FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE

被引：100

作者：

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

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

Agudo, I. ^{[5
,6
]}

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

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

Aller, H. D. ^{[7
]}

Aller, M. F. ^{[7
]}

Antolini, E. ^{[8
,9
]}

Arkharov, A. A. ^{[10
]}

Axelsson, M. ^{[11
,12
,13
]}

Bach, U. ^{[14
]}

Baldini, L. ^{[15
]}

Ballet, J. ^{[16
]}

Barbiellini, G. ^{[17
,18
]}

Bastieri, D. ^{[19
,20
]}

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

Bellazzini, R. ^{[15
]}

Berdyugin, A. ^{[21
]}

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

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

Blinov, D. A. ^{[22
]}

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

Boettcher, M. ^{[23
]}

Bonamente, E. ^{[8
,9
]}

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

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

Bregeon, J. ^{[15
]}

Brez, A. ^{[15
]}

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

Bruel, P. ^{[26
]}

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

Buemi, C. S. ^{[27
]}

Burnett, T. H. ^{[28
]}

Buson, S. ^{[19
,20
]}

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

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

Caraveo, P. A. ^{[30
]}

Carosati, D. ^{[31
]}

Carrigan, S. ^{[20
]}

Casandjian, J. M. ^{[16
]}

Cavazzuti, E. ^{[32
]}

Cecchi, C. ^{[8
,9
]}

Celik, Oe ^{[33
,34
,35
,36
,37
]}

Chekhtman, A. ^{[1
,38
]}

Chen, W. P. ^{[39
]}

Cheung, C. C. ^{[1
,2
]}

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

Ciprini, S. ^{[9
]}

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

Cohen-Tanugi, J. ^{[40
]}

机构：

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

[2] Natl Acad Sci, Washington, DC 20001 USA

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

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

[5] CSIC, Inst Astrofis Andalucia, Granada 18080, Spain

[6] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA

[7] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

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

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

[10] Pulkovo Observ, St Petersburg 196140, Russia

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

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

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

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

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

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

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

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

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

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

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

[22] St Petersburg State Univ, Astron Inst, St Petersburg, Russia

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

[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] Osserv Astrofis Catania, I-95123 Catania, Italy

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

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

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

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

[32] Agenzia Spaziale Italiana ASI, Sci Data Ctr, I-00044 Frascati, Italy

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

[34] NASA, CRESST, Greenbelt, MD 20771 USA

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

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

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

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

[39] Natl Cent Univ, Grad Inst Astron, Chungli 32054, Taiwan

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

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

[42] Inst Univ France, F-75005 Paris, France

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

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

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

[46] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[47] Agrupaci Astron Sabadell, Sabadell 08206, Spain

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

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

[50] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 721卷 / 02期

基金：

俄罗斯基础研究基金会;

关键词：

galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 1510-089); GAMMA-RAY EMISSION; X-RAY; GALACTIC NUCLEI; SPECTRAL PROPERTIES; COMPLETE SAMPLE; BLAZAR; RADIO; SWIFT; JET; RADIATION;

D O I：

10.1088/0004-637X/721/2/1425

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the multi-wavelength observations of PKS 1510-089 (a flat spectrum radio quasar (FSRQ) at z = 0.361) during its high activity period between 2008 September and 2009 June. During this 11 month period, the source was characterized by a complex variability at optical, UV, and gamma-ray bands, on timescales down to 6-12 hr. The brightest gamma-ray isotropic luminosity, recorded on 2009 March 26, was similar or equal to 2 x 1048 erg s-1. The spectrum in the Fermi Large Area Telescope energy range shows a mild curvature described well by a log-parabolic law, and can be understood as due to the Klein-Nishina effect. The. -ray flux has a complex correlation with the other wavelengths. There is no correlation at all with the X-ray band, a weak correlation with the UV, and a significant correlation with the optical flux. The. -ray flux seems to lead the optical one by about 13 days. From the UV photometry, we estimated a black hole mass of similar or equal to 5.4 x 10(8)M(circle dot) and an accretion rate of similar or equal to 0.5M(circle dot) yr(-1). Although the power in the thermal and non-thermal outputs is smaller compared to the very luminous and distant FSRQs, PKS 1510-089 exhibits a quite large Compton dominance and a prominent big blue bump (BBB) as observed in the most powerful gamma-ray quasars. The BBB was still prominent during the historical maximum optical state in 2009 May, but the optical/ UV spectral index was softer than in the quiescent state. This seems to indicate that the BBB was not completely dominated by the synchrotron emission during the highest optical state. We model the broadband spectrum assuming a leptonic scenario in which the inverse Compton emission is dominated by the scattering of soft photons produced externally to the jet. The resulting model-dependent jet energetic content is compatible with a scenario in which the jet is powered by the accretion disk, with a total efficiency within the Kerr black hole limit.

引用

页码：1425 / 1447

页数：23

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