//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9962 SUBJECT: GRB 090929A: Fermi GBM detection DATE: 09/09/29 07:46:14 GMT FROM: Arne Rau at MPE Arne Rau (MPE) report on behalf of the Fermi GBM Team: "At 04:33:03.97 UT on 29 September 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090929A (trigger 275891585 / 090929190). The on-ground calculated location, using the GBM trigger data, is RA = 51.7, DEC = -7.3 (J2000 degrees, equivalent to 03h 27m, -07d 18'), with an uncertainty of 1.3 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 122 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of multiple short peaks with a duration (T90) of about 8.5 +/- 0.4 s (8-1000 keV). The time-averaged spectrum from T0+0.002s to T0+4.896s is best fit by a power law function with an exponential high energy cutoff. The power law index is -0.52 +/- 0.06 and the cutoff energy, parameterized as Epeak, is 610.9 +/- 44.5 keV (chi squared 439 for 393 d.o.f.). The event fluence (8-1000 keV) in this time interval is (1.06 +/- 0.03)E-05 erg/cm^2. The 1.822-sec peak photon flux measured starting from T0+0.002 s in the 8-1000 keV band is 10.9 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9963 SUBJECT: GRB 090929B: Swift detection of a burst DATE: 09/09/29 10:37:12 GMT FROM: David Palmer at LANL C. Pagani (PSU), A. P. Beardmore (U Leicester), S. Campana (INAF-OAB), V. D'Elia (ASDC), C. Gronwall (PSU), D. Grupe (PSU), C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC), N. P. M. Kuin (MSSL), J. Mao (INAF-OAB), P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-IASFPA), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 10:09:07 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090929B (trigger=371050). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 117.705, -0.632 which is RA(J2000) = 07h 50m 49s Dec(J2000) = -00d 37' 55" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with most activity in multiple peaks from T-10 sec to T+50 s, and additional peaks at T+150 sec, during the XRT observations. The peak count rate was ~7000 counts/sec (15-350 keV), at ~40 sec after the trigger. The XRT began observing the field at 10:10:31.3 UT, 84.1 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 117.7202, -0.6574 which is equivalent to: RA(J2000) = 07h 50m 52.84s Dec(J2000) = -00d 39' 26.6" with an uncertainty of 5.3 arcseconds (radius, 90% containment). This location is 106 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 1.49e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 97 seconds with the White filter starting 93 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 19.6 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 0.07. We note there is a bright (10th mag) star less than 2 arcsec from the XRT position which complicates the analysis of the UVOT data. 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.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9964 SUBJECT: GRB 090929: Enhanced Swift-XRT position DATE: 09/09/29 14:00:14 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 2438 s of XRT Photon Counting mode data and 2 UVOT images for GRB 090929, 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 = 117.72015, -0.65764 which is equivalent to: RA (J2000): 07h 50m 52.84s Dec (J2000): -00d 39' 27.5" with an uncertainty of 1.8 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9965 SUBJECT: Correction: GRB 090929B: Enhanced Swift-XRT position DATE: 09/09/29 14:09:34 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team: GCN Circ. 9964 referred to GRB 090929 when, in fact, the position given is for GRB 090929B (GCN Circ. 9963). The correct text should read Using 2438 s of XRT Photon Counting mode data and 2 UVOT images for GRB 090929B, 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 = 117.72015, -0.65764 which is equivalent to: RA (J2000): 07h 50m 52.84s Dec (J2000): -00d 39' 27.5" with an uncertainty of 1.8 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). We apologise for any confusion. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9966 SUBJECT: GRB 090929A BAT location of the Fermi GBM burst DATE: 09/09/29 14:15:48 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift J. R. Cummings (GSFC/UMBC) and H. Krimm (GSFC/USRA) on behalf of the Swift team The Fermi-GBM burst GRB 090929A (Rau, GCN Circular# 9962) occurred during a preplanned Swift slew maneuver. A strong source was found in a mosaic of images from BAT event data, which is often collected during slews. The source location was RA, Dec = 56.494, -5.952 or RA (J2000) 03h 45m 57.9s Dec (J2000) -05d 57' 50" with an estimated 90% containment error radius of 3 arcmin. The partial coding was 73-90% during the burst. We define the trigger time as 04:33:08 UTC. As seen in BAT, the burst had three progressively weaker peaks, at T+1, T+4, and T+8. The peak count rate (15-350 keV) was ~18000 counts/sec at T+2 sec. T90 was about 10 seconds. A Swift TOO has been requested and approved. