THE FERMI-LAT HIGH-LATITUDE SURVEY: SOURCE COUNT DISTRIBUTIONS AND THE ORIGIN OF THE EXTRAGALACTIC DIFFUSE BACKGROUND

被引：170

作者：

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

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

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

Antolini, E. ^{[5
,6
]}

Baldini, L. ^{[7
]}

Ballet, J. ^{[8
]}

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

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

Baughman, B. M. ^{[13
]}

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

Bellazzini, R. ^{[7
]}

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

Blandford, R. D. ^{[3
,4
]}

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

Bonamente, E. ^{[5
,6
]}

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

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

Bregeon, J. ^{[7
]}

Brez, A. ^{[7
]}

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

Bruel, P. ^{[16
]}

Burnett, T. H. ^{[17
]}

Buson, S. ^{[11
]}

Caliandro, G. A. ^{[18
]}

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

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

Carrigan, S. ^{[12
]}

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

Cavazzuti, E. ^{[20
]}

Cecchi, C. ^{[5
,6
]}

Celik, Oe ^{[21
,22
,23
,24
]}

Charles, E. ^{[3
,4
]}

Chekhtman, A. ^{[1
,25
]}

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

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

Ciprini, S. ^{[6
]}

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

Cohen-Tanugi, J. ^{[26
]}

Conrad, J. ^{[27
,28
]}

Costamante, L. ^{[3
,4
]}

Cutini, S. ^{[20
]}

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

de Angelis, A. ^{[29
,30
]}

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

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

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

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

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

Farnier, C. ^{[26
]}

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

机构：

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

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

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

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

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

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

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

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

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

[10] Univ Trieste, Dipartimento 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] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle 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 IN2P3, Lab Leprince Ringuet, Palaiseau, France

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

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

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

[20] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy

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

[22] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA

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

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

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

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

[27] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden

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

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

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

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

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

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

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

[35] ICREA, Barcelona, Spain

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 720卷 / 01期

关键词：

cosmology: observations; diffuse radiation; galaxies: active; galaxies: jets; gamma rays: diffuse background; surveys; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; N-LOG S; LUMINOSITY FUNCTION; SPACE-TELESCOPE; DARK-MATTER; COSMIC-RAYS; BLAZARS; GALAXIES;

D O I：

10.1088/0004-637X/720/1/435

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This is the first of a series of papers aimed at characterizing the populations detected in the high-latitude sky of the Fermi-LAT survey. In this work, we focus on the intrinsic spectral and flux properties of the source sample. We show that when selection effects are properly taken into account, Fermi sources are on average steeper than previously found (e.g., in the bright source list) with an average photon index of 2.40 +/- 0.02 over the entire 0.1-100 GeV energy band. We confirm that flat spectrum radio quasars have steeper spectra than BL Lacertae objects with an average index of 2.48 +/- 0.02 versus 2.18 +/- 0.02. Using several methods, we build the deepest source count distribution at GeV energies, deriving that the intrinsic source (i.e., blazar) surface density at F-100 >= 10(-9) ph cm(2) s(-1) is 0.12(-0.02)(+0.03) deg(-2). The integration of the source count distribution yields that point sources contribute 16(+/- 1.8)% (+/- 7% systematic uncertainty) of the GeV isotropic diffuse background. At the fluxes currently reached by LAT, we can rule out the hypothesis that pointlike sources (i.e., blazars) produce a larger fraction of the diffuse emission.

引用

页码：435 / 453

页数：19

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