This file contains BOTH GRBs 060602 A and B. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5196 SUBJECT: GRB 060602: Swift detection of a burst DATE: 06/06/02 21:49:44 GMT FROM: Scott Barthelmy at NASA/GSFC P Schady (MSSL-UCL), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), J. R. Cummings (NASA/ORAU), J. A. Kennea (PSU), H. A. Krimm (GSFC/USRA), K. M. McLean (LANL/UTD), D. M. Palmer (LANL), T. Sakamoto (NASA/ORAU), G. Sato (GSFC/JSPS/USRA) and M. Stamatikos (NASA/ORAU) report on behalf of the Swift Team: At 21:32:12 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 060602 (trigger=213180). Swift did not slew to the burst because of the Moon constraint. The BAT on-board calculated location is RA,Dec 149.576, +0.323 {09h 58m 18s, +00d 19' 23"} (J2000) with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve has a peak starting at T+0 sec and ending at ~T+15 sec. The peak count rate was ~500 counts/sec (15-350 keV), at ~2 sec after the trigger. This burst will not become visible to Swift NFIs until June 4th, 08:46UT. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5197 SUBJECT: GRB060602 - SDSS Pre-Burst Observations DATE: 06/06/02 22:22:17 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 GRB060602 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/GRB060602 We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=149.576 (09:58:18.2), dec=0.323000 (00:19:22.8); Swift-BAT TRIGGER 213180), 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 GRB060602_sdss.calstar.dat, we report photometry and astrometry of 158 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 GRB060602_sdss.objects_flux.dat and GRB060602_sdss.objects_magnitudes.dat, we report photometry of 496 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 GRB060602_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB060602_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=0.134 mag, A_g=0.099 mag, A_r = 0.072 mag, A_i=0.054 mag, and A_z=0.038 mag. The file GRB060602_sdss.spectro.dat contains a list of the 4 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: 5198 SUBJECT: GRB060602B: BOOTES-IR candidate afterglow DATE: 06/06/03 00:30:00 GMT FROM: Martin Jelinek at Inst.Astrophys.Andalucia,Granada Martin Jelinek (IAA CSIC Granada, Spain) Petr Kubánek (ASU AV CR Ondrejov & ISDC, Versoix), Stanislav Vítek (IAA CSIC Granada, Spain) on behalf of the BOOTES collaboration report: Bootes-IR telescope, located at IAA Observatory de Sierra Nevada, observed position of GRB 060602B (Trigger 213190), starting 10.7 sec post GCN notice (= 14.5 min post GRB). We obtained a series of R-band exposures. An object with R ~ 16 mag is shown at RA 17:49:20.14 DEC -28:07:17.95 (J2000) with estimated uncertanity 1 arcsec which is not at GSC-2 and USNO catalogues. It is also not visible at DSS. According to MPC, there is not any know asteroid nearby. We qualify this object as a possible GRB counterpart. Futher analysis, as well as observations, are in progress. [GCN OPS NOTE(03jun06): Per authors' request, AJC-T was withdrawn from the authors list as it was unintensionally included.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5199 SUBJECT: GRB060602B: Watcher observations - no OT candidate DATE: 06/06/03 00:52:24 GMT FROM: Petr Kubanek at AIO Petr Kubánek (ASU AV CR Ondrejov & ISDC Versoix), Martin Jelínek (IAA Granada), John French (UCD Dublin) on behalf of the Watcher collaboration report: we observed location of GRB 060602B (Trigger 213190), starting 4 sec after Bootes-IR observation (Jelínek et al., GCN 5198), e.g. ~14.5 min post GRB. We detect object at Bootes-IR position. As the object is visible at DSS-R images, we DO NOT consider it as GRB transient. We don't plan any futher observations. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5200 SUBJECT: GRB 060602B: Swift detection of a burst DATE: 06/06/03 00:53:33 GMT FROM: Patricia Schady at MSSL/Swift P. Schady (MSSL-UCL), A. P. Beardmore (U Leicester), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), E. Rol (U Leicester) and G. Sato (GSFC/JSPS/USRA) report on behalf of the Swift Team: At 23:54:33 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 060602B (trigger=213190). Swift slewed immediately to the burst. The BAT on-board calculated location is RA,Dec 267.380, -28.109 {17h 49m 31s, -28d 06' 31"} (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 20 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at 7 sec after the trigger. The XRT began taking data at 23:55:56 UT, 83 seconds after the BAT trigger. We find a faint uncatalogued source in the first 246s of down-linked PC mode data at RA,Dec (J2000) = 17 49 31.7, -28 08 03.7 with an uncertainty of 3.9 arcsec (90% containment). This is 92 arcsec from the on-board BAT position. This source is not consistent with the BOOTES-IR candidate reported in GCN 5198. UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 89 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 18.5 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. We note that this is a crowded field and that a large, but uncertain extinction is expected. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5201 SUBJECT: GRB060602A: Bootes-IR observations DATE: 06/06/03 01:25:24 GMT FROM: Petr Kubanek at AIO Stanislav Vítek, Martin Jelinek, Alberto J. Castro-Tirado (IAA CSIC Granada, Spain), Petr Kubánek (ASU AV CR Ondrejov & ISDC, Versoix) on behalf of the BOOTES collaboration report: Bootes-IR telescope, located at IAA Observatory de Sierra Nevada, observed position of GRB 060602A (S. Barthelmy GCN 5196), starting 13.7 sec post GCN notice (61.6 sec post GRB). At images obtained at considerable airmass, we do not detect any new object down to R~15 mag. Futher analysis is in progress. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5203 SUBJECT: GRB060602A: optical observations(/transient?) DATE: 06/06/03 02:31:33 GMT FROM: Brian Lindgren Jensen at U.of Copenhagen Brian L. Jensen, Jens Hjorth, Johan Fynbo (Dark Cosmology Centre, NBI), Jyri Näränen (University of Helsinki) report: "We have observed the field of GRB060602A (Schady et al., GCN 5196) in the R-band with the NOT+ALFOSC (La Palma), starting at June 2.908 (15 min. after the burst). All R:6x300s cover the full 3' radius BAT error circle. Visual comparison to the SDSS (Cool et al., GCN 5197), does not reveal any new bright sources in the field. However, a faint source, not readily apparent on SDSS (r-band), is observed at: RA = 09:58:16.73 Dec = +00:18:12.7 - located 1.2' from the centre of the BAT error-circle. A preliminary calibration to SDSS photometry of the field (Cool et al., GCN 5197) yields a magnitude for the source of R~22.5+-0.3. Further observations are needed in order to determine whether the source is transient. A finding chart is available at: http://www.astro.ku.dk/~brian_j/grb/grb060602.897/ " //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5205 SUBJECT: GRB 060602B: RTT150 optical observations DATE: 06/06/03 15:32:44 GMT FROM: Rodion Burenin at IKI, Moscow I. Khamitov (TUG), I. Bikmaev, N. Sakhibullin (KSU/AST), Z. Aslan (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.), R. Burenin, M. Pavlinsky (IKI) report: We observed error radius of XRT position of GRB060602B (Swift trigger 213190, Schady et al. GCN5200) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), starting at June 3, 00:19UT, i.e. ~25 min after the burst. A series of frames was taken (7*30s and 5*300 exposures in Rc). Down to our limiting magnitude R=~23, inside of XRT error circle we found the only object (RA=17:49:31.80, DEC=-28:08:02.2). The object is relatively bright (R=18.7) and starlike (PSF FWHM=~1.4''). It is present in DSS and its brightness did not change during our observations, therefore we do not consider this object as optical counterpart of GRB060602B. Our finding chart can be found at: http://hea.iki.rssi.ru/grb/060602b/r.