GRB081109A

This page lists all entries on GRB081109A in GRBweb

Summary Fermi GBM IPN Swift GCN 8500 GCN 8501 GCN 8503 GCN 8504 GCN 8505 GCN 8506 GCN 8507 GCN 8508 GCN 8509 GCN 8510 GCN 8515 GCN 8517 GCN 8523 GCN 8636

Summary table
Variable Value Source
GRB_name_Fermi GRB081109293
T0 7:01:55.503 UTC Fermi_GBM
ra 330.7899° Swift
decl -54.7112° Swift
pos_error 1.04e-04° Swift
T90 58.369 s Fermi_GBM
T90_error 5.221 s Fermi_GBM
T90_start 7:01:55.503 UTC Fermi_GBM
fluence 6.55e-06 erg/cm² Fermi_GBM
fluence_error 5.87e-08 erg/cm² Fermi_GBM
redshift 0.9787 IPN
T100 200.497 s
GBM_located False
mjd 54779.293003506944 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB081109293
trigger_name bn081109293
ra 330.8000°
decl -54.7000°
pos_error 4.01e+00°
datum 2008-11-09
t_trigger 7:02:02.415 UTC
T90 58.369 s
T90_error 5.221 s
T90_start 7:01:55.503 UTC
fluence 6.55e-06 erg/cm²
fluence_error 5.87e-08 erg/cm²
flux_1024 2.64e+00 erg/cm²/s
flux_1024_error 1.65e-01 erg/cm²/s
flux_1024_time 1.36e+01 erg/cm²/s
flux_64 4.37e+00 erg/cm²/s
flux_64_error 1.59e+00 erg/cm²/s
IPN table
GRB_name GRB081109A
ra 330.7875°
decl -54.7167°
pos_error 5.00e-02°
redshift 0.9787
Swift table
GRB_name GRB081109A
t_trigger 7:02:06 UTC
ra 330.7899°
decl -54.7112°
pos_error 1.04e-04°
T90 190.0 s
fluence 3.60e-06 erg/cm²
GCN 8500 table
GRB_name GRB081109A
GCN_number 8500
Detection_method Swift Det
t_trigger 7:02:06 UTC
ra 330.7870°
decl -54.7190°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8500 SUBJECT: GRB 081109: Swift detection of a burst DATE: 08/11/09 07:22:59 GMT FROM: David Palmer at LANL S. Immler (CRESST/GSFC/UMD), A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), S. D. Hunsberger (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 07:02:06 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 081109 (trigger=334112). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 330.787, -54.719 which is RA(J2000) = 22h 03m 09s Dec(J2000) = -54d 43' 06" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a triangular structure with a duration of about 40 sec. The peak count rate was ~2500 counts/sec (15-350 keV), at 20 sec after the trigger. The XRT began observing the field at 07:03:12.2 UT, 65.6 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 330.7911, -54.7114 which is equivalent to: RA(J2000) = 22h 03m 09.86s Dec(J2000) = -54d 42' 41.0" with an uncertainty of 4.8 arcseconds (radius, 90% containment). This location is 28 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. The initial flux in the 2.5 s image was 4.78e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 75 seconds after the BAT trigger. 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 0.02. No afterglow candidate has been detected. Burst Advocate for this burst is S. Immler (immler 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 8501 table
GRB_name GRB081109A
GCN_number 8501
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8501 SUBJECT: GRB 081109: REM NIR afterglow detection DATE: 08/11/09 09:54:49 GMT FROM: Stefano Covino at Brera Astronomical Observatory P. D'Avanzo, S. Covino, L.A. Antonelli, D. Malesani, D. Fugazza, L. Calzoletti, S. Campana, G. Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. D'Alessio, F. Fiore, P. Goldoni, D. Guetta, C. Guidorzi, G.L. Israel, E. Maiorano, N. Masetti, A. Melandri, E.J.A. Meurs, L. Nicastro, E. Palazzi, E. Pian, S. Piranomonte, L. Stella, G. Stratta, G. Tagliaferri, G. Tosti, V. Testa, S.D. Vergani, F. Vitali report on behalf of the REM team: The robotic 60-cm REM telescope located at La Silla (Chile) observed automatically the field of the GRB 081109 (Immler et al. GCN 8500) on Nov 09 starting about 52 s after the burst. Observations were carried out at high airmass (~ 6). We clearly detect