GRB081203A

This page lists all entries on GRB081203A in GRBweb

Summary IPN Swift GCN 8595 GCN 8596 GCN 8598 GCN 8599 GCN 8600 GCN 8601 GCN 8603 GCN 8604 GCN 8609 GCN 8611 GCN 8613 GCN 8615 GCN 8617 GCN 8618 GCN 8619 GCN 8623 GCN 8629 GCN 8632 GCN 8645 GCN 8685 GCN 8695

Summary table
Variable Value Source
T0 13:51:30.368 UTC GCN_circulars,Konus-Wind Det
ra 233.0316° Swift
decl 63.5208° Swift
pos_error 6.47e-05° Swift
T90 294.0 s Swift
T90_start 13:57:11 UTC Swift
fluence 7.70e-06 erg/cm² Swift
redshift 2.0750
T100 634.632 s
GBM_located False
mjd 54803.57743481481 GCN_circulars,Konus-Wind Det
IPN table
GRB_name GRB081203A
ra 233.0333°
decl 63.5000°
pos_error 5.00e-02°
redshift 2.0500
Swift table
GRB_name GRB081203A
t_trigger 13:57:11 UTC
ra 233.0316°
decl 63.5208°
pos_error 6.47e-05°
T90 294.0 s
fluence 7.70e-06 erg/cm²
redshift 2.1000
GCN 8595 table
GRB_name GRB081203A
GCN_number 8595
Detection_method Swift Det
t_trigger 13:57:11 UTC
ra 233.0330°
decl 63.4980°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8595 SUBJECT: GRB 081203: Swift detection of a burst with a bright optical counterpart DATE: 08/12/03 14:09:33 GMT FROM: Scott Barthelmy at NASA/GSFC A. M. Parsons (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), P.A. Curran (MSSL-UCL), P. A. Evans (U Leicester), O. Godet (U Leicester), C. Gronwall (PSU), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), V. La Parola (INAF-IASFPA), V. Mangano (INAF-IASFPA), J. Mao (INAF-OAB), R. Margutti (Univ Bicocca&OAB), F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester), C. Pagani (PSU), K. L. Page (U Leicester), B. Preger (ASDC), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-IASFPA), R. L. C. Starling (U Leicester), E. Troja (INAF-IASFPA), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 13:57:11 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 081203 (trigger=336489). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 233.033, +63.498 which is RA(J2000) = 15h 32m 08s Dec(J2000) = +63d 29' 54" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a two peak structure with a duration of about 70 sec. The peak count rate was ~4000 counts/sec (15-350 keV), at ~32 sec after the trigger. The XRT began observing the field at 13:58:34.7 UT, 83.1 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 233.0316, +63.5207 which is equivalent to: RA(J2000) = 15h 32m 07.58s Dec(J2000) = +63d 31' 14.5" with an uncertainty of 5.9 arcseconds (radius, 90% containment). This location is 81 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. UVOT took a finding chart exposure of 150 seconds with the White filter starting 92 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 15:32:07.58 = 233.03158 DEC(J2000) = +63:31:14.9 = 63.52081 with a 90%-confidence error radius of about 0.74 arc sec. This position is 0.4 arc sec. from the center of the XRT error circle. The estimated magnitude is 14.55 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02. Burst Advocate for this burst is A. M. Parsons (parsons AT milkyway.gsfc.nasa.gov). 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 8596 table
GRB_name GRB081203A
GCN_number 8596
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8596 SUBJECT: GRB081203: optical observation DATE: 08/12/03 15:01:11 GMT FROM: Alexei Pozanenko at IKI, Moscow M. Andreev, A. Sergeev, (Terskol Branch of Institute of Astronomy), Ju. Babina (CrAO) A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the field of GRB 081203 detected by SWIFT ( with the Z-600 telescope of Mt. Terskol observatory. A few first unfiltered images confirm the presence bright afterglow detected by UVOT Parsons et al, GCN Parsons) in coordinates (J2000) 15 32 07.75 +63 31 15.04. A preliminary photometry at Dec.03 (UT) 14:29:30 against USNO-A2.0 (R) is 14.9 mag. Observation is continuing.
