PKS 1502+106: A NEW AND DISTANT GAMMA-RAY BLAZAR IN OUTBURST DISCOVERED BY THE FERMI LARGE AREA TELESCOPE

被引：80

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
]}

Baughman, B. M. ^{[16
]}

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

Bellazzini, R. ^{[10
]}

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

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

Bogaert, G. ^{[17
]}

Bonamente, E. ^{[1
,18
]}

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

Bregeon, J. ^{[10
]}

Brez, A. ^{[10
]}

Brigida, M. ^{[19
,20
,21
]}

Bruel, P. ^{[17
]}

Burnett, T. H. ^{[22
]}

Caliandro, G. A. ^{[23
]}

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

Caraveo, P. A. ^{[24
]}

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

Cavazzuti, E. ^{[25
]}

Cecchi, C. ^{[1
,18
]}

Celik, Oe. ^{[26
,27
,28
,29
]}

Chekhtman, A. ^{[2
,30
]}

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

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

Ciprini, S. ^{[1
]}

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

Cohen-Tanugi, J. ^{[31
]}

Conrad, J. ^{[9
,32
]}

Cutini, S. ^{[25
]}

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

de Angelis, A. ^{[33
,34
]}

de Palma, F. ^{[19
,20
,21
]}

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

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

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

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

Dumora, D. ^{[35
,36
]}

Farnier, C. ^{[31
]}

Favuzzi, C. ^{[19
,20
,21
]}

Fegan, S. J. ^{[17
]}

Ferrara, E. C. ^{[26
]}

Focke, W. B. ^{[4
,5
]}

机构：

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

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

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

[4] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, 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] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

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

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

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

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

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

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

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

[20] Politecn Bari, I-70126 Bari, Italy

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

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

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

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

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

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

[27] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[44] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany

[45] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

[46] Univ Space Res Assoc, Columbia, MD 21044 USA

[47] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan

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

[49] Univ Roma La Sapienza, I-00185 Rome, Italy

[50] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 710卷 / 01期

基金：

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

关键词：

galaxies: active; galaxies: jets; gamma rays: general; quasars: general; quasars: individual (PKS 1502+106); X-rays: galaxies; ACTIVE GALACTIC NUCLEI; MICROWAVE BACKGROUND-RADIATION; EXTRAGALACTIC RADIO-SOURCES; RAPID NONTHERMAL FLARES; BL LACERTAE OBJECTS; SELF-COMPTON MODEL; X-RAY; PARTICLE-ACCELERATION; MULTIWAVELENGTH OBSERVATIONS; ELECTRON ACCELERATION;

D O I：

10.1088/0004-637X/710/1/810

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope discovered a rapid (similar to 5 days duration), high-energy (E > 100 MeV) gamma-ray outburst from a source identified with the blazar PKS 1502+106 (OR 103, S3 1502+10, z = 1.839) starting on 2008 August 5 (similar to 23 UTC, MJD 54683.95), and followed by bright and variable flux over the next few months. Results on the gamma-ray localization and identification, as well as spectral and temporal behavior during the first months of the Fermi all-sky survey, are reported here in conjunction with a multiwaveband characterization as a result of one of the first Fermi multifrequency campaigns. The campaign included a Swift ToO (followed up by a 16 day observation on August 7-22, MJD 54685-54700), VLBA (within the MOJAVE program), Owens Valley Radio Observatory (OVRO) 40 m, Effelsberg-100 m, Metsahovi-14 m, RATAN-600, and Kanata-Hiroshima radio/optical observations. Results from the analysis of archival observations by INTEGRAL, XMM-Newton, and Spitzer space telescopes are reported for a more complete picture of this new gamma-ray blazar. PKS 1502+106 is a sub-GeV peaked, powerful flat spectrum radio quasar (luminosity at E > 100 MeV, L-gamma, is about 1.1 x 10(49) erg s(-1), and black hole mass likely close to 10(9) M-circle dot), exhibiting marked gamma-ray bolometric dominance, in particular during the asymmetric outburst (L-gamma/L-opt similar to 100, and 5 day averaged flux F-E > 100MeV = 2.91 +/- 1.4 x 10(-6) ph cm(-2) s(-1)), which was characterized by a factor greater than 3 of flux increase in less than 12 hr. The outburst was observed simultaneously from optical to X-ray bands (F0.3-10keV = 2.18(-0.12)(+0.15) x 10(-12) erg cm(-2) s(-1), and hard photon index similar to 1.5, similar to past values) with a flux increase of less than 1 order of magnitude with respect to past observations, and was likely controlled by Comptonization of external-jet photons produced in the broad-line region (BLR) in the gamma-ray band. No evidence of a possible blue bump signature was observed in the optical-UV continuum spectrum, while some hints for a possible 4 day time lag with respect to the gamma-ray flare were found. Nonetheless, the properties of PKS 1502+106 and the strict optical/UV, X-, and gamma-ray cross-correlations suggest the contribution of the synchrotron self-Compton (SSC), in-jet, process should dominate from radio to X- rays. This mechanism may also be responsible for the consistent gamma-ray variability observed by the LAT on longer timescales, after the ignition of activity at these energies provided by the BLR-dissipated outburst. Modulations and subsequent minor, rapid flare events were detected, with a general fluctuation mode between pink-noise and a random-walk. The averaged gamma-ray spectrum showed a deviation from a simple power law, and can be described by a log-parabola curved model peaking around 0.4-0.5 GeV. The maximum energy of photons detected from the source in the first four months of LAT observations was 15.8 GeV, with no significant consequences on extragalactic background light predictions. A possible radio counterpart of the gamma-ray outburst can be assumed only if a delay of more than three months is considered on the basis of opacity effects at cm and longer wavelengths. The rotation of the electric vector position angle observed by VLBA from 2007 to 2008 could represent a slow field odering and alignment with respect to the jet axis, likely a precursor feature of the ejection of a superluminal radio knot and the high-energy outburst. This observing campaign provides more insight into the connection between MeV-GeV flares and the moving, polarized structures observed by the VLBI.

引用

页码：810 / 827

页数：18

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