an object in our first K-band image inside the XRT error box (Immler et al. GCN 8500) at the following coordinates (J2000): R.A. = 22:03:09.72 Dec = -54:42:39.5 with an uncertainty of 1.0". The object is not visible in the single RJH images taken approximately at the same epoch. Coadding all the available RJH images taken around the same epoch we obtain the following results: Mean_obs texp #frames_coadd Filter Mag Nov 09.30604 UT 780 s 11 R > 16.5 (3sigma) Nov 09.30707 UT 65 s 4 J > 15.8 (3sigma) Nov 09.29936 UT 75 s 7 H 15.47 0.26 Nov 09.30145 UT 10 s 1 K 14.51 0.27 The object subsequently brightened, reaching K = 14.27 0.16 on Nov 09.30612 UT. No object is detected at this position in the 2MASS and USNO catalogs. We propose this is the NIR afterglow of GRB 081109. We cannot indeed exclude the possibility that the lack of detection blueward of the H band is due to an high-redshift nature of this event. We note, however, that the large airmass badly affects the images in the J and R bands, so that our limits are not very constraining Further deep optical/NIR observations are encouraged.
GCN 8503 table
GRB_name GRB081109A
GCN_number 8503
Detection_method Optical
ra 330.7905°
decl -54.7110°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8503 SUBJECT: GRB 081109A optical upper limit DATE: 08/11/09 14:15:04 GMT FROM: AAVSO GRB Network at AAVSO Peter Nelson (Ellinbank, Victoria, Australia) reports to the AAVSO International High Energy Network the following optical observation of GRB081109A (GCN #8500 Immler et al.; GCN #8501 D'Avanzo et al.): Peter Nelson has obtained a limiting magnitude on the optical afterglow of GRB081109A (Immler et al., GCN #8500). The near IR afterglow position RA: 22:03:09.72 Dec: -54:42:39.5 found by D'Avanzo et al. (GCN #8501) was observed for 120 seconds using a 0.32-meter Newtonian with an SBIG ST8XE CCD and an R filter under poor photometric conditions. The mid-point of the observations was 2008 Nov 09.5188 UT, approximately 5.4 hours after the burst. The afterglow was not detected to an upper limit of R=18.1, using the USNO-A2.0 star 0300-37476396 (R=13.2) as the comparison. A detailed report of these observations is available on the AAVSO website at ftp://ftp.aavso.org/grb/PeterNelson_081109_2454780.06997_.txt A fits image is available at ftp://ftp.aavso.org/grb/PeterNelson_081109_2454780.06997_.fits The AAVSO thanks the Curry Foundation for their continued support of the AAVSO International High Energy Network.
GCN 8504 table
GRB_name GRB081109A
GCN_number 8504
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8504 SUBJECT: GRB 081109: Swift/UVOT upper limits DATE: 08/11/09 15:18:19 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (MSSL/UCL) and S. Immler (CRESST/GSFC/UMD) report on behalf of the Swift UVOT team. The Swift UltraViolet/Optical Telescope (UVOT) began observing GRB 081109 (Swift BAT trigger number 334112; Immler et al., GCN Circ. 8500) on November 9, 2008, with a white filter finding chart at 07:03:23 UT, 75 seconds after the trigger. No new source is detected in any of our images at the position consistent with the reported XRT position in GCN Circ. 8500. The magnitudes and upper limits for GRB081109 at this position are given below: Filter Tstart(s) Tstop(s) Exp(s) Magnitude wh 75 6592 745 >21.49 (3-sigma UL) u 287 6181 501 >20.57 (3-sigma UL) b 543 6387 452 >20.35 (3-sigma UL) uvw2 593 5362 274 >20.03 (3-sigma UL) v 617 5566 274 >19.09 (3-sigma UL) uvm2 641 5771 274 >19.87 (3-sigma UL) uvw1 666 5976 255 >20.00 (3-sigma UL) The values quoted above are on the UVOT Photometric System (Poole et al, 2008, MNRAS 383, 627). They are not corrected for the expected galactic reddening of E(B-V) = 0.019 in the direction of the burst (Schlegel et al. 1998).
