VERITAS 2008-2009 MONITORING OF THE VARIABLE GAMMA-RAY SOURCE M 87

被引：37

作者：

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

Aliu, E. ^{[2
]}

Arlen, T. ^{[3
]}

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

Beilicke, M. ^{[6
]}

Benbow, W. ^{[1
]}

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

Bradbury, S. M. ^{[9
]}

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

Bugaev, V. ^{[6
]}

Byrum, K. ^{[10
]}

Cannon, A. ^{[11
]}

Cesarini, A. ^{[12
]}

Chow, Y. C. ^{[3
]}

Ciupik, L. ^{[13
]}

Cogan, P. ^{[14
]}

Cui, W. ^{[15
]}

Dickherber, R. ^{[6
]}

Duke, C. ^{[16
]}

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

Finnegan, G. ^{[17
]}

Fortin, P. ^{[2
]}

Fortson, L. ^{[13
]}

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

Galante, N. ^{[1
]}

Gall, D. ^{[15
]}

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

Godambe, S. ^{[17
]}

Grube, J. ^{[11
]}

Guenette, R. ^{[14
]}

Gyuk, G. ^{[13
]}

Hanna, D. ^{[14
]}

Holder, J. ^{[7
,8
]}

Hui, C. M. ^{[17
]}

Humensky, T. B. ^{[18
]}

Imran, A. ^{[19
]}

Kaaret, P. ^{[20
]}

Karlsson, N. ^{[13
]}

Kertzman, M. ^{[21
]}

Kieda, D. ^{[17
]}

Konopelko, A. ^{[22
]}

Krawczynski, H. ^{[6
]}

Krennrich, F. ^{[19
]}

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

LeBohec, S. ^{[17
]}

Maier, G. ^{[14
]}

McArthur, S. ^{[6
]}

McCann, A. ^{[14
]}

McCutcheon, M. ^{[14
]}

Millis, J. ^{[23
]}

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

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

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

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

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

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

[12] Natl Univ Ireland Galway, 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] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 716卷 / 01期

基金：

加拿大自然科学与工程研究理事会; 美国国家科学基金会; 爱尔兰科学基金会;

关键词：

galaxies:; individual; (M87; VER J1230+123); gamma rays: galaxies; M87; JET; TEV EMISSION; GALAXY M-87; BLACK-HOLE; HST-1; VARIABILITY; SITE; KNOT;

D O I：

10.1088/0004-637X/716/1/819

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

M 87 is a nearby radio galaxy that is detected at energies ranging from radio to very high energy (VHE) gamma rays. Its proximity and its jet, misaligned from our line of sight, enable detailed morphological studies and extensive modeling at radio, optical, and X-ray energies. Flaring activity was observed at all energies, and multi-wavelength correlations would help clarify the origin of the VHE emission. In this paper, we describe a detailed temporal and spectral analysis of the VERITAS VHE gamma-ray observations of M 87 in 2008 and 2009. In the 2008 observing season, VERITAS detected an excess with a statistical significance of 7.2 standard deviations (sigma) from M 87 during a joint multi-wavelength monitoring campaign conducted by three major VHE experiments along with the Chandra X-ray Observatory. In 2008 February, VERITAS observed a VHE flare from M 87 occurring over a 4 day timespan. The peak nightly flux above 250 GeV was (1.14 +/- 0.26) x 10(-11) cm(-2) s(-1), which corresponded to 7.7% of the Crab Nebula flux. M 87 was marginally detected before this 4 day flare period, and was not detected afterward. Spectral analysis of the VERITAS observations showed no significant change in the photon index between the flare and pre-flare states. Shortly after the VHE flare seen by VERITAS, the Chandra X-ray Observatory detected the flux from the core of M 87 at a historical maximum, while the flux from the nearby knot HST-1 remained quiescent. Acciari et al. presented the 2008 contemporaneous VHE gamma-ray, Chandra X-ray, and Very Long Baseline Array radio observations which suggest the core as the most likely source of VHE emission, in contrast to the 2005 VHE flare that was simultaneous with an X-ray flare in the HST-1 knot. In 2009, VERITAS continued its monitoring of M 87 and marginally detected a 4.2 sigma excess corresponding to a flux of similar to 1% of the Crab Nebula. No VHE flaring activity was observed in 2009.

引用

页码：819 / 824

页数：6

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