GRB141130A

This page lists all entries on GRB141130A in GRBweb

Summary IPN Swift GCN 17120 GCN 17121 GCN 17122 GCN 17123 GCN 17125 GCN 17126 GCN 17127 GCN 17130 GCN 17135 GCN 17148

Summary table
Variable Value Source
T0 23:10:56 UTC GCN_circulars,Swift Det
ra 222.8218° Swift
decl 47.3187° Swift
pos_error 5.82e-05° Swift
T90 62.9 s Swift
T90_start 23:10:56 UTC Swift
fluence 2.80e-06 erg/cm² Swift
T100 62.9 s
GBM_located False
mjd 56991.96592592593 GCN_circulars,Swift Det
IPN table
GRB_name GRB141130A
ra 222.8125°
decl 47.3000°
pos_error 5.00e-02°
Swift table
GRB_name GRB141130A
t_trigger 23:10:56 UTC
ra 222.8218°
decl 47.3187°
pos_error 5.82e-05°
T90 62.9 s
fluence 2.80e-06 erg/cm²
GCN 17120 table
GRB_name GRB141130A
GCN_number 17120
Detection_method Swift Det
t_trigger 23:10:56 UTC
ra 222.8140°
decl 47.3000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17120 SUBJECT: GRB 141130A: Swift detection of a burst with an optical counterpart DATE: 14/11/30 23:26:54 GMT FROM: Scott Barthelmy at NASA/GSFC A. Vargas (PSU), S. D. Barthelmy (GSFC), H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 23:10:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 141130A (trigger=620090). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 222.814, +47.300 which is RA(J2000) = 14h 51m 15s Dec(J2000) = +47d 17' 60" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak structure with a duration of about 35 sec. The peak count rate was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 23:12:20.3 UT, 84.3 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 222.8205, 47.3202 which is equivalent to: RA(J2000) = 14h 51m 16.92s Dec(J2000) = +47d 19' 12.7" with an uncertainty of 2.8 arcseconds (radius, 90% containment). This location is 74 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 consistent with the Galactic value of 1.82 x 10^20 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 8.27e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of nominal 150.000 seconds with the White filter starting 93 seconds after the BAT trigger. There is a candidate afterglow in the list of sources generated on-board at RA(J2000) = 14:51:17.28 = 222.82199 DEC(J2000) = +47:19:07.5 = 47.31876 with a 90%-confidence error radius of about 1.10 arc sec. This position is 4.1 arc sec. from the center of the XRT error circle. The estimated magnitude is 18.74. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02. Burst Advocate for this burst is A. Vargas (avargas AT swift.psu.edu). 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 17121 table
GRB_name GRB141130A
GCN_number 17121
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17121 SUBJECT: GRB 141130A: Mondy optical observations DATE: 14/12/01 00:28:33 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich (ISTP), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 141130A (Vargas et al., GCN 17120) with AZT-33IK telescope of Sayan observatory (Mondy) Nov., 30 starting on (UT) 23:15:04, i.e 248 s after burst trigger. In first images of 10 s exposure we clearly detect fading object in coordinates of the OT candidate reported in (Vargas et al., GCN 17120). The object is absent in DSS2 and we thus confirm optical afterglow of GRB 141130A. The afterglow has faded from R = 18.5 +/- 0.14 at 258 s after burst trigger to R = 19.2 +/- 0.2 at 800 s after burst trigger. The photometry is stil preiminary and based on nearby USNO-B1.0 stars.
GCN 17122 table
GRB_name GRB141130A
GCN_number 17122
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17122 SUBJECT: GRB 141130A: Nanshan optical observations DATE: 14/12/01 00:51:28 GMT FROM: Dong Xu at DARK/NBI D. Xu (DARK/NBI), T.-Z. Yang, G.-J. Feng, A. Esamdin, L. Ma (XAO) report: We observed the field of GRB 141130A (Vargas et al., GCN 17120) with the 1m optical telescope located at Nanshan, Xinjiang, China. Observations started at 23:36:49 UT on 2014-10-30 (i.e., 1553 s after the burst) and a series of 120s, 180s, and 360s R-band images were obtained under some clouds. We detect the optical afterglow at the UVOT position with R~19.1 mag at the median time of 1982 s post-burst, calibrated with four nearby SDSS stars (SDSS J145120.41+471920.1, SDSS J145118.89+471810.3, SDSS J145125.69+471701.0, and SDSS J145114.11+471610.1).
GCN 17123 table
GRB_name GRB141130A
GCN_number 17123
Detection_method Swift-XRT Det
ra 222.8216°
decl 47.3185°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17123 SUBJECT: GRB 141130A: Enhanced Swift-XRT position DATE: 14/12/01 02:22:11 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 621 s of XRT Photon Counting mode data and 1 UVOT images for GRB 141130A, 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 = 222.82159, +47.31852 which is equivalent to: RA (J2000): 14h 51m 17.18s Dec (J2000): +47d 19' 06.7" with an uncertainty of 1.9 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 17125 table
GRB_name GRB141130A
GCN_number 17125
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 17125 SUBJECT: GRB 141130A: Swift-XRT refined Analysis DATE: 14/12/01 11:27:05 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA), J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU) and A. Vargas report on behalf of the Swift-XRT team: We have analysed 11 ks of XRT data for GRB 141130A (Vargas et al. GCN Circ. 17120), from 75 s to 28.5 ks after the BAT trigger. The data comprise 327 s in Windowed Timing (WT) mode (the first 6 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 Goad et al. (GCN Circ. 17123). The late-time light curve (from T0+4.9 ks) can be modelled with a power-law decay with a decay index of alpha=1.14 (+0.26, -0.25). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.31 (+0.07, -0.06). The best-fitting absorption column is 1.50 (+0.17, -0.16) x 10^21 cm^-2, in excess of the Galactic value of 1.8 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.13 (+0.25, -0.21) and a best-fitting absorption column of 3.8 (+4.7, -2.0) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.1 x 10^-11 (3.4 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.8 (+4.7, -2.0) x 10^20 cm^-2 Galactic foreground: 1.8 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.13 (+0.25, -0.21) If the light curve continues to decay with a power-law decay index of 1.14, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.5 x 10^-14 (6.2 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00620090. This circular is an official product of the Swift-XRT team.
