GRB130515A

This page lists all entries on GRB130515A in GRBweb

Summary Fermi GBM IPN Swift GCN 14650 GCN 14653 GCN 14654 GCN 14655 GCN 14656 GCN 14658 GCN 14660 GCN 14661 GCN 14663 GCN 14667 GCN 14668 GCN 14670 GCN 14671 GCN 14688

Summary table
Variable Value Source
GRB_name_Fermi GRB130515056
T0 1:21:17 UTC GCN_circulars,Swift Det
ra 283.4401° Swift
decl -54.2791° Swift
pos_error 3.11e-04° Swift
T90 0.256 s Fermi_GBM
T90_error 0.091 s Fermi_GBM
T90_start 1:21:17.812 UTC Fermi_GBM
fluence 1.09e-06 erg/cm² Fermi_GBM
fluence_error 1.58e-08 erg/cm² Fermi_GBM
T100 1.068 s
GBM_located False
mjd 56427.056446759256 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB130515056
trigger_name bn130515056
ra 283.4221°
decl -54.2811°
pos_error 4.71e+00°
datum 2013-05-15
t_trigger 1:21:17.876 UTC
T90 0.256 s
T90_error 0.091 s
T90_start 1:21:17.812 UTC
fluence 1.09e-06 erg/cm²
fluence_error 1.58e-08 erg/cm²
flux_1024 3.73e+00 erg/cm²/s
flux_1024_error 3.52e-01 erg/cm²/s
flux_1024_time -4.48e-01 erg/cm²/s
flux_64 2.06e+01 erg/cm²/s
flux_64_error 2.33e+00 erg/cm²/s
IPN table
GRB_name GRB130515A
ra 283.4208°
decl -54.2833°
pos_error 5.00e-02°
Swift table
GRB_name GRB130515A
t_trigger 1:21:17 UTC
ra 283.4401°
decl -54.2791°
pos_error 3.11e-04°
T90 0.29 s
fluence 1.50e-07 erg/cm²
GCN 14650 table
GRB_name GRB130515A
GCN_number 14650
Detection_method Swift Det
t_trigger 1:21:17 UTC
ra 283.4220°
decl -54.2810°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14650 SUBJECT: GRB 130515A: Swift detection of a short burst DATE: 13/05/15 01:35:00 GMT FROM: David Palmer at LANL D. Malesani (DARK/NBI), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC), D. Grupe (PSU), S. T. Holland (STScI), J. A. Kennea (PSU), C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report on behalf of the Swift Team: At 01:21:17 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 130515A (trigger=555880). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 283.422, -54.281 which is RA(J2000) = 18h 53m 41s Dec(J2000) = -54d 16' 51" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single short peak with a duration of about 0.6 sec. The peak count rate was ~13000 counts/sec (15-350 keV), at ~0.1 sec after the trigger. The XRT began observing the field at 01:22:32.9 UT, 75.2 seconds after the BAT trigger. Using promptly downlinked data we find a faint uncatalogued X-ray source with an enhanced position: RA, Dec 283.4405, -54.2794 which is equivalent to: RA(J2000) = 18h 53m 45.72s Dec(J2000) = -54d 16' 45.9" with an uncertainty of 3.1 arcseconds (radius, 90% containment). This location is 39 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 5.79 x 10^20 cm^-2 (Kalberla et al. 2005). UVOT took a finding chart exposure of 150 seconds with the White filter starting 78 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.07. Burst Advocate for this burst is D. Malesani (malesani AT dark-cosmology.dk). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN 14653 table
GRB_name GRB130515A
GCN_number 14653
Detection_method Other
ra 283.4409°
decl -54.2797°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14653 SUBJECT: GRB 130515A: VLT acquisition observation DATE: 13/05/15 04:39:26 GMT FROM: Dong Xu at DARK/NBI Dong Xu (DARK/NBI), Andrew J. Levan (Univ. Warwick), Nial R. Tanvir (Univ. Leicester), Daniele Malesani (DARK/NBI), Johan P. U. Fynbo (DARK/NBI), Steve Schulze (PUC and MCSS), report on behalf of the X-shooter GRB GTO collaboration: We observed the field of the short GRB 130515A (Malesani et al., GCN 14650) with the ESO VLT equipped with X-shooter. In a 30-s acquisition image taken in the R band starting at 2:49 UT (1.46 hr after the GRB), we detect a single source S1 consistent with the best currently available XRT position (http://www.swift.ac.uk/xrt_positions/), at coordinates (J2000): (S1) RA = 18:53:45.82 Dec = -54:16:46.9 This source has a magnitude R ~ 21.2, and can be faintly glimpsed in the DSS red. At the present time, we cannot assess its relation to the GRB, though it may be the host galaxy. We also note the presence of two further objects S2 and S3 just outside the XRT error circle, which can also be seen in the DSS, at coordinates: (S1) RA = 18:53:45.26 Dec = -54:16:44.3 (S2) RA = 18:53:46.16 Dec = -54:16:41.1 We acknowledge excellent and prompt support from the observing staff at Paranal, in particular Grant Tremblay.
