//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4723 SUBJECT: GRB060210: Optical afterglow DATE: 06/02/10 05:19:16 GMT FROM: Derek Fox at PSU D.B. Fox (Penn State) and S.B. Cenko (Caltech) report on behalf of a larger collaboration: "We have imaged the XRT localization region for GRB060210 (Swift Trigger #180977) with the robotic Palomar 60-inch telescope, in two 60-second exposures beginning roughly 5 minutes after the BAT trigger. We identify a single point-like, bright, stationary source consistent with the XRT position, at coordinates: R.A. 03:50:57.41, Dec +27:01:34.4 (J2000) with a coordinate uncertainty of less than 2" in each axis. The estimated brightness of the transient at t+5.5 minutes is R=18.3 +/- 0.1 mag by reference to USNO B-1.0 catalog magnitudes of stars in the field." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4724 SUBJECT: GRB 060210: Swift detection of a burst DATE: 06/02/10 05:27:56 GMT FROM: Scott Barthelmy at NASA/GSFC A. Beardmore (U Leicester), S. Barthelmy (GSFC), P. Boyd (GSFC), D. Burrows (PSU), N. Gehrels (GSFC), C. Markwardt (GSFC/UMD), F. Marshall (GSFC), J. Osborne (U Leicester), D. Palmer (LANL), P. Schady (PSU/UCL-MSSL) on behalf of the Swift team: At 04:58:50 UT, Swift-BAT triggered and located GRB 060210 (trigger=180977). The spacecraft slewed immediately. The BAT on-board calculated location is RA,Dec 57.730d,+27.026d {03h 50m 55s,+27d 01' 33"} (J2000), with an uncertainty of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows a two-peak structure with a total duration of ~5 sec. The peak count rate was ~4500 counts/sec (15-350 keV), at ~1 seconds after the trigger. The XRT began observing the field at 05:00:25 UT, 95 seconds after the BAT trigger. XRT found a variable, uncatalogued X-ray source located at RA(J2000) = +03h 50m 57.2s, Dec(J2000) = +27d 01' 38.2", with an estimated uncertainty of 5.4 arcseconds (90% confidence radius). This location is 27 arcseconds from the BAT on-board position, within the BAT error circle. The initial flux in the 2.50s image was 4.6e-09 erg/cm2/s (0.2-10 keV). UVOT took a finding chart exposure of 200 seconds with the V filter starting 99 seconds after the BAT trigger. No afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT 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 XRT error circle. The list of sources is typically complete to about 18.0 mag. No correction has been made for the expected extinction of about 0.3 magnitudes. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4725 SUBJECT: GRB 060210: candidate afterglow DATE: 06/02/10 05:28:55 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li, University of California, Berkeley, on behalf of the KAIT GRB team, report: The robotic 0.76-m Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory observed GRB060210 detected with Swift (Trigger 180977). We identied an new object at the following position in an unfiltered 15s image started at 04:59:53 UT (63.2s after the burst): RA = 03:50:57.35 Dec = +27:01:34.1 (J2000.) the candidate afterglow is at mag 18.1 when calibrated to USNO B1.0 catalog. Further observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4726 SUBJECT: GRB060210:Faulkes Telescope North Afterglow Confirmation DATE: 06/02/10 05:44:19 GMT FROM: Carole Mundell at ARI, JMU,Liverpool C.G. Mundell, A. Melandri, A. Gomboc, C. Guidorzi, I. A. Steele, C.J. Mottram, A. Monfardini, R.J. Smith, M.F. Bode (Liverpool JMU), E. Rol, P. O'Brien, N. Bannister (U. Leicester) report: "The 2-m Faulkes Telescope North robotically followed up GRB060210 (SWIFT trigger 180977) 4.18 min after the GRB trigger time. The automatic "detection mode" procedure detected an uncatalogued candidate at: RA(J2000): 03:50:57.37 Dec(2000): +27:01:34.40 (positional uncertaintly 0.5") with magnitude R = 18.1 mag (wrt USNOB1). This source is coincident with that of Fox et al. (GCN 4723) and Li et al. (GCN 4725) and found to be fading, thus confirming it as the afterglow. Observations and analysis are ongoing. This message may be cited" //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4727 SUBJECT: GRB 060210: optical evolution DATE: 06/02/10 07:12:35 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li, University of California, Berkeley, on behalf of the KAIT GRB team, report: We report further analysis of the KAIT observations of GRB 060210 between 1 to 48 minutes after the burst. The optical afterglow showed an interesting evolution: it was nearly flat (with unfiltered mag of about 18.1) between t = 1 to 5 minutes, brightened to mag 17.7 at t = 9 minutes, then began a fast power-law decline between t = 10 to 48 minutes with an index of -1.05 +/- 0.05. A light curve for the optical afterglow is at http://astron.berkeley.edu/~weidong/grb060210.lc.gif The figure showed both the unfiltered and I-band light curve of the OA, both calibrated to USNO B1.0 red magnitudes. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4728 SUBJECT: GRB060210: Early Optical Observations DATE: 06/02/10 07:29:15 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 began observing the error box of GRB060210 (Swift Trigger 180977, GCN 4724) at 04:59:44.9 UT, 55 seconds 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 Fox et al. (GCN 4723) and Li et al. (GCN 4725) in our earliest exposure to the following 5-sigma limiting magnitude using USNO-B1 stars: t obs (UT) exp t (s) t-t_0 (s) Limit -------------------------------------------------------- 04:59:44.9 10 55.1 R > 17.5 Additional multi-band observations and analysis including image stacking are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4729 SUBJECT: GRB060210: Gemini absorption spectroscopy DATE: 06/02/10 09:12:53 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara (Penn State), D. B. Fox (Penn State), and E. Berger (Carnegie Observatories) report on behalf of a larger collaboration: "We have observed the optical afterglow (Fox & Cenko, GCN 4723) of GRB 060210 (Beardmore et al., GCN 4724) with the GMOS instrument on Gemini-North. Examination of a reduced 1500-s spectrum of the afterglow reveals a strong continuum break at roughly 6000 Angstroms, with only intermittent transmission blueward of this wavelength and multiple strong absorption features to the red, including the NV 1239,1243 doublet, the CIV 1548,1550 doublet, and an array of Si transitions, at the common redshift of z=3.91. We propose this as the redshift of GRB 060210." We acknowledge the rapid response effort of Gemini personnel that yielded these data, and in particular observer I. Song. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4730 SUBJECT: GRB060210: Optical Observations DATE: 06/02/10 09:36:40 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: Further analysis of the 0.6-m Super-LOTIS observations (GCN 4728) of the error box of GRB060210 (GCN 4724) yield detections of the optical afterglow (GCN 4723 and GCN 4725) in the summed R-band data. The summed images include a stack of five 10s exposures and a stack of five 20s exposures. The following table lists the mid-time of the stacked exposures and the resulting photometry using USNO-B1 stars: t_mid (UT) exp_t t_mid - t0 (s) R ----------------------------------------------------------------- 05:00:24.3 5 x 10 s 94.5 R = 18.25 +- 0.29 05:02:14.5 5 x 20 s 204.7 R = 18.30 +- 0.21 Analysis is ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4731 SUBJECT: GRB 060210 : Xinglong and Lulin optical limit DATE: 06/02/10 12:09:44 GMT FROM: Yuji Urata at RIKEN W. Zhou (BAO), C.S. Lin (NCU) Y. Urata (RIKEN), K.Y. Huang (NCU) and Y. Qiu (BAO) on behalf of RAFON report: "The 0.8-m telescope at Xinglong Observatory, China and 1.0-m telescope at Lulin Observatory, Taiwan started to observe GRB 060210 afterglow (Fox et al. # 4723; Li #4725) at 10.73 UT (~ 5.75 hours after burst) and 11.07 UT (~6.08 hours), respectively. No source was detected at afterglow position of our R and I images. Compare with USNO-B1.0, 3-sigma limiting magnitude are summarized as below : Delay time (hour) Filter Exp. limit site Mean time (SN=3) --------------------------------------------------------------------- 5.79 R 600s x 1 19.5 Xinglong 5.97 I 600s x 1 18.7 Xinglong 6.18 R 300s x 3 20.8 Lulin 6.46 I 300s x 3 20.0 Lulin This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4733 SUBJECT: GRB060210: Swift XRT Refined Analysis DATE: 06/02/10 13:36:53 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore, S. Mateos, K.L. Page (UL), D.N. Burrows (PSU) report on behalf of the Swift XRT Team. We have analysed the Swift XRT data from the first 3 orbits of GRB 060210 (Beardmore et al, GCN 4724). The refined XRT position from 2.5 ks of photon counting mode data is RA(J2000) = 3h 50m 57.4s Dec(J2000) = +27d 01' 36.4" with an estimated uncertainty of 3.6 arcsec (90% containment). This position is 29.5 arcseconds from the BAT position given in GCN 4724 and 2.0 arcseconds from the optical afterglow position reported in GCN 4726 (Mundell et al). The fading X-ray light curve shows 2 strong flares 200 s and 385 s after the BAT trigger. Fitting a power law to the data