GCN 17126 table
GRB_name GRB141130A
GCN_number 17126
Detection_method Swift-UVOT Det
ra 222.8218°
decl 47.3187°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17126 SUBJECT: GRB 141130A: Swift/UVOT Detection DATE: 14/12/01 13:26:52 GMT FROM: Paul Kuin at MSSL S. R. Oates (IAA-CSIC/UCL-MSSL) and A. Vargas (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 141130A 95 s after the BAT trigger (Vargas et al., GCN Circ. 17120). A source consistent with the XRT position (Goad et al. GCN Circ. 17123) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 14:51:17.23 = 222.82181 (deg.) Dec (J2000) = +47:19:07.3 = 47.31870 (deg.) with an estimated uncertainty of 0.45 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 95 244 147 18.71 +/- 0.06 v 636 655 19 >17.8 b 562 753 39 >20.1 u 306 556 246 18.85 +/- 0.13 w1 684 704 19 >18.7 w2 611 798 34 >19.0 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). [GCN OPS NOTE(01dec14): Per author's request, the "A" was added to the GRB name.]
GCN 17127 table
GRB_name GRB141130A
GCN_number 17127
Detection_method Swift-BAT Det
ra 222.8040°
decl 47.3230°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17127 SUBJECT: GRB 141130A: Swift-BAT refined analysis DATE: 14/12/01 13:29:51 GMT FROM: Scott Barthelmy at NASA/GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL), A. Vargas (PSU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from recent telemetry downlinks, we report further analysis of BAT GRB 141130A (trigger #620090) (Vargas, et al., GCN Circ. 17120). The BAT ground-calculated position is RA, Dec = 222.804, 47.323 deg which is RA(J2000) = 14h 51m 13.0s Dec(J2000) = +47d 19' 24.3" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 73%. The mask-weighted light curve shows the burst starting at ~T-43 sec, going flat until ~T-10 sec, then peaking at ~T-2 sec, and then returing to baseline ~T+60 sec. T90 (15-350 keV) is 62.9 +- 11.4 sec (estimated error including systematics). The time-averaged spectrum from T-42.75 to T+40.02 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.56 +- 0.08. The fluence in the 15-150 keV band is 2.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-4.69 sec in the 15-150 keV band is 1.2 +- 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/620090/BA/
GCN 17130 table
GRB_name GRB141130A
GCN_number 17130
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17130 SUBJECT: GRB 141130A: Mondy optical light curve DATE: 14/12/01 22:16:19 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich (ISTP), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We report optical light curve of the GRB 141130A (Vargas et al., GCN 17120) based on our observations with AZT-33IK telescope of Sayan observatory (Mondy) on Nov., 30 (Mazaeva et al., GCN 17121). The light curve can be found in http://grb.rssi.ru/GRB141130A/GRB141130A_AZT33IK_lc.png The photometry is based on nearby USNO-B1.0 stars.
GCN 17135 table
GRB_name GRB141130A
GCN_number 17135
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17135 SUBJECT: GRB 141130A: Mondy optical observations DATE: 14/12/04 16:46:27 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Volnova (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich (ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 141130A (Vargas et al., GCN 17120) with AZT-33IK telescope of Sayan observatory (Mondy) Dec., 01 starting on (UT) 21:21:55. We obtained several images in R-filter. In a combined image we do not detect optical afterglow (Vargas et al., GCN 17120; Mazaeva et al., GCN 17121; Xu et al., GCN 17122). Upper limit is based on nearby USNO B1.0 (R2) stars: date UT start t-T0 Filter Exp. OT UL(3 sigma) (mid, days) (s) 2014-12-01 21:21:55 0.95417 R 43*120 n/d 22.1 The finding chart can be found in http://grb.rssi.ru/GRB141130A/GRB141130_20141201_AZT33IK_fc.png
GCN 17148 table
GRB_name GRB141130A
GCN_number 17148
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 17148 SUBJECT: Konus-Wind observation of GRB 141130A DATE: 14/12/08 13:10:46 GMT FROM: Anastasia Tsvetkova at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 141130A (Swift-BAT trigger #620090: Vargas et al., GCN 17120; Lien et al., GCN 17127) was detected by Konus-Wind in the waiting mode. The burst light curve shows a double-peaked structure with a total duration of ~85 s (from ~T0(BAT)-44 s to ~T0(BAT)+41 s). As observed by Konus-Wind, the burst had a fluence of 8.79(-2.39,+2.62)x10^-6 erg/cm2 and a 2.944 s peak flux, measured from ~T0(BAT)-2.725 s, of 2.40(-0.82,+0.87)x10^-7 erg/cm2/s (both estimated in the 20 keV - 10 MeV energy range). Modeling the KW 3-channel time-integrated spectrum (from T0(BAT)-43.941 s to T0(BAT)+41.435 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha =-1.49 ± 0.18, and Ep =307(-108,+467) keV. The K-W light curve of this burst is available at http://www.ioffe.ru/LEA/GRBs/GRB141130A/ All the quoted errors are at 1 sigma confidence level. All the quoted values are preliminary.