 22030 USA

[21] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France

[22] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[23] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[24] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[25] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy

[26] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[27] CNRS, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, IN2P3, F-33175 Gradignan, France

[28] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[29] Univ Maryland, College Pk, MD 20742 USA

[30] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[31] Univ Alabama, Huntsville, AL 35899 USA

[32] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[33] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden

[34] UCO, Lick Observ, Santa Cruz, CA 95064 USA

[35] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan

[36] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan

[37] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

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

[39] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[40] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

[41] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[42] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[43] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

[44] CSIC, IEEC, Inst Ciencias Espai, Barcelona 08193, Spain

[45] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA

[46] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA

[47] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA

[48] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[49] ICREA, Barcelona, Spain

[50] CIFS, I-10133 Turin, Italy

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 712卷 / 01期

基金：

瑞典研究理事会; 美国国家科学基金会;

关键词：

dark matter; galaxies: dwarf; gamma rays: galaxies; VELOCITY DISPERSION PROFILES; EXPLORING HALO SUBSTRUCTURE; GAMMA-RAY EMISSION; LOCAL GROUP; SUPERSYMMETRY-BREAKING; LIKELIHOOD ANALYSIS; GIANT STARS; URSA-MINOR; SEGUE; SATELLITE;

D O I：

10.1088/0004-637X/712/1/147

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the observations of 14 dwarf spheroidal galaxies (dSphs) with the Fermi Gamma-Ray Space Telescope taken during the first 11 months of survey mode operations. The Fermi telescope, which is conducting an all-sky gamma-ray survey in the 20 MeV to > 300 GeV energy range, provides a new opportunity to test particle dark matter models through the expected gamma-ray emission produced by pair annihilation of weakly interacting massive particles (WIMPs). Local Group dSphs, the largest galactic substructures predicted by the cold dark matter scenario, are attractive targets for such indirect searches for dark matter because they are nearby and among the most extreme dark matter dominated environments. No significant gamma-ray emission was detected above 100 MeV from the candidate dwarf galaxies. We determine upper limits to the gamma-ray flux assuming both power-law spectra and representative spectra from WIMP annihilation. The resulting integral flux above 100 MeV is constrained to be at a level below around 10(-9) photons cm(-2) s(-1). Using recent stellar kinematic data, the gamma-ray flux limits are combined with improved determinations of the dark matter density profile in eight of the 14 candidate dwarfs to place limits on the pair-annihilation cross section of WIMPs in several widely studied extensions of the standard model, including its supersymmetric extension and other models that received recent attention. With the present data, we are able to rule out large parts of the parameter space where the thermal relic density is below the observed cosmological dark matter density and WIMPs (neutralinos here) are dominantly produced non-thermally, e. g., in models where supersymmetry breaking occurs via anomaly mediation. The gamma-ray limits presented here also constrain some WIMP models proposed to explain the Fermi and PAMELA e(+)e(-) data, including low-mass wino-like neutralinos and models with TeV masses pair annihilating into muon-antimuon pairs.

引用

页码：147 / 158

页数：12

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