GCN 8598 table
GRB_name GRB081203A
GCN_number 8598
Detection_method Swift-XRT Det
ra 233.0327°
decl 63.5207°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8598 SUBJECT: GRB 081203: Enhanced Swift-XRT position DATE: 08/12/03 18:31:36 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 2654 s of XRT Photon Counting mode data and 4 UVOT images for GRB 081203, 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 = 233.0327, +63.5207 which is equivalent to: RA (J2000): 15h 32m 7.84s Dec (J2000): +63d 31' 14.4" with an uncertainty of 1.7 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 http://www.swift.ac.uk/xrt_positions/Goad.pdf), the current algorithm is an extension of this method. This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 8599 table
GRB_name GRB081203A
GCN_number 8599
Detection_method Swift-BAT Det
ra 233.0710°
decl 63.5140°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8599 SUBJECT: GRB 081203A: Swift-BAT refined analysis DATE: 08/12/03 18:41:04 GMT FROM: Scott Barthelmy at NASA/GSFC T. N. Ukwatta (GWU), 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), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC) (i.e. the Swift-BAT team): Using the data set from T-240 to T+482 sec from recent telemetry downlinks, we report further analysis of BAT GRB 081203A (trigger #336489) (Parsons, et al., GCN Circ. 8595). The BAT ground-calculated position is RA, Dec = 233.071, 63.514 deg, which is RA(J2000) = 15h 32m 16.9s Dec(J2000) = +63d 30' 50.2" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 57%. The mask-weighted light curve shows two overlapping peaks. The first starts at ~T-70 sec and peaks at ~T+10 sec. The second peaks at ~T+32 sec and ends at ~T+400 sec. T90 (15-350 keV) is 294 +- 71 sec (estimated error including systematics). The time-averaged spectrum from T-68.9 to T+405.1 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.54 +- 0.06. The fluence in the 15-150 keV band is 7.7 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+31.12 sec in the 15-150 keV band is 2.9 +- 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/336489/BA/
GCN 8600 table
GRB_name GRB081203A
GCN_number 8600
Detection_method Swift-BAT Det
ra 228.7890°
decl 44.4270°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8600 SUBJECT: GRB 081203A: Burst detection from Swift-BAT slew data DATE: 08/12/03 18:54:02 GMT FROM: Antonio Copete at Harvard U A. Copete, J. Grindlay (Harvard) S. Barthelmy, C. Markwardt, N. Gehrels (NASA/GSFC) We report the detection of a GRB candidate by the BAT Slew Survey (BATSS) in the slew that started at 13:52:02 UT. This is 309 sec before the trigger time for the GRB that followed (A. M. Parsons et al, GCN 8595), which occurs at a different location and should hereafter be referred to as GRB 081203B. The ground-calculated position of GRB 081203A is RA, Dec = 228.789, +44.427 deg, which is RA (J2000) = 15h 15m 09s Dec (J2000) = +44d 25' 36" with an uncertainty of 3.04 arcmin (90% confidence, including systematics). The detection was triggered by simultaneous independent detections of 11.0 sigma and 5.6 sigma from imaging in the 15-50 keV and 50-150 keV energy bands, respectively. The burst mask- tagged lightcurve shows 2 main peaks, the larger one at T+24sec and lasting 2sec as the burst enters the BAT FoV, the second one at T +30sec with a duration of 2sec, and it has largely faded as the pointing observation that follows begins. The measured T90 = 23.4sec and T50 = 8.2sec (15-150keV). Preliminary spectral analysis from T+24.0 to T+50.4 shows a time- averaged spectrum that is best fit by a simple power law with photon index of 1.65. The total fluence in the 15-150 keV band is 2.1 x 10^-6 erg/cm2, and the 1-sec peak flux is 3.5 x 10^-7 erg/cm2/sec. A follow-up Swift ToO observation has been scheduled to begin at 18:26 UT, 4.6 hours after the burst.
