A new analysis of the short-duration, hard-spectrum GRB 051103, a possible extragalactic soft gamma repeater giant flare

被引：38

作者：

Hurley, K. ^{[1
]}

Rowlinson, A. ^{[2
]}

Bellm, E. ^{[1
]}

Perley, D. ^{[3
]}

Mitrofanov, I. G. ^{[4
]}

Golovin, D. V. ^{[4
]}

Kozyrev, A. S. ^{[4
]}

Litvak, M. L. ^{[4
]}

Sanin, A. B. ^{[4
]}

Boynton, W. ^{[5
]}

Fellows, C. ^{[5
]}

Harshmann, K. ^{[5
]}

Ohno, M. ^{[6
]}

Yamaoka, K. ^{[7
]}

Nakagawa, Y. E. ^{[8
]}

Smith, D. M. ^{[9
,10
]}

Cline, T. ^{[11
]}

Tanvir, N. R. ^{[2
]}

O'Brien, P. T. ^{[2
]}

Wiersema, K. ^{[2
]}

Rol, E. ^{[2
,12
]}

Levan, A. ^{[13
]}

Rhoads, J. ^{[14
]}

Fruchter, A. ^{[15
]}

Bersier, D. ^{[16
]}

Kavelaars, J. J. ^{[17
]}

Gehrels, N. ^{[11
]}

Krimm, H. ^{[11
]}

Palmer, D. M. ^{[18
]}

Duncan, R. C. ^{[19
]}

Wigger, C. ^{[20
]}

Hajdas, W. ^{[20
]}

Atteia, J. -L. ^{[21
]}

Ricker, G. ^{[22
]}

Vanderspek, R. ^{[22
]}

Rau, A. ^{[23
]}

von Kienlin, A. ^{[23
]}

机构：

[1] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[2] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[3] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[4] Inst Space Res, Moscow 117997, Russia

[5] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA

[6] JAXA, ISAS, Sagamihara, Kanagawa 2298510, Japan

[7] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan

[8] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan

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

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

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

[12] Univ Amsterdam, NL-1098 SJ Amsterdam, Netherlands

[13] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[14] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[15] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[16] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England

[17] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada

[18] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[19] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA

[20] Paul Scherrer Inst, CH-5232 Villigen, Switzerland

[21] Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France

[22] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[23] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 403卷 / 01期

基金：

英国科学技术设施理事会;

关键词：

stars: neutron; gamma-rays: bursts; RAY BURST CATALOG; 2004; DECEMBER; 27; SUPERNOVA-REMNANTS; HOST GALAXY; INTERPLANETARY NETWORK; IMAGE SUBTRACTION; NEUTRON-STARS; SGR; 1806-20; SGR-1806-20; AFTERGLOW;

D O I：

10.1111/j.1365-2966.2009.16118.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GRB 051103 is considered to be a candidate soft gamma repeater (SGR) extragalactic giant magnetar flare by virtue of its proximity on the sky to M81/M82, as well as its time history, localization and energy spectrum. We have derived a refined interplanetary network localization for this burst which reduces the size of the error box by over a factor of 2. We examine its time history for evidence of a periodic component, which would be one signature of an SGR giant flare, and conclude that this component is neither detected nor detectable under reasonable assumptions. We analyse the time-resolved energy spectra of this event with improved time and energy resolution, and conclude that although the spectrum is very hard its temporal evolution at late times cannot be determined, which further complicates the giant flare association. We also present new optical observations reaching limiting magnitudes of R > 24.5, about 4-mag deeper than previously reported. In tandem with serendipitous observations of M81 taken immediately before and 1 month after the burst, these place strong constraints on any rapidly variable sources in the region of the refined error ellipse proximate to M81. We do not find any convincing afterglow candidates from either background galaxies or sources in M81, although within the refined error region we do locate two UV bright star-forming regions which may host SGRs. A supernova remnant (SNR) within the error ellipse could provide further support for an SGR giant flare association, but we were unable to identify any SNR within the error ellipse. These data still do not allow strong constraints on the nature of the GRB 051103 progenitor, and suggest that candidate extragalactic SGR giant flares will be difficult, although not impossible, to confirm.

引用

页码：342 / 352

页数：11

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