GRB080513A

This page lists all entries on GRB080513A in GRBweb

Summary GCN 7728 GCN 7729 GCN 21765

Summary table
Variable Value Source
T0 5:14:09.927 UTC GCN_circulars,Konus-Wind Det
ra 163.2830° GCN_circulars,IPN Triangulation
decl 28.1950° GCN_circulars,IPN Triangulation
GBM_located False
mjd 54599.218170451386 GCN_circulars,Konus-Wind Det
GCN 7728 table
GRB_name GRB080513A
GCN_number 7728
Detection_method IPN Triangulation
t_trigger 5:14:10 UTC
ra 163.2830°
decl 28.1950°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7728 SUBJECT: IPN triangulation of bright GRB 080513 DATE: 08/05/15 15:39:38 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks on behalf of the Konus-Wind team, K. Hurley and T. Cline on behalf of the Mars Odyssey, Konus, and MESSENGER GRB teams, W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on behalf of the GRS-Odyssey GRB team, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, J. Cummings, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of the Swift-BAT team, A. von Kienlin, G. Lichti, and A. Rau, on behalf of the INTEGRAL SPI-ACS GRB team, report: Mars Odyssey, Konus-Wind, Swift-BAT, and INTEGRAL-SPI-ACS observed the long-duration bright GRB 080513 at about 18850 s UT (05:14:10). The burst was outside the coded field of view of the BAT. The burst light curve shows a multipeaked structure with a duration of ~30 sec, followed by a weak pulse at ~T0+70 sec. We have triangulated the burst to the following, preliminary 3-sigma error box: ----------------------------------------------- RA(2000) Dec(2000) ----------------------------------------------- Center: 163.283 (10h 53m 08s) +28.195 (+28d 11' 43") Corners: 163.291 (10h 53m 10s) +28.731 (+28d 43' 51") 163.334 (10h 53m 20s) +27.777 (+27d 46' 36") 163.268 (10h 53m 04s) +27.646 (+27d 38' 47") 163.227 (10h 52m 55s) +28.606 (+28d 36' 21") ------------------------------------------------- The error box area is 213 sq. arcmin and the maximal distance between the box corners is 1.09 deg. This error box may be improved. Preliminary analysis of the Konus-Wind data yields a burst fluence of ~2x10^-5 erg/cm2 (in the 20 keV - 2 MeV range), and an Epeak of the time-integrated spectrum of ~200 keV. Detailed spectral parameters will be reported later.
GCN 7729 table
GRB_name GRB080513A
GCN_number 7729
Detection_method Konus-Wind Det
t_trigger 5:14:09.927 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 7729 SUBJECT: Konus-Wind observation of GRB 080513 DATE: 08/05/15 16:02:44 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team report: The long GRB 080513 localized by IPN (Golenetskii et al., GCN 7728) triggered Konus-Wind at T0=18849.927 s UT (05:14:09.927). As observed by Konus-Wind the burst had a fluence of 2.02(-0.17, +0.20)x10^-5 erg/cm2, and a 16-ms peak flux measured from T0+24.016 s of (1.15 +/- 0.30)x10^-5 erg/cm2/s (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+32.256 s) can be fitted (in the 20 keV-2 MeV range) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.48(-0.13, +0.12) and Ep = 223(-38, +62) keV (chi2 = 76.6/61 dof). Fitting by GRBM (Band) model yields the same alpha and Ep, and only an upper limit on the high energy photon index: beta < -2.19 (chi2 = 76.0/60 dof). The spectrum of the most intense part (from T0+16.640 to T0+24.064 s) is well fitted (in the same range) by a power law with exponential cutoff model with alpha = -1.31(-0.12, +0.11) and Ep = 317(-50, +73) keV (chi2 = 56.7/61 dof). Fitting by GRBM (Band) model yields the same alpha and Ep, and only an upper limit on the high energy photon index: beta < -2.20 (chi2 = 56.5/60 dof). The fluence of this part is (1.18 +/- 0.10)x10^-5 erg/cm2 (in the 20 keV - 2 MeV energy range). All the quoted errors are at the 90% confidence level. The Konus-Wind light curve of this GRB is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080513_T18849/ [GCN OPS NOTE(15may08): Per author's request, "080515" in the first line was chanegd to "080513".]
GCN 21765 table
GRB_name GRB080513A
GCN_number 21765
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21765 SUBJECT: LIGO/Virgo G298048: Discovery of X-ray emission from SSS17a in NGC4993 DATE: 17/08/30 12:07:12 GMT FROM: Eleonora Troja at GSFC/Swift E. Troja (UMD/GSFC), L. Piro (INAF/IAPS), T. Sakamoto (AGU), S. B. Cenko (NASA/GSFC), and A. Lien (UMBC/GSFC) report on behalf of a larger collaboration: We observed the field of SSS17a (Coulter et al., LVC GCN 21529) with the Chandra X-ray Observatory under our approved guest observer program (18500489; PI: E. Troja). Observations were carried out on 2017-08-26 (~9 days after the LVC trigger) for a total exposure of 50 ks. We detect the extended X-ray source visible in previous observations (Evans et al., LVC GCN 21612; Margutti et al., LVC GCN 21648) at a comparable flux level. In addition, we detect an X-ray source at the optical/IR transient position, approximately 10 arcsecond from the centroid of the extended X-ray emission. The probability to find an unrelated X-ray source within the small localization of the optical transient is negligible (<1E-5). Previous candidate kilonovae (e.g. GRB080513, Perley et al. 2009; GRB130603B; Tanvir et al. 2013) were associated to transient X-ray emission, although bright X-rays are not a basic prediction of this model. In our case, the properties of the X-ray emission and the overall spectral energy distribution appear different. The most likely explanation seems that the observed X-rays arise from the afterglow of GRB170817A (Connaughton et al., LVC GCN 21506; Savchenko et al., LVC GCN 21507), thus confirming the spatial association between the short GRB and SSS17a. A newborn spinning-down magnetar could power a long-lived and nearly constant X-ray emission (Zhang & Meszaros, 2001). However, the observed timescale and X-ray luminosity would imply unrealistic values of the initial spin period and magnetic field. The previous lack of detection from Chandra (Margutti et al., LVC GCN 21648) further disfavors this magnetar model. Other models (e.g. Metzger & Piro, 2014) also do not match our observed luminosities and timescales. For a standard on-axis afterglow, the extrapolation of the observed flux would violate the upper limits reported by Evans et al. (LVC GCN 21550), and Cenko et al. (LVC GCN 21572). Our observations are instead consistent with the onset of an off-axis afterglow from the GRB jet. This would explain the low luminosity of the observed gamma-ray emission, and the lack of early afterglow detections. Further observations are planned. We thank Belinda Wilkes and the entire CXC staff for rapidly scheduling these observations.