GCN 8601 table
GRB_name GRB081203A
GCN_number 8601
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8601 SUBJECT: GRB081203A: Swift/UVOT grism redshift DATE: 08/12/03 19:36:15 GMT FROM: Wayne Landsman at GSFC/SSAI W. Landsman (NASA/GSFC), M. DePasquale(MSSL), P. Kuin (MSSL), P. Schady (MSSL), P. Smith (MSSL), and A.Parsons (NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT obtained a 49s UV grism spectrum of GRB 081203A starting 249 s after the BAT trigger (Parsons et al. GCN.8595). The spectrum covers the wavelength range from 2000-4900 A. Longward of 2850 A in the quicklook spectrum there is an approximately flat continuum of 2.5e-14 erg s-1 cm-2 A-1 with a strong absorption at 3850 A. If the 2850 A cutoff is identified with the Lyman edge, and the 3850 A absorption with Lyman alpha, then the redshift of GRB081203A is ~2.1. Analysis is continuing.
GCN 8603 table
GRB_name GRB081203A
GCN_number 8603
Detection_method Swift-UVOT Det
ra 233.0316°
decl 63.5208°
redshift 2.1000
Circular_text TITLE: GCN CIRCULAR NUMBER: 8603 SUBJECT: Swift UVOT observations of GRB 081203A DATE: 08/12/03 22:06:27 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSSL/UCL) and A. Parsons (GSFC) reports, on the behalf of the Swift UVOT team: Swift UVOT began settled exposures of GRB081203A (trigger 336489, Parsons et al, GCN circular 8595) 93 s after the burst trigger. A bright optical transient is detected at the following coordinates: RA = 15h 32m 07.58s (=233.031580), Dec = +63d 31m 14.9s (=63.520810) J2000 with an uncertainty of 0.5'' (90% confidence level). This position is consistent with the XRT refined error circle (Goad et al, GCN circ 8598). The source is detected in all filters but um2. Below, we show time of observations, the exposure time and the magnitude and 3 sigma upper limits for this optical afterglow. T_start (s) T_stop (s) Exp (s) Mag wh 93 242 146.2 14.53 +/- 0.01 wh 586 605 19.5 13.91 +/- 0.01 v 636 655 19.5 13.30 +/- 0.03 b 561 580 19.5 13.53 +/- 0.01 u 306 555 246 13.07 +/- 0.01 u 709 728 19.5 13.53 +/- 0.02 uw1 685 704 19.5 14.82 +/- 0.07 um2 660 679 19.5 > 17.57 um2 660 6008 412.6 > 20.1 uw2 611 630 19.5 17.19 +/- 0.25 The nondetection in the um2 filter is consistent with the redshift z=2.1 derived from grism spectra (Landsman et al, GCN circ 8601). The detection in the uw2 filter is consistent with this redshift due to the long-wavelength tail of the uw2 filter response. The above magnitudes have not been corrected for the Galactic extinction corresponding to E(B-V) = 0.02 (Schlegel et al 1998) The photometry is on the UVOT flight system described in Poole et al (2008, MNRAS, 383,627) [GCN OPS NOTE(03dec08): Per author's request, the "A" was added to the burst name.]
GCN 8604 table
GRB_name GRB081203A
GCN_number 8604
Detection_method Optical
ra 233.0317°
decl 63.5208°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8604 SUBJECT: GRB 081203A: optical observations DATE: 08/12/03 23:08:16 GMT FROM: Igor Volkov at Asro.Inst.Slovak Acad.Sciences On 2008 December 03 I have monitored the field of GRB 081203A detected by SWIFT (Parsons, et al., GCN Circ. 8595) with the 0.5m reflector and ST-10XME CCD camera of Stara Lesna (Slovak Republic) observatory. My frames confirm the presence of the afterglow close to coordinates (J2000) RA = 15h 32m 07.6s, Dec = +63d 31m 14.9s (M. De Pasquale and A. Parsons, GCN Circ. 8603 ). Observations continued from UT 15:24:45 to UT 16:58:45 in Rc photometric system. The object faided from Rc=15.74+/-0.04 to Rc=17.20+/-0.06 during this time interval. Several BVIc measurements were also obtained. GSC 4184 1309 served as a comparison star. The reduction of the data is in progress and will be available on request. This study was supported by the SAI scholarship. Igor Volkov, Astronomical Institute of the Slovak Academy of Sciences, 059 60 Tatranska Lomnica, Slovak Republic; e-mail: volkov@ta3.sk
GCN 8609 table
GRB_name GRB081203A
GCN_number 8609
