FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG

被引：1199

作者：

Acero, F. ^{[1
]}

Ackermann, M. ^{[2
]}

Ajello, M. ^{[3
]}

Albert, A. ^{[4
,5
]}

Atwood, W. B. ^{[6
,7
]}

Axelsson, M. ^{[8
,9
,10
]}

Baldini, L. ^{[11
,12
]}

Ballet, J. ^{[1
]}

Barbiellini, G. ^{[13
,14
]}

Bastieri, D. ^{[15
,16
]}

Belfiore, A. ^{[17
]}

Bellazzini, R. ^{[12
]}

Bissaldi, E. ^{[18
]}

Blandford, R. D. ^{[4
,5
]}

Bloom, E. D. ^{[4
,5
]}

Bogart, J. R. ^{[4
,5
]}

Bonino, R. ^{[19
,20
]}

Bottacini, E. ^{[4
,5
]}

Bregeon, J. ^{[21
]}

Britto, R. J. ^{[22
]}

Bruel, P. ^{[23
]}

Buehler, R. ^{[2
]}

Burnett, T. H. ^{[24
]}

Buson, S. ^{[15
,16
]}

Caliandro, G. A. ^{[4
,5
,25
]}

Cameron, R. A. ^{[4
,5
]}

Caputo, R. ^{[6
,7
]}

Caragiulo, M. ^{[18
]}

Caraveo, P. A. ^{[17
]}

Casandjian, J. M. ^{[1
]}

Cavazzuti, E. ^{[26
]}

Charles, E. ^{[4
,5
]}

Chaves, R. C. G. ^{[21
]}

Chekhtman, A. ^{[27
]}

Cheung, C. C. ^{[28
]}

Chiang, J. ^{[4
,5
]}

Chiaro, G. ^{[16
]}

Ciprini, S. ^{[26
,29
,30
]}

Claus, R. ^{[4
,5
]}

Cohen-Tanugi, J. ^{[21
]}

Cominsky, L. R. ^{[31
]}

Conrad, J. ^{[8
,10
,32
]}

Cutini, S. ^{[26
,29
,30
]}

D'Ammando, F. ^{[33
,34
]}

de Angelis, A. ^{[35
,36
]}

DeKlotz, M. ^{[37
]}

de Palma, F. ^{[18
,38
]}

Desiante, R. ^{[13
,39
]}

Digel, S. W. ^{[4
,5
]}

Di Venere, L. ^{[40
]}

机构：

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

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

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

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

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

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

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

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

[9] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden

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

[11] Univ Pisa, I-56127 Pisa, Italy

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

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

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

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

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

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

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

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

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

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

[22] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa

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

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

[25] CIFS, I-10133 Turin, Italy

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

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

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

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

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

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

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

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

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

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

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

[37] Stellar Solut Inc, Palo Alto, CA 94306 USA

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

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

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

[41] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

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

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

[44] Univ Orleans CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France

[45] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[46] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

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

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

[49] CRESST, Greenbelt, MD 20771 USA

[50] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2015年 / 218卷 / 02期

基金：

美国国家航空航天局;

关键词：

catalogs; gamma-rays: general; GAMMA-RAY EMISSION; ALL-SKY SURVEY; PULSAR WIND NEBULAE; GALACTIC POPULATION; GLOBULAR-CLUSTERS; WMAP OBSERVATIONS; MAGELLANIC-CLOUD; MGRO J2019+37; RADIO-SOURCES; DISCOVERY;

D O I：

10.1088/0067-0049/218/2/23

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the third Fermi Large Area Telescope (LAT) source catalog (3FGL) of sources in the 100 MeV-300 GeV range. Based on the first 4 yr of science data from the Fermi Gamma-ray Space Telescope mission, it is the deepest yet in this energy range. Relative to the Second Fermi LAT catalog, the 3FGL catalog incorporates twice as much data, as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse.-ray emission, a refined procedure for source detection, and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above 4 sigma significance, with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 238 sources are considered as identified based on angular extent or correlated variability (periodic or otherwise) observed at other wavelengths. For 1010 sources we have not found plausible counterparts at other wavelengths. More than 1100 of the identified or associated sources are active galaxies of the blazar class; several other classes of non-blazar active galaxies are also represented in the 3FGL. Pulsars represent the largest Galactic source class. From source counts of Galactic sources we estimate that the contribution of unresolved sources to the Galactic diffuse emission is similar to 3% at 1 GeV.

引用

页数：41

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