//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4885 SUBJECT: GRB 060319: Swift detection of a burst DATE: 06/03/19 01:25:58 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT H. Z. Ziaeepour (UCL-MSSL), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), A. J. Blustin (UCL-MSSL), D. N. Burrows (PSU), J. R. Cummings (NASA/ORAU), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), E. Rol (U Leicester) and T. Sakamoto (NASA/ORAU) report on behalf of the Swift Team: At 00:55:42 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 060319 (trigger=202035). Swift slewed immediately to the burst. The BAT on-board calculated location is RA,Dec 176.370, +59.990 {11h 45m 29s, +59d 59' 25"} (J2000) with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 15 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~4 sec after the trigger. The XRT began taking data at 00:57:56 UT, 134 seconds after the BAT trigger. The XRT on-board centroid algorithm did not find a source in the image and no prompt position is available. We are waiting for down-linked data to detect and determine a position for the source. UVOT took a finding chart exposure of 100 seconds with the WHITE filter starting 140 seconds after the BAT trigger. No 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 18th 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 18.0 mag. No correction has been made for extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4886 SUBJECT: GRB060319: Swift/XRT position DATE: 06/03/19 02:25:11 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT J. A. Kennea, D. N. Burrows (PSU) and A. P. Beardmore (U Leicester) report on behalf of the Swift/XRT team: We report on a preliminary analysis of downlinked data from GRB060319 (GCN 4885) from the Swift/XRT. We find a previously uncatalogued, fading point source at the following coordinates: RA(J2000): 11:45:33.7 Dec(J2000): +60:00:40.5 with an estimated uncertainty of 5 arcseconds radius (90% containment). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4887 SUBJECT: GRB060319 - SDSS Pre-burst Observations DATE: 06/03/19 02:28:01 GMT FROM: Richard J. Cool at U.of AZ/Steward Obs Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona), David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel (LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report: The Sloan Digital Sky Survey (SDSS) imaged the field of burst GRB060319 prior to the burst. As these data should be useful as a pre-burst comparison and for calibrating photometry, we are supplying the images and photometry measurements for this GRB field to the community. Data from the SDSS, including 5 FITS images, 3 JPGS, and 3 files of photometry and astrometry, are being placed at http://mizar.as.arizona.edu/~grb/public/GRB060319 We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=176.370 (11:45:28.8), dec=59.9900 (59:59:24.0); GCN 4885), as well as 3 gri color-composite JPGs (with different stretches). The units in the FITS images are nanomaggies per pixel. A pixel is 0.396 arcsec on a side. A nanomaggie is a flux-density unit equal to 10^-9 of a magnitude 0 source or, to the extent that SDSS is an AB system, 3.631e-6 Jy. The FITS images have WCS astrometric information. In the file GRB060319_sdss.calstar.dat, we report photometry and astrometry of 201 bright stars (r<20.5) within 15' of the burst location. The magnitudes presented in this file are asinh magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118, 1406). Beware that some of these stars are not well-detected in the u-band; use the errors and object flags to monitor data quality. In the files GRB060319_sdss.objects_flux.dat and GRB060319_sdss.objects_magnitudes.dat, we report photometry of 414 objects detected within 6' of the GRB position. We have removed saturated objects and objects with model magnitudes fainter than 23.0 in the r-band. The fluxes listed in GRB060319_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB060319_sdss.objects_magnitudes.dat are asinh magnitudes. All quantities reported are standard SDSS photometry, meaning that they are very close to AB zeropoints and magnitudes are quoted in asinh magnitudes. Photometric zeropoints are known to about 2% rms. None of the photometry is corrected for dust extinction. The Schlegel, Finkbeiner, and Davis (1998) predictions for this region are A_U=0.110 mag, A_g=0.081 mag, A_r = 0.059 mag, A_i=0.044 mag, and A_z=0.031 mag. The file GRB060319_sdss.spectro.dat contains a list of the 1 objects with SDSS spectroscopy within 6 arcminutes of the GRB position. In addition to the redshift and 1-sigma error for each object, this file also lists the object spectroscopic classification. SDSS astrometry is generally better than 0.1 arcsecond per coordinate. Users requiring high precision astrometry should take note that the SDSS astrometric system can differ from other systems such as those used in other notices; we have not checked the offsets in this region. More detailed information pertaining to our SDSS GRB releases can be found in our initial data release paper (Cool et al. 2006, astro-ph/0601218). See the SDSS DR4 documentation for more details: http://www.sdss.org/dr4. These data have been reduced using a slightly different pipeline than that used for SDSS public data releases. We cannot guarantee that the values here will exactly match those in the data release in which these data are included. In particular, we expect the photometric calibrations to differ by of order 0.01 mag. This note may be cited, but please also cite the SDSS data release paper, Adelman-McCarthy et al. (2006, ApJS, in press, astro-ph/0507711), when using the data or referring to the technical documentation. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4888 SUBJECT: GRB060319: MASTER optical observation DATE: 06/03/19 02:35:21 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, A.Belinski, E.Gorbovskoy, A.Krylov, G.Borisov, A.Sankovich, M.Sinitsin, P.Gritsyk, S.Korobkin Sternberg Astronomical Institute, Moscow Union 'Optic' MASTER robotic system (http://observ.pereplet.ru) responded to GRB060319.0 (GRB_TIME is 2006-03-19 00:55:42.92) by all cameras. The first unfiltred image was at 2006-03-19 00:58:24.96 UT, 80 s after notice time and 162 after the GRB time The first spectral image was at 2006-03-19 00:58:33 UT, 88 s after notice time and 170 after the GRB time The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B). The robot not find OT-candidate in error box brighter then 17.7 (s/n=3). The reduction is continuing. This work is supported by RFFI 04-02-16411 grant. This message can be cited. Mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4889 SUBJECT: GRB060319 : Liverpool Telescope optical limit DATE: 06/03/19 03:32:28 GMT FROM: Andrea Melandri at Liverpool John Moores U A. Melandri, A. Gomboc, C.G. Mundell, C. Guidorzi, A. Monfardini, C.J. Mottram, R.J. Smith, I.A. Steele, D. Carter, M. Burgdorf, S. Kobayashi, D. Bersier, M.F. Bode (Liverpool JMU) report: "The 2-m Liverpool Telescope followed up the field of GRB060319 (Ziaeepour et al., GCN 4885) and started observing its position about 7.0 minutes after the GRB. The automatic "detection mode" procedure did not reveal any obvious afterglow candidate at the preliminary XRT position reported by Kennea et al. (GCN 4886), brighter than about R~19 mag from 6x10-sec images, confirmed by visual inspection. Limiting magnitude has been derived with reference to USNOB1. Further analysis is still ongoing." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4890 SUBJECT: GRB 060319 optical observations at TNG DATE: 06/03/19 05:26:19 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo (INAF-OAB), G.L. Israel (INAF-OARm) R. Cosentino (TNG) report on behalf of a larger collaboration: We observed the field of GRB 060319 (Ziaeepour et al., GCN 4885) with the 3.6 m TNG italian telescope sited in Canary Island equipped with the DOLORES camera. We performed five minutes of R-band imaging, starting on March 19.16 UT (about 3 hours after the burst). We do not find any new source inside the XRT error box ((Kennea et al., GCN 4886) up to a magnitude limit of R > 23 (3sigma confidence) with respect to the USNOB1 catalog. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4891 SUBJECT: GRB 060319: Swift-BAT refined analysis DATE: 06/03/19 05:26:40 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (GSFC/ORAU), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger ((BYU-Idaho), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), G. Sato (ISAS), J. Tueller (GSFC) Using the data set from T-299 to T+303 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060319 (trigger #202035) (Ziaeepour, et al., GCN 4885). The BAT ground-calculated is RA,Dec = 176.366, 60.041 deg {11h 45m 27.7s, 60d 2' 29.3"} (J2000) +- 2.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows two peaks. The first and second spikes peak around T+4 sec and T+12 sec respectively. Due to the pre-plan target observation, GRB 060319 was outside of the BAT FOV before T-60 sec. Thus, we do not know any activity about GRB 060319 before T-60 sec. T90 (15-350 keV) is 12.0 +- 1 sec (estimated error including systematics). The time-averaged spectrum from T+1.0 to T+18.0 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.35 +- 0.27. The fluence in the 15-150 keV band is 2.7 +- 0.4 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T+4.00 sec in the 15-150 keV band is 1.1 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4892 SUBJECT: GRB060319: MASTER limit DATE: 06/03/19 06:44:21 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, A.Belinski, E.Gorbovskoy, A.Krylov, G.Borisov, A.Sankovich, M.Sinitsin, P.Gritsyk, S.Korobkin Sternberg Astronomical Institute, Moscow Union 'Optic' MASTER robotic system (http://observ.pereplet.ru) responded to GRB060319.0 (Ziaeepour, et al., GCN 4885 ) by all cameras (unfiltred, R-filtred, spectral and high time resolution). The first unfiltred image was at 2006-03-19 00:58:24.96 UT, 80 s after notice time and 162 after the GRB time The first spectral image was at 2006-03-19 00:58:33 UT, 88 s after notice time and 170 after the GRB time. There is no OT brighter than 17.7 . We have aboute 50 unfiltered images. The limit of sum of first 10 best images is about 19.5 (s/n=3). The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B). We do not see any new sources inside XRT position