GCN 8505 table
GRB_name GRB081109A
GCN_number 8505
Detection_method Fermi GBM Det
t_trigger 7:02:02.420 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 8505 SUBJECT: GRB 081109: Fermi GBM detection DATE: 08/11/09 15:56:47 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 07:02:02.42 UT on 09 November 2008, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 081109 (trigger 247906923 / 081109293), which was also detected by the SWIFT (S. Immler et al. 2008, GCN 8500). The GBM on-ground location is consistent with the Swift position. The GBM light curve shows a single peak with a duration (T90) of about 45 s (8-1000 keV). The time-averaged spectrum from T0-6.144 s to T0+26.624 s is best fit by a power law function with an exponential high energy cutoff. The power law index is -1.28 +/- 0.09 and the cutoff energy, parameterized as Epeak is 240 +/- 60 keV. (chi squared 510 for 478 d.o.f.) The event fluence (8-1000 keV) in this time interval is (6.53 +/- 0.43)E-06 erg/cm^2. The 1-sec photon flux measured starting from T0+9.216 s in the 8-1000 keV band is 3.2 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 8506 table
GRB_name GRB081109A
GCN_number 8506
Detection_method Swift-XRT Other
ra 330.7905°
decl -54.7118°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8506 SUBJECT: GRB 081109A: Swift-XRT refined analysis DATE: 08/11/09 16:19:07 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, K.L. Page (U. Leicester) and S. Immler (CRESST/GSFC/UMD) report on behalf of the Swift-XRT team. The Swift-XRT started observing the field of GRB 081109A (trigger #334112, Immler et al., GCN 8500) at 07:03:12.2 UT, 65.6 s after the BAT trigger. The XRT observed the GRB in Windowed Timing (WT) mode until 318 s after the trigger and Photon Counting (PC) mode thereafter. Using 4661 s of XRT Photon Counting mode data and 7 UVOT images, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching to the USNO-B1 catalogue) of RA, Dec = 330.7905, -54.7118 which is equivalent to : RA (J2000): 22h 03m 9.72s Dec (J2000): -54d 42m 42.5s with an uncertainty of 1.4 arcsec (90% confidence). This is 2.98 arcsec from the reported possible NIR counterpart of D'Avanzo (GCN 8501). The X-ray light curve from the first three orbits can be modelled with a broken powerlaw with an initial decay slope of 1.78 +/- 0.06, a break time of 353 +/- 40 s, followed by a shallower decay slope of 0.99 +/- 0.04. The spectrum of the WT data from orbit 1 (from T+71.9 s to T+318.4 s, where T is the trigger time) can be well fit by an absorbed powerlaw with a photon index of 1.72 +/- 0.08 and column density of (1.84 +/- 0.22) x 10^21 cm^-2, compared with the Galactic column density of 1.6 x 10^20 cm^-2 in the direction of the burst. The observed 0.3-10 keV flux is (7.4 +/- 0.4) x 10^-10 erg cm^-2 s^-1. The corresponding unabsorbed 0.3-10 keV flux is (9.5 +/- 0.5) x 10^-10 erg cm^-2 s^-1. A powerlaw fit to a spectrum obtained from PC mode data spanning orbits 2 to 3 (T+4.76 ks to T+12.88 ks) is best fit with a photon index of 2.20 +/- 0.20 and column density (3.1 +/- 0.7) x 10^21 cm^-2. The observed 0.3-10 keV flux over this interval is (7.3 +/- 0.7) x 10^-12 erg cm^-2 s^-1. The count-to-observed-flux conversion factor is 6.0e-11 erg cm^-2 count^-1. Assuming the X-ray emission from the burst continues to decline at the same rate we predict an XRT count rate of 0.018 count s^-1 at T+24 hour, or an observed 0.3-10 keV X-ray flux of 1.1 x 10^-12 erg cm^-2 s^-1. This circular is an official product of the Swift-XRT team.
