GRB080905A

This page lists all entries on GRB080905A in GRBweb

Summary Fermi GBM IPN Swift GCN 8180 GCN 8181 GCN 8185 GCN 8187 GCN 8190 GCN 8195 GCN 8202 GCN 8203 GCN 8204 GCN 8208 GCN 21550

Summary table
Variable Value Source
GRB_name_Fermi GRB080905499
T0 11:58:54 UTC GCN_circulars,Swift Det
ra 287.6741° Swift
decl -18.8802° Swift
pos_error 2.07e-04° Swift
T90 0.96 s Fermi_GBM
T90_error 0.345 s Fermi_GBM
T90_start 11:58:54.974 UTC Fermi_GBM
fluence 8.50e-07 erg/cm² Fermi_GBM
fluence_error 4.62e-08 erg/cm² Fermi_GBM
redshift 0.1218
T100 1.934 s
GBM_located False
mjd 54714.499236111114 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB080905499
trigger_name bn080905499
ra 287.7000°
decl -18.9000°
pos_error 4.70e+00°
datum 2008-09-05
t_trigger 11:58:55.038 UTC
T90 0.96 s
T90_error 0.345 s
T90_start 11:58:54.974 UTC
fluence 8.50e-07 erg/cm²
fluence_error 4.62e-08 erg/cm²
flux_1024 2.34e+00 erg/cm²/s
flux_1024_error 1.35e-01 erg/cm²/s
flux_1024_time -6.40e-02 erg/cm²/s
flux_64 6.32e+00 erg/cm²/s
flux_64_error 6.75e-01 erg/cm²/s
IPN table
GRB_name GRB080905A
ra 287.6625°
decl -18.8833°
pos_error 5.00e-02°
redshift 0.1218
Swift table
GRB_name GRB080905A
t_trigger 11:58:54 UTC
ra 287.6741°
decl -18.8802°
pos_error 2.07e-04°
T90 1.0 s
fluence 1.40e-07 erg/cm²
redshift 0.1218
GCN 8180 table
GRB_name GRB080905A
GCN_number 8180
Detection_method Swift Det
t_trigger 11:58:54 UTC
ra 287.6620°
decl -18.8770°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8180 SUBJECT: GRB 080905: Swift detection of a probably-short burst DATE: 08/09/05 12:19:45 GMT FROM: Claudio Pagani at PSU/Swift-XRT C. Pagani (PSU), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (CRESST/GSFC/USRA), J. Mao (INAF-OAB), C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), B. Preger (ASDC), J. L. Racusin (PSU), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-IASFPA), P. Schady (MSSL-UCL), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), M. C. Stroh (PSU), E. Troja (INAF-IASFPA), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 11:58:54 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080905 (trigger=323870). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 287.662, -18.877 which is RA(J2000) = 19h 10m 39s Dec(J2000) = -18d 52' 37" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows 3 peaks with a total duration of about 2 sec. The spectrum is hard, with most response above 25 keV in the BAT energy range. The peak count rate was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 12:01:05.3 UT, 130.4 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 287.67363, -18.87986 which is equivalent to: RA(J2000) = 19h 10m 41.67s Dec(J2000) = -18d 52' 47.5" with an uncertainty of 2.8 arcseconds (radius, 90% containment). This location is 40 arcseconds from the BAT onboard position, within the BAT error circle. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 8.95e+20 cm^-2 (Kalberla et al. 2005). UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 114 seconds after the BAT trigger. No 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 3-sigma upper limit at the location of the XRT position is 17.8 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.14. Burst Advocate for this burst is C. Pagani (pagani AT astro.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 8181 table