GCN 14654 table
GRB_name GRB130515A
GCN_number 14654
Detection_method Swift-XRT Det
ra 283.4401°
decl -54.2791°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14654 SUBJECT: GRB 130515A: Enhanced Swift-XRT position DATE: 13/05/15 05:59:47 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 719 s of XRT Photon Counting mode data and 1 UVOT images for GRB 130515A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 283.44011, -54.27906 which is equivalent to: RA (J2000): 18h 53m 45.63s Dec (J2000): -54d 16' 44.6" with an uncertainty of 2.4 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 14655 table
GRB_name GRB130515A
GCN_number 14655
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 14655 SUBJECT: GRB 130515A: GROND Observations DATE: 13/05/15 06:01:37 GMT FROM: Sebastian Schmidl at TLS Tautenburg S. Schmidl, D. A. Kann (both TLS Tautenburg) and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of the short GRB 130515A (Swift trigger 555880; Malesani et al., GCN 14650) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile). Observations started as soon as the position became visible above the pointing limit, at 02:12:08 UT on May 15th, 51 minutes after the BAT trigger. They were performed at an average seeing of 1".6 and at an average airmass of 2.4. Inside the 2".9 SPER XRT error circle (RA = 18:53:45.79, Dec. -54:16:45.2), we detect a faint source, and additionally a significantly brighter, possibly extended source on the western edge of the XRT error circle. We find the following positions (J2000) for these sources: In the error circle: RA = 18:53:45.79, Dec. = -54:16:47.3 On the western edge: RA = 18:53:45.24, Dec. = -54:16:44.5 with an error of 0".5 in each case. Based on an observation with 780 s integration time in g'r'i'z' and 720 s integration time in JHK, centered at 0.043586 days after the trigger, we estimate preliminary magnitudes 3-sigma upper limits (all in AB system) of g' > 23.86, r' = 22.55 +/- 0.15, z' = 21.17 +/- 0.11, J = 19.74 +/- 0.27, H > 19.4 and K > 19.1 for the object inside the error circle, and g' = 22.12 +/- 0.08., r' = 20.68 +/- 0.03., z' = 19.51 +/- 0.03., J = 18.50 +/- 0.09, H = 18.45 +/- 0.14 and K = 18.47 +/- 0.17 for the possible galaxy on the western edge. Given magnitudes are calibrated against GROND zero points (g'r'i'z') as well as 2MASS field stars (JHK) and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.07 mag in the direction of the burst (Schlegel et al. 1998).