GCN 8507 table
GRB_name GRB081109A
GCN_number 8507
Detection_method Swift-BAT Det
ra 330.7980°
decl -54.7110°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8507 SUBJECT: GRB 081109A, Swift-BAT refined analysis DATE: 08/11/09 16:42:12 GMT FROM: Scott Barthelmy at NASA/GSFC C. B. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), S. Immler (CRESST/GSFC/UMD), H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (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 081109A (trigger #334112) (Immler, et al., GCN Circ. 8500). The BAT ground-calculated position is RA, Dec = 330.798, -54.711 deg, which is RA(J2000) = 22h 03m 11.5s Dec(J2000) = -54d 42' 40.5" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 73%. The mask-weighted light curve shows a smooth rise to a single peak starting at ~T-90 sec, peaking at ~T+5 sec, and roughly exponentially decaying back to baseline at ~T+400 sec. T90 (15-350 keV) is 190 +- 60 sec (estimated error including systematics). The time-averaged spectrum from T-15.9 to T+416.1 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.72 +- 0.09. The fluence in the 15-150 keV band is 3.6 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+7.64 sec in the 15-150 keV band is 1.1 +- 0.0 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/334112/BA/
GCN 8508 table
GRB_name GRB081109A
GCN_number 8508
Detection_method Other
ra 330.7570°
decl -54.7186°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8508 SUBJECT: GRB 081109A: Faulkes Telescope South observations DATE: 08/11/09 19:27:53 GMT FROM: David Bersier at Liverpool John Moores U C. Guidorzi (INAF-OAB), D. Bersier, M. Burgdorf, C.G. Mundell (LJMU) and N. Tanvir (U. Leicester) report on behalf of a larger collaboration: We observed GRB 081109A (Immler et al. GCN Circ. 8500) with the 2m Faulkes Telescope South starting on November 11 at 11:50:36 UT (corresponding to 4.81 hours post burst) in the R and i' filters. We do not detect any object at the position of the REM afterglow (D'Avanzo et al., GCN Circ 8501) down to magnitudes 21.0 and 21.2 in the R and i' filters respectively. These upper limits are conservative however, as there is a possible flux excess at the position of the REM afterglow but further analysis is required to ascertain the reality of this source. The calibration was performed using the R2 and I values of the nearby USNOB1 star RA=22:03:01.679, Dec=-54:43:07.05 (R2=16.88, I=16.46).
GCN 8509 table
GRB_name GRB081109A
GCN_number 8509
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 8509 SUBJECT: GRB 081109A: Possible Swift-UVOT detection DATE: 08/11/10 01:35:23 GMT FROM: Stefan Immler at NASA/GSFC S. Immler (CRESST/UMD/GSFC), N. P. M. Kuin (MSSL/UCL), and S. T. Holland (CRESST/USRA/GSFC) report on behalf of the Swift UVOT team: Further analysis of Swift Ultraviolet/Optical Telescope (UVOT) data of GRB 081109A (Immler et al., GCN Circ. 8500), starting 75 sec after the BAT trigger, gives a tentative detection of an optical source at the reported REM position (D'Avanzo et al., GCN Circ 8501) in the white filter at a 3.3-sigma level of confidence. The source is not detected in any of the other UVOT filters at the limiting magnitudes reported below. Filter Tstart(s) Tstop(s) Exp(s) Magnitude wh 75 6592 745 21.6+/-0.3 u 287 6181 501 >21.5 (3-sigma UL) b 543 6387 452 >20.9 (3-sigma UL) uvw2 593 5362 274 >21.6 (3-sigma UL) v 617 5566 274 >20.9 (3-sigma UL) uvm2 641 5771 274 >21.5 (3-sigma UL) uvw1 666 5976 255 >21.5 (3-sigma UL) The possible detection in the white filter, combined with the lack of a detection in the v filter, is consistent with the source having a redshift greater than 5.5. Follow-up observations, especially in the infrared, are encouraged.
