FERMI OBSERVATIONS OF THE VERY HARD GAMMA-RAY BLAZAR PG 1553+113

被引:44
作者
Abdo, A. A. [1 ,2 ]
Ackermann, M. [3 ,4 ]
Ajello, M. [3 ,4 ]
Atwood, W. B. [5 ,6 ]
Axelsson, M. [7 ,8 ]
Baldini, L. [9 ]
Ballet, J. [10 ]
Barbiellini, G. [11 ,12 ]
Bastieri, D. [13 ,14 ]
Bechtol, K. [3 ,4 ]
Bellazzini, R. [9 ]
Berenji, B. [3 ,4 ]
Bloom, E. D. [3 ,4 ]
Bonamente, E. [15 ,16 ]
Borgland, A. W. [3 ,4 ]
Bregeon, J. [9 ]
Brez, A. [9 ]
Brigida, M. [17 ,18 ]
Bruel, P. [19 ]
Burnett, T. H. [20 ]
Caliandro, G. A. [17 ,18 ]
Cameron, R. A. [3 ,4 ]
Caraveo, P. A. [21 ]
Casandjian, J. M. [10 ]
Cavazzuti, E. [22 ]
Cecchi, C. [15 ,16 ]
Celik, Oe. [23 ,24 ]
Charles, E. [3 ,4 ]
Chekhtman, A. [1 ,25 ]
Cheung, C. C.
Chiang, J. [3 ,4 ]
Ciprini, S. [15 ,16 ]
Claus, R. [3 ,4 ]
Cohen-Tanugi, J. [26 ]
Conrad, J. [8 ,27 ]
Cutini, S. [22 ]
Dermer, C. D. [1 ]
de Angelis, A. [28 ,29 ]
de Palma, F. [17 ,18 ]
do Couto e Silva, E. [3 ,4 ]
Drell, P. S. [3 ,4 ]
Dubois, R. [3 ,4 ]
Dumora, D. [30 ,31 ]
Farnier, C. [26 ]
Favuzzi, C. [17 ,18 ]
Fegan, S. J. [19 ]
Focke, W. B. [3 ,4 ]
Fortin, P. [19 ]
Frailis, M. [28 ,29 ]
Fukazawa, Y. [32 ]
机构
[1] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA
[2] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA
[3] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA
[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA
[5] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[7] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden
[8] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden
[9] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy
[10] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France
[11] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy
[12] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy
[13] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy
[14] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy
[15] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy
[16] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy
[17] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy
[18] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy
[19] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[20] Univ Washington, Dept Phys, Seattle, WA 98195 USA
[21] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy
[22] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy
[23] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA
[24] Univ Maryland, Baltimore, MD 21250 USA
[25] George Mason Univ, Fairfax, VA 22030 USA
[26] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France
[27] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden
[28] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy
[29] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy
[30] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France
[31] CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France
[32] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan
[33] Univ Maryland, College Pk, MD 20742 USA
[34] Univ Alabama, Huntsville, AL 35899 USA
[35] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA
[36] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan
[37] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan
[38] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan
[39] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-30128 Toulouse 4, France
[40] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy
[41] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA
[42] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[43] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan
[44] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria
[45] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria
[46] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain
[47] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden
[48] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA
[49] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA
[50] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA
基金
美国国家航空航天局; 瑞典研究理事会;
关键词
BL Lacertae objects: individual (PG 1553+113); gamma rays: observations; BL LACERTAE OBJECTS; EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; SPACE-TELESCOPE SURVEY; LARGE-AREA TELESCOPE; RADIO-SOURCES; MAGIC TELESCOPE; ENERGY-SPECTRA; HOST GALAXIES; CRAB-NEBULA;
D O I
10.1088/0004-637X/708/2/1310
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the observations of PG 1553+113 during the first similar to 200 days of Fermi Gamma-ray Space Telescope science operations, from 2008 August 4 to 2009 February 22 (MJD 54682.7-54884.2). This is the first detailed study of PG 1553+113 in the GeV gamma-ray regime and it allows us to fill a gap of three decades in energy in its spectral energy distribution (SED). We find PG 1553+113 to be a steady source with a hard spectrum that is best fit by a simple power law in the Fermi energy band. We combine the Fermi data with archival radio, optical, X-ray, and very high energy (VHE) gamma-ray data to model its broadband SED and find that a simple, one-zone synchrotron self-Compton model provides a reasonable fit. PG 1553+113 has the softest VHE spectrum of all sources detected in that regime and, out of those with significant detections across the Fermi energy bandpass so far, the hardest spectrum in that energy regime. Thus, it has the largest spectral break of any gamma-ray source studied to date, which could be due to the absorption of the intrinsic gamma-ray spectrum by the extragalactic background light (EBL). Assuming this to be the case, we selected a model with a low level of EBL and used it to absorb the power-law spectrum from PG 1553+113 measured with Fermi (200 MeV-157 GeV) to find the redshift, which gave the best fit to the measured VHE data (90 GeV-1.1 TeV) for this parameterization of the EBL. We show that this redshift can be considered an upper limit on the distance to PG 1553+113.
引用
收藏
页码:1310 / 1320
页数:11
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