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8609 SUBJECT: GRB081203A: Swift-XRT refined analysis DATE: 08/12/04 08:56:13 GMT FROM: Valentina La Parola at INAF-IASPA V. La Parola, B. Sbarufatti, V. Mangano (INAF-IASF Pa), A. Parsons (GSFC) report on behalf of the Swift XRT team: We have analysed the first 3 orbits of Swift-XRT data obtained for GRB 081203A (trigger #336489, Parsons et al., GCN Circ.8595), that includes 550 s of Windowed Timing (WT) and 15.5 ks of Photon Counting (PC) mode data, respectively, between 87 s and 16 ks after the trigger. The UVOT-enhanced XRT position was given by Evans et al. in GCN Circ 8598. The light-curve can be modelled with a broken power-law, with a steep decay alpha_1=4.32 0.16 and a break time at T_b=T0+(150+/-3) s. After the break the decay flattens to alpha_2=1.175 0.015 The spectrum extracted from the WT data has an exposure of 558 s. It can be modelled with an absorbed power-law, with Gamma =1.97 0.04 and an intrinsic NH = (5.5 0.8)x10^20 cm-2, in excess to the Galactic value of 1.7x10^20 cm-2. The observed (unabsorbed) 0.3 -10 keV averaged flux over this time interval is 8.6x10^-10 (10x10^-10) erg cm-2 s-1. The spectrum extracted from the PC data in the time interval 0.6-16 ks (with an exposure time of 4.7 ks) can be modelled with an absorbed power-law, with Gamma = 2.1 0.08 and an intrinsic column density of NH = (6.0 1.7)x10^20 cm-2. The observed (unabsorbed) 0.3 -10 keV averaged flux over this time interval is 2.8x10^-11 (3.6x10^-11) erg cm-2 s-1. Uncertainties are given at 90% confidence. If the light-curve continues to decay with the present rate, the count rate 24 (36) hours after the burst is estimated to be 0.02 (0.013) count s-1, which corresponds to an observed flux of 7x10^-13 (4.5x10^-13) erg cm-2 s-1. The results of the xrt automatic analysis are available at http://www.swift.ac.uk/xrt_products/00336489. This is an official product of the Swift-XRT team.
GCN 8611 table
GRB_name GRB081203A
GCN_number 8611
Detection_method Konus-Wind Det
t_trigger 13:51:30.368 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 8611 SUBJECT: Konus-Wind observation of GRB 081203A DATE: 08/12/04 16:01:56 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, D. Svinkin, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team report: The long GRB 081203A (Parsons et al., GCN 8595, Ukwatta et al., GCN 8599) was detected by Konus-Wind in the same trigger record as GRB 081203B (Copete et al., GCN 8600, 8602; Golenetskii et al., GCN 8610) at ~T0(KW)+260s. (T0(KW)=49890.368 s UT (13:51:30.368). Correcting for the propagation time delay from Wind to Swift of 0.7s, one sees that T0(BAT) corresponds to T0(KW)+339.9s). Since this burst occurred after the end of the time history record (=T0(KW)+229s) we do not have the light curve of this GRB with good time resolution. Instead we have KW multichannel spectra accumulated until T0(KW)+490s (that is until T0(BAT)+150s), which were converted to a 3-band light curve with a time resolution of 8.192 s. The burst light curve shows a weak emission starting at ~T0(BAT)-80s (=T0(KW)+260s), the main double-peaked pulse starting at ~T0(BAT)-14s (=T0(KW)+326s) and the decaying tail seen at least until T0(BAT)+134s (=T0(KW)+474s). As observed by Konus-Wind the burst had a fluence of 3.05(-0.89, +1.40)x10^-5 erg/cm2 (in the 20 keV - 3 MeV energy range). The time-integrated spectrum of the burst (from T0(BAT)-79s to T0(BAT)+134 s) is well fitted (in the 20 keV-3 MeV range) by a simple power law model with index 1.54 +/- 0.08 (chi2 = 65.8/69 dof). Fitting by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = -1.33(-0.20, +0.27) and Ep = 578(-290, +2398) keV (chi2 = 61.2/68 dof). The spectrum of the main pulse (from T0(BAT)-14s to T0(BAT)+52s) is well fitted (in the 20 keV-3 MeV range) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.29(-0.13, +0.15) and Ep = 497(-156, +383) keV (chi2 = 66.2/68 dof). All the quoted errors are at the 90% confidence level. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB081203A/
GCN 8613 table
GRB_name GRB081203A
GCN_number 8613
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8613 SUBJECT: VLA Radio upper limit on GRB 081203A DATE: 08/12/04 18:06:19 GMT FROM: Poonam Chandra at U Virginia/NRAO Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of the Caltech-NRAO-Carnegie GRB Collaboration: "We used the Very Large Array to observe the field of view toward optically bright GRB 081203A (GCN 8595) at a frequency of 8.46 GHz on 2008 Dec 04.39 UT. The GRB radio afterglow is undetected and the peak radio flux at the UVOT position (GCN 8595) is 76 54 uJy. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc."
