Resolving the Extragalactic γ-Ray Background above 50 GeV with the Fermi Large Area Telescope

被引：141

作者：

Ackermann, M. ^{[1
]}

Ajello, M. ^{[2
]}

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

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

Baldini, L. ^{[3
,4
,7
,8
]}

Ballet, J. ^{[9
]}

Barbiellini, G. ^{[10
,11
]}

Bastieri, D. ^{[12
,13
]}

Bechtol, K. ^{[14
,15
]}

Bellazzini, R. ^{[16
]}

Bissaldi, E. ^{[17
]}

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

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

Bonino, R. ^{[18
,19
]}

Bregeon, J. ^{[20
]}

Britto, R. J. ^{[21
]}

Bruel, P. ^{[22
]}

Buehler, R. ^{[1
]}

Caliandro, G. A. ^{[3
,4
,23
]}

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

Caragiulo, M. ^{[17
,24
,25
]}

Caraveo, P. A. ^{[26
]}

Cavazzuti, E. ^{[27
]}

Cecchi, C. ^{[28
,29
]}

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

Chekhtman, A. ^{[30
,31
]}

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

Chiaro, G. ^{[13
]}

Ciprini, S. ^{[27
,28
]}

Cohen-Tanugi, J. ^{[20
]}

Cominsky, L. R. ^{[32
]}

Costanza, F. ^{[17
]}

Cutini, S. ^{[27
,28
,33
]}

D'Ammando, F. ^{[34
,35
]}

de Angelis, A. ^{[36
,37
]}

de Palma, F. ^{[17
,38
]}

Desiante, R. ^{[18
,39
]}

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

Di Mauro, M. ^{[3
,4
]}

Di Venere, L. ^{[17
,24
,25
]}

Dominguez, A. ^{[2
]}

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

Favuzzi, C. ^{[17
,24
,25
]}

Fegan, S. J. ^{[22
]}

Ferrara, E. C. ^{[40
]}

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

Fukazawa, Y. ^{[41
]}

Funk, S. ^{[42
]}

Fusco, P. ^{[17
,24
,25
]}

Gargano, F. ^{[17
]}

机构：

[1] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[2] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA

[3] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, 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] Univ Pisa, I-56127 Pisa, Italy

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

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

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

[11] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

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

[13] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[14] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA

[15] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA

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

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

[18] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[19] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy

[20] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34059 Montpellier, France

[21] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa

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

[23] CIFS, I-10133 Turin, Italy

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

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

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

[27] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy

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

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

[30] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA

[31] Naval Res Lab, Washington, DC 20375 USA

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

[33] INAF Osservatorio Astron Roma, I-00040 Rome, Italy

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

[35] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

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

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

[38] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy

[39] Univ Udine, I-33100 Udine, Italy

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

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

[42] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

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

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

[45] NASA, Postdoctoral Program, New York, NY USA

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

[47] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland

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

[49] Leopold Franzens Univ Innsbruck, Inst Theoret Physik, A-6020 Innsbruck, Austria

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

来源：

PHYSICAL REVIEW LETTERS | 2016年 / 116卷 / 15期

关键词：

X-RAY; STATISTICS; EMISSION; SPECTRUM; BLAZARS; ORIGIN; HOLE;

D O I：

10.1103/PhysRevLett.116.151105

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The Fermi Large Area Telescope (LAT) Collaboration has recently released a catalog of 360 sources detected above 50 GeV (2FHL). This catalog was obtained using 80 months of data re-processed with Pass 8, the newest event-level analysis, which significantly improves the acceptance and angular resolution of the instrument. Most of the 2FHL sources at high Galactic latitude are blazars. Using detailed Monte Carlo simulations, we measure, for the first time, the source count distribution, dN= dS, of extragalactic.-ray sources at E > 50 GeV and find that it is compatible with a Euclidean distribution down to the lowest measured source flux in the 2FHL (8 x 10(-12) ph cm(-2) s(-1)). We employ a one-point photon fluctuation analysis to constrain the behavior of dN= dS below the source detection threshold. Overall, the source count distribution is constrained over three decades in flux and found compatible with a broken power law with a break flux, Sb, in the range [8 x 10-12; 1.5 x 10-11] ph cm(-2) s(-1) and power-law indices below and above the break of a 2. [1.60; 1.75] and a 1 +/- 2.49 +/- 0.12, respectively. Integration of dN= dS shows that point sources account for at least 86_16 -14 % of the total extragalactic gamma-ray background. The simple form of the derived source count distribution is consistent with a single population (i. e., blazars) dominating the source counts to the minimum flux explored by this analysis. We estimate the density of sources detectable in blind surveys that will be performed in the coming years by the Cherenkov Telescope Array.

引用

页数：8

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