//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9540 SUBJECT: GRB 090621: Swift detection of a burst DATE: 09/06/21 04:53:59 GMT FROM: David Palmer at LANL P.A. Curran (MSSL-UCL), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester), D. M. Palmer (LANL), M. Stamatikos (NASA/ORAU), M. C. Stroh (PSU), T. N. Ukwatta (GSFC/GWU) and H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team: At 04:22:43 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090621 (trigger=355303). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 10.986, +61.968 which is RA(J2000) = 00h 43m 57s Dec(J2000) = +61d 58' 04" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed weak emission during the 8 seconds of the trigger interval. The peak count rate was ~1000 counts/sec (15-350 keV), at ~4 sec after the trigger. There was a second BAT trigger (trigger=355304) at 04:27:05, about 4 minutes after the initial trigger from the same location. This portion of the BAT light curve is not immediately available from TDRSS, but the retrigger could indicate an extended prompt phase. The XRT began observing the field at 04:24:40.46 UT, 117.3 seconds after the BAT trigger. XRT found an uncatalogued, variable X-ray source located at RA, Dec 11.0191, 61.9417 which is equivalent to: RA(J2000) = 00h 44m 04.58s Dec(J2000) = +61d 56' 30.2" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 110 arcseconds from the BAT onboard position, within the BAT error circle. There is a bright peak at about 250s after the initial trigger which could be X-ray emission during prolonged prompt emission. UVOT took a finding chart exposure of 150 seconds with the White filter starting 122 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 25% of the BAT 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 BAT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the large, but uncertain extinction expected. Burst Advocate for this burst is P.A. Curran (pac AT mssl.ucl.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: 9543 SUBJECT: GRB 090621: Swift-XRT Team refined analysis DATE: 09/06/21 12:18:05 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester) & P.A. Curran (UCL-MSSL) report on behalf of the Swift-XRT team: We have analysed the first four orbits of XRT data obtained for GRB 090621 (Curran et al., GCN Circ. 9540), comprising 192 s of Windowed Timing (WT) mode and 6.4 ks of Photon Counting (PC) mode. The refined XRT position is RA, Dec = 11.01982, 61.94115, which is equivalent to RA (J2000) = 00 44 04.76 Dec(J2000) = +61 56 28.1 with an uncertainty of 3.6 arcsec (radius, 90% containment). The X-ray light-curve shows a large increase in emission peaking at 264 s after the initial trigger, corresponding to the time of the second BAT trigger (Curran et al., GCN Circ. 9540). The underlying decay, however, can be parameterised as a single power-law with alpha = 0.81 +/- 0.04. As is common, there is clear spectral evolution during the flare. A spectrum extracted from the PC mode data after the flare subsides (500 s after the trigger) can be modelled with a power-law of Gamma = 2.07 +0.37/-0.35 and a total absorbing column of (1.5 +/- 0.4)x10^22 cm^-2; the Galactic column in this direction is 5.6x10^21 cm^-2 (Kalberla et al. 2005). Using this spectrum, the counts to observed (unabsorbed) flux conversion factor is 6.3x10^-11 (1.5x10^-10) erg cm^-2 count^-1. If the light-curve continues to decay with alpha ~ 0.81, the predicted count rate at 24 hours is 0.015 count s^-1, corresponding to an observed (unabsorbed) flux of 9.5x10^-13 (2.2x10^-12) erg cm^-2 s^-1. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9544 SUBJECT: GRB 090621: Swift/UVOT Upper Limits DATE: 09/06/21 12:29:18 GMT FROM: Peter Curran at MSSL P.A. Curran (UCL-MSSL) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 090621 123 s after the BAT trigger (Curran et al., GCN 9540). No optical afterglow consistent with the refined XRT position (Page et al., GCN 9543) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag wh 123 7115 805 >21.5 v 613 6089 333 >19.4 b 538 6910 310 >20.5 u 282 6705 736 >20.5 uw1 662 6500 320 >19.8 um2 637 6295 333 >19.7 uw2 588 5884 333 >19.9 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9545 SUBJECT: GRB 090621B: Swift detection of a short hard burst DATE: 09/06/21 22:38:35 GMT FROM: Scott Barthelmy at NASA/GSFC P.A. Curran (MSSL-UCL), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC), P. Schady (MSSL-UCL), M. C. Stroh (PSU) and H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team: At 22:07:25 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090621B (trigger=355359). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 313.432, +69.013 which is RA(J2000) = 20h 53m 44s Dec(J2000) = +69d 00' 48" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single spike with a duration less than 128 millisec. The peak count rate was ~7000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 22:08:36UT, 70.7 s after the BAT trigger. In promptly downlinked data, XRT found a faint uncatalogued source at RA, Dec (J2000) = 313.4700, 69.0282, which is RA = 20h 53m 52.8s Dec = +69d 01' 41.5" with an uncertainty of 8.0 arcseconds (radius, 90% containment). This location is 73 arcseconds from the BAT onboard position, within the BAT error circle. UVOT took a finding chart exposure of nominal 150 seconds with the White filter starting 76 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products at the XRT position. Data from the 2.7'x2.7' sub-image are not available at this time. The 8'x8' region for the list of sources generated on-board covers 100% of the BAT 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 0.43 (Schlegel et al. 1998). Burst Advocate for this burst is P.A. Curran (pac AT mssl.ucl.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: 9546 SUBJECT: GRB 090621A: Swift-BAT refined analysis DATE: 09/06/22 01:14:19 GMT FROM: Scott Barthelmy at NASA/GSFC J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), P.A. Curran (MSSL-UCL), 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), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+243 sec from recent telemetry downlinks, we report further analysis of BAT GRB 090621A (trigger #355303) (Curran, et al., GCN Circ. 9540). The BAT ground-calculated position is RA, Dec = 10.987, 61.938 deg, which is RA(J2000) = 00h 43m 56.8s Dec(J2000) = +61d 56' 17.6" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 77%. The mask-weighted light curve shows two small precursor peaks starting at ~T-30 sec, peaking at ~T-20 and T+10 sec, and returning to background at ~T+100 sec. Then the mmain emission starts at ~T+210 sec, peaks at ~T+240 and T+265 sec, and returns to background around T+350 sec. T90 is not possible because of a lack of the complete set of event by event data set for this burst. This also prevents giving spectral results. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9547 SUBJECT: GRB 090621B: Optical Observations DATE: 09/06/22 01:41:48 GMT FROM: Andrew Levan at U.of Leicester A.J. Levan (U. Warwick), P. Curran (MSSL), K. Wiersema (U. Leicester) and P. Groot (Nijmegen) report: "We observed the location of the short GRB 090621B (Curran et al. GCN 9545) with the WHT, beginning at 23:48:33 UT. Observations were obtained in the i-band, with a total exposure time of 1800s. Inside the XRT error box we find a faint object at RA = 20 53 53.07 Dec = +69 01 40.8 with errors of approximately 0.5" in each axis. The object is significantly fainter than the DSSII limit, and shows no obvious variability between the first and last exposures (taken ~1.7 and ~2.3 hours post burst). Given the relatively high foreground extinction the probability of a chance alignment within the XRT error box is non-trivial. Hence we are unable to make strong statements about the association of this source with GRB 090621B at this stage." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9549 SUBJECT: GRB 090621B: RTT150 optical observations DATE: 09/06/22 09:55:15 GMT FROM: Rodion Burenin at IKI, Moscow A. Galeev, I. Bikmaev, N. Sakhibullin (KSU/AST), R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.) report: We observed the field of the Swift-BAT GRB 090621B (Curran et al., GCN9545) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), starting at 21 Jun, 22:52:55 UT, i.e. approximately 45 minutes after the burst, using TFOSC. We made 3x300s exposures in Rc band. On combined image we do not detect any new source inside the XRT error circle (Curran et al., GCN 9545) besides the source reported by Levan et. al. (GCN 9547), which is detected only marginally. There is also one more brighter point-like source (RA=20:53:51.25, DEC=+69:01:37.4, J2000) outside but close to the edge of XRT error circle. Using USNO-B1 stars we estimate its magnitude as m_Rc=21.8+/-0.06. The limiting magnitude of combined image is m_Rc ~23.6. The finding chart can be found at: http://hea.iki.rssi.ru/grb/090621b/indexeng.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9550 SUBJECT: GRB 090621B: Swift-XRT refined analysis DATE: 09/06/22 10:16:55 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, K.L. Page (U. Leicester) and P.A. Curran (UCL-MSSL) report on behalf of the Swift-XRT team: We have analysed five orbits of Swift-XRT photon counting (PC) mode data from GRB 090621B (Curran et al., GCN Circ. 9545), spanning the interval T+80 s to T+19.5 ks after the trigger. In 10.0 ks we find a refined XRT position of RA, Dec = 313.47049, 69.02845, which is equivalent to RA (J2000) = 20:53:52.92 Dec(J2000) = +69:01:42.4 with an uncertainty of 4.0 arcsec (90% containment). This position is 1.2 arcsec from the XRT position quoted in GCN Circ. 9545. The X-ray light-curve shows a faint, fading source with a decay index of 0.61 +/- 0.19. If the source continues to decay at the same rate we predict an XRT count rate of 8.6e-4 count s^-1 at T+24 hours. The PC mode spectrum from T+80 s to T+17.1 ks can be fit by an absorbed powerlaw with a photon index of 1.47+/-0.66, assuming a Galactic column density of 1.9e21cm^-2 in the direction of the burst. The observed (unabsorbed) 0.3-10keV flux for this model is 3.8e-13 (4.5e-13) erg cm^-2 s^-1. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9551 SUBJECT: GRB 090621B: Swift-BAT refined analysis DATE: 09/06/22 13:08:54 GMT FROM: Scott Barthelmy at NASA/GSFC H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), P.A. Curran (MSSL-UCL), E. E. Fenimore (LANL), N. Gehrels (GSFC), 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), T. N. 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 short hard burst GRB 090621B (trigger #355359) (Curran, et al., GCN Circ. 9545). The BAT ground-calculated position is RA, Dec = 313.455, 69.034 deg, which is RA(J2000) = 20h 53m 49.3s Dec(J2000) = +69d 02' 02.9" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 69%. The mask-weighted light curve shows a single peak starting a ~T+0 sec and ending at ~T+0.2 sec. There is a 2.5-sigma hint of extended emission from ~T+150 to ~T+240 sec. T90 (15-350 keV) is 0.14 +- 0.04 sec (estimated error including systematics). The time-averaged spectrum from T-0.028 to T+0.148 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.82 +- 0.23. The fluence in the 15-150 keV band is 7.0 +- 1.0 x 10^-8 erg/cm2. The 1-sec peak photon flux measured from T-0.44 sec in the 15-150 keV band is 3.9 +- 0.5 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/355359/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9552 SUBJECT: GRB 090621B: Swift/UVOT Upper Limits DATE: 09/06/22 13:45:39 GMT FROM: Peter Curran at MSSL P.A. Curran (MSSL-UCL) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 090621B 76s after the BAT trigger (Curran et al., GCN 9545). No optical afterglow consistent with the refined XRT position (Beardmore et al., GCN 9550) or the optical source observed by Levan et al. (GCN 9547) is detected in the UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag wh 76 18173 1221 >22.29 v 618 10774 1142 >20.67 b 544 23952 1986 >21.88 u 289 29731 2675 >21.77 uw1 668 29017 2882 >21.63 um2 643 28110 2006 >21.32 uw2 594 6589 432 >20.50 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.44 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9555 SUBJECT: GRB 090621B: VLA observations DATE: 09/06/22 16:03:04 GMT FROM: Edo Berger at Harvard E. Berger and W.-f. Fong (Harvard) report: "We observed the field centered on the XRT error circle of the short GRB 090621B (GCNs #9545,9550) with the VLA at a frequency of 8.46 GHz starting on 2009 June 22.53 UT (14.6 hours post burst). We do not detect any sources within the refined XRT error circle to a 3-sigma limit of 54 microJy." [GCN OPS NOTE(22jun09): Per author's request, the missing "B" was added to the GCN name.