GRB_name GRB080905A
GCN_number 8181
Detection_method Optical
ra 287.6730°
decl -18.8823°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8181 SUBJECT: GRB 080905: R & I-band optical observations DATE: 08/09/05 16:47:34 GMT FROM: Javier Gorosabel at IAA-CSIC P. Tristram (MOA, Univ. of Canterbury), A.J. Castro-Tirado (IAA-CSIC, Granada), P. Yock (Univ. of Auckland), J. Gorosabel (IAA-CSIC, Granada), A. de Ugarte Postigo (ESO, Santiago), report on behalf of a larger collaboration: "Following the detection by Swift of GRB 080905 (Pagani et al. GCNC 8180), we have obtained R & I-band images at the 0.6m telescope of the Mt. John Observatory, New Zealand. The images were taken starting on Sep 5.529 UT (i.e. 43 min post-burst). We do not detect any object brighter than R=20.8 and I=20.3 consistent with the XRT position. We note the presence of two extended R~15 (R~15.4) objects 8.5" (10") South (North-East) (Object A at RA(J2000)=19:10:41.51, DEC(J2000)=-18:52:56.2 and Object B at RA(J2000)=19:10:41.10, DEC(J2000)=-18:52:40.6, respectively) from the XRT position which could be hosting the probably-short GRB 080905. A finding chart can be found at http://www.sc.eso.org/~adeugart/GRB/080905/080905fc.jpg"
GCN 8185 table
GRB_name GRB080905A
GCN_number 8185
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8185 SUBJECT: GRB 080905A: Swift-XRT Refined Analysis DATE: 08/09/06 02:31:56 GMT FROM: Claudio Pagani at PSU/Swift-XRT C. Pagani and J. Racusin (PSU) report on behalf of the Swift-XRT team: We have analyzed the first orbit of Swift-XRT data for the short GRB 080905A (Pagani et al., GCN 8180) beginning at T0+130 seconds to T0+1.1 ks. The enhanced XRT position given in GCN Circ 8180 is 40 arcseconds from the BAT onboard position, within the BAT error circle. The XRT lightcurve shows an initial count rate of approximately 6 counts/s for the first 100 seconds of observations, followed by a steep decay and a shallower phase. The decaying lightcurve can be fit with a broken power-law with an initial decay index of 6.4+/-2.0, a break at approximately T0+400 seconds and a later decay index of 1.0+/-0.5. The spectrum of 1 ks of Photon counting mode data from the first orbit can be fit by an absorbed power-law with a photon index of 1.3+/-0.3 and absorption consistent with the Galactic value along the line of sight (9e20 cm^-2, Kalberla et al. 2005). The average observed (unabsorbed) flux of the PC mode data is 2.9e-9 (3.1e-10) ergs cm^-2 s^-1. Assuming the X-ray emission continues to decline at the same rate, we predict a 0.3-10.0 keV XRT count rate of 0.001 counts/s at T+24hr, which corresponds to an observed flux of 7e-14 ergs cm^-2 s^-1. This Circular is an official product of the Swift-XRT team.
