GRB190511A

This page lists all entries on GRB190511A in GRBweb

Summary Fermi GBM IPN Swift GCN 24471 GCN 24472 GCN 24481 GCN 24482 GCN 24483 GCN 24492 GCN 24494 GCN 24498 GCN 24499 GCN 24502 GCN 24534 GCN 24587

Summary table
Variable Value Source
GRB_name_Fermi GRB190511302
T0 7:14:24 UTC GCN_circulars,Fermi GBM final loc
ra 126.4435° Swift
decl -20.2593° Swift
pos_error 5.44e-05° Swift
T90 27.648 s Fermi_GBM
T90_error 1.145 s Fermi_GBM
T90_start 7:14:26.918 UTC Fermi_GBM
fluence 2.10e-05 erg/cm² Fermi_GBM
fluence_error 8.39e-08 erg/cm² Fermi_GBM
T100 51.7 s
GBM_located False
mjd 58614.301666666666 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB190511302
trigger_name bn190511302
ra 126.4450°
decl -20.2597°
pos_error 2.49e+00°
datum 2019-05-11
t_trigger 7:14:24.358 UTC
T90 27.648 s
T90_error 1.145 s
T90_start 7:14:26.918 UTC
fluence 2.10e-05 erg/cm²
fluence_error 8.39e-08 erg/cm²
flux_1024 1.42e+01 erg/cm²/s
flux_1024_error 4.13e-01 erg/cm²/s
flux_1024_time 2.42e+01 erg/cm²/s
flux_64 1.75e+01 erg/cm²/s
flux_64_error 1.78e+00 erg/cm²/s
IPN table
GRB_name GRB190511A
ra 126.4375°
decl -20.2333°
pos_error 5.00e-02°
Swift table
GRB_name GRB190511A
t_trigger 7:14:48 UTC
ra 126.4435°
decl -20.2593°
pos_error 5.44e-05°
T90 27.7 s
fluence 7.40e-06 erg/cm²
GCN 24471 table
GRB_name GRB190511A
GCN_number 24471
Detection_method Fermi GBM final loc
t_trigger 7:14:24 UTC
ra 123.8000°
decl -24.3000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24471 SUBJECT: GRB 190511A: Fermi GBM Final Real-time Localization DATE: 19/05/11 07:25:58 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 07:14:24 UT on 11 May 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190511A (trigger 579251669.35821 / 190511302). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 123.8, Dec = -24.3 (J2000 degrees, equivalent to J2000 08h 15m, -24d 18'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 19.0 degrees. The skymap can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190511302/quicklook/glg_skymap_all_bn190511302.png The HEALPix FITS file, including the estimated localization systematic, can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190511302/quicklook/glg_healpix_all_bn190511302.fit The GBM light curve can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190511302/quicklook/glg_lc_medres34_bn190511302.gif
GCN 24472 table
GRB_name GRB190511A
GCN_number 24472
Detection_method Swift Det
t_trigger 7:14:48 UTC
ra 126.4360°
decl -20.2420°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24472 SUBJECT: GRB 190511A: Swift detection of a burst DATE: 19/05/11 07:42:00 GMT FROM: Boris Sbarufatti at PSU M. G. Bernardini (INAF-OAB), H. A. Krimm (NSF/USRA), N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester), B. Sbarufatti (PSU) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 07:14:48 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190511A (trigger=903158). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 126.436, -20.242 which is RA(J2000) = 08h 25m 45s Dec(J2000) = -20d 14' 30" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 20 sec. The peak count rate was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 07:16:51.2 UT, 122.9 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 126.44482, -20.25978 which is equivalent to: RA(J2000) = 08h 25m 46.76s Dec(J2000) = -20d 15' 35.2" with an uncertainty of 3.9 arcseconds (radius, 90% containment). This location is 70 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. No spectrum from the promptly downlinked event data is yet available to determine the column density. The initial flux in the 2.5 s image was 9.43e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 95 seconds with the U filter starting 290 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 19.2 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 18.0 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.09. Burst Advocate for this burst is M. G. Bernardini (grazia.bernardini AT brera.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/)
GCN 24481 table
GRB_name GRB190511A
GCN_number 24481
Detection_method Swift-XRT Det
ra 126.4443°