GCN 14656 table
GRB_name GRB130515A
GCN_number 14656
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14656 SUBJECT: GRB 130515A: Gemini/GMOS Observations DATE: 13/05/15 06:32:58 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley), A Cucchiara (UCSC), D. Xu (DARK/NBI), and A. J. Levan (U. Warwick) report on behalf of a larger collaboration: We obtained a single 240 s r'-band image of the field of GRB 130515A (Malesani et al., GCN 14650) with the Gemini Multi-Object Spectrograph mounted on the 8 m Gemini South telescope. The observation commenced at 01:59 UT (~ 38 min after the Swift trigger) under poor seeing conditions. We identify the same 3 sources in the vicinity of the XRT error circle as Xu et al. (GCN 14653). For reference, we measure J2000 positions for these sources with respect to nearby point sources from the 2MASS catalog to be: S1: 18:53:45.79, -54:16:47.1 S2: 18:53:45.23, -54: 16:44.4 S3: 18:53:46.13, -54:16:41.2 We have compared photometry from our Gemini images directly with that obtained by the VLT approximately 50 minutes later. For these three point sources, we measure the following change in magnitude (VLT - Gemini): S1: -0.37 +/- 0.18 mag S2: -0.03 +/- 0.10 mag S3: -0.03 +/- 0.10 mag There is this marginal evidence that S1 has brightened between the two epochs. However, we cannot rule out that the discrepancy results from a color difference between the two images (r' vs R). Further observations are planned. [GCN OPS NOTE(15may13): Per author's request, the 14653 reference was corrected to "Xu et al".]
GCN 14658 table
GRB_name GRB130515A
GCN_number 14658
Detection_method Swift-BAT Det
ra 283.4360°
decl -54.2830°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14658 SUBJECT: GRB 130515A: Swift-BAT refined analysis DATE: 13/05/15 11:57:33 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. Malesani (DARK/NBI), D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from recent telemetry downlinks, we report further analysis of BAT GRB 130515A (trigger #555880) (Malesani, et al., GCN Circ. 14650). The BAT ground-calculated position is RA, Dec = 283.436, -54.283 deg, which is RA(J2000) = 18h 53m 44.6s Dec(J2000) = -54d 16' 57.3" with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 69%. The mask-weighted light curve shows two overlapping peaks starting at ~T+0.00, peaking at ~T+0.00 and ~T+0.30, and ending at ~T+0.40 sec. T90 (15-350 keV) is 0.29 +- 0.06 sec (estimated error including systematics). The time-averaged spectrum from T-0.04 to T+0.33 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.77 +- 0.18. The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.35 sec in the 15-150 keV band is 1.4 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/555880/BA/
GCN 14660 table
GRB_name GRB130515A
GCN_number 14660
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14660 SUBJECT: GRB 130515A: Swift/UVOT Upper Limits DATE: 13/05/15 14:16:02 GMT FROM: Samantha Oates at MSSL S. R. Oates (MSSL-UCL), M. De Pasquale (MSSL-UCL) and D. Malesani (DARK/NBI) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 130515A 79 s after the BAT trigger (Malesani et al., GCN Circ. 14650). In the intial UVOT exposures, we do not detect an optical afterglow consistent with the refined XRT position (Beardmore et al. GCN Circ. 14654). We also do not detect an optical source consistent with the positions of s1 and s2 reported by the VLT (Xu et al. GCN Circ. 14653) and Gemini (Cenko et al., GCN Circ. 14656), nor at the positions of the sources reported by GROND (Schmidl et al., GCN Circ. 14655). However, we do marginally detect VLT s3 (Xu et al. GCN Circ. 14653) in white at a magnitude of 21.59 +/- 0.39, which is also observed in the DSS. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures at the refined XRT position are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 79 229 147 >21.2 u_FC 291 541 246 >20.2 white 79 6414 580 >21.7 v 620 5388 236 >19.8 b 546 6209 432 >21.0 u 291 6003 659 >20.7 w1 669 5798 413 >20.7 m2 645 5592 236 >20.0 w2 596 6603 415 >20.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.07 in the direction of the burst (Schlegel et al. 1998).
GCN 14661 table
GRB_name GRB130515A
GCN_number 14661
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14661 SUBJECT: GRB 130515A: Swift-XRT refined Analysis DATE: 13/05/15 16:11:31 GMT FROM: Binbin Zhang at PSU B.-B. Zhang (PSU) and D. Malesani (DARK/NBI) report on behalf of the Swift-XRT team: We have analysed 8.1 ks of XRT data for GRB 130515A (Malesani et al. GCN Circ. 14650), from 82 s to 34.1 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN. Circ 14654). The source is fading with alpha >0.8. If the light curve continues to decay with a power-law decay index of 0.8, the count rate at T+24 hours will be 1.4 x 10^-4 count s^-1 The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00555880. This circular is an official product of the Swift-XRT team. [GCN OPS NOTE(15may13): Per author's request, the ).8" was added to the end of the first line in the 2nd paragraph.]