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9556 SUBJECT: GRB 090621: Fermi GBM observation DATE: 09/06/22 17:28:10 GMT FROM: Arne Rau at MPE Arne Rau (MPE) reports on behalf of the Fermi GBM Team: "At 04:26:34.49 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090621 (trigger 267251196 / 090621185) which was also detected by the Swift/BAT (Curan et al. 2009, GCN 9540). The GBM triggered on the second BAT trigger (355304) and at approx. 4 min after the initial BAT trigger (355303) for this event. The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 12 degrees. The GBM light curve shows a faint peak coinciding with the initial Swift trigger (355303) and two brighter peaks starting at the GBM trigger time. The burst duration (T90) including the first faint peak is about 294 s (8-1000 keV). The time-averaged spectrum of the two brighter peaks starting from the GBM trigger time T0-6.10 s to T0+45.06 s is best fit by a Band function with Epeak = 56.0 +/- 10.7 keV, alpha = -1.1 +/- 0.2, and beta = -2.12 +/- 0.09 (chi squared 377 for 366 d.o.f.). The event fluence (8-1000 keV) in the above time interval is (4.4 +/- 1.0)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+35.840 s in the 8-1000 keV band is 1.92 +/- 0.06 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: 9557 SUBJECT: GRB 090621B: P60 Observations DATE: 09/06/22 17:40:24 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley), A. J. Levan (U. Warwick), M. M. Kasliwal, S. R. Kulkarni (Caltech) report on behalf of a larger collaboration: We have imaged the field of the short GRB090621B (Curran et al., GCN 9545) with the automated Palomar 60-inch telescope. Observations consisted of 20 x 180 s images in the i' filter at a mean epoch of 5:37 UT on 22 June 2009 (~ 7.5 hours after the burst). We detect the candidate afterglow reported by Levan et al. (GCN 9547) and Galeev et al. (GCN 9549) at low significance. Using several USNO-B sources in the field for reference, we measure a magnitude of I ~ 22.9. No other sources are detected inside the revised XRT error circle (Beardmore et al., GCN 9550). Directly comparing our P60 image with the WHT image from ~ 2 hours after the burst (GCN 9547), we find the candidate has faded marginally by 0.5 +- 0.3 mag. Further late-time observations will be needed to confirm if this is the optical afterglow of GRB090621B. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9558 SUBJECT: GRB 090621C: Fermi GBM detection DATE: 09/06/22 19:42:15 GMT FROM: Arne Rau at MPE Arne Rau (MPE) reports on behalf of the Fermi GBM Team: "At 10:00:52.10 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090621C (trigger 267271254 / 090621417). The on-ground calculated location, using the GBM trigger data, is RA = 257.5 deg, DEC = -28.5 deg (J2000 degrees, equivalent to 17 h 10 m, -28 d 28 '), with an uncertainty of 3.3 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 52 degrees. The GBM light curve consists of multiple short peaks with a duration (T90) of about 59.9 s (8-1000 keV). The time-averaged spectrum from T0-3.072 s to T0+28.672 s is well fit by a power law function with an exponential high energy cutoff. The power law index is -1.4 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 148 +/- 34 keV (chi squared 444 for 461 d.o.f.). The event fluence (8-1000 keV) in the above mentioned time interval is (1.8 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+4.096 s in the 8-1000 keV band is 2.29 +/- 0.06 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: 9559 SUBJECT: GRB 090621B: Gemini spectrum of afterglow candidate DATE: 09/06/22 19:42:32 GMT FROM: Edo Berger at Harvard E. Berger (Harvard), A. Cucchiara, D.B. Fox (Penn State), and A.J. Levan (U. Warwick) report: "On 2009 June 22.41 UT we used the GMOS instrument mounted on the Gemini-North 8-m telescope to obtain spectroscopic observations of the candidate optical afterglow (GCN #9547) of the short GRB 090621B (GCN #9545). A pair of 1800 sec exposures were obtained with a wavelength coverage of 4500-7500A. The combined spectrum of the source reveals broad features typical of an early M dwarf star. We therefore conclude that this object is unrelated to the GRB." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9560 SUBJECT: GRB 090621D: Fermi GBM detection DATE: 09/06/22 19:47:45 GMT FROM: Arne Rau at MPE Arne Rau (MPE) reports on behalf of the Fermi GBM Team: "At 10:43:45.14 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090621D (267273827 / 090621447). The on-ground calculated location, using the GBM trigger data, is RA = 12.3, DEC = -22.6 (J2000 degrees, equivalent to 00 h 49 m, -22 d 36 '), with an uncertainty of 4.9 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 79 degrees. The GBM light curve consists of two peaks with a duration (T90) of about 39.9 s (8-1000 keV). The time-averaged spectrum from T0-1.024 s to T0+20.480 s is adequately fit by a simple power law function with index -1.66 +/- 0.05 (chi squared 752 for 694 d.o.f.). The event fluence (8-1000 keV) in this time interval is (1.34 +/- 0.03)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0-1.024 s in the 8-1000 keV band is 1.74 +/- 0.05 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: 9561 SUBJECT: GRB 090621B: I-band observations from 1.23m CAHA DATE: 09/06/22 20:05:29 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC), P. Kubanek (GACE and IAA-CSIC), S. Mottola (DLR), U. Carsenty (DLR), A. Levan (U. Warwick), M. Jelinek (IAA- CSIC), A.J. Castro-Tirado (IAA-CSIC), A. de Ugarte Postigo (ESO, INAF/ OAB), report on behalf of a larger collaboration: "Following the detection of the short-hard GRB 090621B by SWIFT (Curran et al. GCNC 9545) we carried out I-band observations with the 1.23m telescope at Observatory of Calar Alto. The observations were done on June 22.094-22.161 UT (4.14-5.75 hours post burst) with a total exposure time of 22x240s. The candidates reported by Levan et al. (GCNC 9547) and Galeev (GCNC 9549) are preliminarily detected at I~22.5 and I~20.6, respectively, against USNO-B field stars." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9562 SUBJECT: GRB 090621B: Fermi GBM detection DATE: 09/06/23 00:03:11 GMT FROM: Adam Goldstein at Fermi-GBM/UAH A. Goldstein (UAH) and J.M. Burgess (UAH) report on behalf of the Fermi GBM Team: "At 22:07:25.70 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090621B (trigger 267314847 / 090621922) which was also detected by the Swift BAT (P.A. Curran et al. 2009, GCN 9545). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 108 degrees. The GBM light curve consists of one short spike with a duration (T90) of about 0.128 s (8-1000 keV). The time-averaged spectrum from T0-0.064 s to T0+0.064 s is best fit by a Band function with Epeak = 321.60 +/- 129.00 keV, alpha = -0.13 +/- 0.38, and beta = -1.57 +/- 0.08 (chi squared 401 for 481 d.o.f.). The event fluence (8-1000 keV) in this time interval is (3.71 +/- 0.58)E-07 erg/cm^2. The 0.128-sec peak photon flux measured starting from T0-0.064 s in the 8-1000 keV band is 6.4 +/- 1.4 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: 9564 SUBJECT: GRB 090621A: GRT Optical Observation DATE: 09/06/23 02:08:36 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC), T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU) We observed the field of GRB 090621A detected by Swift (trigger #355303; Curran et al., GCN #9540) with the 14-inch Goddard Robotic Telescope (GRT) located at the Goddard Geophysical and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/). 100 set of 30 sec exposures were taken in the R filter starting from June 21 05:00:15 (UT) about 37.3 min after the trigger and stopped on June 21 05:56:22 (UT). We do not detect the optical afterglow both in the individual images and the combined image inside the XRT position (Page et al., GCN #9543). The estimated three sigma upper limit of the combined image (total exposure of 2850 sec; excluding five bad quality images) is ~17.9 mag using the USNO-B1 catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9565 SUBJECT: GRB 090621B: GRT Optical Observation DATE: 09/06/23 02:18:16 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC), T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU) We observed the field of GRB 090621B detected by Swift (trigger #355359; Curran et al., GCN #9545) with the 14-inch Goddard Robotic Telescope (GRT) located at the Goddard Geophysical and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/). 