Kennea et al. (GCN 4886) brighter 19.5 . We see faint uncatalogizeted object near but outside XRT position Kennea et al. (GCN 4886). The magnitude is about 19.0 at images between 3 - 8 minutes after GRB time. ra = 11 45 31.59 dec= +60 00 26 The reduction is continuing. The sum JPG-image available at http://observ.pereplet.ru/images/GRB060319may-be.jpg . This work is supported by RFFI 04-02-16411 grant. This message can be cited. Mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4893 SUBJECT: GRB 060319: Re-analysis of TNG data DATE: 06/03/19 07:47:53 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo (INAF-OAB), G.L. Israel (INAF-OARm), on behalf of a larger collaboration report: Further analysis of our optical data (D'Avanzo et al., GCN 4890) of GRB 060319 (Ziaeepour et al., GCN 4885), does not reveal any obvious object at the position reported by Lipunov et al. (GCN 4892) with a magnitude limit of R > 23 (3sigma confidence). This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4894 SUBJECT: GRB060319: Swift/UVOT upper limits DATE: 06/03/19 08:34:34 GMT FROM: Alexander Blustin at MSSL-UCL A. J. Blustin (UCL-MSSL), H. Ziaeepour (UCL-MSSL), F. E. Marshall (NASA/GSFC) on behalf of the Swift/UVOT team The Swift/UVOT began taking data on the field of GRB060319 at 00:58:02 on 2006-03-19, 139 s after the BAT trigger (Ziaeepour et al., GCN 4885). In the initial 100 s White filter image no new source is detected at the XRT position (Kennea et al., GCN 4886) down to a 3-sigma magnitude upper limit of 20.6. No source is detected in summed images from any of the filters down to the following 3-sigma upper limits. Filter T_range(s) Exp(s) 3sigUL(mag) V 500-2150 544 19.9 B 448-2102 128 20.2 U 423-2078 158 20.0 UVW1 400-2054 178 19.8 UVM2 245-2030 308 19.9 UVW2 476-2141 158 20.2 White 139-2116 276 20.7 These magnitudes are not corrected for Galactic extinction; E(B-V)=0.022. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4895 SUBJECT: GRB060319: Swift XRT refined analysis DATE: 06/03/19 10:40:25 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, K.L. Page (U Leicester), J.A. Kennea, D.N. Burrows (PSU) and H. Ziaeepour (UCL-MSSL) report on behalf of the Swift/XRT team: We have analysed the first two orbits of Swift XRT data on the BAT GRB 060319 (Ziaeepour, et al., GCN 4885; Sakamato et al., GCN 4891). The XRT began observing in Photon Counting mode at 00:58:04UT on 2006-03-19, 173 s after the BAT trigger. With an exposure time of 4.5ks, the refined XRT position is RA(J2000) = 11h 45m 33.8s Dec(J2000) = +60d 00' 39.0" with an uncertainty of 3.6" (90% containment). This is 2' away from the centre of the refined BAT position quoted in GCN 4891 (Sakamoto et al.), and 1.7" away from the initial XRT position quoted in GCN 4886 (Kennea et al.). The 0.3-10 keV X-ray light curve initially rises from 0.5 count/s at T+173s to a maximum of 2 count/s at T+265s, then shows a power-law decline with a decay index of 1.02+/-0.05. The X-ray spectrum covering the time period from T+173s to T+7.3ks is well fit by an absorbed power-law with a photon index of 2.10+/-0.15 and column density of (4.6+/-0.6)e21 cm**-2. We note the Galactic column density in the direction of the source is 1.37e20 cm**-2. The observed (unabsorbed) 0.3-10 keV flux for this spectrum is 1.2e-11 (2.2e-11) erg/cm**2/s. Assuming the X-ray emission continues to decline at the same rate, we predict a 0.3-10 keV XRT count rate of 0.005 count/s at T+24hr, which corresponds to an observed 0.3-10 keV flux of 2.7e-13 erg/cm**2/s. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4896 SUBJECT: GRB 060319: IAC-80 optical observations DATE: 06/03/19 11:54:19 GMT FROM: Sergei Guziy at IAA S. Guziy (IAA-CSIC Granada), G. Gómez Velarde (IAC Tenerife) and A. J. Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration, report: We have taken BVRI frames at the position of GRB 060319 (Ziaeepour et al. GCNC 4885) with the IAC-80 telescope at Observatorio del Teide (Canary Islands). Images were obtained starting at 02:23 UT (i.e. 1.45 hr after the onset of the burst). We do not see any optical source within the revised SWIFT/XRT position (Beardmore et al. GCNC 4895) down to R = 21. In particular, we do not see any counterpart at this time to the MASTER source reported by Lipunov et al. (GCNC 4892) in agreement with D'Avanzo et al. (GCNC 4893). This message can be quoted. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4897 SUBJECT: GRB 060319: WHT K-band candidate afterglow DATE: 06/03/19 16:23:49 GMT FROM: Nial Tanvir at IofA U.Cambridge N.R. Tanvir (U. Hertfordshire), E. Rol (U. Leicester), K. Wiersema, R. Starling (U. Amsterdam) and N. O'Mahoney (ING) report on behalf of a larger collaboration: We observed the field of GRB 060319 with WHT/LIRIS. A 10 min K-band exposure was made beginning at Mar 19 06.38 UT (ie. approximately 5.4 hours post-burst). A faint source is visible within the XRT error circle reported by Beardmore et al. (GCN 4895). The coordinates of the source are (relative to DSS system) approximately: 11 45 33.5 +60 00 39.0 (J2000) The magnitude relative to two nearby 2MASS stars is K=19.0+-0.3. It is not possible to tell whether the source is constant or variable.