GCN 14663 table
GRB_name GRB130515A
GCN_number 14663
Detection_method Fermi GBM Det
t_trigger 1:21:17.880 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14663 SUBJECT: GRB 130515A: Fermi GBM detection DATE: 13/05/15 17:16:56 GMT FROM: Peter Jenke at MSFC P. Jenke (UAH) reports on behalf of the Fermi GBM Team: "At 01:21:17.88 UT on May 15 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130515A (trigger 390273680 / 130515056), which was also detected by the Swift/BAT (Malesani et al., GCN Circ. 14650). The GBM on-ground location is consistent with the Swift position. The angle of the Fermi LAT boresight is 120 degrees from the Swift location. The GBM light curve consists of a single pulse with a FRED-like shape with a duration (T90) of about 0.26 s (50-300 keV). The time-averaged spectrum from T0-0.064 s to T0+0.256 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -1.90 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 450 +/- 100 keV. The event fluence (10-1000 keV) in this time interval is (10.4 +/- 0.5)E-07 erg/cm^2. The 0.064-sec peak photon flux measured starting from T0+0.0 s in the 10-1000 keV band is 22 +/- 2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 14667 table
GRB_name GRB130515A
GCN_number 14667
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14667 SUBJECT: GRB 130515A: FORS2 spectroscopy of candidate counterpart DATE: 13/05/16 09:04:17 GMT FROM: Nial Tanvir at U.Leicester A. J. Levan (U. Warwick) and N. R. Tanvir (U. Leicester) report for a larger collaboration: We observed the location of GRB 130515A (Malesani et al. GCN 14650) with VLT/FORS2, beginning at ~03:30 UT, 2 hours after the burst. At this epoch we obtained imaging and spectroscopy of the brightest source in the XRT error box (S1 in Xu et al. GCN 14653 and Cenko et al. GCN 14656). This spectrum exhibits several broad absorption features consistent with an M-dwarf star at z=0, indicating that it is not the host galaxy of GRB 130515A. In fact, preliminary analysis of our imaging suggests that sources S2 and S3 referred to by Xu et al. and Cenko et al. are also consistent with being point-like. The nearest evidently extended, and reasonably bright, source is a galaxy at position 18:53:45.01 -54:16:50.9, approximately 8 arcsec from the current enhanced X-ray position (http://www.swift.ac.uk/xrt_positions/00555880/). We thank the staff at Paranal for their excellent support with these observations.
GCN 14668 table
GRB_name GRB130515A
GCN_number 14668
Detection_method Konus-Wind Det
t_trigger 1:21:20.440 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14668 SUBJECT: Konus-Wind observation of GRB 130515A DATE: 13/05/16 10:01:58 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team report: The short-duration GRB 130515A (Swift-BAT trigger #555880: Malesani et al., GCN 14650, Barthelmy et al., GCN 14658; Fermi-GBM detection: Jenke, GCN 14663) triggered Konus-Wind at T0=04880.440s UT (01:21:20.440) The burst light curve shows a single pulse from ~T0-0.05 s to ~T0-0.2 s, with a total duration of ~0.25s. The K-W light curve of this burst is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB130515_T04880/ As observed by Konus-Wind, the burst had a fluence of (1.1 0.2)x10-6 erg/cm2 and a 16-ms peak flux, measured from T0-0.016 s, of (2.1 0.5)x10-5 erg/cm2 (both in the 20 - 1500 keV energy range). Modelling the K-W 3-channel time-integrated spectrum (from T0-0.064 s to T0+0.192 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = 0.0 0.4, and Ep = 410 90 keV Modelling the K-W 3-channel spectrum at the maximum count rate (from T0-0.064 s to T0) by a power law with exponential cutoff model yields alpha = -0.5 0.4, and Ep = 715 360 keV All the quoted errors are at the 1 sigma confidence level.