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9967 SUBJECT: GRB 090929B: RAPTOR Discovery of Optical Counterpart DATE: 09/09/29 16:46:34 GMT FROM: James Wren at LANL J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis, B. Norman of Los Alamos National Laboratory report: The RAPTOR telescope system responded to Swift trigger 371050 (Pagani et al., GCN 9963) under good observing conditions. Our narrow-field instruments began observing the location at 10:20:53.37 UTC, 11.77 minutes after the initial BAT trigger. Our initial images show an R~16.8 optical counterpart at the enhanced XRT location (Page et al., GCN 9965). The object fades steadily reaching R~18.0 at 10:50 UTC. Our unfiltered images were calibrated against the USNO-B1 R-band. Unfortunately, an 11th magnitude star is only 19 arcseconds away, limiting our photometric accuracy. Further analysis is ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9968 SUBJECT: Konus-RF observation of GRB 090929A DATE: 09/09/29 17:45:37 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, and D. Svinkin on behalf of the Konus-RF team, report: The bright GRB 090929A (Fermi-GBM trigger trigger 275891585: Rau, GCN 9962) localized by Swift-BAT (Cummings and Krimm , GCN 9966) triggered Konus-RF at T0=16384.747 s UT (04:33:04.747). The burst light curve shows several multipeaked pulses with a total duration of ~6 s. As observed by Konus-RF the burst had a fluence of 1.24(-0.11, +0.12)x10^-5 erg/cm2, and a 16-ms peak flux measured from T0-0.040 s of (2.02 +/- 0.46)x10^-5 erg/cm2/s (both in the 20 keV - 3 MeV energy range). The time-integrated spectrum of the burst (from T0-1.2 to T0+4.5 s) is well fitted (in the 10 keV - 3 MeV range) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), with alpha = -0.55(-0.11, +0.12), and Ep = 480(-54, +64) keV (chi2 = 120.1/119 dof). The spectrum accumulated over the burst maximum (from T0-0.2 to T0+0.1 s) is well fitted (in the 10 keV - 3 MeV range) by a power law with exponential cutoff model with alpha = -0.28(-0.14, +0.15), and Ep = 633(-71, +81) keV (chi2 = 44.0/56 dof). Fitting by GRB (Band) model yields the same alpha and Ep, and only an upper limit on the high energy photon index: beta < -3.06 (chi2 = 44.0/55 dof). All the quoted values are preliminary. All the quoted errors are at the 90% confidence level. The Konus-RF light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB090929_T16384/KRF/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9969 SUBJECT: GRB 090929B: Swift/UVOT Observations DATE: 09/09/29 19:13:57 GMT FROM: Peter Curran at MSSL P.A. Curran (MSSL-UCL), F. Marshall (GSFC), S. Holland (GSFC) and C. Pagani (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 090929B 94s after the BAT trigger (Pagani et al., GCN Circ. 9963). No optical afterglow is detected in the b, u or uvw2 UVOT exposures. There is a detection in the white filter, consistent with the enhanced XRT position (Goad et al. GCN 9964, Page et al. GCN 9965), the proposed optical counterpart (Wren et al. GCN 9967) and a USNO catalogued star (R2=19.3). Since the photometry is contaminated by a bright (R = 9.5), near-by star, we cannot determine the nature of the source at this time. Preliminary magnitudes and 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag ---------------------------------------------------------------- white 94 4032 292 18.7 +/- 0.5 b 3627 3827 197 >20.5 u 3422 3622 197 >20.3 uvw2 4038 4224 183 >20.3 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.07 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9970 SUBJECT: GRB 090929B: Skynet/DSO Observations DATE: 09/09/29 20:28:10 GMT FROM: Josh Haislip at U.North Carolina J. Haislip, D. Reichart, A. Smith, D. Caton, L. Hawkins, K. Ivarsen, M. Schubel, A. LaCluyze, A. Foster, J. Moore, A. Oza, M. Schubel, J. Styblova, A. Trotter, J. A. Crain, and M. Nysewander report: Skynet observed the Swift/BAT localization of GRB 090929B (Pagani et al., GCN 9963) with the 14" Dark Sky Observatory telescope in North Carolina beginning 12.0 minutes after the trigger in I. We do not detect