after the flares gives a late time decay slope of 0.7. The X-ray spectrum from the first orbit (T+103s to T+600s) is well fit by an absorbed power law, with a photon index of 1.93+/-0.03 and a column density of 1.64+/-0.3 e22 cm**-2 in the rest frame of the burst (assuming z = 3.91; Cucchiara et al, GCN 4729), in addition to the Galactic value of 8.5e20 cm**-2. The observed 0.2-10 keV flux is 9.4e-10 ergs cm**-2 s**-1, which corresponds to an unabsorbed flux of 1.3e-09 ergs cm**-2 s**-1. Assuming the X-ray emission from the GRB continues to decay at the same rate, the predicted count rate 24 hrs after the burst trigger is 0.1 count/s, which corresponds to an observed (unabsorbed) 0.2-10 keV flux of 3.4e-12 (4.8e-12) ergs cm**-2 s**-1. This circular is an official product of the Swift XRT Team. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4734 SUBJECT: GRB 060210: Refined analysis of the Swift-BAT burst DATE: 06/02/10 16:13:38 GMT FROM: Scott Barthelmy at NASA/GSFC A. Parsons (GSFC), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/ORAU), G. Sato (ISAS), J. Tueller (GSFC) on behalf of the Swift-BAT team: Using the data set from T-61 to T+122 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060210 (trigger #180977) (Beardmore, et al., GCN 4724). The BAT ground-calculated position is (RA,Dec) = 57.728, 27.022 deg {3h 50m 54.8s, 27d 1' 18.9"} (J2000) +- 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 41%. There is significant emission starting at T-45 sec, lasting all the way to a spike at T_zero. Then there is decaying emission out to ~T+15 (with a small peak at ~T+10), and then there is flat soft emission out to at least T+122 sec. We currently have data downlinked out to T+122, so we can not say what the lightcurve looks like past that point, although it seems likely there is emision beyond T+122. T90 (15-350 keV) is 46 +- 10 sec (estimated error including systematics). We will issue a another circular when the full data set becomes available (probably Saturday). The time-averaged spectrum from T-45.0 to T+9.3 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.47 +- 0.07. The fluence in the 15-150 keV band is (4.0 +- 0.2) x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T-0.02 sec in the 15-150 keV band is (2.7 +- 0.3) ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4742 SUBJECT: GRB 060210: Optical Observations DATE: 06/02/11 17:54:44 GMT FROM: Kuntal Mishra at ARIES,Nainital,India Kuntal Misra (ARIES, Nainital) on behalf of a larger Indian GRB collaboration We observed the field of GRB 060210 (swift trigger = 180977) using the 1-m reflector at ARIES, Nainital. The afterglow candidate reported by Fox and Cenko (#GCN 4723) is seen in our R band frame of 900 sec exposure, ~8.8 hrs after the burst, at a magnitude of 20.5 +/- 0.2 in comparison to four nearby USNO-B1.0 stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4746 SUBJECT: GRB060210: Swift/UVOT Upper Limits DATE: 06/02/11 23:29:28 GMT FROM: Peter Brown at PSU P. J. Brown (PSU), A. Beardmore (U Leicester), P. Schady (PSU/UCL-MSSL), N. Gehrels (GSFC) on behalf of the Swift/UVOT team report: The Swift/UVOT began taking data on the field of GRB 060210 at 05:00:28 UT on 2006-02-10, approximately 98 s after the BAT trigger (Beardmore et al., GCN 4724). No source is detected in the refined XRT error circle (Beardmore et al., GCN 4733) or at the position of the afterglow identified by Fox & Cenko (GCN 4723) in either the 200s finding chart images or summed images down to the following 3-sigma magnitude upper limits: Filter T_range(s) Exp(s) 3sigUL(mag) V 98-297 200 18.9 V 98-17151 1574 20.1 B 305-504 200 19.9 B 305-28728 2557 21.3 U 3750-27815 1594 20.6 UVW1 606-12060 1289 20.8 UVM2 582-17970 1402 21.1 UVW2 535-23754 2231 21.5 White 510-29539 2170 21.4 These magnitudes are uncorrected for Galactic extinction; E(B-V) = 0.09. These non-detections are consistent with the spectrum described by Cucchiara, Fox & Berger (GCN 4729) //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4748 SUBJECT: GRB 060210: Further refined analysis of the Swift-BAT burst DATE: 06/02/12 00:57:32 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 (UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), G. Sato (ISAS), J. Tueller (GSFC), A. Beardmore (U Leicester) on behalf of the Swift-BAT team: Using the data set from T-299.8 to T+302.2 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060210 (trigger #180977) (Beardmore, et al., GCN 4724; Parsons, et al., GCN 4734). The BAT ground-calculated position is (RA,Dec) = 57.729, 27.024 deg {3h 50m 55.1s, 27d 1' 27.5"} (J2000) +- 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 41%. The mask-weighted lightcurve shows many peaks with significant emission peaks starting at T-230 sec and the last peak at T+200. We caution that this on-going activity is a significant fraction of the t-300 to T+300 sec data interval we have received so far. This burst may have earlier or later activity. The main activity is from T-75 to T+20 sec with the brightest peak at T_zero. T90 (15-350 keV) is (255 +- 10) sec (estimated error including systematics). The time-averaged spectrum from T-227.5 to T+205.8 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.52 +- 0.09. The fluence in the 15-150 keV band is (7.7 +- 0.4) x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band is (2.8 +- 0.3) ph/cm2/sec. All the quoted errors are at the 90% confidence level. [GCN OPS NOTE(11feb06): Per author's request, the Beardmore author was added.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4753 SUBJECT: GRB 060210: ARC NIR Detection of Afterglow and Possible Host Galaxy DATE: 06/02/13 04:27:48 GMT FROM: Don Lamb at U.Chicago GRB 060210: ARC NIR Detection of Afterglow and Possible Host Galaxy F. Hearty (Colorado), M. Bayliss (Chicago), D. Q. Lamb (Chicago), R. McMillan (APO), B. Ketzeback (APO), J. Barentine (APO), J. Dembicky (APO), and D. G. York (Chicago) report: We observed the afterglow (Fox and Cenko, GCN 4723; Li, GCN 4725, 2727; Williams and Milne, GCN 4728, 4730; Misra, GCN 4742) of GRB 060210, a bright burst localized by Swift (Beardmore et al. GCN 4724, 4733; Takamoto et al. GCN 4748), on the night of February 10, using NIC-FPS on the ARC 3.5-meter telescope at Apache Point Observatory. The observation began at 2.65 UT on 11 February (21.75 hours after the burst) and ended at 3.35 UT on 11 February (22.37 hours after the burst). The observation consisted of a series of 90 20-second exposures in Ks. Using these exposures, we have constructed a stacked image of the GRB field, corresponding to a 30-minute exposure. Further 20-second exposures amounting to a total of 3300 seconds of exposure were taken immediately following this and are being processed. We detect an object at greater than the 5-sigma confidence level at the location of the optical afterglow to within 0.5". The PSF of the object overlaps with that of an adjacent extended source, but appears to be consistent with that of a point source. We identify the object as the NIR afterglow of GRB 060210. We measure Ks = 19.3 ± 0.2 mag, calibrated relative to the 2MASS stars in the field. We also detect an extended object centered 2"-3" to the north and immediately adjacent to the afterglow at Ks = 20.2 ± 0.3 mag, which may be the host galaxy of the burst. NIC-FPS is currently in its commissioning phase. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4761 SUBJECT: GRB 060210: Radio Observations DATE: 06/02/14 18:17:12 GMT FROM: Dale A. Frail at NRAO Dale A. Frail (NRAO) reports on behalf of a larger collaboration: "We used the Very Large Array to observe the GRB060210 (GCN 4724; GCN 4733; GCN 4734) at a frequency of 8.46 GHz on 2006 February 14.16 UT. No radio emission is detected within the +/-0.5 arcsecond error radius of the optical afterglow (GCN 4726) with a 3-sigma limit of 72 uJy. No further observations are planned. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5147 SUBJECT: GRB 060210: Jet Break in the XRT light curve DATE: 06/05/18 00:59:16 GMT FROM: Xinyu Dai at Ohio State U X. Dai and K. Z. Stanek (Ohio State Univ.) We analyzed the Swift-XRT light curve of GRB 060210 (Beardmore et al. 2006 GCN 4724). We added new data points to the X-ray light curve presented in Stanek et al. 2006 (astro-ph/0602495 v1) up to 1.e6 sec after the BAT trigger. We detected a smooth jet break (t_j = 7.9^{+2.2}_{-1.6} hr, observed) with the extended XRT light curve. We fitted both a single power-law and a broken power-law model to the XRT light curve from 3.e3 sec to 1.e6 sec after the BAT trigger. For the single power-law model we found alpha=1.09 and chi^2(dof) = 292.3(69). For the broken power-law model we found alpha1 = 0.7, alpha2 = 1.4, t_j = 7.9 hr, and chi^2(dof) = 64.8(67). We note that the power-law decay index for the X-ray light curve before the jet break (alpha1 ~ 0.7) is not consistent with the optical index (alpha_o ~ 1.3, Stanek et al. 2006 astro-ph/0602495). The XRT light curve for GRB 060210 is at http://www.astronomy.ohio-state.edu/~xinyu/grb/060210.jpg This message may be cited.