This file contains both GRB 060510A and GRB 060510B //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5095 SUBJECT: GRB 060510: Swift detection of a burst with optical transient DATE: 06/05/10 08:33:55 GMT FROM: Scott Barthelmy at NASA/GSFC H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), M. Capalbi (ASDC), M.L. Conciatore (ASDC), N. Gehrels (NASA/GSFC), C. Gronwall (PSU), S. T. Holland (GSFC/USRA), K. L. Page (U Leicester), D. M. Palmer (LANL), M. Perri (ASDC), E. Troja (INAF-IASFPA) and L. Vetere (ASDC) report on behalf of the Swift Team: At 07:43:27 UT, Swift-BAT triggered and located GRB 060510 (trigger=209351). The spacecraft slewed immediately. The BAT on-board calculated location is RA,Dec 95.870d,-1.162d {06h 23m 29s,-1d 09' 43"} (J2000), with an uncertainty of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows a multi-peak structure with a total duration of ~30 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~1 seconds after the trigger. The XRT began observing the field at 07:44:57 UT, 90 seconds after the BAT trigger. The on-board centroiding algorithm was confused by a cosmic ray close to the X-ray afterglow and the position sent out in the automated GCN Notice was incorrect. Using ground-processed data, we find a bright X-ray source located at RA(J2000) = 06h 23m 28.1s, Dec(J2000) = -01d 09' 44.9", with an estimated uncertainty of 8 arcseconds (90% confidence radius). This location is 11 arcseconds from the BAT on-board position, within the BAT error circle. UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 100 seconds after the BAT trigger. A fading source was found at RA,Dec = 06h 23m 28.0s -1d 09' 46" (J2000) with a mag of 18.2. There is nothing in DSS. No correction has been made for the expected extinction corresponding to E(B-V) of 0.41. This burst (trigger 209351) should not be confused with the second Swift-BAT trigger (209352) 38 minutes later. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5096 SUBJECT: GRB 060510B: Swift detection of a burst DATE: 06/05/10 08:57:19 GMT FROM: Scott Barthelmy at NASA/GSFC H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), M. Capalbi (ASDC), M.L. Conciatore (ASDC), N. Gehrels (NASA/GSFC), C. Gronwall (PSU), S. T. Holland (GSFC/USRA), J. P. Osborne (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), M. Perri (ASDC) and L. Vetere (ASDC) report on behalf of the Swift Team: At 08:22:14 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 060510B (trigger=209352). Swift slewed immediately to the burst. The BAT on-board calculated location is RA,Dec 239.141, +78.559 {15h 56m 34s, +78d 33' 33"} (J2000) with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). Because this is an image trigger, the TDRSS BAT light curve does not show any significant activity around the trigger time, but we note that there is possible activity at T+150 and T+300 sec. This possible long duration could be an indication of a high redshift burst. The XRT began observing the field at 08:24:13 UT, 119 seconds after the BAT trigger. XRT found a bright, possibly fading, uncatalogued X-ray source located at RA(J2000) = 15h 56m 29.3s, Dec(J2000) = +78d 34' 09.4", with an estimated uncertainty of 4.7 arcseconds (90% confidence radius). This location is 39 arcseconds from the BAT on-board position, within the BAT error circle. The initial flux in the 2.5s image was 7.1e-09 erg/cm2/s (0.2-10 keV). UVOT took a finding chart exposure of nominal 100 seconds with the White (160-650nm) filter starting 129 seconds after the BAT trigger. No afterglow candidate has beeen found in the initial data products. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for extinction. We note that this is the second Swift burst within 38 minutes. Because the second burst (GRB 060510B) overwrites the first (GRB 060510A) in the on-board automated observing program, the NFI follow-up observations for GRB 060510A will not be available until that burst can be uploaded as a ToO during normal working hours at the Swift Mission Operations Center. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5097 SUBJECT: GRB 060510B: MDM Observations and candidate OT DATE: 06/05/10 09:17:40 GMT FROM: Nestor Mirabal at U Michigan N. Mirabal (U. Michigan) and J. P. Halpern (Columbia U.) report on behalf of the MDM Observatory GRB follow-up team: "We have observed the Swift BAT location of GRB 060510 (Krim et al., GCN 5096) with the MDM 1.3m telescope on May 10 08:50 UT, 26 minutes after the trigger. We detect a faint source located at RA:15 56 29.615, Dec: 79 34 13.02 (+/- 2'') in a 600-s I band exposure, which is a potential optical afterglow for this event. The object appears to be fainter than R~22.5 in a previous 600~s exposure. This supports the idea that GRB 060510B could be a high-redshift or highly-reddened burst. Further observations are encouraged. Results here are very preliminary and analysis is in progress. This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5098 SUBJECT: GRB 060510B: Coordinate correction DATE: 06/05/10 09:36:01 GMT FROM: Nestor Mirabal at U Michigan N. Mirabal (U. Michigan) and J. P. Halpern (Columbia U.) report on behalf of the MDM Observatory GRB follow-up team: "The correct position of the object reported in our previous circular (GCN 5097) should read RA:15 56 29.615, Dec: 78 34 13.02 (+/- 2''). We apologize for this mistake. We thank Ken'ichi Torii for pointing it out." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5099 SUBJECT: GRB 060510b: NIR observations DATE: 06/05/10 10:18:47 GMT FROM: Paul Price at IfA,UH P.A. Price (IfA, Hawaii), T. Minezaki (IoA, Tokyo), L.L. Cowie, Y. Kakazu (IfA, Hawaii) and Y. Yoshii (IoA, Tokyo) report: We have observed the XRT localisation of GRB 060510b (GCN #5096) with the robotic MAGNUM telescope + MIPS dual-beam imager in the J band. Our observations consisted of 10 x 30 sec exposures commencing 2006 May 10.374 UTC. We do not detect any afterglow candidate at the XRT position, or at the faint optical afterglow candidate position of Mirabal & Halpern (GCN #5098), to an estimated limiting magnitude of J ~ 19.0 mag (based on comparison with the 2MASS catalogue star at 239.065708,78.573784 with J = 12.9 mag). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5100 SUBJECT: GRB 060510B: Super-LOTIS Observations DATE: 06/05/10 10:22:13 GMT FROM: Grant Williams at Steward Observatory G. G. Williams (MMTO) and P. A. Milne (Steward Observatory), on behalf of the Super-LOTIS Collaboration, report: The robotic 0.6-m Super-LOTIS telescope was manually triggered and began observing the error box of GRB 060510B (Swift Trigger 209352, GCN 5096) at 08:50:00.7 UT, ~28 minutes after the burst. Our initial observations include 5 x 10s exposures, 5 x 20s exposures, and 30 x 60s exposures, all in the R-band. We do not detect the afterglow reported by Mirabal et al. (GCN 5097) or any other new source within the XRT error box in our first several 60-second exposures to the following 3-sigma limiting magnitude estimated using nearby USNO-B1.0 stars: t obs (UT) exp t (s) t-t_0 (s) Limit -------------------------------------------------------- 08:53:41 60 1877 R > 18.6 Additional observations and analysis are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5101 SUBJECT: GRB 060510b: Gemini NIR observations DATE: 06/05/10 11:23:00 GMT FROM: Paul Price at IfA,UH P.A. Price (IfA, Hawaii), S.B. Cenko (Caltech) and D.B. Fox (Penn State) report on behalf of a larger collaboration: We have observed the XRT localisation of GRB 060510b (GCN #5096) with the Gemini North telescope + NIRI. Our observations consisted of 18 x 60 sec integrations commencing 2006 May 10.415 UTC. We detect the optical afterglow candidate of Mirabal & Halpern (GCN #5098), and estimate that the source is J ~ 19 mag (based on comparison with 2MASS star at 239.121115,+78.575104 with J = 16.6 mag). A finding chart is available at: http://www.ifa.hawaii.edu/~price/grb060510b.ps We have triggered optical spectroscopy observations with Gemini North. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5102 SUBJECT: GRB 060510B : Planned XMM-Newton observation DATE: 06/05/10 11:23:34 GMT FROM: Norbert Schartel at XMM-Newton/ESA XMM-Newton will observe GRB 060510B at location (RA=15h 56m 29.3s, DEC=+78d 34' 09.4", J2000), starting at 12:35 UT, on May 10, 2006, for an exposure of 43000 seconds. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5103 SUBJECT: GRB060510B : Faulkes North Telescope detection DATE: 06/05/10 11:51:18 GMT FROM: Andrea Melandri at Liverpool John Moores U A. Melandri, C. Guidorzi, C. Mundell, A. Gomboc, I.A. Steele, C.J. Mottram, A. Monfardini, S. Kobayashi, R.J. Smith, M.F. Bode (Liverpool JMU), P. O'Brien, E. Rol, N. Bannister (Leicester) report: "The 2-m Faulkes North Telescope robotically followed up GRB060510B (Krimm et al., GCN 5096) and began observing 2.8 minutes after the GRB trigger time. We confirm the detection of fading OT at the location identified by Mirabel et al. (GCN 5097) and Price et al. (GCN 5101). The automatic "detection mode" procedure did not detect an optical afterglow candidate in the XRT error circle (Krimm et al., GCN 5096) reported by Mirabal et al. (GCN 5097) in the first short-exposure R images. However, following visual inspection of subsequent co-added and single-frame images, the afterglow was clearly detected and found to be fading. We estimate source magnitudes to be i'~20.2 +/- 0.2, at 31 min post trigger, and R~21.0 +/- 0.5 for the co-added image from 2.8 to 20.2 min after the burst (total exposure time 240 sec). Further analysis and observation are still ongoing." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5104 SUBJECT: GRB 060510b: Redshift DATE: 06/05/10 14:18:08 GMT FROM: Paul Price at IfA,UH P.A. Price (IfA, Hawaii) reports on behalf of a larger collaboration: We have observed the optical afterglow of GRB 060510b (GCN #5098) with the Gemini North telesecope + GMOS. Observations consisted of 2 x 1000 sec exposures with the 400 lines/mm grating, with the source at an airmass ~ 2. Based on the presence of a strong continuum break around 7250A which we identify as due to Ly alpha, we estimate a redshift of z = 4.9. PAP thanks Nestor Mirabal for helpful discussion. We also thank the Gemini North observing team for performing these observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5105 SUBJECT: GRB060510 - SDSS Pre-Burst Observations DATE: 06/05/10 15:40:09 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 GRB060510 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/GRB060510 We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=95.8671 (06:23:28.1), dec=-1.16247 (-01:09:44.9); GCN 5095), 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 GRB060510_sdss.calstar.dat, we report photometry and astrometry of 1819 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 GRB060510_sdss.objects_flux.dat and GRB060510_sdss.objects_magnitudes.dat, we report photometry of 2209 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 GRB060510_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB060510_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=2.083 mag, A_g=1.533 mag, A_r = 1.112 mag, A_i=0.843 mag, and A_z=0.598 mag. There are currently no objects within 6 arcminutes of the GRB position in the SDSS spectroscopic database. 