decl -20.2594°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24481 SUBJECT: GRB 190511A: Enhanced Swift-XRT position DATE: 19/05/11 12:08:39 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 411 s of XRT Photon Counting mode data and 2 UVOT images for GRB 190511A, 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 = 126.44426, -20.25935 which is equivalent to: RA (J2000): 08h 25m 46.62s Dec (J2000): -20d 15' 33.7" with an uncertainty of 2.0 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 24482 table
GRB_name GRB190511A
GCN_number 24482
Detection_method Fermi GBM Det
t_trigger 7:14:24.360 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 24482 SUBJECT: GRB 190511A: Fermi GBM observation DATE: 19/05/11 12:43:21 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 07:14:24.36 UT on 11 May 2019, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 190511A (trigger 579251669 / 190511302), which was also detected by the Swift/BAT (Bernardiniet al. 2019, GCN 24472) The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 23.7 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of a multipeaked emission episode with a duration (T90) of about 28 s (50-300 keV). The time-averaged spectrum from T0-2.048 s to T0+31.745 s is best fit by a Band function with Epeak = 147.8 +/- 7.2 keV, alpha = -0.58 +/- 0.05, and beta = -2.4 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (2.21 +/- 0.05)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+24.1924 s in the 10-1000 keV band is 14.2 +/- 0.4 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 24483 table
GRB_name GRB190511A
GCN_number 24483
Detection_method Fermi LAT Det
t_trigger 7:14:24.360 UTC
ra 126.3600°
decl -20.2500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24483 SUBJECT: GRB 190511A: Fermi-LAT detection DATE: 19/05/11 13:15:11 GMT FROM: Magnus Axelsson at Stockholm U. M. Axelsson (KTH and Stockholm Univ.), F. Longo (Univ. and INFN Trieste), M. Arimoto (Kanazawa Univ.) and F. Dirirsa (Univ. of Johannesburg) report on behalf of the Fermi-LAT team: On May 11, 2019, Fermi-LAT detected high-energy emission from GRB 190511A, which was also detected by Fermi-GBM (trigger 579251669 / 190511302; GCN 24482) and Swift (GCNs 24472 and 24481). The best LAT on-ground location is found to be RA, Dec 126.36, -20.25 (degrees, J2000) with an error radius of 0.2 deg (90% containment, statistical error only). This was 24 deg from the LAT boresight at the time of the GBM trigger: T0 = 07:14:24.36 UT. The data from the Fermi-LAT show a significant increase in the event rate after the GBM trigger that is spatially correlated with the GBM emission with high significance and consistent with the Swift location. The photon flux above 100 MeV in the time interval 0-1400s after the GBM trigger is 3.6e-6 ph/cm2/s. The estimated photon index above 100 MeV is -2.0 +/- 0.2. The Fermi-LAT point of contact for this burst is Feraol Dirirsa (fdirirsa@uj.ac.za). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 24492 table
GRB_name GRB190511A
GCN_number 24492
Detection_method Optical
ra 126.4436°
decl -20.2593°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24492 SUBJECT: GRB 190511A: NOT optical afterglow DATE: 19/05/11 22:13:23 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst Daniele B. Malesani (DAWN/NBI and DARK/NBI), Dong Xu (NAOC/CAS), Joonas Viuho (NOT and DAWN/NBI) report on behalf of a larger collaboration: We observed the field of the Swift and Fermi GRB 190511A (Bernardini et al., GCN 24472; von Kienlin, GCN 24482; Axelsson et al., GCN 24483) using the Nordic Optical Telescope (NOT) equipped with the AlFOSC camera. Observations started in twilight and were carried out at high airmass due to the poor target visibility. Just outside the enhanced XRT error position (Goad et al., GCN 24481), we clearly detect a source not visible in the archival Pan-STARRS images of the same area, which we suggest to be the optical afterglow of GRB 190511A. Its coordinates are (J2000): RA = 08:25:46.46 Dec = -20:15:33.4 Using nearby stars from the Pan-STARRS survey as calibrators, we measure for the afterglow a magnitude r = 20.89 +- 0.09 AB, at a mean epoch May 11.8648 UT (13.51 hr after the trigger).