GCN 8615 table
GRB_name GRB081203A
GCN_number 8615
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8615 SUBJECT: GRB081203A: optical observation DATE: 08/12/04 18:32:07 GMT FROM: Alexei Pozanenko at IKI, Moscow M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy), Ju. Babina (CrAO), A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the field of GRB 081203 (Parsons et al, GCN 8595) with the Z-600 telescope of Mt. Terskol observatory between (UT) Dec.03 14:29-14:38 (unfiltered exposures of 15 s), Dec.03 14:50 - Dec.04 01:45 (R-band exposures of 60 s), and starting (UT) Dec.04 15:27. In mid time Dec.04 (UT) 00:50 the afterglow is detected on combined images and R=19.5 +/-0.2. In mid time Dec. 04 (UT) 15:32 we do not detect the afterglow up to R=20.6 (3 sigma). The photometry is still preliminary and basen on star of SDSS J153155.64+632959.4 (=USNO-B1.0 1534-0214259), assuming R=14.69.
GCN 8617 table
GRB_name GRB081203A
GCN_number 8617
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8617 SUBJECT: GRB 081203A: Skynet/GORT Detections DATE: 08/12/05 01:15:13 GMT FROM: James Philip West at UNC/Chapel Hill J. P. West, K. McLin, T. Brennan, J. Haislip, D. Reichart, L. Cominsky, T. Graves, G. Spear, K. Ivarsen, J. A. Crain, A. Foster, R. Holmes, A. LaCluyze, M. Schubel, J. Styblova, A. Trotter, and E. Weaver report: Skynet observed the localization of GRB 081203A (Parsons et al., GCN 8595) with the 14" GORT telescope at Hume Observatory in California beginning 122 seconds after the trigger (101 seconds after notification) in RI. Only five exposures were taken before morning twilight. We detect the afterglow (Parsons et al., GCN 8595) in all five exposures. Calibrated to five USNO B1 stars, we find: mean time since trigger exposure filter magnitude (sec) (sec) 134 20 I 12.79 +/- 0.02 235 40 R 12.60 +/- 0.01 345 40 I 11.58 +/- 0.01 476 80 R 12.51 +/- 0.01 625 80 I 12.02 +/- 0.01 [GCN OPS NOTE(05dec08): Per author's request, the "magnutude time" column label was changed to "magnitude".]
