VERITAS OBSERVATIONS OF THE BL LAC OBJECT 1ES 1218+304

被引：55

作者：

Acciari, V. A. ^{[1
,2
]}

Aliu, E. ^{[3
]}

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

Beilicke, M. ^{[6
]}

Benbow, W. ^{[1
]}

Bradbury, S. M. ^{[7
]}

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

Bugaev, V. ^{[6
]}

Butt, Y. ^{[8
]}

Byrum, K. L. ^{[9
]}

Celik, O. ^{[10
]}

Cesarini, A. ^{[1
,11
]}

Ciupik, L. ^{[12
]}

Chow, Y. C. K. ^{[10
]}

Cogan, P. ^{[13
]}

Colin, P. ^{[14
]}

Cui, W. ^{[15
]}

Daniel, M. K. ^{[7
]}

Ergin, T. ^{[16
]}

Falcone, A. D. ^{[17
]}

Fegan, S. J. ^{[10
]}

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

Fortin, P. ^{[18
]}

Fortson, L. F. ^{[12
]}

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

Gillanders, G. H. ^{[11
]}

Grube, J. ^{[19
]}

Guenette, R. ^{[13
]}

Gyuk, G. ^{[12
]}

Hanna, D. ^{[13
]}

Hays, E. ^{[1
,9
]}

Holder, J. ^{[3
]}

Horan, D. ^{[9
]}

Hui, C. M. ^{[14
]}

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

Imran, A. ^{[21
]}

Kaaret, P. ^{[22
,23
]}

Karlsson, N. ^{[12
]}

Kertzman, M.

Kieda, D. B. ^{[14
]}

Kildea, J. ^{[1
]}

Konopelko, A. ^{[15
]}

Krawczynski, H. ^{[6
]}

Krennrich, F. ^{[21
]}

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

LeBohec, S. ^{[14
]}

Maier, G. ^{[13
]}

McCann, A. ^{[13
]}

McCutcheon, M. ^{[13
]}

Moriarty, P. ^{[2
]}

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, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 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] Washington Univ, Dept Phys, St Louis, MO 63130 USA

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

[8] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA

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

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

[11] Natl Univ Ireland, Dept Phys, Galway, Ireland

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

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

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

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

[16] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA

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

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

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

[20] Univ Coll Dublin, Sch Phys, Dublin 2, Ireland

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 695卷 / 02期

基金：

爱尔兰科学基金会; 加拿大自然科学与工程研究理事会; 美国国家科学基金会;

关键词：

BL Lacertae objects: individual (1ES 1218+304); galaxies: active; gamma rays: observations; EXTRAGALACTIC BACKGROUND LIGHT; ENERGY GAMMA-RAYS; RADIATION-FIELDS; TEV BLAZARS; X-RAY; TELESCOPE; EMISSION; SPECTRA; DISCOVERY; HESS;

D O I：

10.1088/0004-637X/695/2/1370

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The VERITAS collaboration reports the detection of very-high-energy gamma-ray emission from the high-frequency-peaked BL Lac object 1ES 1218+304 located at a redshift of z = 0.182. A gamma-ray signal was detected with a statistical significance of 10.4 standard deviations (10.4 sigma) for the observations taken during the first three months of 2007, confirming the discovery of this object made by the MAGIC collaboration. The photon spectrum between similar to 160 GeV and similar to 1.8 TeV is well described by a power law with an index of Gamma = 3.08 +/- 0.34(stat) +/- 0.2(sys). The integral flux is Phi (E > 200 GeV) = (12.2 +/- 2.6) x 10(-12) cm(-2) s(-1), which corresponds to similar to 6% of that of the Crab Nebula. The light curve does not show any evidence for very high energy flux variability. Using lower limits on the density of the extragalactic background light in the near to mid-infrared, we are able to limit the range of intrinsic energy spectra for 1ES 1218+304. We show that the intrinsic photon spectrum has an index that is harder than Gamma = 2.32 +/- 0.37(stat). When including constraints from the spectra of 1ES 1101-232 and 1ES 0229+200, the spectrum of 1ES 1218+ 304 is likely to be harder than Gamma = 1.86 +/- 0.37(stat).

引用

页码：1370 / 1375

页数：6

共 41 条

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