GRB120514A

This page lists all entries on GRB120514A in GRBweb

Summary IPN Swift GCN 13289 GCN 13290 GCN 13291 GCN 13292 GCN 13293 GCN 13294 GCN 13296 GCN 13297 GCN 13298 GCN 13301

Summary table
Variable Value Source
T0 1:12:49 UTC GCN_circulars,Swift Det
ra 283.0007° Swift
decl -4.2636° Swift
pos_error 1.94e-04° Swift
T90 164.4 s Swift
T90_start 1:12:49 UTC Swift
fluence 2.80e-06 erg/cm² Swift
T100 164.4 s
GBM_located False
mjd 56061.05056712963 GCN_circulars,Swift Det
IPN table
GRB_name GRB120514A
ra 282.9917°
decl -4.2500°
pos_error 5.00e-02°
Swift table
GRB_name GRB120514A
t_trigger 1:12:49 UTC
ra 283.0007°
decl -4.2636°
pos_error 1.94e-04°
T90 164.4 s
fluence 2.80e-06 erg/cm²
GCN 13289 table
GRB_name GRB120514A
GCN_number 13289
Detection_method Swift Det
t_trigger 1:12:49 UTC
ra 282.9910°
decl -4.2520°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13289 SUBJECT: GRB 120514A: Swift detection of a burst DATE: 12/05/14 01:32:44 GMT FROM: David Palmer at LANL V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU) and B.-B. Zhang (PSU) report on behalf of the Swift Team: At 01:12:49 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 120514A (trigger=522197). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 282.991, -4.252 which is RA(J2000) = 18h 51m 58s Dec(J2000) = -04d 15' 06" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure consisting of two overlapping peaks with a duration of about 80 sec and an additional weaker peak at ~T+150 sec coincident with a peak observed by the XRT. The peak count rate was ~2500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 01:14:31.2 UT, 101.3 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 282.99969, -4.26375 which is equivalent to: RA(J2000) = 18h 51m 59.93s Dec(J2000) = -04d 15' 49.5" with an uncertainty of 4.0 arcseconds (radius, 90% containment). This location is 52 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (6.09 x 10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.4 (+1.29/-0.95) x 10^22 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 3.94e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 110 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. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the large, but uncertain extinction expected. We note that this source is 2 degrees from the Galactic plane. Although the BAT lightcurve and energy distribution is typical for a GRB, the possibility of this being a Galactic source will have to be assessed from further observations. Burst Advocate for this burst is V. Mangano (vanessa AT ifc.inaf.it). 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 13290 table
GRB_name GRB120514A
GCN_number 13290
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 13290 SUBJECT: GRB 120514A: TAROT Calern observatory optical observations DATE: 12/05/14 01:55:14 GMT FROM: Alain Klotz at CESR-CNRS GRB 120514A: TAROT Calern observatory optical observations ---------------------------------------------------------------------- Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR), Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report: We imaged the field of GRB 120514A detected by SWIFT (trigger 522197) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 534s after the GRB trigger. The elevation of the field increased from 37 degrees above horizon and weather conditions were good. We co-added a series of exposures. We do not detect any OT in the XRT error box with a limiting magnitude of: t0+534s to t0+909s : R > 18.1 Galactic coordinates are lon= 29.2060 lat= -2.0542 and the galactic extinction in R band is 4.3 magnitudes estimated from D. Schlegel et al. 1998ApJ...500..525S. Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. This message may be cited.