100 set of 30 sec exposures were taken in the R filter starting from June 22 01:51:44 (UT) about 3.7 hours after the trigger and stopped on June 22 02:47:51 (UT). We do not detect the optical afterglow both in the individual images and the combined image inside the XRT position (Beardmore et al., GCN #9550). The estimated three sigma upper limit of the combined image (total exposure of 2880 sec; excluding four bad quality images) is ~17.8 mag using the USNO-B1 catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9567 SUBJECT: GRB 090621A: Enhanced Swift-XRT position DATE: 09/06/24 09:24:00 GMT FROM: Kim Page at U.of Leicester K.L. Page, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team: Using 5877 s of XRT Photon Counting mode data and 11 UVOT images, 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 = 11.02150, 61.94110 which is equivalent to: RA (J2000): 00 44 5.16 Dec (J2000): +61 56 28.0 with an uncertainty of 1.4 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, arXiv:0812.3662). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9656 SUBJECT: GRB 090621B: MTM-500 optical observations DATE: 09/07/11 20:19:43 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), A. Volnova (SAI MSU), V. Kouprianov, Ya. Naiden, V. Slesarenko, A. Devyatkin (Pulkovo Observatory), report on behalf of larger GRB follow-up collaboration: We observed the field of the Swift GRB 090621B (Curran et al, GCN 9545) with MTM-500 telescope of Kislovodsk solar station of the Pulkovo observatory in two series in R-filter between (UT) 2009-06-21 22:31 - 2009-06-22 00:01, i.e. starting ~24 minutes after burst onset. The upper limit of a stacked image of first 15 frames based on USNO B1.0 stars is following T0+ Filter Exp. mag. (mid, d) s 0.02147 R 15x60 >18.5 (3 sigma) While we do not detect objects reported in GCN 9547 (Levan et al.) and GCN 9549 (Galeev et al.) in the stacked image above, we may suggest a possible object near the edge of the refined XRT error box (Beardmore et al., GCN 9550) in coordinates (J2000) RA = 20:53:53.24 Dec = +69:01:45.5. This possible object appears more intense in the stacked image of the first five frames, and does not appear in the second epoch of our observations started on Jun.21 (UT) 23:37. Due to low S/N ratio we cannot confirm the object is real. We encourage re-analysis of later deep observations to clarify the nature of the object. The finding chart can be found at http://grb.rssi.ru/GRB090621B/grb090621B_MTM.png , where source labeled #5 is the USNO B1.0 star 1590-0172172 (RA(J2000)=20:53:57.28, Dec(J2000)=+69:01:47.8, R2=19.41) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9763 SUBJECT: GRB 090621A: MAGIC telescope GeV observation DATE: 09/08/11 07:00:09 GMT FROM: Markus Garczarczyk at MPI/MAGIC Carosi A. (INAF Rome), Gaug M. (IAC Tenerife), Antonelli L.A. (INAF Rome), Bastieri D. (Univ. Padova), Becerra Gonzalez J. (IAC Tenerife), Covino S. (INAF Rome), Galante N. (MPI Munich), Garczarczyk M. (IFAE Barcelona), La Barbera A. (INAF Palermo), Longo F. (INFN Trieste), Scapin V. (Univ. Udine) and Spiro S. (INAF Rome) for the MAGIC collaboration The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up observation of the BAT burst GRB090621A (Curran et al., GCN Circ. 9540). The burst was also triggered by Fermi-GBM (Arne Rau, GCN Circ. 9556) We received the GCN alert at 04:23:38 UT (T0+55s). Data taking with MAGIC started at 04:36:18 UT (T0+815s), when the GRB zenith angle reached 46 degrees. The observation continued for 1833 s. No evidence for VHE gamma-ray emission above the analysis threshold of 196 GeV was found. The observation was carried out in twilight condition. A preliminary analysis, for the hypothesis of steady emission and assumption of a differential photon spectral index of -2.5, yields the following 95% CL differential flux upper limits, including a 30% systematic uncertainty on