GCN 8187 table
GRB_name GRB080905A
GCN_number 8187
Detection_method Swift-BAT Det
ra 287.6630°
decl -18.8650°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8187 SUBJECT: GRB 080905A, Swift-BAT refined analysis DATE: 08/09/06 16:51:33 GMT FROM: Scott Barthelmy at NASA/GSFC J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), C. Pagani (PSU), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) (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 080905A (trigger #323870) (Pagani, et al., GCN Circ. 8180). The BAT ground-calculated position is RA, Dec = 287.663, -18.865 deg, which is RA(J2000) = 19h 10m 39.1s Dec(J2000) = -18d 51' 55.4" with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 56%. The mask-weighted light curve shows three peaks; the first two are partially overlapping, starting at T+0.0 and ending at ~T+0.4 sec. The third peak starts at ~T+0.6 and ends at ~T+1.3 sec. T90 (15-350 keV) is 1.0 +- 0.1 sec (estimated error including systematics). The time-averaged spectrum from T+0.0 to T+1.1 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.85 +- 0.24. The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band is 1.3 +- 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/323870/BA/
GCN 8190 table
GRB_name GRB080905A
GCN_number 8190
Detection_method Other
ra 287.6739°
decl -18.8798°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8190 SUBJECT: GRB 080905A: NOT and VLT observations DATE: 08/09/06 18:40:26 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani (DARK/NBI), A. de Ugarte Postigo (ESO), J. P. U. Fynbo (DARK/NBI), A. J. Levan (Univ. Warwick), E. Rol (Univ. Leicester), N. R. Tanvir (Univ. Leicester), C. C. Thoene (DARK/NBI), J. Telting (NOT), A. Baran (Cracow Univ.), report on behalf of a larger collaboration: We observed the field of the short GRB 080905A (Pagani et al., GCN 8180) with the NOT and the VLT telescopes equipped with ALFOSC and FORS2, respectively. The NOT observations started on 2008 Sep 5.854 UT (8.51 hr after the GRB) and the total exposure time was 30 min. The VLT observations started on 2008 Sep 6.097 UT (14.3 hr after the GRB) and the total exposure was 40 min. All images were taken with the R filter. Inside the XRT error circle, we detect a single, faint source with R ~ 24 (against USNO-B1 stars), visible in both the NOT and VLT images. No variability of the source can be robustly determined, hence we cannot assess the relationship of this object with the GRB, especially given the relatively crowded field (Galactic latitude -12.6). Further observations are planned. The coordinates of this object are: RA(J2000) = 19:10:41.73 Dec(J2000) = -18:52:47.3 with an error of ~0.6". We note that in our NOT images (seeing ~1"), the extended objects identified by Tristram et al. (GCN 8181) appear resolved into several pointlike sources. Finding charts can be found at the following URL: http://www.astro.ku.dk/~malesani/GRB/080905A We acknowledge significant support from the observing staff at Paranal, in particular Swetlana Hubrig, Elena Mason and Andres Pino.
GCN 8195 table
GRB_name GRB080905A
GCN_number 8195
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 8195 SUBJECT: GRB 080905A: optical afterglow DATE: 08/09/07 10:35:30 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst A. de Ugarte Postigo (ESO), D. Malesani (DARK/NBI), A. J. Levan (Univ. Warwick), J. Hjorth (DARK/NBI), N. R. Tanvir (Univ. Leicester), report on behalf of a larger collaboration: We observed again the field of the short GRB 080905A (Pagani et al., GCN 8180) with the ESO VLT equipped with FORS2. R-band observations were carried out starting on 2008 Sep 7.004 UT (1.50 days after the GRB) and the total exposure time was 40 minutes. The object located inside the XRT error circle visible in our early VLT images (Malesani et al., GCN 8190) has clearly faded between the two observations, and is thus likely the optical afterglow of GRB 080905A. We note that this object is located outside the revised 2.2"-radius (90%) UVOT-enhanced XRT error circle (distance from center 4.6"), as provided at http://www.swift.ac.uk/xrt_positions/index.php (value of Sep 7.4 UT). In our second epoch image, which is deeper and has a better seeing (~0.9"), we also note the presence of a bright extended object, possibly a spiral galaxy, about 9" S, 3" E of the afterglow (partially covered by foreground stars). Finding charts can be found at http://www.astro.ku.dk/~malesani/GRB/080905A/#epoch2 We acknowledge significant support from the ESO observing staff at Paranal, in particular Elena Mason, Andres Pino and Swetlana Hubrig.