GCN 8510 table
GRB_name GRB081109A
GCN_number 8510
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 8510 SUBJECT: GRB 081109: GROND Detection of the Optical/NIR Afterglow Candidate DATE: 08/11/10 03:34:52 GMT FROM: Christian Clemens at MPE C. Clemens, T. Kruehler, J. Greiner (all MPE Garching) and G. Szokoly (Eoetvoes Univ., Budapest and MPE) report on behalf of the GROND team: We observed the field of GRB 081109 (Swift trigger #334112; Immler et al., GCN #8500) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla Observatory (Chile). Observations started at 00:08 UT on November 10th, 2008, 17.1 hr after the GRB trigger, and are continuing. They were performed during astronomical twilight at an average seeing of 1.0" and at an average airmass of 1.1 as well as under bright Moon. Based on the first 7.7 min of total exposures in g'r'i'z' and 8.0 min in JHK, we detect the afterglow candidate reported by D'Avanzo et al. (GCN #8501) and estimate preliminary magnitudes (all in AB system) of g' > 22.8 r' ~ 22.8 +/- 0.3 i' ~ 21.8 +/- 0.15 z' ~ 21.4 +/- 0.15 J ~ 20.4 +/- 0.10 H ~ 19.7 +/- 0.15 K ~ 18.9 +/- 0.20 These magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars. The spectral energy distribution is very red, and requires an extinction of A_V > 0.5. With this strong extinction, and our g'-band limit being compromised by the nearby full Moon, we cannot derive a redshift at this stage.
GCN 8515 table
GRB_name GRB081109A
GCN_number 8515
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 8515 SUBJECT: GRB 081109: GROND redshift limit and host extinction DATE: 08/11/10 19:25:43 GMT FROM: Jochen Greiner at MPI C. Clemens, T. Kruehler, J. Greiner (all MPE Garching) report on behalf of the GROND team: We report on further analysis of the GROND data of GRB 081109 detected by Swift (trigger 334112; Immler et al., GCN #8500) and Fermi/GBM (von Kienlin 2008, GCN #8505) taken simultaneously in g'r'i'z'JHK. In a combined 2~h exposure at a midtime of 18.5~hours after the burst, we clearly detect the afterglow reported by D'Avanzo et al. (GCN #8501) and Clemens et al. (GCN #8510) in all filters. Using 2MASS field stars in JHK and the GROND zeropoints in g'r'i'z' we estimate preliminary AB magnitudes of g' = 23.14 +- 0.18 mag, r' = 22.55 +- 0.15 mag, i' = 22.00 +- 0.16 mag, z' = 21.54 +- 0.15 mag, J = 20.49 +- 0.07 mag, H = 19.56 +- 0.06 mag and K = 18.84 +- 0.10 mag which have been corrected for the expected Galactic reddening of E_(B-V)=0.02 (Schlegel et al. 1998). Assuming Ly-alpha absorption, the g' band detection implies a redshift of z < 3.5. The Galactic foreground corrected broad band SED is best fit with a power law template and significant extinction in the host. Depending on the used model, the best fit intrinsic extinction A_V^{host} varies between 0.6 and 1.2. We caution however, that this is strongly dependent on the unknown redshift and subject to changes due to an future improved calibration.