GCN 13291 table
GRB_name GRB120514A
GCN_number 13291
Detection_method Swift-BAT Det
ra 283.0020°
decl -4.2580°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13291 SUBJECT: GRB 120514A: Swift-BAT refined analysis DATE: 12/05/14 04:22:25 GMT FROM: Scott Barthelmy at NASA/GSFC W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), 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-239 to T+721 sec from the recent telemetry downlink, we report further analysis of BAT GRB 120514A (trigger #522197) (Mangano, et al., GCN Circ. 13289). The BAT ground-calculated position is RA, Dec = 283.002, -4.258 deg which is RA(J2000) = 18h 52m 00.4s Dec(J2000) = -04d 15' 28.6" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 61%. The mask-weighted light curve shows 3 main peaks. The first starts at ~T-40 sec, and peaks at ~T+1 sec. The second overlaps the tail of the first and peaks at ~T+52 and ends at ~T+115 sec. The third peak starts at ~T+120 sec, peaks at ~T+150 sec and ends at ~T+200 sec. At the 2-sigma level, there is possible precursor emission from ~T-160 to T-80 sec, and a possible forth peak from ~T+260 to ~T+420 sec. T90 (15-350 keV) is 164.4 +- 5.8 sec (estimated error including systematics). The time-averaged spectrum from T-8.75 to T+165.55 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.62 +- 0.10. The fluence in the 15-150 keV band is 2.8 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.22 sec in the 15-150 keV band is 1.9 +- 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/522197/BA/
GCN 13292 table
GRB_name GRB120514A
GCN_number 13292
Detection_method Swift-XRT Det
ra 283.0008°
decl -4.2636°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13292 SUBJECT: GRB 120514A: Enhanced Swift-XRT position DATE: 12/05/14 04:34:05 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 932 s of XRT Photon Counting mode data and 2 UVOT images for GRB 120514A, 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 = 283.00078, -4.26359 which is equivalent to: RA (J2000): 18h 52m 0.19s Dec (J2000): -04d 15' 48.9" with an uncertainty of 1.8 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 13293 table
GRB_name GRB120514A
GCN_number 13293
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13293 SUBJECT: GRB 120514A: APEX observations of the submm counterpart DATE: 12/05/14 12:11:51 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. de Breuck, T. Stanke, C. Agurto (ESO), M. Valencia-S. (U. Koeln), A. Remy (CEA-Saclay), F. Montenegro (ESO), J. Gorosabel, R. Sanchez-Ramirez (IAA-CSIC), J.P.U. Fynbo (DARK/NBI) report on behalf of a larger collaboration: We have observed the field of GRB 120514A (Mangano et al. GCNC 13289) using LABOCA/APEX at Chajnantor (Chile) in the 870 micrometer band. The weather conditions were good, with precipitable water vapour at the time of the observation of ~0.5mm. Observations began on May 14 at 4:55 UT (3.7 hr after the burst) and were performed using the photometric mode, centred at the enhanced X-ray position (Evans et al. GCNC 13292). On a preliminary analysis of 160 min on source, we detect a flux density at the position of the afterglow of 6.2+/-2.3 mJy. Further observations are foreseen. We encourage follow-up observations in other wavelengths.
GCN 13294 table
GRB_name GRB120514A
GCN_number 13294
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13294 SUBJECT: GRB 120514A: Swift-XRT refined Analysis DATE: 12/05/14 13:32:06 GMT FROM: Phil Evans at U of Leicester G. Stratta (ASDC), P. D'Avanzo (INAF-OAB), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC) and V. Mangano report on behalf of the Swift-XRT team: We have analysed 6.5 ks of XRT data for GRB 120514A (Mangano et al. GCN Circ. 13289), from 90 s to 28.8 ks after the BAT trigger. The data comprise 132 s in Windowed Timing (WT) mode (the first 10 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN. Circ 13292). The late-time light curve (from T0+4.4 ks) can be modelled with a power-law decay with a decay index of alpha=1.22 (+0.29, -0.24). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.90 (+0.12, -0.11). The best-fitting absorption column is 1.68 (+0.15, -0.14) x 10^22 cm^-2, in excess of the Galactic value of 6.1 x 10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.2 (+/-0.3) and a best-fitting absorption column of 2.4 (+0.5, -0.4) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 6.8 x 10^-11 (2.3 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.4 (+0.5, -0.4) x 10^22 cm^-2 Galactic foreground: 6.1 x 10^21 cm^-2 Excess significance: 6.6 sigma Photon index: 2.2 (+/-0.3) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00522197. This circular is an official product of the Swift-XRT team.
