THE SPECTRAL ENERGY DISTRIBUTION OF FERMI BRIGHT BLAZARS

被引：794

作者：

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

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

Agudo, I. ^{[5
]}

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

Aller, H. D. ^{[6
]}

Aller, M. F. ^{[6
]}

Angelakis, E. ^{[7
]}

Arkharov, A. A. ^{[8
]}

Axelsson, M. ^{[9
,10
,11
]}

Bach, U. ^{[7
]}

Baldini, L. ^{[12
]}

Ballet, J. ^{[13
]}

Barbiellini, G. ^{[14
,15
]}

Bastieri, D. ^{[16
,17
]}

Baughman, B. M. ^{[18
]}

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

Bellazzini, R. ^{[12
]}

Benitez, E. ^{[19
]}

Berdyugin, A. ^{[20
]}

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

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

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

Boettcher, M. ^{[21
]}

Bonamente, E. ^{[22
,23
]}

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

Bregeon, J. ^{[12
]}

Brez, A. ^{[12
]}

Brigida, M. ^{[24
,25
]}

Bruel, P. ^{[26
]}

Burnett, T. H. ^{[27
]}

Burrows, D. ^{[28
]}

Buson, S. ^{[16
]}

Caliandro, G. A. ^{[29
]}

Calzoletti, L. ^{[30
]}

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

Capalbi, M. ^{[30
]}

Caraveo, P. A. ^{[31
]}

Carosati, D. ^{[32
]}

Casandjian, J. M. ^{[13
]}

Cavazzuti, E. ^{[30
]}

Cecchi, C. ^{[22
,23
]}

Celik, Oe. ^{[33
,34
,35
,36
]}

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

Chaty, S. ^{[13
]}

Chekhtman, A. ^{[1
,37
]}

Chen, W. P. ^{[38
]}

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

Chincarini, G. ^{[39
]}

Ciprini, S. ^{[23
]}

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

机构：

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

[2] Natl Acad Sci, Natl Res Council, 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] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[6] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

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

[8] Pulkovo Observ, St Petersburg 196140, Russia

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

[10] Lund Observ, SE-22100 Lund, Sweden

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

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

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

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

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

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

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

[18] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA

[19] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico

[20] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland

[21] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA

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

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

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

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

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

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

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

[29] IEEC CSIC, Inst Ciencias Espai, Barcelona 08193, Spain

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

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

[32] EPT Observ, Tijarafe, La Palma, Spain

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

[34] CRESST, Greenbelt, MD 20771 USA

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

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

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

[38] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan

[39] Univ Milan, Dipartimento Fis, I-20126 Milan, Italy

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

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

[42] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[43] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy

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

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

[46] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy

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

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

[49] Agrupacio Astron Sabadell, Sabadell 08206, Spain

[50] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 716卷 / 01期

基金：

美国国家科学基金会; 美国国家航空航天局; 瑞典研究理事会; 俄罗斯基础研究基金会;

关键词：

BL Lacertae objects: general; galaxies: active; gamma rays: galaxies; quasars: general; radiation mechanisms: non-thermal; GAMMA-RAY EMISSION; MICROWAVE BACKGROUND-RADIATION; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; PEAKED BL LACS; ALL-SKY SURVEY; MULTIWAVELENGTH OBSERVATIONS; ELECTRON ACCELERATION; PARTICLE-ACCELERATION; 3C; 454.3;

D O I：

10.1088/0004-637X/716/1/30

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have conducted a detailed investigation of the broadband spectral properties of the gamma-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi gamma-ray spectra with Swift, radio, infra-red, optical, and other hard X-ray/gamma-ray data, collected within 3 months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous spectral energy distributions (SED) for 48 LBAS blazars. The SED of these gamma-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual log nu-log nu F-nu representation, the typical broadband spectral signatures normally attributed to a combination of low-energy synchrotron radiation followed by inverse Compton emission of one or more components. We have used these SED to characterize the peak intensity of both the low-and the high-energy components. The results have been used to derive empirical relationships that estimate the position of the two peaks from the broadband colors (i.e., the radio to optical, alpha(ro), and optical to X-ray, alpha(ox), spectral slopes) and from the gamma-ray spectral index. Our data show that the synchrotron peak frequency (nu(S)(peak)) is positioned between 10(12.5) and 10(14.5) Hz in broad-lined flat spectrum radio quasars (FSRQs) and between 10(13) and 10(17) Hz in featureless BL Lacertae objects. We find that the gamma-ray spectral slope is strongly correlated with the synchrotron peak energy and with the X-ray spectral index, as expected at first order in synchrotron-inverse Compton scenarios. However, simple homogeneous, one-zone, synchrotron self-Compton (SSC) models cannot explain most of our SED, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. More complex models involving external Compton radiation or multiple SSC components are required to reproduce the overall SED and the observed spectral variability. While more than 50% of known radio bright high energy peaked (HBL) BL Lacs are detected in the LBAS sample, only less than 13% of known bright FSRQs and LBL BL Lacs are included. This suggests that the latter sources, as a class, may be much fainter gamma-ray emitters than LBAS blazars, and could in fact radiate close to the expectations of simple SSC models. We categorized all our sources according to a new physical classification scheme based on the generally accepted paradigm for Active Galactic Nuclei and on the results of this SED study. Since the LAT detector is more sensitive to flat spectrum gamma-ray sources, the correlation between nu(S)(peak) and gamma-ray spectral index strongly favors the detection of high energy peaked blazars, thus explaining the Fermi overabundance of this type of sources compared to radio and EGRET samples. This selection effect is similar to that experienced in the soft X-ray band where HBL BL Lacs are the dominant type of blazars.

引用

页码：30 / 70

页数：41

共 103 条

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Abdo, A. A. ;

Ackermann, M. ;

Ajello, M. ;

Atwood, W. B. ;

Axelsson, M. ;

Baldini, L. ;

Ballet, J. ;

Barbiellini, G. ;

Bastieri, D. ;

Bechtol, K. ;

Bellazzini, R. ;

Berenji, B. ;

Blandford, R. D. ;

Bloom, E. D. ;

Bonamente, E. ;

Borgland, A. W. ;

Bouvier, A. ;

Bregeon, J. ;

Brez, A. ;

Brigida, M. ;

Bruel, P. ;

Burnett, T. H. ;

Buson, S. ;

Caliandro, G. A. ;

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Cavazzuti, E. ;

Cecchi, C. ;

Celik, Oe ;

Charles, E. ;

Chekhtman, A. ;

Cheung, C. C. ;

Chiang, J. ;

Ciprini, S. ;

Claus, R. ;

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Berenji, B. ;

Blandford, R. ;

Bloom, E. D. ;

Bonamente, E. ;

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