GCN 8517 table
GRB_name GRB081109A
GCN_number 8517
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8517 SUBJECT: GRB 081109: TAROT La Silla observatory optical observations DATE: 08/11/12 09:21:09 GMT FROM: Alain Klotz at CESR-CNRS Klotz, A. (CESR-OMP), Gendre B. (LAM-OAMP), Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report: We imaged the field of GRB 081109 detected by SWIFT (trigger 334112) with the TAROT robotic telescope (D=25cm) located at the European Southern Observatory, La Silla observatory, Chile. The observations started 29.4s after the GRB trigger. The elevation of the field decreased from 11 degrees above horizon and weather conditions were excellents. The first image is trailed with a duration of 60.0s (see the description in Klotz et al., 2006, A&A 451, L39). We do not detect the afterglow mentioned by D'Avanzo et al. (GCNC 8501) with a limiting magnitude of: t0+29.4s to t0+89.4s : R > 16.9 This image was taken during the gamma emission. This means that there was no bright optical flash associated to this burst. The second image is 30.0s exposure in tracking mode. We detect the afterglow: t0+95.1s to t0+125.1s : R ~ 17.8 +/- 0.2 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. This message may be cited.
GCN 8523 table
GRB_name GRB081109A
GCN_number 8523
Detection_method Swift-UVOT Other
ra 330.7899°
decl -54.7112°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8523 SUBJECT: GRB 081109A: confirmation of possible detection host galaxy DATE: 08/11/17 00:02:24 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (MSSL/UCL) and S. Immler(CRESST/GSFC/UMD) report on behalf of the Swift UVOT team. Continued observations by the Swift UltraViolet/Optical Telescope (UVOT) of the field of GRB 081109A (Immler et al., GCN Circ. 8500, Kuin and Immler, GCN Circ. 8504, Immler et al., GCN Circ. 8509) confirm that a weak source is present close to the REM position (D'Avanzo et al, GCN Circ. 8501) and also close to the refined XRT position (Beardmore et al., GCN Circ. 8506). We detect a constant source in 166 images totaling 54.4 ks of exposure time over a period of 544 ks (~1 week) in the UVOT white filter at position: RA = 22:03:09.579, Dec = -54.42.40.49 (J2000) with an uncertainty of 0.8 arcsec (90% confidence). The source magnitude in the summed image is wh = 22.86 +/- 0.09 mag (11.5 sigma detection). The values quoted above are on the UVOT Photometric System (Poole et al, 2008, MNRAS 383,627). They are not corrected for the expected galactic reddening of E(B-V) = 0.019 in the direction of the burst (Schlegel et al. 1998). We interpret this image as the possible host galaxy. In that case the REM position offset suggests that the GRB took place on the edge of the host galaxy. The source we detect is also just outside the XRT error circle.
GCN 8636 table
GRB_name GRB081109A
GCN_number 8636
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8636 SUBJECT: Radio observation of GRB 081109 with ATCA DATE: 08/12/08 04:16:50 GMT FROM: Aquib Moin at CIRA/ATNF Aquib Moin (Curtin Institute of Radio Astronomy / Australia Telescope National Facility), Steven Tingay (Curtin Institute of Radio Astronomy), Chris Phillips (Australia Telescope National Facility), Gregory Taylor (University of New Mexico), Mark Wieringa (Australia Telescope National Facility) and Ralph Martin (Perth Observatory) report: We observed the REM position of the GRB 081109 optical afterglow (GCN 8501) at 4.800 and 4.928 GHz with the Australia Telescope Compact Array (ATCA) between 01:15:05 UT, November 24, 2008 and 20:35:30 UT, November 25, 2008. We did not detect a radio source at the optical afterglow position of the GRB 081109 (GCN 8501). The data at 4.800 and 4.928 GHz were merged and the radio flux density at the afterglow position found out to be 25 +/- 92 uJy/beam (1-sigma). The Australia Telescope Compact Array (/ Parkes telescope / Mopra telescope / Long Baseline Array) is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. See the 4.800 & 4.928 GHz combined image at: http://cira.ivec.org/dokuwiki/doku.php/grb/grb081109_field_image