the afterglow (Pagani et al., GCN 9963, Wren et al., GCN 9967) within the enhanced Swift/XRT localization (Goad et al., 9964; Page, GCN 9965). However, the nearby I = 9.07 mag (USNO B1) star complicates photometry. mean 1-sig. 1-sig. time 3-sig. sys. stat. since lim. cal. cal. cal. trig. tel. exp. fil. mag. stars unc. unc. (h) (# x s) (mag) (mag) 12.0 DSO-14 1 x 80 I 17.1 183 USNO B1 0.400 0.001 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9971 SUBJECT: GRB 090929B: Gemini-N upper limits DATE: 09/09/29 21:12:50 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara, D. B. Fox (PSU), N. Tanvir (U. Leicester), E. Berger (Harvard U.) and A. Levan (U. Warwick) report: On September 29.58 UT we observed the field of GRB 090929B (Pagani et al. GCN 9963) with Gemini-North + NIRI. We took a sequence of YJHK bands images under twilight conditions. No clear afterglow candidate has been found in the XRT refined error circle (GCN 9964 and 9965) to the following limits (3-sigma): J > 21.10 mag H > 19.53 mag K > 18.06 mag Our limits are estimated using detected 2MASS objects at comparable distance to the bright star (R = 9.5) which is located near the XRT error circle. We note the presence of a USNO catalogued star inside the refined error circle; the above limits are exclusive of that star. We thank the Gemini staff for performing these observations, in particular Ricardo Schiavon. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9973 SUBJECT: GRB 090929B: Swift-XRT refined analysis DATE: 09/09/30 01:40:54 GMT FROM: Claudio Pagani at PSU/Swift-XRT C. Pagani and L. Vetere (PSU) report on behalf of the Swift-XRT team: We have analysed 3.7 ks of XRT data for GRB 090929B (Pagani et al. GCN Circ. 9963), from 90 s to 16.3 ks after the BAT trigger. The first orbit of data was entirely taken in Windowed Timing (WT) mode for a total of 100 s. The remaining orbits are in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Page (GCN. Circ 9965). The light curve shows intense flaring activity during the first orbit with the strongest emission at approximately 180 counts s^-1 at T+150 s, during a peak also detected by the BAT (GCN Circ. 9963). The following orbits can be modeled with a broken power-law decay with an shallow phase of index of alpha=0.5 (+1.0, -0.6) followed by a steeper decay of index alpha=1.2+/-0.3 after ~T+5.6 ks. A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.68 (+/-0.05). The best-fitting absorption column is 2.2 (+/-0.1) x 10^21 cm^-2, in excess of the Galactic value of 5.4 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.01 (+0.18, -0.17) and a best-fitting absorption column of 1.6 (+0.5, -0.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.1 x 10^-11 (5.7 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 1.2, the count rate at T+24 hours will be 0.015 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.1 x 10^-12 (8.6 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00371050. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9975 SUBJECT: Konus-Wind observation of GRB 090929B DATE: 09/09/30 13:30:14 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 090929B (Swift-BAT trigger #371050: Pagani et al., GCN 9963) triggered Konus-Wind at T0=36565.377 s UT (10:09:25.377). The burst light curve shows a multipeaked structure with a total duration of ~20 s. As observed by Konus-Wind the burst had a fluence of (1.16 +/- 0.12)x10^-5 erg/cm2, and a 256-ms peak flux measured from T0+16.208 s of (3.80 +/- 0.90)x10^-6 erg/cm2/s (both in the 20 keV - 1 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+16.640 s) is well fitted (in the 20 keV - 1 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = -0.41 (-0.77, +1.16), the high energy photon index beta = -1.82(-0.59, +0.24), the peak energy Ep = 282(-78, +169) keV (chi2 = 52.4/59 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/GRB090929_T36565/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9976 SUBJECT: Konus-Wind observation of GRB 090929A DATE: 09/09/30 16:16:53 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The bright GRB 090929A (Fermi-GBM trigger trigger 275891585: Rau, GCN 9962) localized by Swift-BAT (Cummings and Krimm, GCN 9966) triggered Konus-Wind at T0=16387.790 s UT (04:33:07.790). As observed by Konus-Wind the burst had a fluence of 1.32(-0.24, +0.23)x10^-5 erg/cm2, and a 16-ms peak flux measured from T0+0.736 s of 2.04(-0.61, +0.60)x10^-5 erg/cm2/s (both in the 20 keV - 3 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+8.448 s) 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 = -0.47(-0.22, +0.25), and Ep = 574(-100, +151) keV (chi2 = 66.2/65 dof). Fitting by GRB (Band) model yields: the low-energy photon index alpha = -0.36(-0.29, +0.62), the high energy photon index beta = -2.16(-1.41, +0.43), the peak energy Ep = 494(-191, +175) keV (chi2 = 62.1/64 dof). These values are consistent with the Konus-RF results (Golenetskii et al., GCN 9968). 