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5206 SUBJECT: GRB 060602A: Swift-BAT Refined Analysis DATE: 06/06/03 18:39:05 GMT FROM: Hans Krimm 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), M. Koss (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), G. Sato (GSFC/JSPS/USRA), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), on behalf of the Swift-BAT team: Using the data set from T-119.7 to T+182.3 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060602A (trigger #213180) (Schady, et al., GCN 5196). The BAT ground-calculated position is (RA,Dec) = 149.576, 0.322 deg {9h 58m 18.3s, 0d 19' 20.7"} (J2000) +- 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 43%. The light curve shows a single broad triangular shaped peak lasting from ~T+0 to ~T+70 sec. The burst is most prominent in the 50-100 keV band and shows clear evidence of hard to soft spectral evolution. T90 (15-350 keV) is 60 +- 10 sec (estimated error including systematics). The time-averaged spectrum from T-0.7 to T+67.0 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.14 +- 0.16. The fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+7.74 sec in the 15-150 keV band is 0.1 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5207 SUBJECT: GRB 060602B: Swift/UVOT observations DATE: 06/06/03 22:33:46 GMT FROM: Alexander Blustin at MSSL-UCL A. J. Blustin (UCL-MSSL), P. Schady (UCL-MSSL) and S. B. Pandey (UCL-MSSL) report on behalf of the Swift/UVOT team: The Swift/UVOT began observing the field of GRB 060602B at 23:56:01 on 2006-06-02, 87 s after the BAT trigger (Schady et al., GCN 5200). No new source with respect to the DSS was detected within the XRT error circle (Schady et al., GCN 5200) in coadded images in any filter down to the following 3-sigma magnitude upper limits: Filter T_range(s) Exposure(s) 3sig_UL V 193-29437 2320 20.2 B 670-18594 897 20.6 U 646-24379 1793 20.8 W1 622-23647 1998 20.1 M2 598-30163 2557 20.6 W2 699-28524 1110 20.3 White 87-6795 312 20.2 These upper limits are not corrected for Galactic extinction (E(B-V) ~ 35.7; note that extinction estimates are unreliable for Galactic latitudes < 5 deg). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5208 SUBJECT: GRB 060602B: Swift-BAT Refined Analysis DATE: 06/06/04 00:00:01 GMT FROM: Hans Krimm at NASA-GSFC D. Palmer (LANL), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (BYU-Idaho), M. Koss (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), A. Parsons (GSFC), T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/JSPS/USRA), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), on behalf of the Swift-BAT team: Using the data set from T-119.1 to T+182.9 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060602B (trigger #213190) (Schady, et al., GCN 5200). The BAT ground-calculated position is (RA,Dec) = 267.368, -28.121 deg {17h 49m 28.2s, -28d 7' 15.5"} (J2000) +- 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The light curve shows a single boxcar shaped peak from ~T-1.0 to ~T+12.0 sec. The peak is strongest in the 15-25 keV band and is not seen above 50 keV. T90 (15-350 keV) is 9.0 +- 2 sec (estimated error including systematics). The time-averaged spectrum from T-1.1 to T+8.8 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 5.02 +- 0.52. The fluence in the 15-150 keV band is 1.8 +- 0.2 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T+5.94 sec in the 15-150 keV band is 0.8 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. We note that this is one of the softest spectra yet seen in the BAT for a GRB. The spectra plus the galactic coordinates of the source: galactic lon, lat: 1.15, -0.30 deg suggest that this source may be an X-ray burster rather than a classical GRB. Analysis of XRT and other ground and satellite based observations will help to settle this question. Therefore further observations are encouraged. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5209 SUBJECT: GRB 060602B: Swift-XRT Refined Analysis DATE: 06/06/04 00:33:38 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, O. Godet (U. Leicester) and T. Sakamoto (GSFC/ORAU) report on behalf of the Swift-XRT team : We have analysed the first 11.4ks of Swift XRT PC mode data from the BAT trigger GRB060602B (Schady et al., GCN 5200; trigger number 213190). We find a refined XRT position of: RA(J2000) = 17:49:31.6 Dec(J2000) = -28:08:03.2 with an estimated uncertainty of 3.7 arcsec (90% containment). This is 1.4 arcsec away from the XRT position reported in GCN 5200 and 64.2 arcsec from the refined BAT position (Palmer et al., GCN 5208). The X-ray light curve shows a small rise in intensity until T+200s, then follows a simple power-law decay with a index of 1.05 +/- 0.07. The X-ray spectrum over the same interval (T+100s to T+40ks) can be well modelled by an absorbed power-law, with a photon index of 3.1 +/- 0.6 and a column density of 5.0 +/- 1.4 E22 cm^-2. The measured galactic column density in this direction is 1.4E22 cm^-2. The observed 0.3-10keV flux is 3.2E-12 ergs cm**-2 s**-1, which corresponds to an unabsorbed flux of 5.0E-11 ergs cm**-2 s**-1. The measured spectral and temporal indices are difficult to reconcile with standard GRB afterglow models. The X-ray spectrum can also be equally well fit by an absorbed blackbody model, with a temperature of 0.90+/-0.09 keV and a column density of 2.1 +/- 0.7 E22 cm^-2. This model has an observed (unabsorbed) 0.3-10 keV flux of 2.8E-12 (4.3E-12) ergs cm**-2 s**-1. Assuming the source decays at the same rate, we predict an XRT count rate of 0.0011 count/s at T+48 hrs, which corresponds to an observed flux of 8.8E-14 ergs cm**-2 s**-1. This Circular is an official product of the Swift XRT Team. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5210 SUBJECT: GRB 060602B: XMM-Newton Survey Source DATE: 06/06/04 01:54:48 GMT FROM: Jules Halpern at Columbia U. I note that a faint source was detected by XMM-Newton in a survey observation of the Galactic plane on 2000 September 23 at a position consistent, to within their combined uncertainties, with the Swift XRT source (Beardmore et al., GCN 5209) in the error circle of the possible GRB 060602B (trigger #213190: Schady et al., GCN 5200). R.A.(2000) Dec.(2000) +/-(") -------------------------------------------------- Swift XRT 17 49 31.6 -28 08 03.2 3.7 XMM-Newton 17 49 31.59 -28 08 08.7 4 -------------------------------------------------- It is listed in the XMMSSC-XMM-Newton Serendipitous Source Catalog as having a flux of 6.9x10^-14 erg/cm2/s in the 0.2-12 keV range. Therefore, it is possible that this is a Galactic X-ray burster, as noted by Palmer et al. (GCN 5208). If at a distance of 8 kpc, for example, its 15-150 keV fluence in the BAT of 1.8x10^-7 erg/cm2 (Palmer et al., GCN 5208) corresponds to an average luminosity of 1.1x10^38 erg/s in this band over the 13 s duration of the burst, and its 0.2-12 keV luminosity seen by XMM was 5.3x10^32 erg/s, within the range of quiescent LMXBs (e.g., Tomsick et al. 2004, ApJ, 610, 933). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5211 SUBJECT: GRB 060602A: Swift-BAT Refined Analysis: Correction DATE: 06/06/04 02:13:48 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (GSFC/ORAU) on behalf of the Swift-BAT team: There is an error in the 1-s peak photon flux reported in Sakamoto et al. (GCN Circular 5206). Due to hard and weak nature of the burst, only the 90% upper limit of 0.5 ph/cm2/s is possible to constrain from a power-law fit. We apologize for this mistake. We thank Kazutaka Yamaoka for pointing it out. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5229 SUBJECT: GRB060602B : REM infrared observations DATE: 06/06/06 13:20:23 GMT FROM: Andrea Melandri at Liverpool John Moores U A. Melandri, E. Distefano, S. Covino, E. Molinari, G. Chincarini, F.M. Zerbi, L.A. Antonelli, V. Testa, G. Tosti, F. Vitali, P. Conconi, G. Cutispoto, G. Malaspina, L. Nicastro, E. Palazzi, E. Meurs, P. Goldoni, on behalf of the REM/ROSS Team, report: We imaged the field of GRB 060602B (Schady et al., GCN 5200) with the 60 cm robotic telescope REM starting at June 3, 01:37:43.5 UT, i.e about 1.72 hours after the burst. Due to poor meteo conditions at LaSilla a short serie of images with the infrared camera were taken with J,H and K filters for a total integration time of 100s in each filter. The analysis of the entire dataset do not show any infrared source inside of XRT error circle (Schady et al., GCN 5200; Beardmore et al., GCN 5209) down to limiting magnitude of 15.1, 13.2 and 12.2 respectively (5 sigma uper limit) This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5245 SUBJECT: GRB060602A: Swift/UVOT upper limits DATE: 06/06/08 12:41:19 GMT FROM: Alexander Blustin at MSSL-UCL A. J. Blustin (UCL-MSSL) and P. Schady (UCL-MSSL) report on behalf of the Swift/UVOT team: Due to a moon constraint, Swift/UVOT did not begin observing the field of GRB060602A until 15:55:25 on 2006-06-04, 1.766 days after the BAT trigger (Schady et al., GCN 5196). We observe no optical/UV afterglow candidate within the refined BAT error circle (Sakamoto et al. 5206) or at the position of the afterglow candidate reported by the NOT team (Jensen et al., GCN 5203). 3-sigma magnitude upper limits, in coadded images, at the position of the NOT afterglow candidate are as follows: Filter T_range(days) Exp(s) 3sig_UL(mag) V 1.831-3.555 1775 21.3 B 1.827-3.567 1572 22.3 U 1.826-3.564 1775 22.1 UVW1 1.766-3.561 1850 21.7 UVM2 1.832-3.558 1922 22.0 UVW2 1.828-3.617 2265 22.3 Where the time range of the images post-trigger is given in days. The upper limits are not corrected for Galactic extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5251 SUBJECT: GRB 060602A: Swift/XRT analysis DATE: 06/06/12 21:23:42 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT K. L. Page, A. P. Beardmore (U. Leicester) and J. A. Kennea (PSU) report on behalf of the Swift/XRT team: We have analysed 37.8 ks of XRT data obtained for the field of GRB 060602A (Schady et al.; GCN 5196), starting 1.8 days after the trigger, when the burst was no longer Moon constrained. A faint source was found within the BAT error circle, at a position of RA(J2000) = 09 58 16.80 Dec(J2000) = +00 18 14.8 with an estimated uncertainty of 4.2 arcsec (90% containment). This source is fading with an approximate slope of alpha = 1.10, so is very likely the X-ray afterglow. This source is 2.3 arcsec from the possible counterpart identified by Jensen et al. (GCN 5203). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6997 SUBJECT: GRB 060602A: host redshift DATE: 07/10/25 12:44:19 GMT FROM: Pall Jakobsson at U Hertfordshire Pall Jakobsson (U. Hertfordshire), Daniele Malesani, Johan P. U. Fynbo, Jens Hjorth, Paul M. Vreeswijk (DARK, NBI) and Nial R. Tanvir (U. Leicester) report on behalf of a larger collaboration: Using FORS1 on the Very Large Telescope, we obtained 2*20 min spectra (grism 300V+GG375 covering 4000-8000 A) of the GRB 060602A host galaxy on 28 December 2006. A firm upper limit of z < 2.3 can be placed on the host redshift from the lack of Ly-alpha forest lines in the combined spectrum. We do detect a strong emission line at 6664 A. If it corresponds to H-alpha at z = 0.015, we would expect to detect H-beta and the [O III] doublet in our spectrum. However, no features are visible at their predicted locations. In addition, this redshift would imply a very faint absolute magnitude of M_R = -10.3. If the emission line corresponds to [O III] 5008 at z = 0.331, we would expect to detect [O II] 3728 which we do not. The most probable association is with [O II] 3728, corresponding to a redshift of z = 0.787. Using the relations by Kennicutt (1998, ARA&A, 36, 189), the flux of the proposed [O II] line corresponds to a star formation rate (SFR) of approximately 1.9 M_Sun/year. This value has not been corrected for host extinction, and is therefore a strict lower limit to the actual SFR. The specific SFR is around 13.6 M_Sun/year (L/L*)^-1, typical for GRB host galaxies (Christensen et al., 2004, A&A, 425, 913).