GCN 8202 table
GRB_name GRB080905A
GCN_number 8202
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 8202 SUBJECT: GRB 080905A: MITSuME Akeno optical upper limits DATE: 08/09/08 13:33:19 GMT FROM: Nobuyuki Kawai at Tokyo Tech H. Nakajima, T. Shimokawabe, Y.A. Mori, Y. Kudou, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We performed optical imaging observation of the field of GRB 080905A (C. Pagani et al. GCN 8180) with the 3-color 50cm MITSuME Telescope at Akeno, Japan from 12:40:12 UT (42min after the trigger) to 14:32:07 UT. In the co-added images of Ic, Rc, and g' bands, we did not detect any afterglow candidate in the XRT error circle. The 3-sigma limiting magnitudes based on USNO-B1.0 (I-band) and NOMAD (R-band,g'-band) stars are following: Filter Start(UT) End(UT) Exposure LimitMag --------------------------------------------------- g' 12:40:12 13:14:31 30 x 60 s 17.1 Rc 12:40:12 13:14:31 30 x 60 s 17.6 Ic 12:40:12 13:14:31 30 x 60 s 17.6 ---------------------------------------------------
GCN 8203 table
GRB_name GRB080905A
GCN_number 8203
Detection_method Swift-XRT Det
ra 287.6739°
decl -18.8802°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8203 SUBJECT: GRB 080905A: Enhanced Swift-XRT position DATE: 08/09/08 15:06:05 GMT FROM: Phil Evans at U of Leicester P.A. Evans, J.P. Osborne and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team: Using more data than were available at the time of de Ugarte Postigo et al. (GCN Circ 8195), the UVOT-enhanced X-ray position of GRB 080905A has been improved to RA, Dec = 287.67390, -18.88022 which is equivalent to: RA (J2000): 19 10 41.74 Dec (J2000): -18 52 48.8 with an uncertainty of 1.6 arcsec (90% confidence). This position lies 1.5" from the optical counterpart identified by Malesani et al (GCN Circ. 8190), consistent with that position. Position enhancement, using the XRT-UVOT alignment and matching to the USNO-B1 catalogue, 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 is an official product of the Swift-XRT team.
GCN 8204 table
GRB_name GRB080905A
GCN_number 8204
Detection_method Swift-BAT Det
ra 286.3000°
decl -18.2000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 8204 SUBJECT: GRB 080905A: Fermi Gamma-ray Burst Monitor detection DATE: 08/09/09 12:03:02 GMT FROM: Elisabetta Bissaldi at MPE E. Bissaldi, S. McBreen (MPE), V. Connaughton (UAH) and A. von Kienlin (MPE) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 11:58:55 UT on 5 September 2008, the Fermi GBM triggered and located GRB 080905A (trigger 242308736 / 080905499), which was also detected by Swift (Pagani et al., GCN 8180). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 286.3, Dec = -18.2 (J2000 degrees) (equivalent to J2000 19h 05m, -18d 12'), with a statistical uncertainty of 4.6 degree (radius, 1-sigma containment; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). This position is 1.5 deg from the Swift refined position (Evans et al., GCN 8203). The angle from the Fermi LAT boresight to the Swift position is 28 degrees. This short GRB consists of two peaks, the first from T0 to T0+0.4 sec and the second from T0+0.6 sec to T0+1.1 sec. The first peak shows substructure in agreement with the Swift-BAT refined analysis (J. Cummings et al., GCN 8187). T90 (50-300 keV) is about 1 sec. The time-averaged spectrum from T0 to T0+1 sec is well fit by a power law function with index -0.96 +/- 0.05. The fluence (50-300 keV) is 2.8(+/-0.2)E-07 erg/cm2 and the peak flux (50-300 keV) is 6.1 +/- 0.8 ph/cm2/s. The spectral analysis results presented above are preliminary; final results will be published in the Fermi GBM GRB Catalog."