GCN 24494 table
GRB_name GRB190511A
GCN_number 24494
Detection_method Swift-UVOT Det
ra 126.4435°
decl -20.2593°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24494 SUBJECT: GRB 190511A: Swift/UVOT Detection DATE: 19/05/11 23:50:25 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL), M. de Pasquale (U. of Istanbul) and M. G. Bernardini (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190511A 131 s after the BAT trigger (Bernardini et al., GCN Circ. 24472). A source consistent with the XRT position (Goad et al. GCN Circ. 24481) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 08:25:46.44 = 126.44350 (deg.) Dec (J2000) = -20:15:33.6 = -20.25933 (deg.) with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence). There is a catalogued star at a distance of 1.3 arcsec. The extrapolated brightness using the SED from the Vizier photometry tool ( http://cdsportal.u-strasbg.fr/gadgets/ifr?url=http://cdsportal.unistra.fr/widgets/SED_plotter.xml&SED_plot_object=126.442680%2C%20-20.259685&SED_plot_radius=2 ) shows a brightness consistent with that of the white count rate seen at several ks after the trigger. We subtract here therefore the late time count rate in the following preliminary UVOT photometry of this GRB, knowing that this has to be refined using truely late time data. Where we did not have a late time measurement yet available, the photometry will be reported in due time. 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 131 281 147 16.0 +/- 0.1 b 5684 5884 197 21.6 +/- 0.3 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998). The afterglow was also discovered by NOT (Malasani et al. GCN Circ. 24492).
GCN 24498 table
GRB_name GRB190511A
GCN_number 24498
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24498 SUBJECT: GRB 190511A: Swift-XRT refined Analysis DATE: 19/05/12 07:42:36 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M.G. Bernadini (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester) and M.G. Bernardini report on behalf of the Swift-XRT team: We have analysed 4.0 ks of XRT data for GRB 190511A (Bernardini et al. GCN Circ. 24472), from 129 s to 46.3 ks after the BAT trigger. The data comprise 188 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 24481). The light curve can be modelled with a power-law decay with a decay index of alpha=1.177 (+0.031, -0.028). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.07 (+0.08, -0.07). The best-fitting absorption column is consistent with the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.12 (+0.24, -0.23) and a best-fitting absorption column of 1.6 (+0.7, -0.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.6 (+0.7, -0.5) x 10^21 cm^-2 Galactic foreground: 1.1 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 2.12 (+0.24, -0.23) If the light curve continues to decay with a power-law decay index of 1.177, the count rate at T+24 hours will be 9.3 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x 10^-13 (4.2 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00903158. This circular is an official product of the Swift-XRT team.
GCN 24499 table
GRB_name GRB190511A
GCN_number 24499
Detection_method Fermi LAT Det
t_trigger 7:14:24.360 UTC
ra 126.3600°
decl -20.2500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24499 SUBJECT: GRB 190511A: en DATE: 19/05/12 10:18:31 GMT FROM: Alberto J. Castro-Tirado at IAA-CSIC Hola Alberto, Han encontrado la contrapartida de este GRB, en coordenadas: RA = 08:25:46.46 Dec = -20:15:33.4 estando en mag. 20 13 h después, con lo que tuvo que ser bastante brillante. Como fue a las 07:14:24.36 UT del 11 de mayo, igual lo tenemos desde B3 (N. Zelanda). Si la cúpula estaba abierta y hacía buen tiempo, claro. Un abrazo desde Nanjing, Alberto El 2019-05-11 21:15, GCN Circulars escribió: > TITLE: GCN CIRCULAR > NUMBER: 24483 > SUBJECT: GRB 190511A: Fermi-LAT detection > DATE: 19/05/11 13:15:11 GMT > FROM: Magnus Axelsson at Stockholm U. > > M. Axelsson (KTH and Stockholm Univ.), F. Longo (Univ. and INFN > Trieste), M. Arimoto (Kanazawa Univ.) and F. Dirirsa (Univ. of > Johannesburg) report on behalf of the Fermi-LAT team: > > On May 11, 2019, Fermi-LAT detected high-energy emission from GRB > 190511A, which was also detected by Fermi-GBM (trigger 579251669 / > 190511302; GCN 24482) and Swift (GCNs 24472 and 24481). > > The best LAT on-ground location is found to be > > RA, Dec 126.36, -20.25 (degrees, J2000) > > with an error radius of 0.2 deg (90% containment, statistical error > only). > This was 24 deg from the LAT boresight at the time of the GBM trigger: > > T0 = 07:14:24.36 UT. > > The data from the Fermi-LAT show a significant increase in the event > rate after the GBM trigger that is spatially correlated with the GBM > emission with high significance and consistent with the Swift > location. > > The photon flux above 100 MeV in the time interval 0-1400s after the > GBM trigger is 3.6e-6 ph/cm2/s. > > The estimated photon index above 100 MeV is -2.0 +/- 0.2. > > The Fermi-LAT point of contact for this burst is Feraol Dirirsa > (fdirirsa@uj.ac.za). > > The Fermi-LAT is a pair conversion telescope designed to cover the > energy band from 20 MeV to greater than 300 GeV. It is the product of > an international collaboration between NASA and DOE in the U.S. and > many scientific institutions across France, Italy, Japan and Sweden.