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/GRB090929_T16384/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9977 SUBJECT: GRB 090929A: Swift-XRT non-detection DATE: 09/09/30 16:21:47 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team: Swift performed a short Target of Opportunity observation of GRB 090929A about 13 hours after the burst (Rau, GCN Circ. 9962; Cummings & Krimm, GCN Circ. 9966; Golenetskii et al., GCN Circ. 9968). This area of sky was a hot target for the XRT, so only a short observation was performed, with 1.4 ks of data being collected in Photon Counting mode. We do not detect a source within the BAT error circle, to a 90% upper limit of 0.015 count s^-1 over 0.3-10 keV. Assuming a typical counts to flux conversion of 3.8 x 10^-11 erg cm^-2 ct^-1 (Evans et al., 2009, MNRAS, 397, 1177), this corresponds to an observed flux of 5.7 x 10^-13 erg cm^-2 s^-1. We note that this is not a very constraining upper limit, because of the greater than usual background caused by the high XRT CCD temperature and the short exposure time. Filtering out all photons below 1 keV, a more stringent upper limit of 9 x 10^-3 count s^-1 (1-10 keV; observed flux of ~3.4 x 10^-13 erg cm^-2 s^-1) can be determined. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9979 SUBJECT: GRB 090929B, Swift-BAT refined analysis DATE: 09/09/30 21:04:27 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), C. Pagani (PSU), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+691 sec from the recent telemetry downlink, we report further analysis of BAT GRB 090929 (trigger #371050) (Pagani, et al., GCN Circ. 9963). The BAT ground-calculated position is RA, Dec = 117.712, -0.645 deg which is RA(J2000) = 07h 50m 50.9s Dec(J2000) = -00d 38' 41.2" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 63%. The mask-weighted lightcurve shows many peaks interspersed with intervals with no detected flux, from T-10 to T+380 sec when the source left the coded field of view due to a observing constraint. There may have been small and/or low-energy peaks beyond this time. The largest peak was at about T+30 to T+40 sec. T90 (15-350 keV) was 360 +- 20 sec (estimated error including systematics). The time-averaged spectrum from T-9.8 to T+371.0 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.85 +- 0.08. The fluence in the 15-150 keV band is 5.9 +- 0.3 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+30.67 sec in the 15-150 keV band is 3.3 +- 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/371050/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9980 SUBJECT: GRB 090929A, Swift-BAT refined analysis DATE: 09/09/30 21:06:52 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), K. Page (U Leicester), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): We report further analysis of Fermi-GBM GRB 090929A (Rau, et al., GCN Circ. 9962). The BAT ground-calculated position is the same as stated in Cummings et al. (GCN Circ. 9966), RA, Dec = 56.494, -5.952 or RA (J2000) 03h 45m 57.9s Dec (J2000) -05d 57' 50" with an estimated 90% containment error radius of 3 arcmin. The partial coding was 73-90% during the burst. The mask-weighted lightcurve shows multiple peaks and spikes, at T+1, T+2, T+4, T+5, and T+10 sec, where T0 is 04:33:07. T90 was 7 +- 2 seconds. The time-averaged spectrum from T0 to T+12 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.96 +- 0.04. The fluence in the 15-150 keV band is 1.69 +- 0.07 x 10^-06 ergs/cm2. The 1-sec peak photon flux measured from T+0.5 sec in the 15-150 keV band is 5.9 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9981 SUBJECT: GRB 090929A: Swift/UVOT Observations DATE: 09/09/30 22:34:16 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and K. L. Page (U. Leicester) report on behalf of the Swift/UVOT team. Swift/UVOT began settled observations of GRB 090929A about 13 hours after the burst (Rau, GCN Circ. 9962; Cummings & Krimm, GCN Circ. 9966; Golenetskii et al., GCN Circ. 9968; Page, GCN Circ 9977). Due to the presence of a 9th magnitude (V) star 45" from the center of the BAT position, data were