VERITAS OBSERVATIONS OF A VERY HIGH ENERGY γ-RAY FLARE FROM THE BLAZAR 3C 66A

被引：88

作者：

Acciari, V. A. ^{[2
]}

Aliu, E. ^{[3
,4
]}

Arlen, T. ^{[5
]}

Beilicke, M. ^{[6
]}

Benbow, W. ^{[1
]}

Boettcher, M. ^{[7
]}

Bradbury, S. M. ^{[8
]}

Buckley, J. H. ^{[6
]}

Bugaev, V. ^{[6
]}

Butt, Y. ^{[9
]}

Byrum, K. ^{[10
]}

Cannon, A. ^{[11
]}

Celik, O. ^{[5
]}

Cesarini, A. ^{[12
]}

Chow, Y. C. ^{[5
]}

Ciupik, L. ^{[13
]}

Cogan, P. ^{[14
]}

Cui, W. ^{[15
]}

Daniel, M. K. ^{[8
]}

Dickherber, R. ^{[6
]}

Ergin, T. ^{[9
]}

Falcone, A. ^{[16
]}

Fegan, S. J. ^{[5
]}

Finley, J. P. ^{[15
]}

Fortin, P. ^{[17
]}

Fortson, L. ^{[13
]}

Furniss, A. ^{[18
,19
]}

Gall, D. ^{[15
]}

Gibbs, K. ^{[1
]}

Gillanders, G. H. ^{[12
]}

Godambe, S. ^{[20
]}

Grube, J. ^{[11
]}

Guenette, R.

Gyuk, G. ^{[13
]}

Hanna, D. ^{[14
]}

Hays, E. ^{[21
]}

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

Horan, D. ^{[22
]}

Hui, C. M. ^{[20
]}

Humensky, T. B. ^{[23
]}

Imran, A. ^{[24
]}

Kaaret, P. ^{[25
]}

Karlsson, N. ^{[13
]}

Kertzman, M. ^{[26
]}

Kieda, D. ^{[20
]}

Kildea, J. ^{[1
]}

Konopelko, A. ^{[27
]}

Krawczynski, H. ^{[6
]}

Krennrich, F. ^{[24
]}

Lang, M. J. ^{[12
]}

机构：

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

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

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

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

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

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

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

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

[9] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

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

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

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

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

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

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

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

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

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

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

[20] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA

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

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

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

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

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

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

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

[28] Anderson Univ, Dept Phys, Anderson, IN 46012 USA

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

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2009年 / 693卷 / 02期

基金：

美国国家科学基金会; 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 (3C 66A); galaxies: active; gamma rays: observations; BL LACERTAE OBJECTS; ATMOSPHERIC CHERENKOV TELESCOPES; X-RAY; EMISSION; 3C-66A; DISCOVERY; RADIATION; ASTRONOMY; OPACITY; ARRAY;

D O I：

10.1088/0004-637X/693/2/L104

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The intermediate-frequency peaked BL Lacertae (IBL) object 3C 66A is detected during 2007-2008 in VHE ( very high energy; E > 100 GeV) gamma rays with the VERITAS stereoscopic array of imaging atmospheric Cherenkov telescopes. An excess of 1791 events is detected, corresponding to a significance of 21.2 standard deviations (sigma), in these observations (32.8 hr live time). The observed integral flux above 200 GeV is 6% of the Crab Nebula's flux and shows evidence for variability on the timescale of days. The measured energy spectrum is characterized by a soft power law with photon index Gamma = 4.1 +/- 0.4(stat) +/- 0.6(sys). The radio galaxy 3C 66B is excluded as a possible source of the VHE emission.

引用

页码：L104 / L108

页数：5