GCN 13296 table
GRB_name GRB120514A
GCN_number 13296
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13296 SUBJECT: GRB 120514A: UKIRT IR observations DATE: 12/05/14 16:38:51 GMT FROM: Andrew Levan at U.of Leicester A.J Levan (Warwick), N.R. Tanvir, K. Wiersema (Leicester), T. Wold (JAC) report on behalf of a larger collaboration: "We obtained K-band observations of GRB 120514A (Mangano et al. GCN 13289) with the United Kingdom Infrared Telescope (UKIRT) on Mauna Kea, with a midpoint approximately 12 hours after the initial burst detection. Comparison of a preliminary reduction of these images with archival images taken as part of the UKIRT Galactic Plane Survey (GPS; Lucas et al. 2008 MNRAS 391 136) does not reveal any new sources within the refined XRT position (Evans et al. GCN 13292). Given the crowded nature of the field we do note there are several sources whose location is formally consistent with the X-ray position, but none of these show clear evidence for variability between the two epochs."
GCN 13297 table
GRB_name GRB120514A
GCN_number 13297
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13297 SUBJECT: GRB 120514A: Swift/UVOT Upper Limits DATE: 12/05/14 16:42:24 GMT FROM: Erik Hoversten at Swift/Penn State E. A. Hoversten (PSU) and V. Mangano (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 120514A 110 s after the BAT trigger (Mangano et al., GCN Circ. 13289). No optical afterglow consistent with the enhanced XRT position (Evans et al., GCN Circ. 13292) is detected in the initial UVOT exposures. 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 are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 110 260 147 >20.6 u_FC 324 574 246 >20.5 white 110 1029 295 >20.9 u 324 574 246 >20.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 1.63 in the direction of the burst (Schlegel et al. 1998).
GCN 13298 table
GRB_name GRB120514A
GCN_number 13298
Detection_method GROND
ra 283.0004°
decl -4.2641°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13298 SUBJECT: GRB 120514A: GROND upper limits DATE: 12/05/14 16:45:37 GMT FROM: Vladimir Sudilovsky at MPE A. Nicuesa Guelbenzu (TLS Tautenburg), S. Schmidl (TLS Tautenburg), V. Sudilovsky (MPE Garching), and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 120514A (Mangano et al., GCN #13289) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile). Observation started at 03:39 UT, 2.4 h after the trigger and ended at 11:10 UT. We detect two sources just outside of the enhanced 1.8" XRT error circle at RA,DEC 18:52:00.1, -04:15:50.8 and 18:52:00.2, -04:15:46.8 with a positional uncertainty of +/- 0.3". We note that neither source varies in r' brightness relative to USNO field stars over a period of 2 hours. Additionally, the southern source exhibits a thermal spectrum. Therefore, neither of these two sources are likely associated with the GRB. Based on exposures of 1480 seconds in g'r'i'z' and 1200 seconds in JHK, we do not detect a source within the 1.8" XRT error circle of the X-ray counterpart candidate (Evans et al., GCN #13292) to the following 3-sigma upper limits (AB system): g' > 22.7, r' > 23.0 i' > 23.0 z' > 23.0 J > 20.5 H > 19.6 K > 18.5 These magnitudes are calibrated against GROND zeropoints (g'r'i'z') and 2MASS (JHK) and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=1.7 mag in the direction of the burst (Schlegel et al. 1998).
GCN 13301 table
GRB_name GRB120514A
GCN_number 13301
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 13301 SUBJECT: GRB 120514A : Suzaku WAM observation of the prompt emission DATE: 12/05/21 03:08:04 GMT FROM: Norisuke Ohmori at Miyazaki U M. Akiyama, N. Ohmori, M. Yamauchi (Univ. of Miyazaki), K. Yamaoka, Y. E. Nakagawa (Waseda U.), W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto, H. Ueno (Saitama U.), Y. Hanabata, T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, M. Ohno, Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The long GRB 120514A (Swift/BAT trigger #522197 ; Siegel et al., GCN 13289) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 01:12:43.252 UT (=T0). The observed light curve shows a single peak starting at T0-2 s, ending at T0+16 s, with a duration (T90) of about 14 seconds. The fluence in 100 - 1000 keV was 1.62(-0.69, +0.50) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0 s was 0.71(-0.20, +0.18) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-2 s to T0+16 s is well fitted by a single power-law with a photon index of 2.30 (-0.54, 0.75) (chi^2/d.o.f = 43.1/32). 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 now available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html