GCN 8208 table
GRB_name GRB080905A
GCN_number 8208
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 8208 SUBJECT: GRB080905A: Swift/UVOT Upper Limits DATE: 08/09/10 13:18:20 GMT FROM: Peter Brown at PSU P. J. Brown and C. Pagani (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of GRB 080905A starting about 114 s after the BAT detection (Pagani et al., GCN Circ. 8180). We do not detect any source in the revised XRT error circle (Evans et al., GCN Circ. 8203) including the faint optical afterglow seen by Malesani et al. (GCN Circ. 8190) in any of the UVOT filters down to the following 3 sigma upper limits (where T_start and T_stop represent the elapsed time since the BAT trigger in seconds). Filter T_start(s) T_stop Exp(s) MagLimit white 114 970 198 >21.3 uvw2 730 750 19 >18.1 uvm2 626 4520 95 >19.2 uvw1 651 825 39 >18.8 u 675 850 39 >19.2 b 700 865 15 >18.9 v 220 1250 1014 >20.6 The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E(B-V) = 0.14 mag (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383,627).
GCN 21550 table
GRB_name GRB080905A
GCN_number 21550
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21550 SUBJECT: LIGO/VIRGO G298048: Swift UVOT detection and XRT upper limits DATE: 17/08/18 07:24:04 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), J.A. Kennea (PSU), A.A. Breeveld (UCL-MSSL), S. Campana (INAF-OAB), S.B. Cenko (NASA/GSFC), E. Troja (NASA/GSFC/UMCP), P.T. O'Brien (U. Leicester), S.D. Barthelmy (NASA/GSFC), A.P. Beardmore (U. Leicester), D.N. Burrows (PSU), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V.D'Elia(ASDC), S.W.K. Emery (UCL-MSSL), P. Giommi (ASI), C. Gronwall (PSU), H.A. Krimm (CRESST/GSFC/USRA), N.P.M. Kuin (UCL-MSSL), A.Y. Lien (GSFC/UMBC), F.E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J.A. Nousek (PSU), S.R. Oates (U. Warwick), J.P. Osborne (U. Leicester), C. Pagani (U. Leicester), K.L. Page (U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J.L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M.H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU) report on behalf of the Swift team: Swift has performed ToO observations of the proposed optical counterpart of LIGO/Virgo G298048 (Coulter et al. LVC GCN 21529). We obtained 2 ks of data from 53.8 to 55.8 ks after the LVC trigger. No X-ray source is detected at the location of the transient reported by Coulter et al. The 3-sigma upper limit at this location is 4.5e-3 ct/sec. For a typical GRB spectrum this corresponds to 1.8e-13 erg/cm^2/s (0.3-10 keV). Assuming a distance of 40 Mpc this corresponds to a 0.3-10 keV luminosity of 3.5e40 erg/s. D'Avanzo et al (2014, MNRAS, 442, 2342) compiled the observed 2-10 keV luminosity at 11 hours post-trigger for a complete sample of Swift-detected short GRBs; these were typically of order 1e41-1e43 erg/s. Our measurement corresponds to a 2-10 keV luminosity of 2.3e40 erg/s, ~an order of magnitude fainter than all of the other sGRBs in that paper apart from GRB 080905. However those authors also showed a correlation between Eiso and X-ray afterglow luminosity, so given the low Eiso (Goldstein et al., LVC Circ. 21528) this may not be surprising. The afterglow is detected in the Swift-UVOT data. Analysis is complicated by the nearby presence the galaxy NGC4993, but we obtain the following magnitudes: Filter Magnitude Start time Stop time u 16.9 ± 0.06 T0+53.8 ks T0+54.5 ks w1 17.74 ± 0.09 T0+55.0 ks T0+55.3 ks m2 19.26 ± 0.18 T0+54.5 ks T0+55.0 ks w2 19.12 ± 0.17 T0+55.3 ks T0+55.8 ks We note that it is very unusual for an optical counterpart to be found but no X-ray counterpart, especially given the brightness of the optical counterpart. Therefore, if this object is a GRB afterglow, it is atypical compared to the sample of Swift-BAT triggered objects observed to date. We suggest therefore that the object may be a blue (i.e. lanthanide-free) kilonova. This circular is an official product of the Swift team. [GCN OPS NOTE(18aug17): Per author's request, the trigger ID in the Subject-line was corected from 298045 to 298048.]