GCN 8618 table
GRB_name GRB081203A
GCN_number 8618
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8618 SUBJECT: GRB 081203A: Optical observations of Xinglong TNT telescope DATE: 08/12/05 07:57:42 GMT FROM: L.P. Xin at NAOC H. Liu, J. Wang, L.P. Xin, Y.L. Qiu, J.Y. Wei, J.Y. Hu, J.S. Deng, W.K. Zheng and Y. Urata on behalf of EAFON report: We have observed GRB081203A (Parsons et al., GCN 8595) with Xinglong TNT telescope from Dec.03th,13:57:11(UT), 6.43 hr after the burst to Dec.03,22:19:37.67 (UT). A series of R band and V band have been obtained. The optical afterglow was clearly detected in all the images. Further observations of GRB081203A were also made with Xinglong TNT telescope from Dec.04th,21:29:30.409(UT). The OT was still marginal detected after combined 11*600s images. we found the afterglow dacayed from R=19.0 at 7.25 hr to R=21.1 at 24.6 hr. The decay slope index is about 1.59, which is consistent with the index derived from Volkov et al,(GCN 8604). Further observations are encouraged. This message may be cited. For more information about Xinglong GRBs Follow-up observations, please visit the website: http://www.xinglong-naoc.org/grb/
GCN 8619 table
GRB_name GRB081203A
GCN_number 8619
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 8619 SUBJECT: GRB081203A: MITSuME optical observation DATE: 08/12/05 11:04:48 GMT FROM: Michitoshi Yoshida at Okayama Astrophysical Obs Y. A. Mori, H. Nakajima, T. Shimokawabe, N. Kawai (Tokyo Tech), D. Kuroda, M. Yoshida, K. Yanagisawa, Y. Shimizu, H. Toda, and S. Nagayama (OAO, NAOJ) report on behalf of the MITSuME collaboration: We performed optical imaging observation of the field of GRB 081203A (Parsons, et al., GCN Circ. 8595) with the 3-color 50cm MITSuME Telescopes at Akeno Observatory and Okayama Astrophysical Observatory from UT 17:50 to UT 20:55, 3.9 hours after the trigger. In the co-added images of Rc, and g' bands, we detected the optical afterglow detected with UVOT (Parsons, et al., GCN Circ. 8595). Photometric calibration was done using the GSC2.3 catalogs. The results are following: Akeno: MID-MJD MID-UT EXP-T g' Rc ---------------------------------------------------------- 54803.753779 18:12:54 1620.0 18.50+/-0.24 18.11+/-0.25 ---------------------------------------------------------- Okayama: MID-MJD MID-UT EXP-T g' Rc ---------------------------------------------------------- 54803.790960 18:58:59 1500.0 18.87+/-0.26 18.36+/-0.19 54803.811830 19:29:03 1500.0 19.18+/-0.25 17.89+/-0.15 54803.833037 19:59:35 1560.0 19.11+/-0.23 18.49+/-0.24 54803.854522 20:30:31 1560.0 19.63+/-0.32 18.91+/-0.19 ----------------------------------------------------------
GCN 8623 table
GRB_name GRB081203A
GCN_number 8623
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8623 SUBJECT: GRB081203A: Radio upper limit at 15 GHz DATE: 08/12/05 17:33:51 GMT FROM: Guy Pooley at MRAO, Cambridge, UK Guy Pooley (MRAO/Cavendish Astrophysics, University of Cambridge) reports: We used the AMI large array (the rebuilt/upgraded Ryle Telescope) in the band 14 - 17 GHz to observe the field of the optically bright GRB 081203A (GCN 8595). There was no detection of the afterglow on either of two observations. The measured flux densities at the optical position are: 2008 Nov 04.26 116 +- 300 microJy 2008 Nov 05.24 80 +- 200 microJy (cf Chandra & Frail, GCN 8613, for an upper limit at 8.46 GHz)
GCN 8629 table
GRB_name GRB081203A
GCN_number 8629
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8629 SUBJECT: GRB081203A: Optical observations at Ishigaki DATE: 08/12/06 13:25:53 GMT FROM: Mizuki Isogai at NAOJ M. Isogai (IAO, NAOJ) and N. Kawai (Tokyo Tech) report with support of MITuME collaboration: We observed the field of GRB 081203A(Parsons, et al., GCN Circ. 8595) with the optical 3-color imager attached to the 105cm Murikabushi Telescope at Ishigakizima Astronomical Observatory in Japan from UT 19:52, 5.9 hours after the trigger. In the co-added images of Ic, Rc, and g' bands, we detected a fading point source and measured its magnitude. Photometric calibration was performed using the GSC2.3 catalogs. The results are following: MID-MJD MID-UT EXP-T g' Rc Ic ---------------------------------------------------------------------- 54803.837345 20:05:46 720.0 18.50+/-0.09 54803.837345 20:05:46 900.0 19.43+/-0.11 18.76+/-0.06 54803.847273 20:20:04 720.0 19.39+/-0.11 54803.848363 20:21:38 900.0 18.83+/-0.06 18.49+/-0.08 54803.859451 20:37:36 900.0 19.57+/-0.11 18.96+/-0.06 18.67+/-0.09 54803.870356 20:53:18 900.0 19.77+/-0.11 18.94+/-0.07 18.72+/-0.10 54803.881257 21:09:00 900.0 19.71+/-0.12 19.04+/-0.07 18.71+/-0.10
GCN 8632 table
