THE SPECTRUM OF ISOTROPIC DIFFUSE GAMMA-RAY EMISSION BETWEEN 100 MeV AND 820 GeV

被引：506

作者：

Ackermann, M. ^{[1
]}

Ajello, M. ^{[2
]}

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

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

Baldini, L. ^{[7
]}

Ballet, J. ^{[8
]}

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

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

Bechtol, K. ^{[13
]}

Bellazzini, R. ^{[7
]}

Bissaldi, E. ^{[14
,15
]}

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

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

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

Brandt, T. J. ^{[16
]}

Bregeon, J. ^{[17
]}

Bruel, P. ^{[18
]}

Buehler, R. ^{[1
]}

Buson, S. ^{[11
,12
]}

Caliandro, G. A. ^{[3
,4
,19
]}

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

Caragiulo, M. ^{[20
]}

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

Cavazzuti, E. ^{[22
]}

Cecchi, C. ^{[23
,24
]}

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

Chekhtman, A. ^{[25
]}

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

Chiaro, G. ^{[12
]}

Ciprini, S. ^{[22
,26
]}

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

Cohen-Tanugi, J. ^{[17
]}

Conrad, J. ^{[27
,28
,29
]}

Cuoco, A. ^{[28
,30
,31
]}

Cutini, S. ^{[22
,26
]}

D'Ammando, F. ^{[32
,33
]}

de Angelis, A. ^{[34
,35
]}

de Palma, F. ^{[20
,36
]}

Dermer, C. D. ^{[37
]}

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

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

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

Favuzzi, C. ^{[20
,38
]}

Ferrara, E. C. ^{[16
]}

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

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

Fukazawa, Y. ^{[39
]}

Funk, S. ^{[3
,4
]}

Fusco, P. ^{[20
,38
]}

Gargano, F. ^{[20
]}

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, 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, 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, Dipartimento Fis, I-34127 Trieste, Italy

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

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

[13] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

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

[15] Univ Trieste, I-34127 Trieste, Italy

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

[17] Univ Montpellier 2, Lab Universe & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier, France

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

[19] CIFS, I-10133 Turin, Italy

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

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

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

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

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

[25] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA

[26] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy

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

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

[29] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden

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

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

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

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

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

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

[36] Univ Telemat Pegaso, I-80132 Naples, Italy

[37] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA

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

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

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

[41] Pontificia Univ Catolica Chile, Dept Fis, Santiago, Chile

[42] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium

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

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

[45] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan

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

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

[48] CRESST, Greenbelt, MD 20771 USA

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

[50] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 799卷 / 01期

基金：

美国国家科学基金会;

关键词：

diffuse radiation; gamma rays: diffuse background; LARGE-AREA TELESCOPE; STAR-FORMING GALAXIES; X-RAY; BACKGROUND-RADIATION; FERMI OBSERVATIONS; DARK-MATTER; PROPAGATION; NEUTRINOS; CATALOG; HALOS;

D O I：

10.1088/0004-637X/799/1/86

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The gamma-ray sky can be decomposed into individually detected sources, diffuse emission attributed to the interactions of Galactic cosmic rays with gas and radiation fields, and a residual all-sky emission component commonly called the isotropic diffuse gamma-ray background (IGRB). The IGRB comprises all extragalactic emissions too faint or too diffuse to be resolved in a given survey, as well as any residual Galactic foregrounds that are approximately isotropic. The first IGRB measurement with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi) used 10 months of sky-survey data and considered an energy range between 200 MeV and 100 GeV. Improvements in event selection and characterization of cosmic-ray backgrounds, better understanding of the diffuse Galactic emission (DGE), and a longer data accumulation of 50 months allow for a refinement and extension of the IGRB measurement with the LAT, now covering the energy range from 100 MeV to 820 GeV. The IGRB spectrum shows a significant high-energy cutoff feature and can be well described over nearly four decades in energy by a power law with exponential cutoff having a spectral index of 2.32 +/- 0.02 and a break energy of (279 +/- 52) GeV using our baseline DGE model. The total intensity attributed to the IGRB is (7.2 +/- 0.6) x 10(-6) cm(-2) s(-1) sr(-1) above 100 MeV, with an additional +15%/-30% systematic uncertainty due to the Galactic diffuse foregrounds.

引用

页数：24

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