GeV GAMMA-RAY FLUX UPPER LIMITS FROM CLUSTERS OF GALAXIES

被引：136

作者：

Ackermann, M. ^{[1
,2
]}

Ajello, M. ^{[1
,2
]}

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

Baldini, L. ^{[3
]}

Ballet, J. ^{[4
]}

Barbiellini, G. ^{[5
,6
]}

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

Bechtol, K. ^{[1
,2
]}

Bellazzini, R. ^{[3
]}

Blandford, R. D. ^{[1
,2
]}

Blasi, P. ^{[9
]}

Bloom, E. D. ^{[1
,2
]}

Bonamente, E. ^{[10
,11
]}

Borgland, A. W. ^{[1
,2
]}

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

Brandt, T. J. ^{[12
,13
]}

Bregeon, J. ^{[3
]}

Brigida, M. ^{[14
,15
]}

Bruel, P. ^{[16
]}

Buehler, R. ^{[1
,2
]}

Buson, S. ^{[7
,8
]}

Caliandro, G. A. ^{[17
]}

Cameron, R. A. ^{[1
,2
]}

Caraveo, P. A. ^{[18
]}

Carrigan, S. ^{[8
]}

Casandjian, J. M. ^{[4
]}

Cavazzuti, E. ^{[19
]}

Cecchi, C. ^{[10
,11
]}

Celik, Oe ^{[20
,21
,22
,23
]}

Charles, E. ^{[1
,2
]}

Chekhtman, A. ^{[24
,25
]}

Cheung, C. C. ^{[24
,26
]}

Chiang, J. ^{[1
,2
]}

Ciprini, S. ^{[11
]}

Claus, R. ^{[1
,2
]}

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

Colafrancesco, S. ^{[19
]}

Cominsky, L. R. ^{[28
]}

Conrad, J. ^{[29
,30
]}

Dermer, C. D. ^{[24
]}

de Palma, F. ^{[14
,15
]}

Silva, E. do Couto e ^{[1
,2
]}

Drell, P. S. ^{[1
,2
]}

Dubois, R. ^{[1
,2
]}

Dumora, D. ^{[31
,32
]}

Edmonds, Y. ^{[1
,2
]}

Farnier, C. ^{[27
]}

Favuzzi, C. ^{[14
,15
]}

Frailis, M. ^{[33
,34
,35
]}

Fukazawa, Y. ^{[36
]}

机构：

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

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

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

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

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

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

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

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

[9] Osserv Astrofis Arcetri, I-50125 Florence, Italy

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

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

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

[13] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA

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

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

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

[17] IEEC CSIC, Inst Ciencies Espai, Barcelona 08193, Spain

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

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

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

[21] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

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

[28] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA

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

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

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

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

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

[34] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, Udine, Italy

[35] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy

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

[37] INAF, Ist Radioastron, I-40129 Bologna, Italy

[38] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

[39] ICREA, Barcelona, Spain

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

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

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

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

[44] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

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

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

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

[48] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

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

[50] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 717卷 / 01期

基金：

美国国家航空航天局; 瑞典研究理事会;

关键词：

cosmic rays; galaxies: clusters: general; gamma rays: galaxies: clusters; radiation mechanisms: non-thermal; LARGE-AREA TELESCOPE; DIFFUSE RADIO-EMISSION; X-RAY; NONTHERMAL EMISSION; RELIC CANDIDATES; COMA CLUSTER; COSMIC-RAYS; SEARCH; HALO; DISCOVERY;

D O I：

10.1088/2041-8205/717/1/L71

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The detection of diffuse radio emission associated with clusters of galaxies indicates populations of relativistic leptons infusing the intracluster medium (ICM). Those electrons and positrons are either injected into and accelerated directly in the ICM, or produced as secondary pairs by cosmic-ray ions scattering on ambient protons. Radiation mechanisms involving the energetic leptons together with the decay of neutral pions produced by hadronic interactions have the potential to produce abundant GeV photons. Here, we report on the search for GeV emission from clusters of galaxies using data collected by the Large Area Telescope on the Fermi Gamma-ray Space Telescope from 2008 August to 2010 February. Thirty-three galaxy clusters have been selected according to their proximity and high mass, X-ray flux and temperature, and indications of non-thermal activity for this study. We report upper limits on the photon flux in the range 0.2-100 GeV toward a sample of observed clusters (typical values (1-5) x 10(-9) photon cm(-2) s(-1)) considering both point-like and spatially resolved models for the high-energy emission and discuss how these results constrain the characteristics of energetic leptons and hadrons, and magnetic fields in the ICM. The volume-averaged relativistic-hadron-to-thermal energy density ratio is found to be <5%-10% in several clusters.

引用

页码：L71 / L78

页数：8

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