//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9122 SUBJECT: GRB 090410: Swift detection of a burst DATE: 09/04/10 17:10:20 GMT FROM: David Palmer at LANL D. Grupe (PSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (MSSL), K. L. Page (U Leicester), D. M. Palmer (LANL), J. L. Racusin (PSU), M. H. Siegel (PSU), M. Stamatikos (NASA/ORAU), M. C. Stroh (PSU) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 16:57:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090410 (trigger=348929). Swift could not slew to the GRB due to a Sun constraint. The BAT on-board calculated location is RA, Dec 334.980, +15.471 which is RA(J2000) = 22h 19m 55s Dec(J2000) = +15d 28' 16" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex peak from T-10 to T+40, followed by another broad peak from T+80 to T+140. The peak count rate was ~6000 counts/sec (15-350 keV), at ~6 sec after the trigger. Swift cannot slew to the BAT position. The burst is sun-constrained until Tuesday, 2009 April 14. There will thus be no XRT or UVOT data for this trigger. Burst Advocate for this burst is D. Grupe (grupe 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: 9123 SUBJECT: GRB 090410: Swift-BAT refined analysis DATE: 09/04/10 23:59:04 GMT FROM: Scott Barthelmy at NASA/GSFC S.D. Barthelmy (GSFC), W.H. Baumgartner (GSFC/UMBC), J.R. Cummings (GSFC/UMBC), E.E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU), H.A. Krimm (GSFC/USRA), C.B. Markwardt (GSFC/UMD), D.M. Palmer (LANL), 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 sets from T-240 to T+963 sec from recent telemetry downlinks, we report further analysis of BAT GRB 090410 (trigger #348929) (Grupe, et al., GCN Circ. 9122). The BAT ground-calculated position is RA, Dec = 334.956, 15.419 deg, which is RA(J2000) = 22h 19m 49.4s Dec(J2000) = +15d 25' 08.6" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows two main peaks with some precursor activity. The precursor activity starts at ~T-55 sec. And because the target location only came into the BAT FOV at T-110 sec, there may have been even earlier activity. The first main peak started at ~T-10 sec, peaked at ~T+7 sec, and ended around T+45 sec. The second main peak started at ~T+80 sec, peaked at ~T+120 sec, and returned to baseline T+170 sec. The burst location left the BAT FOV at ~T+390 sec. T90 (15-350 keV) is 165 +- 8 sec (estimated error including systematics). The time-averaged spectrum from T-49.2 to T+139.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.19 +- 0.05. The fluence in the 15-150 keV band is 5.6 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+8.90 sec in the 15-150 keV band is 1.9 +- 0.1 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/348929/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9126 SUBJECT: GRB 090410: MITSuME optical upper limits DATE: 09/04/13 08:31:45 GMT FROM: Michitoshi Yoshida at Okayama Astrophysical Obs M. Yoshida, D. Kuroda, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda (OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 090410 (Grupe et al. GCN 9122; Barthelmy et al. GCN 9123) with optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. We started the observation at 18:12:59 UT, 4507s after the alert. We did not detect any new point source within the BAT error circle (Barthelmy et al. GCN 9123). 3-sigma upper limits to our observation are listed below. We used GSC2.3 catalog for flux calibration. Mid-UT Td EXP-T g' Rc Ic ------------------------------------------------------------- 2009-04-10 18:57:15 7163sec 72x60sec >17.9 >18.1 >18.5 ------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9128 SUBJECT: GRB 090410: GROND upper limits DATE: 09/04/14 16:18:34 GMT FROM: Jochen Greiner at MPI P. Afonso, T. Kruehler, A. Rau and J. Greiner (MPE Garching), report on behalf of the GROND team: GROND (Greiner et al. 2008, PASP 120, 405), the 7-channel imager mounted at the 2.2m ESO/MPI telescope at La Silla Observatory (Chile) started follow-up observations of GRB 090410 (Grupe et al. 2009, GCN #9122) on April 11, at 10:17 UTC (17.3 h after the burst). In addition, a second epoch of imaging was obtained, which started on April 12, 10:10 UTC. Observations were performed at high airmass (~2.5) and limited to a total of 4 min exposures in each J, H and K in both epochs because of Sun constraints. We do not detect any new object with respect to 2MASS inside the enhanced BAT error circle (Barthelmy et al. 2009, GCN #9123), and image subtraction between the two epochs does not reveal any obvious variable source. Upper limits from the first observation are as follows (all in the AB system): J > 19.1 mag H > 19.0 mag K > 18.1 mag The upper limits have been obtained using 2MASS field stars as reference. The given magnitudes are not corrected for the expected Galactic foreground extinction of E(B-V) of 0.05 mag. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9129 SUBJECT: GRB 090410: Suzaku WAM observation of the prompt emission DATE: 09/04/16 13:21:12 GMT FROM: Masanori Ohno at ISAS/JAXA W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.), Y. Urata (NCU), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa, T. Tamagawa (RIKEN), T. Uehara, T. Takahashi, Y. Fukazawa, Y. Hanabata (Hiroshima U.), E. Sonoda, M. Yamauchi, N. Ohmori, K. Kono, H. Hayashi (Univ. of Miyazaki), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.), on behalf of the Suzaku WAM team, report: The long GRB 090410 (Swift/BATtrigger #348929 ; Grupe et al., GCN 9122) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 16:57:53.392 UT (=T0). The observed light curve shows main peaks starting at T0-5s, ending at T0+25s, followed by a long weak tail seen up to T0+150s. And the precursor activity reported by Swift/BAT (Barthelmy et al., GCN 9123) is also seen at T0-55s. The total T90 duration including this precursor is about 166 seconds. The fluence in 100 - 1000 keV was 1.2 +/- 0.3 x 10^-5 erg/cm^2. The 1-s scaled peak flux measured from T0+5s was 3.0 (-0.3, +0.2) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-60s to T0+150s is well fitted by a single power-law with a photon index of 2.3 (-0.3, +0.3) (chi^2/d.o.f = 4.9/8), and the spectrum of the main bright peak from T0-5s to T0+25s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.3 +/-0.5, and Epeak 304 (-79, +60) keV (chi^2/d.o.f. = 7.9/7). 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: 9189 SUBJECT: GRB 090410: GAO 150cm telescope Optical Observation DATE: 09/04/22 10:59:01 GMT FROM: Kenzo Kinugasa at Gunma Astro. Obs/Japan K. Kinugasa, S. Honda, O. Hashimoto, H. Takahashi, H. Taguchi (Gunma Astronomical Observatory) report: The field of GRB 090410 (Grupe et al. GCN 9122) was observed with the 150 cm telescope of the Gunma Astronomical Observatory. Starting at 18:33 UT (1.60 hours after the trigger), Rc and Ic frames were acquired for 3 x 3-min and 5 x 3-min exposures under a high airmass (sec z ~3) condition. We did not detect any new point source within the ground-calculated BAT error circle (Barthelmy et al. GCN 9123) to limiting magnitudes of Rc=19.0 and Ic=19.0 relative to USNO-B1.0 R2 and I magnitudes at the meantime of 18:41 UT and 18:56 UT, respectively. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9193 SUBJECT: GRB 090410: Erratum in GCN 9189 DATE: 09/04/22 14:53:38 GMT FROM: Kenzo Kinugasa at Gunma Astro. Obs/Japan K.Kinugasa et al. (Gunma Astronomical Observatory); I also made a typo in GCN 9189. We observed "GRB 090410 (Grupe et al. GCN 9122)" instead of "GRB 080410" in subject. I apologize for my carelessness.