the telescope efficiency: E(175 - 300 GeV): 0.25 * 10^-10 erg cm^-2 s^-1 E(300 - 1000 GeV): 0.10 * 10^-10 erg cm^-2 s^-1 for the whole time of observation (from 04:36:18 UT to 05:06:51 UT). We can also exclude emission of a constant flux in any 100s time bin smaller than: E(175 - 300 GeV): 2.74 * 10^-10 erg cm^-2 s^-1 E(300 - 1000 GeV): 1.01 * 10^-10 erg cm^-2 s^-1 for a time window from 04:36:18 UT to 05:06:51 UT This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9764 SUBJECT: GRB 090621B: MAGIC telescope GeV observation DATE: 09/08/11 07:10:46 GMT FROM: Markus Garczarczyk at MPI/MAGIC Carosi A. (INAF Rome), Gaug M. (IAC Tenerife), Antonelli L.A. (INAF Rome), Bastieri D. (Univ. Padova), Becerra Gonzalez J. (IAC Tenerife), Covino S. (INAF Rome), Galante N. (MPI Munich), Garczarczyk M. (IFAE Barcelona), La Barbera A. (INAF Palermo), Longo F. (INFN Trieste), Scapin V. (Univ. Udine) and Spiro S. (INAF Rome) for the MAGIC collaboration The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up observation of the BAT short burst GRB090621B (Curran et al., GCN Circ. 9545). The burst was also triggered by Fermi-GBM (Goldstein et al., GCN Circ. 9562). We received the GCN alert at 22:07:38 UT (T0+13s). Data taking with MAGIC started at 22:43:33 UT (T0+2169s), when the GRB zenith angle went below 60 degrees. The observation continued for 12570 s. No evidence for VHE gamma-ray emission above the analysis threshold was found. A preliminary analysis, for the hypothesis of steady emission and assumption of a differential photon spectral index of -2.5, yields the following 95% CL differential flux upper limits, including a 30% systematic uncertainty on the telescope efficiency. Because of improving sensitivities and analysis threshold due to decreasing zenith angle during the observation, the data sample was split into 4 parts: E ( 300-1000 GeV): 0.42 * 10^-10 erg cm^-2 s^-1 for a time window from 22:43:33 UT to 23:38:37 UT Analysis threshold: 407 GeV E ( 175- 300 GeV): 5.61 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 0.19 * 10^-10 erg cm^-2 s^-1 for a time window from 23:38:37 UT to 00:32:31 UT Analysis threshold: 291 GeV E ( 175- 300 GeV): 4.97 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 0.24 * 10^-10 erg cm^-2 s^-1 for a time window from 00:32:31 UT to 01:23:06 UT Analysis threshold: 224 GeV E ( 125- 175 GeV): 15.27 * 10^-10 erg cm^-2 s^-1 E ( 175- 300 GeV): 1.25 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 0.22 * 10^-10 erg cm^-2 s^-1 for a time window from 01:23:06 UT to 02:13:04 UT Analysis threshold: 186 GeV We can also exclude emission of a constant flux in any 100s time bin smaller than: E ( 300-1000 GeV): 4.02 * 10^-10 erg cm^-2 s^-1 for a time window from 22:43:33 UT to 23:38:37 UT Analysis threshold: 407 GeV E ( 175- 300 GeV): 23.60 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 1.52 * 10^-10 erg cm^-2 s^-1 for a time window from 23:38:37 UT to 00:32:31 UT Analysis threshold: 291 GeV E ( 175- 300 GeV): 15.33 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 1.41 * 10^-10 erg cm^-2 s^-1 for a time window from 00:32:31 UT to 01:23:06 UT Analysis threshold: 224 GeV E ( 125- 175 GeV): 22.23 * 10^-10 erg cm^-2 s^-1 E ( 175- 300 GeV): 7.87 * 10^-10 erg cm^-2 s^-1 E ( 300-1000 GeV): 1.15 * 10^-10 erg cm^-2 s^-1 for a time window from 01:23:06 UT to 02:13:04 UT Analysis threshold: 186 GeV This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10001 SUBJECT: Short-Duration GRB 090621: Skynet/Dolomiti Observations DATE: 09/10/08 15:11:31 GMT FROM: Josh Haislip at U.North Carolina J. Haislip, D. Reichart, M. Maturi, K. Ivarsen, 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 short-duration GRB 090621 (Curran et al., GCN 9545) with the 16" telescope at the Dolomiti Astronomical Observatory in Italy beginning 26.2 minutes after the trigger in Red, which we have calibrated to R. We do not detect the afterglow (Curran et al., GCN 9545). Stacking only images that increase the limiting magnitude yields: mean 1-sig. 1-sig. time 3-sig. sys. stat. since lim. cal. cal. cal. trig. tel. exp. fil. mag. stars unc. unc. (m) (# x s) (mag) (mag) 35.3 DAO-16 4 x 160 R 19.9 1518 USNO B1 0.277 0.000 + 3 x 80