GCN 14670 table
GRB_name GRB130515A
GCN_number 14670
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14670 SUBJECT: GRB 130515A: Further Gemini Observations DATE: 13/05/16 23:23:55 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley) and A. Cucchiara (UCSC) report on behalf of a larger collaboration: We re-imaged the field of GRB 130515A (Malesani et al., GCN 14650) with the Gemini Multi-Object Spectrograph mounted on the 8 m Gemini South telescope. Images were obtained in the r' filter beginning at 4:38 UT on 2013 May 16 (~ 1.1 days after the Swift trigger). Comparing with our previous epoch of observations (Cenko et al., GCN 14656), we find no evidence for variability in or around the enhanced XRT error circle (Beardmore et al., GCN 14654). Specifically, we note that the three sources S1, S2, and S3 identified previously (Xu et al., GCN 14653, Schmidl et al., GCN 14655, Levan et al., GCN 14677) all maintain a constant brightness level. Using digital image subtraction, we limit the optical afterglow at the time of our first epoch of observations (~ 38 min after the Swift trigger) to be R > 23.7 mag (calibrated with respect to nearby USNO-B1 point sources). We thank the Gemini staff for the prompt execution of these observations.
GCN 14671 table
GRB_name GRB130515A
GCN_number 14671
Detection_method Swift-BAT Det
ra 283.4408°
decl -54.2797°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14671 SUBJECT: GRB 130515A: IRSF NIR Observation DATE: 13/05/17 08:07:22 GMT FROM: Daisuke Kuroda at OAO/NAOJ Takahiro Nagayama (Nagoya Univ.) and Shogo Nishiyama (NAOJ) on behalf of OISTER collaboration. We observed the field of GRB 130515A (David Palmer, GCN Circular 14650) with the Infrared Survey Facility 1.4m telescope and NIR camera SIRIUS (Nagayama et al., 2003) at Sutherland Observatory in South Africa. The observation was made with the JHKs bands simultaneously from 2013-05-15 01:26 (UT), 5 minutes after the BAT trigger, to 04:41. We have also detected the source detected by VLT (Dong Xu, GCN Circular 14653) and GROND (Sebastian Schmidl, GCN Circular 14650) at RA=18:53:45.79, DEC=-54:16:47.1 (J2000). Preliminary photometry results are as follows All combined images (Total exposure time: 154 min, 2013-05-15 01:26 - 04:41) J = 20.1 $B!^(B 0.2 H = 18.6 $B!^(B 0.2 Ks =18.7 $B!^(B 0.3 First 120 images (Total exposure time: 60 min, 2013-05-15 01:26 - 2:45) J = 19.4 $B!^(B 0.2 H = 18.9 $B!^(B 0.2 Ks: Non detection These magnitudes are in the Vega system and not corrected for Galactic extinction in the direction of the GRB.
GCN 14688 table
GRB_name GRB130515A
GCN_number 14688
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14688 SUBJECT: GRB 130515A: Suzaku WAM observation of the prompt emission DATE: 13/05/21 14:13:58 GMT FROM: Masanori Ohno at Hiroshima U W. Iwakiri(RIKEN), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The short GRB 130515A (Swift/BAT trigger #555880 ; Malesani et al., GCN 14650; Barthelmy et al., GCN 14658; Fermi-GBM detection: Jenke, GCN 14663; Konus-Wind detection : Golenetskii et al., GCN 14668) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at UT 01:21:17.679 (=T0). The observed light curve shows a single peak starting at T0+0.1 s, ending at T0+0.4 s with a duration (T90) of about 0.25 seconds. The fluence in 100 - 1000 keV was 1.48 (+1.67 / -0.99) x 10-6 erg/cm2. The 1-s peak flux measured from T0+0 s was 1.4 (+0.4/-0.8) photons/cm2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0+0 s to T0+0.5 s is well fitted by a single power-law with a photon index of 2.17 (+0.53/-0.36) (chi2/d.o.f = 36.6/25). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html