A SEARCH FOR ENHANCED VERY HIGH ENERGY GAMMA-RAY EMISSION FROM THE 2013 MARCH CRAB NEBULA FLARE

被引：23

作者：

Aliu, E. ^{[1
]}

Archambault, S. ^{[2
]}

Aune, T. ^{[3
]}

Benbow, W. ^{[4
]}

Berger, K. ^{[5
,6
]}

Bird, R. ^{[7
]}

Bouvier, A. ^{[8
,9
]}

Buckley, J. H. ^{[10
]}

Bugaev, V. ^{[10
]}

Byrum, K. ^{[11
]}

Cerruti, M. ^{[4
]}

Chen, X. ^{[12
,13
]}

Ciupik, L. ^{[14
]}

Connolly, M. P. ^{[15
]}

Cui, W. ^{[16
]}

Dumm, J. ^{[17
]}

Errando, M. ^{[1
]}

Falcone, A. ^{[18
]}

Federici, S. ^{[12
,13
]}

Feng, Q. ^{[16
]}

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

Fortin, P. ^{[4
]}

Fortson, L. ^{[17
]}

Furniss, A. ^{[8
,9
]}

Galante, N. ^{[4
]}

Gillanders, G. H. ^{[15
]}

Griffin, S. ^{[2
]}

Griffiths, S. T. ^{[19
]}

Grube, J. ^{[14
]}

Gyuk, G. ^{[14
]}

Hanna, D. ^{[2
]}

Holder, J. ^{[5
,6
]}

Hughes, G. ^{[13
]}

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

Kaaret, P. ^{[19
]}

Kertzman, M. ^{[21
]}

Khassen, Y. ^{[7
]}

Kieda, D. ^{[22
]}

Krennrich, F. ^{[23
]}

Kumar, S. ^{[5
,6
]}

Lang, M. J. ^{[15
]}

Lyutikov, M. ^{[16
]}

Maier, G. ^{[13
]}

McArthur, S. ^{[24
]}

McCann, A. ^{[25
]}

Meagher, K. ^{[26
,27
]}

Millis, J. ^{[28
]}

Moriarty, P. ^{[29
]}

Mukherjee, R. ^{[1
]}

de Bhroithe, A. O'Faolain ^{[7
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

[12] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany

[13] DESY, D-15738 Zeuthen, Germany

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

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

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

[17] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

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

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

[20] Columbia Univ, Dept Phys, New York, NY 10027 USA

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

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

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

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

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

[26] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA

[27] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

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

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

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

[31] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2014年 / 781卷 / 01期

基金：

美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

gamma rays: general; ISM: individual objects (Crab Nebula); LARGE-AREA TELESCOPE; VARIABILITY;

D O I：

10.1088/2041-8205/781/1/L11

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In 2013 March, a flaring episode from the Crab Nebula lasting similar to 2 weeks was detected by Fermi-LAT (Large Area Telescope on board the Fermi Gamma-ray Space Telescope). The Very Energetic Radiation Imaging Telescope Array System (VERITAS) provides simultaneous observations throughout this period. During the flare, Fermi-LAT detected a 20 fold increase in flux above the average synchrotron flux >100 MeV seen from the Crab Nebula. Simultaneous measurements with VERITAS are consistent with the non-variable long-term average Crab Nebula flux at TeV energies. Assuming a linear correlation between the very high energy flux change >1 TeV and the flux change seen in the Fermi-LAT band >100 MeV during the period of simultaneous observations, the linear correlation factor can be constrained to be at most 8.6 x 10(-3) with 95% confidence.

引用

页数：7

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