GRB_name GRB081203A
GCN_number 8632
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8632 SUBJECT: GRB081203A: Ashra-1 observation of early optical and VHE-neutrino emission DATE: 08/12/07 16:54:46 GMT FROM: Makoto Sasaki at ICRR/U.Tokyo Y.Aita, Y.Asaoka, T.Chonan, Y.Higashi, K.Noda, and M.Sasaki (ICRR,Univ.Tokyo), Y.Morimoto, S.Ogawa (Toho Univ.), J.Learned (Univ.Hawaii Manoa), R.Fox (Univ.Hawaii Hilo) report on behalf of the Ashra-1 collaboration: We have searched for optical and VHE-neutrino emission in the field of GRB081203A (A. M. Persons et al., GCN Circ. 8595) around the BAT-triggered GRB time (T0) with one of the light collector units in the Ashra-1 detector (http://www.icrr.u-tokyo.ac.jp/~ashra) on Mauna Loa on Hawaii Island (latitude = 19.5412 deg. N, longitude =155.5676 deg. W, altitude =3330m). The Ashra-1 light collector unit has the achieved resolution of a few arcmin, viewing 42 degree circle region of which center is located at Alt = 11.7 deg, Azi = 22.1 deg. The sensitive region of wavelength is similar with the B-band. We quickly analyzed 83 images covering the field of GRB081203A every 7.2s with 6s exposure time respectively during the observation between T0-300s and T0+300s. We detected no new optical object within the PSF resolution around the GRB081203A determined by Swift-UVOT (M. De Pasquale et al.,GCN Circ. 8603). As a result of our preliminary analysis, the following 3-sigma limiting magnitudes are derived: ---------------------------------------------------------------------- Starting&Ending Exp.Time, 3-sigma Limit. Mag. ---------------------------------------------------------------------- -297.7 -291.7 11.9 -290.7 -284.7 11.9 . . . . . . -1.7 4.3 11.9 5.3 11.3 11.8 . . . . . . 287.3 293.3 11.9 294.3 300.3 11.9 ---------------------------------------------------------------------- The limiting magnitudes were estimated in comparison with stars in Tycho-2 Catalog to be distributed between 11.7 and 12.0 as above partly listed. Adding that we have searched for VHE-neutrino emission with the primary neutrino energy above 10^16eV by detecting Cherenkov lights from tau-decay induced air-showers. VHE neutrinos are expected to be produced at the GRB behind Mauna Kea and converted into tau leptons in the mountain rock. The GRB position was passed through our triggering region viewing onto the face of Mauna Kea from 11:07UT to 11:49UT (2.83 hours to 2.13 hours before the GRB). We have no signal come out of the mountain. The limiting flux is now under analysis. Figures of limiting optical magnitudes vs time comparing with other measurements and more details on the VHE neutrino observation can be found at: http://www.icrr.u-tokyo.ac.jp/~ashra/GRB081203A. This message may be cited. //////////////////////////////////////////////////////////////// SASAKI Makoto ICRR, University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa 277-8582 tel/fax +81-4-7136-3143 ////////////////////////////////////////////////////////////////
GCN 8645 table
GRB_name GRB081203A
GCN_number 8645
Detection_method Optical
ra 233.0316°
decl 63.5208°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8645 SUBJECT: GRB 081203A: optical observations DATE: 08/12/10 02:07:24 GMT FROM: Alexei Pozanenko at IKI, Moscow V. Rumyantsev, K. Antonyuk (CrAO), M. Andreev(Terskol Branch of Institute of Astronomy), A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the field of GRB 081203 (Parsons et al, GCN 8595) with the AZT-11 telescope of CrAO observatory starting Dec. 03 (UT) 15:44:29 under good weather conditions and seeing of about ~2 arcsec. Several exposures were obtained in VRI bands up to 17:13:56 and then between Dec. 04 (UT) 01:19:13 - 02:47:51. Coordinates of the afterglow are RA(J2000)= 15:32:07.58 Dec(J2000)= +63:31:14.8 with uncertainty of 0.2 arcsec which is compatible with the coordinates of the afterglow (Parsons et al, GCN 8595). Preliminary photometry based on SDSS star J153200.06+633229.9 (RA(J2000)=15:32:00.01 Dec(J2000)=+63:32:30.4) assuming V=17.28 R=16.85 I=16.46 is following T0+ Filter Exp. mag. s s 6528 V 180 16.84 +/-0.02 6712 R 180 16.63 +/-0.02 6896 I 180 16.22 +/-0.02 11524 V 180 17.68 +/-0.05 11708 R 180 17.53 +/-0.03 11892 I 180 17.15 +/-0.04 41196 R 3x180 20.27 +/-0.15 46144 R 3x180 20.20 +/-0.14 While light curves in a time interval 6500 - 12000 s after burst onset in R and I bands look similar with a power law decay index of about 0.66, the power law decay index in V-band is ~0.59 and one can suggest a spectral variability of the afterglow. Also we observed steep decay between 12000 - 46000 s with a power law index of about 1.9.