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: 5106 SUBJECT: GRB060510A: XRT refined analysis DATE: 06/05/10 18:20:08 GMT FROM: Maria Laura Conciatore at ASDC M.L. Conciatore, M. Capalbi, M. Perri, L. Vetere (ASDC), H. A. Krimm (GSFC/USRA)D. Burrows (PSU) report on behalf of the Swift/XRT team: We have analysed the first orbit of XRT data from GRB 060510A. A 1.8ks Photon Counting (PC) mode image provides a refined XRT position: RA(J2000) = 06 23 28.0 Dec(J2000)= -01 09 44.2 with an uncertainty of 3.5 arcsec (90% containment). This position is 1.3 arcsec away from the ground-calculated XRT position quoted in Krimm et al. (GCN 5095), 15.2 arcseconds from the BAT position (GCN 5095) and it is consistent with the UVOT position given in GCN 5095. A power-law fit of the PC spectrum with a column density fixed to the Galactic one (4.1 e21 cm^-2) gives a photon index of 2.1+/-0.5. The 0.2-10.0 keV observed flux is 2.0E-10 erg cm^-2 s^-1, which corresponds to an unabsorbed flux of 3.2E-10 erg cm^-2 s^-1. The light curve shows a fast initial decay, followed by a flattening phase. At about 1.2 ks from the trigger, it starts to decay again. Further osbervations are ongoing. This circular is an official product of the Swift XRT Team. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5107 SUBJECT: GRB 060510B: Swift-BAT Refined Analysis DATE: 06/05/10 19:33:16 GMT FROM: Hans Krimm at NASA-GSFC S. Barthelmy (GSFC), L. Barbier (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), M. Koss (GSFC/UMD), C. Markwardt (GSFC/UMD), D. Palmer (LANL), 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-239.0 to T+423 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060510B (trigger #209352) (Krimm, et al., GCN 5096). The BAT ground-calculated position is (RA,Dec) = 239.215, 78.597 deg {15h 56m 51.6s, 78d 35' 48.7"} (J2000) +- 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weighted light curve shows a very long period of emission extending from T+ ~25 sec to T+ ~330 sec. There are numerous (6-10) overlapping peaks in the light curve, with the two brightest peaks at T+ ~140 sec and T+ ~290 sec. T90 (15-350 keV) is 276 +- 10 sec (estimated error including systematics). This stretched-out emission is consistent with this burst being at high redshift (z=4.9, Price, GCN 5104). We have only fragmentary event data after T+423 sec, but the onboard mask-tagged light curves show no significant emission after this time. The time-averaged spectrum from T-16.3 sec to T+326.1 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.76 +- 0.08. The fluence in the 15-150 keV band is 4.2 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+136.24 sec in the 15-150 keV band is 0.6 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Given a redshift of z=4.9, we compute Eiso to be 2.04 X 10^53 ergs (88.5 - 885 keV in the rest frame.) This assumes a cosmology with Omega_M=0.3, Omega_lambda=0.7 and H0=65. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5108 SUBJECT: GRB 060510A: Refined analysis of the Swift-BAT burst DATE: 06/05/10 19:43:53 GMT FROM: Scott Barthelmy at NASA/GSFC L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), M. Koss (UMD), C. Markwardt (GSFC/UMD), D. Palmer (LANL), 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-240 to T+962 sec from recent telemetry downlinks, we report further analysis of BAT GRB 060510A (trigger #209351) (Krimm, et al., GCN 5095). The BAT ground-calculated position is RA,Dec = 95.855, -1.166 deg {6h 23m 25.1s, -1d 9' 56.5"} (J2000) +- 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 6%. The mask-weighted lightcurves shows several overlapping peaks starting at T-8 sec amd ;lasting out to T+25 sec. T90 (15-350 keV) is 21 +- 3 sec (estimated error including systematics). The time-averaged spectrum from T-7.0 to T+17.1 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.55 +- 0.10. The fluence in the 15-150 keV band is 9.8 +- 0.5 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.29 sec in the 15-150 keV band is 17.0 +- 1.9 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Because this burst occured at the edge of the BAT FOV (note the low partial coding percentage), the spectral fit values have an extra systematic error contribution of about 10%. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5109 SUBJECT: GRB 060510B: Swift/UVOT Upper Limits DATE: 06/05/10 20:27:52 GMT FROM: Stephen Holland at USRA/NASA/GSFC/SSC GRB 060510B: Swift/UVOT Upper Limits S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT team: The Swift UVOT began observing GRB 060510B (trigger #209351, Krimm et al., GCN Circular 5096) 111 seconds after the BAT trigger. No optical afterglow is detected at the location of the optical afterglow (Mirabal & Halpern 2006, GCN Circular 5097). The lack of detection in any UVOT filter is consistent with the burst having a redshift of z = 4.9 (Price 2006, GCN Circular 5104). Midpoint Coadded Upper Filter Time Exposure Limit (sec) (sec) (3 sigma) V 1034 1598 21.2 B 5141 403 21.4 U 4950 433 21.1 UVW1 4736 413 20.6 UVM2 4852 1056 20.9 UVW2 5446 197 19.7 White 479 699 21.9 No correction has been made for the Galactic reddening of to E(B-V) = 0.04 mag (Schlegel et al. 1998) along the line of sight to GRB //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5110 SUBJECT: GRB060510B: Swift XRT refined analysis DATE: 06/05/10 22:07:59 GMT FROM: Matteo Perri at ISAC/ASDC M. Perri, M. Capalbi, M.L. Conciatore, L. Vetere (ASDC), H.A. Krimm (GSFC/USRA) and D.N. Burrows (PSU) report on behalf of the Swift/XRT team: We have analyzed the first four orbits of Swift XRT data on the BAT GRB 060510B (Krimm, et al., GCN 5096; Barthelmy et al., GCN 5107). A 5.3 ks Photon Counting (PC) mode image gives a refined X-ray position of: RA(J2000) = 15h 56m 29.9s Dec(J2000) = +78d 34' 09.7" with an uncertainty of 3.6 arcsec (90% containment). This is 2 arcmin away from the center of the refined BAT position quoted in GCN 5107, and 1.8 arcsec away from the initial XRT position reported in GCN 5096. The early 0.3-10 keV light curve has a complex behavior. The first orbit of data shows an initial shallow decay with slope ~ -0.3, a temporal break at about T+350s followed by a steep decay with slope ~ -11. Three X-ray flares at about T+200s, T+300s and T+880s are also observed during the first orbit. The afterglow decay between the second and the fourth orbit has a slope of ~ -0.4. The X-ray spectrum covering the time period from T+128s to T+456s is well fit by an absorbed power-law with a photon index of 1.42+/-0.13 and column density of (1.5+/-0.1)e21 cm**-2. We note the Galactic column density in the direction of the source is 3.8e20 cm**-2. The observed (unabsorbed) 0.3-10 keV flux for this spectrum is 4.3e-9 (4.9e-9) erg/cm**2/s. All the quoted errors are at the 90% confidence level. If the burst continues decaying at the current rate we estimate an XRT count rate of 6e-3 counts/s at T+24hr, which corresponds to an unabsorbed 0.3-10.keV flux of 3e-13 ergs cm**-2 s**-1. This circular is an official product of the Swift XRT Team. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5113 SUBJECT: Konus-Wind observation of GRB 060510A DATE: 06/05/11 13:39:12 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team report: The long GRB 060510A (Swift-BAT trigger #209351; Krimm et al., GCN 5095; Barbier et al., GCN 5108) triggered Konus-Wind at 27796.301 s UT (07:43:16.301). As observed by Konus-Wind it had a duration of ~25 s, fluence 2.55(-0.22,+0.07)x10^-5 erg/cm2, and the 64-ms peak flux measured from T0+7.488 s 4.29(-0.72, +0.63)x10^-6 erg/cm2/s (both in the 20 keV - 1 MeV energy range). The burst shows a strong hard-to-soft spectral evolution. Fitting the time-integrated spectrum of the burst (from T0 to T0+24.064 s; in the 20 keV - 1 MeV range) by a power law with exponential cutoff model: dN/dE ~ E^(-alpha)*exp(-E*(2-alpha)/Ep) yields alpha = 1.661(-0.076, +0.072) and Ep = 184 (-24, +36) keV (chi2 = 63/48 dof). All the quoted errors are at the 90% confidence level. The K-W light curve is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB060510_T27796/ //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5116 SUBJECT: GRB 060510A: Swift/UVOT Detection of an Optical Afterglow DATE: 06/05/12 12:31:19 GMT FROM: Stephen Holland at USRA/NASA/GSFC/SSC GRB 060510A: Swift/UVOT Detection of an Optical Afterglow S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT team: The Swift UVOT began observing GRB 060510A (trigger #209351, Krimm et al., GCN Circular 5095) 82 seconds after the BAT trigger. We detect the UVOT optical transient reported in the above Circular in the White, V-, and U-band filters. The J2000 coordinates of the afterglow are RA = 06:23:27.98 Dec = -01:09:46.2 with an uncertainty of +/- 0.56 arcseconds (90% containment). Magnitudes and 3-sigma upper limits are reported below. Midpoint Coadded Upper Filter Time Exposure Mag Err Limit (sec) (sec) (3 sigma) V 405 394 18.38 0.13 V 1060 394 18.85 0.16 B 688 10 18.4 B 1503 20 19.2 U 817 20 18.06 0.40 U 1479 20 18.3 UVW1 645 20 17.1 UVW1 793 20 17.4 UVM2 769 20 17.5 UVM2 1431 20 17.6 UVW2 721 20 17.6 UVM2 1384 20 17.7 White 150 99 18.04 0.15 White 702 10 18.24 0.50 White 1318 99 18.87 0.18 White 1521 10 18.12 0.40 White 1680 10 18.7 No correction has been made for the Galactic reddening of E(B-V) = 0.42 mag (Schlegel et al. 1998) along the line of sight to GRB 060510A. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5157 SUBJECT: XMM-Newton observation of GRB060510b DATE: 06/05/23 14:45:56 GMT FROM: Sergio Campana at INAF-OAB Sergio Campana (INAF/OAB) and Andrea DeLuca (INAF/IASF Milano) report: We have analyzed the XMM-Newton observation of the field of GRB060510B, discovered by Swift/BAT on May 10 2006, 08:22:14 UT (Krimm et al., GCN 5096). The XMM-Newton observation started ~5 hours after the GRB trigger and lasted for ~40 ks. The observation is affected by a high particle background, resulting in about 17 ks of usable data. We report here on data collected by the EPIC/pn camera. The afterglow of GRB060510B is detected at the following coordinates: RA(J2000): 15h 56m 29s.2, Dec(J2000): +78d 34' 12.0", with an uncertainty of 1.5 arcsec (1sigma), fully consistent with the reported Swift/XRT (Krimm et al.) and optical (Mirabal et al. GCN5097) positions. Extracting source events from a circle of 30 arcsec radius, the pn time-averaged, background-subtracted count rate in the 0.5-8 keV range is of 0.11+/-0.003 cts/s. The source is clearly fading with a power law decay with alpha=-0.7+/-0.1 (error at 90% c.l. for a single parameter) with reduced chi2=1.3, 16 d.o.f. The time-integrated X-ray spectrum is well fit (reduced chi2=1.0, 72 d.o.f.) by a power law absorbed by a column NH=(9.4+/-3.5)x10^20 cm^-2 (error at 90% confidence level), slightly larger than the Galactic value of NH_gal=3.8x10^20 cm^-2 (Dickey & Lockman 1990), and with a photon index Gamma=2.7+/-0.3. Since the redshift of the GRB afterglow is known we consider also an intrinsic absorption at z=4.9 (Price, GCN5104). The fit is similarly good (reduced chi2=0.99, 72 d.o.f.) with NH_z=(2.1+/-1.2)x10^22 cm^-2 and Gamma=2.5+/-0.2. The observed flux (0.5-10 keV) is of 1.4x10^-13 erg cm^-2 s^-1, corresponding to an unabsorbed flux of 1.8x10^-13 erg cm^-2 s^-1. No spectral evolution as a function of time (first 16 ks vs. remaining 22 ks of data) has been observed.