//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8932 SUBJECT: GRB 090305: Swift detection of a short burst DATE: 09/03/05 05:38:42 GMT FROM: David Palmer at LANL A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC), S. T. Holland (CRESST/USRA/GSFC), C. B. Markwardt (CRESST/GSFC/UMD), C. Pagani (PSU), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Swift Team: At 05:19:51 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090305 (trigger=345127). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 241.756, -31.567 which is RA(J2000) = 16h 07m 02s Dec(J2000) = -31d 34' 00" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single short spike with a duration of about 0.4 sec. The peak count rate was ~2500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 05:21:23.8 UT, 92.7 seconds after the BAT trigger. No source was detected in the promptly available XRT data in an exposure time of 92.8 seconds before Swift slewed away. We are waiting for the full dataset to detect and localise the XRT counterpart. UVOT took a finding chart exposure of 102 seconds with the White filter starting 96 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. Because part of the 2.7'x2.7' sub-image was not received, the overlap with the BAT error circle is uncertain. The overlap is at most 25%. The coverage of the BAT error circle by the 8'x8' region for the list of sources generated on-board is uncertain because the large number of sources filled the available telemetry. No correction has been made for the expected extinction corresponding to E(B-V) of 0.22. We note the presence of a ROSAT survey source, 1RXS J160703.2-313251, within the BAT error circle. Further data are required to determine whether this object is related to the burst. Burst Advocate for this burst is A. P. Beardmore (apb AT star.le.ac.uk). 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: 8933 SUBJECT: GRB090305: GMOS-S Candidate Optical Afterglow DATE: 09/03/05 10:32:47 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko, B. E. Cobb, D. A. Perley, and J. S. Bloom (UC Berkeley) report on behalf of a larger collaboration: We have imaged the field of the short GRB 090305 (Beardmore et al., GCN 8932) with GMOS mounted on the Gemini South telescope beginning approximately 27 minutes after the burst. Observations were taken in the Sloan g', r', and i' filters and cover nearly the entire BAT error circle. Inside the BAT error circle, we find a fading point source at the location (J2000.0): RA: 16:07:07.61 Dec: -31:33:21.9 Calibrating with respect to the USNO-B1 object at 16:07:06.58, -31:33:37.9 (R2=18.99), we measure an initial magnitude of R ~ 23.3. The source fades by approximately 1.1 mag over the next two hours, corresponding to a power-law decay index of ~ 0.6 (assuming no contribution from an underlying host galaxy). At this point we tentatively consider this source the afterglow of GRB090305, although we await confirmation from the XRT. We wish to thank the staff at Gemini South, in particular Peter Pessev, for performing our target of opportunity observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8934 SUBJECT: GRB 090305: Magellan confirmation of the optical afterglow DATE: 09/03/05 12:40:28 GMT FROM: Edo Berger at Harvard E. Berger (Harvard) and D. Kelson (OCIW) report: "We imaged the BAT error circle of the short GRB 090305 (GCN 8932) with IMACS on the Magellan/Baade 6.5-m telescope. Observations were taken in R band on 2009 March 5 at 06:48 and 09:11 UT (88 and 231 min after the burst, respectively). We confirm the existence of the fading source reported by Cenko et al. from Gemini South observations (GCN 8933) and consider this source to be the afterglow of GRB 090305." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8936 SUBJECT: GRB 090305, Swift-BAT refined analysis DATE: 09/03/05 18:15:07 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), 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-61 to T+242 sec from the recent telemetry downlink, we report further analysis of BAT GRB 090305 (trigger #345127) (Beardmore et al., GCN 8932). The BAT ground-calculated position is RA, Dec = 241.764, -31.572 deg which is RA(J2000) = 16h 07m 03.5s Dec(J2000) = -31d 34' 20.9" with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment). This position is 1.3 arcmin from the optical afterglow reported by Cenko et al. (GCN Circ 8933). The partial coding was 50%. The lightcurve consists of two pulses, the first about 0.08 seconds long and the second about 0.28 seconds long. T90 (15-350 keV) is 0.4 +- 0.1 sec (estimated error including systematics). There was very little emission seen in the BAT low energy band, 15-25 keV. The time-averaged spectrum from T+0.0 to T+0.