GCN 8685 table
GRB_name GRB081203A
GCN_number 8685
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8685 SUBJECT: Modification of Swift/UVOT response to bright GRBs DATE: 08/12/19 21:10:47 GMT FROM: Wayne Landsman at GSFC/SSAI W. Landsman (GSFC), P. Kuin (MSSL), F. Marshall (GSFC), M. Page (MSSL), P. Roming (PSU), N. Gehrels (GSFC) report on behalf of the Swift/UVOT team The Swift/UVOT has modified its automated response to GRBs with a BAT trigger rate larger than 100 cps. For these bright GRBs, a 50s UV grism exposure is now inserted following the first 150s finding chart in the white filter. Roughly half of all Swift GRBs are sufficiently bright to trigger the use of the grism. The UVOT grism covers the spectral range 1700 - 5500 A, and can provide useful spectra for GRBs brighter than about V~13. Further details are available in Kuin et al. (2008, astro-ph 0812/2943 ) who report their analysis of the UVOT grism spectrum of GRB081203A. The grism zero-order spectrum in the 50s exposure can provide photometry for sources brighter than B-18. The zero-order spectrum includes visible light and its brightness roughly correlates with Johnson B magnitude, with a scatter of about 0.23 mag.
GCN 8695 table
GRB_name GRB081203A
GCN_number 8695
Detection_method Optical
redshift 2.0500
Circular_text TITLE: GCN CIRCULAR NUMBER: 8695 SUBJECT: GRB081203A: BTA observation DATE: 08/12/22 12:38:47 GMT FROM: Vladimir Sokolov at SAO RAS T. Fatkhullin, A. Moskvitin (SAO RAS, Russia), A. Posanenko (IKI RAS, Russia), E. Sonbas (SAO RAS,University of Cukurova, Turkey ), A. Volnova (SAI MSU), V. Rumyantsev (CrAO), V. Kouprianov (GAO RAS), V. Sokolov (SAO RAS) and A.J. Castro-Tirado ((IAA-CSIC Granada, Spain) on behalf of a larger collaboration report: We observed the field of the GRB081203A (A. M. Parsons et al., GCN #8595) in the Rc-band with the 6-m telescope of the SAO RAS in Caucasus. In total 15 3-min exposures were obtained starting from 01:42 7 Dec. 2008 UT (T-T_0 = 3.49 days). We clearly detected an object at the position of the UVOT optical transient (M. De Pasquale and A. Parsons, GCN #8603). Calibration based on the SDSS stars yields the brightness of the OT as R = 23.94 +/- 0.13 (errors are statistical only). At the 3.2 +/- 0.2 arcsec to the South-West from the OT position we also detect an extended object with R = 22.74 +/- 0.07. For redshift of z=2.05 (N.P.M Kuin et al, astro-ph/0812.2943) it corresponds to ~26 kpc in projection (H0=71, Omega_M=0.3, Omega_L=0.7). It is unlikely that this object is a host galaxy of the GRB081203A but redshift measurements are needed for certainty. Further observations are planned. Our finding chart can be dowloaded from ftp://ftp.sao.ru/pub/grb/GRB081203A/GRB081203A_OT.jpg This message can be cited