MULTI-WAVELENGTH OBSERVATIONS OF BLAZAR AO 0235+164 IN THE 2008-2009 FLARING STATE

被引：49

作者：

Ackermann, M. ^{[1
]}

Ajello, M. ^{[2
,3
]}

Ballet, J. ^{[4
]}

Barbiellini, G. ^{[5
,6
]}

Bastieri, D. ^{[7
,8
]}

Bellazzini, R. ^{[9
]}

Blandford, R. D. ^{[2
,3
]}

Bloom, E. D. ^{[2
,3
]}

Bonamente, E. ^{[10
,11
]}

Borgland, A. W. ^{[2
,3
]}

Bottacini, E. ^{[2
,3
]}

Bregeon, J. ^{[9
]}

Brigida, M. ^{[12
,13
]}

Bruel, P. ^{[14
]}

Buehler, R. ^{[2
,3
]}

Buson, S. ^{[7
,8
]}

Caliandro, G. A. ^{[15
]}

Cameron, R. A. ^{[2
,3
]}

Caraveo, P. A. ^{[16
]}

Casandjian, J. M. ^{[4
]}

Cavazzuti, E. ^{[17
]}

Cecchi, C. ^{[10
,11
]}

Charles, E. ^{[4
]}

Chekhtman, A. ^{[18
]}

Chiang, J. ^{[2
,3
]}

Ciprini, S. ^{[11
,17
]}

Claus, R. ^{[2
,3
]}

Cohen-Tanugi, J. ^{[19
]}

Cutini, S. ^{[17
]}

D'Ammando, F. ^{[20
,21
]}

de Palma, F.

Dermer, C. D. ^{[22
]}

do Couto e Silva, E. ^{[2
,3
]}

Drell, P. S. ^{[2
,3
]}

Drlica-Wagner, A. ^{[2
,3
]}

Dubois, R. ^{[2
,3
]}

Favuzzi, C. ^{[12
,13
]}

Fegan, S. J. ^{[14
]}

Ferrara, E. C. ^{[23
]}

Focke, W. B. ^{[2
,3
]}

Fortin, P. ^{[14
]}

Fuhrmann, L. ^{[24
]}

Fukazawa, Y. ^{[25
]}

Fusco, P. ^{[12
,13
]}

Gargano, F. ^{[13
]}

Gasparrini, D. ^{[17
]}

Gehrels, N. ^{[23
]}

Germani, S. ^{[11
]}

Giglietto, N. ^{[12
,13
]}

Giommi, P. ^{[17
]}

机构：

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

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

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

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

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

[6] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

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

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

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

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

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

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

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

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

[15] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain

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

[17] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy

[18] Artep Inc, Ellicott City, MD 21042 USA

[19] Univ Montpellier 2, CNRS IN2P3, Lab Univ & Particules Montpellier, Montpellier, France

[20] IASF Palermo, I-90146 Palermo, Italy

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

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

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

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

[25] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan

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

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

[28] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan

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

[30] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[31] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan

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

[33] CNRS, IRAP, F-31028 Toulouse 4, France

[34] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France

[35] Stockholm Univ, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden

[36] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden

[37] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden

[38] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan

[39] Univ Bordeaux 1, CEN Bordeaux Gradignan, CNRS IN2p3, F-33175 Gradignan, France

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

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

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

[43] Boise State Univ, Dept Phys, Boise, ID 83725 USA

[44] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan

[45] Inst Space & Astronaut Sci, JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan

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

[47] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 751卷 / 02期

基金：

美国国家航空航天局; 芬兰科学院; 美国国家科学基金会; 瑞典研究理事会;

关键词：

BL Lacertae objects: individual (AO 0235+164); galaxies: active; galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal; BL-LACERTAE OBJECTS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; SPECTRAL ENERGY-DISTRIBUTIONS; LARGE-AREA TELESCOPE; X-RAY-SPECTRA; ABSORPTION-LINE; COMPLETE SAMPLE; WEBT CAMPAIGN; RADIO-SOURCES; VARIABILITY;

D O I：

10.1088/0004-637X/751/2/159

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The blazarAO 0235+164 (z=0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to gamma-ray bands between 2008 September and 2009 February. In this paper, we summarize the rich multi-wavelength data collected during the campaign (including F-GAMMA, GASP-WEBT, Kanata, OVRO, RXTE, SMARTS, Swift, and other instruments), examine the cross-correlation between the light curves measured in the different energy bands, and interpret the resulting spectral energy distributions in the context of well-known blazar emission models. We find that the gamma-ray activity is well correlated with a series of near-IR/optical flares, accompanied by an increase in the optical polarization degree. On the other hand, the X-ray light curve shows a distinct 20 day high state of unusually soft spectrum, which does not match the extrapolation of the optical/UV synchrotron spectrum. We tentatively interpret this feature as the bulk Compton emission by cold electrons contained in the jet, which requires an accretion disk corona with an effective covering factor of 19% at a distance of 100 R-g. We model the broadband spectra with a leptonic model with external radiation dominated by the infrared emission from the dusty torus.

引用

页数：20

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