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.86 +- 0.33. The fluence in the 15-150 keV band is 7.5 +- 1.3 x 10^-08 erg/cm2. The 1-sec peak photon flux measured from T-0.29 sec in the 15-150 keV band is 1.9 +- 0.4 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/345127/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8937 SUBJECT: GRB 090305: Swift-XRT refined analysis DATE: 09/03/06 01:17:55 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, K. L. Page, P.A. Evans (U. Leicester), C. Pagani, J. Kennea, D.N. Burrows (PSU) report on behalf of the Swift-XRT team : The Swift-XRT began observing the field of the short GRB 090305 (Beardmore et al. GCN Circ. 8932) in photon counting mode at 2009-03-05T05:21:37, 103.4 s after the trigger. The first orbit of data lasted only 90 s before the spacecraft slewed to another target because of an observing constraint. The default data processing does not reveal any X-ray source during the first orbit (103.4 to 193.5 s post trigger), either within the BAT refined error circle (Krimm et al. GCN Circ. 8936) or at the location of the optical afterglow (Cenko et al. GCN Circ. 8933) - the latter occurring close to a bad-column on the XRT CCD. However, by relaxing the default screening criteria we find 8 counts in a 10 pixel radius circle extraction region at the location of the optical afterglow, compared with a predicted background level of 1.0 count (where an annulus with radii 15 to 100 pixels was used to sample the local background level), implying a greater than 99.99 percent confidence detection (Kraft, Burrows, and Nousek 1991, Ap. J., 374, 344). The clustering of the counts, their proximity to the location of the optical afterglow and their detection significance allow us to conclude the afterglow was detected by the XRT at this time. The estimated count rate is 0.112 +0.051 -0.041 count/s (where a systematic error of 5 percent has been included in the 1 sigma error estimate to account for the PSF correction uncertainty). Applying a canonical GRB count to observed flux conversion factor of 5e-11 erg cm^-2 count^-1 (for a photon index of 1.98, Evans et al. 2009, MNRAS, submitted. arXiv:0812.3662, http://www.swift.ac.uk/xrt_spectra), we estimate the observed 0.3-10 keV flux was (5.5 +2.6 -2.0)e-12 erg cm^-2 s^-1. A further 2.05 ks of data was taken in orbit two, from 3.92 to 5.97 ks after the trigger, where the optical afterglow position was located away from the XRT CCD bad column. This showed the source was no longer detected and a 3 sigma upper limit to the count rate of 7.0e-3 count/s was obtained. Using all of the available data after the first orbit (i.e. presently an exposure of 12.64 ks from 3.92 to 46.1 ks post trigger) reduces the 3 sigma upper limit to 1.7e-3 count/s. The X-ray data suggest the source faded with a decay slope of at least ~0.8. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8938 SUBJECT: GRB 090305: Swift/UVOT Upper Limits DATE: 09/03/06 12:49:24 GMT FROM: Stephen Holland at USRA/NASA/GSFC/SSC S. T. Holland (CRESST/GSFC/USRA) and A. P. Beardmore (U Leicester) report on the behalf of the Swift UVOT team: The Swift/UVOT observed the field of GRB 090305 starting 78 s after the BAT trigger (Beardmore, et al. 2009, GCN Circ. 8932). Settled exposures started at T+96 s. We do not find any new source, relative to the DSS, USNO-B1.0, or 2MASS, or any variable source at the position of the GMOS-S afterglow (Cenko, et al. 2009, GCN Circ. 8933). Preliminary 3-sigma upper limits for detecting a source in the white finding chart, and the co-added images, using a 2.5 arcsecond radius circular aperture, are Filter T_start T_stop Exp(s) Mag ------------------------------------------ white 96 198 100 >20.6 v 3503 11,765 1034 >20.6 b 4323 15,980 1278 >21.8 u 4118 5755 393 >20.6 uvw1 3913 5550 393 >20.6 uvm2 3708 5345 393 >20.3 uvw2 4734 17,549 1723 >21.6 white 4528 16,892 1982 >22.7 ------------------------------------------ The quoted upper limits have not been corrected for the expected Galactic extinction along the line of sight corresponding to a reddening of E_{B-V} = 0.21 mag (Schlegel, et al., 1998, ApJS, 500, 525). All photometry is on the UVOT photometry system described in Poole et al. (2008, MNRAS, 383, 627). The GMOS-S afterglow is located in the wings of the B = 13.72 mag USNO-B1.0 star 0584-0391760. UVOT photometry at this location is contaminated by this star. Please update my e-mail address in your Address Book to . / \ / //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8941 SUBJECT: IPN localization of short GRB 090305C DATE: 09/03/06 18:09:18 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 and Konus-RF teams, K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku-WAM team, J. Cummings, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of the Swift-BAT team, A. von Kienlin, G. Lichti, and A. Rau, and K. Hurley on behalf of the INTEGRAL SPI-ACS team report: Suzaku-WAM, Konus-Wind, Konus-RF, Swift-BAT, and INTEGRAL-SPI-ACS observed the short GRB 090305C at about 62379 s UT (17:19:39). The burst was outside the coded field of view of the BAT. The burst light curve shows a multipeaked structure with a duration of ~1 sec. We have triangulated it to the following 3-sigma error box: ----------------------------------------------- RA(2000), deg Dec(2000), deg ----------------------------------------------- Center: 34.187 (02h 16m 45s) -22.840 (-22d 50' 23") Corners: 34.482 (02h 17m 56s) -17.203 (-17d 12' 09") 34.645 (02h 18m 35s) -19.974 (-19d 58' 28") 33.140 (02h 12m 34s) -28.787 (-28d 47' 14") 33.533 (02h 14m 08s) -25.759 (-25d 45' 32") ----------------------------------------------- The error box area is 2.524 sq. deg. This error box may be improved. The Konus-Wind light curve of this GRB and the IPN triangulation map is available at http://www.ioffe.ru/LEA/GRBs/GRB090305_T62376/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8957 SUBJECT: GRB 090305C: Suzaku WAM observation of the prompt emission DATE: 09/03/09 09:36:28 GMT FROM: Makoto Tashiro at Saitama U/Swift GRB 090305C: Suzaku WAM observation of the prompt emission W. Iwakiri, M. Tashiro, Y. Terada, Y. Urata, A. Endo, K. Onda, N. Kodaka, K. Morigami, T. Sugasahara (Saitama U.), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Sugita, K. Yamaoka (Aoyama Gakuin U.), M. Ohno, M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa (RIKEN), T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.), E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara, N. Ohmori, K. Kono, H. Hayashi, (Univ. of Miyazaki), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The IPN localized short GRB 090305C (Golenetskii et al., GCN 8941) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 17:19:38.326 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0 +0.2s, ending at T0+1.3s with a duration (T90) of about 0.9 seconds. The fluence in 100 - 1000 keV was 1.85(-0.58, +0.13)x 10^-06 erg/cm2. The 0.5-s scaled peak flux measured from T0+0s was 4.13(-0.97, +0.19) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0+0s to T0+1.5s is fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.05(-0.49, 0.38), and Epeak 835 ( -237, 618) keV (chi^2/d.o.f. = 5.20/13). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8972 SUBJECT: GRB090305B: Fermi GBM detection DATE: 09/03/10 17:50:24 GMT FROM: Colleen A. Wilson at NASA/MSFC/NSSTC Colleen A. Wilson-Hodge (NASA/MSFC) reports on behalf of the Fermi GBM Team: "At 01:14:35.72 UT on 05 March 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090305B (trigger 257908477 / 090305052). The on-ground calculated location, using the GBM trigger data, is RA = 155.1, DEC = 68.1 (J2000 degrees, equivalent to 10 h 20 m, 68 d 06'), with an uncertainty of 5.4 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 40 degrees. The GBM light curve shows/consists of a single peak with a duration (T90) of about 2 s (8-1000 keV). The time-averaged spectrum from T0-0.5 s to T0+2.5 s is best fit by a Band function with Epeak = 770+/- 230 keV, alpha = -0.50 +/- 0.17, and beta = -1.9 +/- 0.2. The event fluence (8-1000 keV) in this time interval is (2.7 +/- 0.2)E-06 erg/cm^2. The 64-msec peak photon flux measured starting from T0+0.288 s in the 8-1000 keV band is 11 +/- 2 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: 9004 SUBJECT: GRB090305B: MASTER-net prompt optical short burst observations DATE: 09/03/16 10:21:16 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.V. Parhomenko, Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh, T.Kopytova Ural State University, Kourovka S.Yazev, K.Ivanov Irkutsk State University There are 6 MASTER Very Wide Field cameras located at Kislovodsk and Irkutsk with common FOW = 6000 square degrees (http://observ.pereplet.ru/). One of the four MASTER Very Wide Field Cameras located at Kislovodsk (D=50 mm, 4x1000 square degrees, 11 Mpx) has observed ~80% 1-sigma Fermi error box (Colleen A. Wilson-Hodge, GCN 8972) with 1s exposure during all night: 7 hours befoure, during and 1 hours after GRB Time without time gap between images. Our unfiltered images are calibrated relative to Tycho stars (V). The magnitude limit of the each emage is ~9.5 m at the edge of FOW. We do not detect OT inside part of the error box (Colleen A. Wilson-Hodge, GCN 8972) brighter than 9.2 mag before and after trigger time. We conclude in case that GRB inside our FOW that: 1). the optical fluence during the short 2 s GRBurst is limited by ~<= 1 x 10E-8 erg/cm_2 excluding possible host galaxy absorbtion. The event fluence (8-1000 keV) in this time interval is (2.7 +/- 0.2)E-06 erg/cm^2 (Colleen A. Wilson-Hodge, GCN 8972). So: 2). Optical-Fluence/Gamma-Fluence(8-1000 keV) ~ < 1/100 The same ratio for long GRB080319B is Optical-Fluence/Gamma-Fluence(8 - 1000 keV) ~ 1/140 (Naked Eye GRB, Racusin, Karpov et al., Nature, vol.455, 183, 2008). The film of our observations (from 10 s before and 15 s after GRB time) is available at http://observ.pereplet.ru/images/GRB090305B/GRB090305B_full2.gif White & black circles are the 1-sigma & 3-sigma+systematic (2 degrees) error boxes correspondingly. Black rectangle is the IPN error box (Palshin et al., private communication). The FOWs of the 2 cameras are available at http://observ.pereplet.ru/images/GRB090305B/FOW090305.png The reduction is continued. The message may be cited. mailto: lipunov@sai.msu.ru