THE DISCOVERY OF γ-RAY EMISSION FROM THE BLAZAR RGB J0710+591

被引：73

作者：

Acciari, V. A. ^{[1
]}

Aliu, E. ^{[2
]}

Arlen, T. ^{[3
]}

Aune, T. ^{[4
,5
]}

Bautista, M. ^{[6
]}

Beilicke, M. ^{[7
]}

Benbow, W. ^{[1
]}

Boettcher, M. ^{[8
]}

Boltuch, D. ^{[9
,10
]}

Bradbury, S. M. ^{[11
]}

Buckley, J. H. ^{[7
]}

Bugaev, V. ^{[7
]}

Byrum, K. ^{[12
]}

Cannon, A. ^{[13
]}

Cesarini, A. ^{[14
]}

Ciupik, L. ^{[15
]}

Cui, W. ^{[16
]}

Dickherber, R. ^{[7
]}

Duke, C. ^{[17
]}

Falcone, A. ^{[18
]}

Finley, J. P. ^{[16
]}

Finnegan, G. ^{[19
]}

Fortson, L. ^{[15
]}

Furniss, A. ^{[4
,5
]}

Galante, N. ^{[1
]}

Gall, D. ^{[16
]}

Gibbs, K. ^{[1
]}

Gillanders, G. H. ^{[14
]}

Godambe, S. ^{[19
]}

Grube, J. ^{[13
]}

Guenette, R. ^{[6
]}

Gyuk, G. ^{[15
]}

Hanna, D. ^{[6
]}

Holder, J. ^{[9
,10
]}

Hui, C. M. ^{[19
]}

Humensky, T. B. ^{[20
]}

Imran, A. ^{[21
]}

Kaaret, P. ^{[22
]}

Karlsson, N. ^{[15
]}

Kertzman, M. ^{[23
]}

Kieda, D. ^{[19
]}

Konopelko, A. ^{[24
]}

Krawczynski, H. ^{[7
]}

Krennrich, F. ^{[21
]}

Lang, M. J. ^{[14
]}

Lamerato, A. ^{[8
]}

LeBohec, S. ^{[19
]}

Maier, G. ^{[6
]}

McArthur, S. ^{[7
]}

McCann, A. ^{[6
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA

[2] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA

[3] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

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

[5] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA

[6] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[7] Washington Univ, Dept Phys, St Louis, MO 63130 USA

[8] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA

[9] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[10] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

[11] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[12] Argonne Natl Lab, Argonne, IL 60439 USA

[13] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

[14] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland

[15] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA

[16] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA

[17] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA

[18] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA

[19] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA

[20] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[21] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

[22] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA

[23] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA

[24] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA

[25] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland

[26] European So Observ, D-85748 Garching, Germany

[27] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina

[28] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[29] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland

[30] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[49] CRESST, Greenbelt, MD 20771 USA

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 715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; 爱尔兰科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

BL Lacertae objects: individual (RGB J0710+591; VER J0710+591); gamma rays: galaxies; BL-LACERTAE OBJECTS; SPACE-TELESCOPE SURVEY; BACKGROUND-RADIATION; LAC OBJECTS; SAMPLE; CONSTRAINTS; VERITAS; ARRAY;

D O I：

10.1088/2041-8205/715/1/L49

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The high-frequency-peaked BL Lacertae object RGB J0710+591 was observed in the very high-energy (VHE; E > 100 GeV) wave band by the VERITAS array of atmospheric Cherenkov telescopes. The observations, taken between 2008 December and 2009 March and totaling 22.1 hr, yield the discovery of VHE gamma rays from the source. RGB J0710+591 is detected at a statistical significance of 5.5 standard deviations (5.5 sigma) above the background, corresponding to an integral flux of (3.9 +/- 0.8) x 10(-12) cm(-2) s(-1) (3% of the Crab Nebula's flux) above 300 GeV. The observed spectrum can be fit by a power law from 0.31 to 4.6 TeV with a photon spectral index of 2.69 +/- 0.26(stat) +/- 0.20(sys). These data are complemented by contemporaneous multiwavelength data from the Fermi Large Area Telescope, the Swift X-ray Telescope, the Swift Ultra-Violet and Optical Telescope, and the Michigan-Dartmouth-MIT observatory. Modeling the broadband spectral energy distribution (SED) with an equilibrium synchrotron self-Compton model yields a good statistical fit to the data. The addition of an external-Compton component to the model does not improve the fit nor brings the system closer to equipartition. The combined Fermi and VERITAS data constrain the properties of the high-energy emission component of the source over 4 orders of magnitude and give measurements of the rising and falling sections of the SED.

引用

页码：L49 / L55

页数：7

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