Fermi Large Area Telescope Search for Photon Lines from 30 to 200 GeV and Dark Matter Implications

被引：177

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
]}

Bouvier, A. ^{[3
,4
]}

Bregeon, J. ^{[7
]}

Brez, A. ^{[7
]}

Brigida, M. ^{[15
,16
,17
]}

Bruel, P. ^{[18
]}

Burnett, T. H. ^{[19
]}

Buson, S. ^{[12
]}

Caliandro, G. A. ^{[20
]}

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

Caraveo, P. A. ^{[21
]}

Carrigan, S. ^{[12
]}

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

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

Celik, Oe. ^{[22
,23
,24
,25
]}

Chekhtman, A. ^{[1
,26
]}

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

Ciprini, S. ^{[14
]}

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

Cohen-Tanugi, J. ^{[27
]}

Conrad, J. ^{[28
,29
]}

Dermer, C. D. ^{[1
]}

de Angelis, A. ^{[30
,31
]}

de Palma, F. ^{[15
,16
,17
]}

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. ^{[32
,33
]}

Edmonds, Y. ^{[3
,4
]}

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

Farnier, C. ^{[27
]}

Favuzzi, C. ^{[15
,16
,17
]}

Fegan, S. J. ^{[18
]}

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

Fortin, P. ^{[18
]}

机构：

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

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

[3] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, 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, CEA Saclay, Serv Astrophys, 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] M Merlin Univ, Dipartimento Fis, I-70126 Bari, Italy

[16] Politecn Bari, I-70126 Bari, Italy

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

[18] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, Palaiseau, France

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

[20] CSIC, IEEC, Inst Ciencies Espai, E-08003 Barcelona, Spain

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

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

[23] CRESST, Greenbelt, MD 20771 USA

[24] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

[25] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

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

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

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

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

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

[31] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[32] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[33] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

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

[35] Sci Data Ctr, ASI, I-00044 Rome, Italy

[36] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

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

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

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

[40] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

[41] ICREA, Barcelona, Spain

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

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

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

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

[46] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan

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

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

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

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

来源：

PHYSICAL REVIEW LETTERS | 2010年 / 104卷 / 09期

基金：

瑞典研究理事会; 美国国家航空航天局;

关键词：

MILKY-WAY HALO; NEUTRALINO ANNIHILATION; OBSERVABILITY; QUARKONIUM; RAYS; MASS;

D O I：

10.1103/PhysRevLett.104.091302

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Dark matter (DM) particle annihilation or decay can produce monochromatic gamma rays readily distinguishable from astrophysical sources. gamma- ray line limits from 30 to 200 GeV obtained from 11 months of Fermi Large Area Space Telescope data from 20-300 GeV are presented using a selection based on requirements for a gamma-ray line analysis, and integrated over most of the sky. We obtain gamma-ray line flux upper limits in the range 0.6-4.5 x 10(-9) cm(-2) s(-1), and give corresponding DM annihilation cross-section and decay lifetime limits. Theoretical implications are briefly discussed.

引用

页数：6

共 37 条

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