SPECTRAL PROPERTIES OF BRIGHT FERMI-DETECTED BLAZARS IN THE GAMMA-RAY BAND

被引：178

作者：

Abdo, A. A. ^{[2
,3
]}

Ackermann, M. ^{[4
,5
]}

Ajello, M. ^{[4
,5
]}

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

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

Baldini, L. ^{[10
]}

Ballet, J. ^{[11
]}

Barbiellini, G. ^{[12
,13
]}

Bastieri, D. ^{[14
,15
]}

Bechtol, K. ^{[4
,5
]}

Bellazzini, R. ^{[10
]}

Berenji, B. ^{[4
,5
]}

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

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

Bonamente, E. ^{[16
,17
]}

Borgland, A. W. ^{[4
,5
]}

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

Bregeon, J. ^{[10
]}

Brez, A. ^{[10
]}

Brigida, M. ^{[18
,19
]}

Bruel, P. ^{[20
]}

Burnett, T. H. ^{[21
]}

Buson, S. ^{[14
]}

Caliandro, G. A. ^{[22
]}

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

Caraveo, P. A. ^{[23
]}

Carrigan, S. ^{[15
]}

Casandjian, J. M. ^{[11
]}

Cavazzuti, E. ^{[24
]}

Cecchi, C. ^{[16
,17
]}

Celik, Oe ^{[25
,26
,27
,28
]}

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

Chekhtman, A. ^{[2
,29
]}

Cheung, C. C. ^{[2
,3
]}

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

Ciprini, S. ^{[17
]}

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

Cohen-Tanugi, J. ^{[30
]}

Conrad, J. ^{[31
]}

Cutini, S. ^{[24
]}

Dermer, C. D. ^{[2
]}

de Angelis, A. ^{[32
,33
]}

de Palma, F. ^{[18
,19
]}

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

do Couto e Silva, E. ^{[4
,5
]}

Drell, P. S. ^{[4
,5
]}

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

Dumora, D. ^{[1
,34
]}

Farnier, C. ^{[30
]}

Favuzzi, C. ^{[18
,19
]}

机构：

[1] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[26] NASA, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA

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

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

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

[30] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticule, Montpellier, France

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

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

[33] Ist Nazl Fis Nucl, Sez Trieste, I-33100 Udine, Italy

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

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

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

[37] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

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

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

[40] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[41] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 710卷 / 02期

关键词：

BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma rays: general; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SOURCE LIST; EGRET DATA; SYNCHROTRON; EMISSION; ACCELERATION; RADIATION; CATALOG; MODEL;

D O I：

10.1088/0004-637X/710/2/1271

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The gamma-ray energy spectra of bright blazars of the LAT Bright AGN Sample LBAS) are investigated using Fermi-LAT data. Spectral properties hardness, curvature, and variability) established using a data set accumulated over 6 months of operation are presented and discussed for different blazar classes and subclasses: flat spectrum radio quasars (FSRQs), low-synchrotron peaked BLLacs (LSP-BLLacs), intermediate-synchrotron peaked BLLacs (ISP-BLLacs), and high-synchrotron peaked BLLacs (HSP-BLLacs). The distribution of photon index G, obtained from a power-law fit above 100 MeV) is found to correlate strongly with blazar subclass. The change in spectral index from that averaged over the 6 months observing period is < 0.2-0.3 when the flux varies by about an order of magnitude, with a tendency toward harder spectra when the flux is brighter for FSRQs and LSP-BLLacs. A strong departure from a single power-law spectrum appears to be a common feature for FSRQs. This feature is also present for some high-luminosity LSP-BLLacs, and a small number of ISP-BLLacs. It is absent in all LBAS HSP-BLLacs. For 3C 454.3 and AO 0235+164, the two brightest FSRQ source and LSP-BLLac source, respectively, a broken power law (BPL) gives the most acceptable of power law, BPL, and curved forms. The consequences of these findings are discussed.

引用

页码：1271 / 1285

页数：15

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