only obtained in the UVM2 filter. We do not detect any uncatalogued UV source within the BAT error circle. The 3-sigma upper limit and summed exposure is reported below: FILTER T_start(s) T_stop Exposure Mag/3UL ============================================================= UVM2 47411 52924 2252 >21.26 ============================================================= This magnitude is not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.07 (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9992 SUBJECT: GRB 090929A: Suzaku WAM observation of the prompt emission DATE: 09/10/05 08:59:49 GMT FROM: Norisuke Ohmori at Miyazaki U N. Ohmori, E. Sonoda, K. Kono, H. Hayashi, A. Daikyuji, Y. Nishioka, K. Noda, M. Yamauchi (Univ. of Miyazaki), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa, T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.), Y. Urata (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The long GRB 090929A (Fermi-GBM trigger 275891585 / 090929190; Arne Rau et al., GCN9962) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 04:33:04.634 UT (=T0). The observed light curve shows a bright multi-peaked structure starting at T0-1 s, ending at T0+5 s. The total T90 duration is about 3.8 seconds. The fluence in 100 - 1000 keV was 4.96 (-4.47, +5.32) x10-6 erg/cm2. The 1-s peak flux measured from T0-0.5s was 5.59 (-0.68, +0.53) photons/cm2/s in the same energy range. The incident angle for this burst is not good, so the fluence and peak flux might have large systematic uncertainties. Preliminary result shows that the time-averaged spectrum from T0-1s to T0+5s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.86(-0.80, +0.36), and Epeak 557(-98, +117) keV (chi2/d.o.f. = 125/98). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst is available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9993 SUBJECT: GRB 090929B: Suzaku WAM observation of the prompt emission DATE: 09/10/05 09:02:34 GMT FROM: Norisuke Ohmori at Miyazaki U N. Ohmori, E. Sonoda, K. Kono, H. Hayashi, A. Daikyuji, Y. Nishioka, K. Noda, M. Yamauchi (Univ. of Miyazaki), K. Yamaoka (Aoyama Gakuin U.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.), Y. Urata (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), Y. E. Nakagawa, T. Tamagawa (RIKEN), S. Hong (Nihon U.), S. Sugita (Nagoya U.), N. Vasquez (Tokyo Tech.), on behalf of the Suzaku WAM team, report: The long GRB 090929B (Swift-BAT trigger #371050; Pagani et al., GCN 9963, Krimm et al. GCN 9979) was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 10:09:23.633 UT (=T0). The observed light curve shows a multi-peaked structure, starting at T0-2 s and ending at T0+20 s, with a total duration (T90) of about 18 s. The fluence in 100 - 1000 keV was (3.92 $B!^(B 0.63) x 10-6 erg/cm2. The 1-s peak flux measured from T0+1 s was 1.42 (-0.25. +0.24) photons/cm2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-2 s to T0+20 s is well fitted by a single power-law with a photon index of 1.96 (-0.17, +0.20) (chi2/d.o.f = 23.4/27). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10010 SUBJECT: Detection of a short GRB 090929A by RT-2 Experiment DATE: 09/10/11 06:52:39 GMT FROM: Sandip K. Chakrabarti at S.N. Bose Nat. Centre for Basic Sci. S. K. Chakrabarti, A. Nandi, D. Debnath, T. C. Kotoch (ICSP, Kolkata, India), A. R. Rao, J. P. Malkar, M. K. Hingar, V. K. Agrawal (TIFR, Mumbai, India), T. R. Chidambaram, P. Vinod, S. Sreekumar (VSSC, Thiruvananthapuram, India), Y. D. Kotov, A. S. Buslov, V. N. Yurov, V. G. Tyshkevich, A. I. Arkhangelskij, R. A.Zyatkov (MephI, Moscow, Russia) report: The RT-2 Experiment onboard the CORONAS-PHOTON satellite has detected GRB 090929A (Fermi-GBM trigger 275891585/090929190; Rau, GCN 9962) which is triggered at T0 = 04h 33m 04s (UT). The satellite was in the LIGHT mode (pointing towards the SUN) with GOOD time (away from the polar and SAA regions) observation of 1537 sec starting at 04h 21m 20sec (UT) and ending at 04h 46m 57sec (UT). The burst light curve (1 sec bin) shows double peak profile of total duration of around 5 sec. The strongest peak count rate is ~ 310 cts/sec. This burst is also independently detected by KONUS-RF, another instrument onboard CORONAS-PHOTON satellite (Golenetskii et al., 2009, GCN 9968). Both RT-2/S and RT-2/G detectors have registered the prompt emission from the GRB090929A in the energy band of 60 – 1000 with strongest emission in the energy band of 60 – 215 keV. The light curve is available at the web-site: http://csp.res.in/rt2_files/grb090929-lc.html