GCN 24502 table
GRB_name GRB190511A
GCN_number 24502
Detection_method Swift-BAT Det
ra 126.4430°
decl -20.2520°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24502 SUBJECT: GRB 190511A: Swift-BAT refined analysis DATE: 19/05/12 16:15:20 GMT FROM: Hans Krimm at NSF/NASA-GSFC S. D. Barthelmy (GSFC), M. G. Bernardini (INAF-OAB), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 190511Atrigger #903158) (Bernardini, et al., GCN Circ. 24472). The BAT ground-calculated position is RA, Dec = 126.443, -20.252 deg which is RA(J2000) = 08h 25m 46.2s Dec(J2000) = -20d 15' 05.6" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 9%. The mask-weighted light curve shows a complex, multi-peaked structure, starting at about T-25 sec, peaking at T+0 sec and declining to background by T+10 sec. The spacecraft slewed away from the burst position by T+475 sec. T90 (15-350 keV) is 27.7 +- 2.4 sec (estimated error including systematics). The time-averaged spectrum from T-24.27 to T+6.88 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.19 +- 0.10. The fluence in the 15-150 keV band is 7.4 +- 0.5 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.36 sec in the 15-150 keV band is 6.2 +- 1.2 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/903158/BA/
GCN 24534 table
GRB_name GRB190511A
GCN_number 24534
Detection_method Konus-Wind Det
t_trigger 7:14:27.524 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 24534 SUBJECT: Konus-Wind observation of GRB 190511A DATE: 19/05/14 10:00:01 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 190511A (Swift-BAT detection: Bernardini et al., GCN Circ. 24472, Barthelmy et al., GCN Circ. 24502; Fermi-GBM observation: Kienlin et al., GCN Circ. 24482; Fermi-LAT detection: Axelsson et al., GCN Circ. 24483) triggered Konus-Wind at T0=26067.524 s UT (07:14:27.524). The burst light curve shows a multipeaked structure which started at ~T0-2.6 s and had a total duration of ~31.8 s. The emission is seen up to ~2 MeV. As observed by Konus-Wind, the burst had a fluence of 1.93(-0.11,+0.12)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+21.936 s, of 3.81(-0.90,+0.91)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+33.024 s) is best fit 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 = -0.69(-0.16,+0.17) and Ep = 185(-15,+18) keV (chi2 = 49/58 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.4 (chi2 = 48/57 dof) The spectrum near the maximum count rate (measured from T0+16.640 to T0+24.832 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model with alpha = -0.52(-0.23,+0.26) and Ep = 193(-20,+26) keV (chi2 = 53/58 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.0 (chi2 = 53/57 dof) The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB190511_T26067/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 24587 table
GRB_name GRB190511A
GCN_number 24587
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24587 SUBJECT: GRB 190511A: Swift/UVOT further analysis DATE: 19/05/17 20:15:07 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and M. G. Bernardini (INAF-OAB) report on behalf of the Swift/UVOT team: In GCN Circ. 24494 (Kuin and Bernardini) we described how we detect the afterglow of the GRB, but that the photometry was affected by an object located at a distance of 1.3 arcsec. Further Swift observations show that the uv-optical afterglow was no longer detected in white beyond 26ks after the trigger. Data that were taken after that time are considered template observations that provide the background contribution to the photometry. The template net corrected count rates, with instrumental effects removed, are found to be as follows for a 3" radius circular aperture at the location of the GRB as reported in GCN 24494: White = 1.066 +/- 0.031 c/s; u = 0.149 +/- 0.016 c/s; b = 0.509 +/- 0.061 c/s; uvw2 = 0.011 +/- 0.011 c/s; v = 0.272 +/- 0.042 c/s; while uvm2 and uvw1 were not observed until after the afterglow became too faint. After removal of the template contribution, the following preliminary detections and 3-sigma upper limits were determined from the count rates using the zeropoints in the UVOT photometric system (Poole et al. 2008, MNRAS 383, 627; Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the image mode exposures: Filter T_start(s) T_stop(s) Exp(s) Mag white 131 281 147 15.96 +/- 0.05 u 290 385 93 19.62 +/- 0.42 b 5684 5884 197 > 20.13 white 5888 6088 197 20.61 +/- 0.37 uvw2 6094 11850 518 > 17.81 v 17150 17450 300 > 19.35 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998).