////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Wed 11 Dec 02 11:18:56 UT NOTICE_TYPE: HETE S/C_Alert TRIGGER_NUM: 2493, Seq_Num: 1 GRB_DATE: 12619 TJD; 345 DOY; 02/12/11 GRB_TIME: 40714.03 SOD {11:18:34.03} UT TRIGGER_SOURCE: Trigger on the 25-400 keV band. GAMMA_RATE: 287 [cnts/s] on a 0.160 [sec] timescale SC_-Z_RA: 110 [deg] SC_-Z_DEC: 11 [deg] SC_LONG: 246 [deg East] WXM_CNTR_RA: 122.238d {+08h 08m 57s} (J2000), 122.277d {+08h 09m 06s} (current), 121.569d {+08h 06m 17s} (1950) WXM_CNTR_DEC: +6.713d {+06d 42' 47"} (J2000), +6.704d {+06d 42' 16"} (current), +6.860d {+06d 51' 37"} (1950) WXM_MAX_SIZE: 28.00 [arcmin] diameter WXM_LOC_SN: 13 sig/noise (pt src in image) WXM_IMAGE_SN: X= 8.7 Y= 10.7 [sig/noise] WXM_LC_SN: X= 19.7 Y= 24.7 [sig/noise] SUN_POSTN: 258.30d {+17h 13m 12s} -23.00d {-23d 00' 08"} SUN_DIST: 134.71 [deg] MOON_POSTN: 350.36d {+23h 21m 26s} -9.86d {-09d 51' 30"} MOON_DIST: 132.35 [deg] MOON_ILLUM: 48 [%] GAL_COORDS: 215.76,20.28 [deg] galactic lon,lat of the burst ECL_COORDS: 122.95,-13.11 [deg] ecliptic lon,lat of the burst COMMENTS: Probable GRB. COMMENTS: WXM error box is circular; not rectangular. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Wed 11 Dec 02 11:19:04 UT NOTICE_TYPE: HETE S/C_Update TRIGGER_NUM: 2493, Seq_Num: 2 GRB_DATE: 12619 TJD; 345 DOY; 02/12/11 GRB_TIME: 40714.03 SOD {11:18:34.03} UT TRIGGER_SOURCE: Trigger on the 25-400 keV band. GAMMA_RATE: 287 [cnts/s] on a 0.160 [sec] timescale SC_-Z_RA: 110 [deg] SC_-Z_DEC: 11 [deg] SC_LONG: 246 [deg East] WXM_CNTR_RA: 122.228d {+08h 08m 55s} (J2000), 122.268d {+08h 09m 04s} (current), 121.560d {+08h 06m 14s} (1950) WXM_CNTR_DEC: +6.735d {+06d 44' 05"} (J2000), +6.726d {+06d 43' 33"} (current), +6.882d {+06d 52' 54"} (1950) WXM_MAX_SIZE: 28.00 [arcmin] diameter WXM_LOC_SN: 19 sig/noise (pt src in image) WXM_IMAGE_SN: X= 12.5 Y= 15.0 [sig/noise] WXM_LC_SN: X= 25.5 Y= 25.5 [sig/noise] SUN_POSTN: 258.30d {+17h 13m 12s} -23.00d {-23d 00' 08"} SUN_DIST: 134.73 [deg] MOON_POSTN: 350.36d {+23h 21m 26s} -9.86d {-09d 51' 30"} MOON_DIST: 132.35 [deg] MOON_ILLUM: 48 [%] GAL_COORDS: 215.73,20.28 [deg] galactic lon,lat of the burst ECL_COORDS: 122.94,-13.10 [deg] ecliptic lon,lat of the burst COMMENTS: Probable GRB. COMMENTS: WXM error box is circular; not rectangular. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Wed 11 Dec 02 11:21:19 UT NOTICE_TYPE: HETE S/C_Update TRIGGER_NUM: 2493, Seq_Num: 3 GRB_DATE: 12619 TJD; 345 DOY; 02/12/11 GRB_TIME: 40714.03 SOD {11:18:34.03} UT TRIGGER_SOURCE: Trigger on the 25-400 keV band. GAMMA_RATE: 287 [cnts/s] on a 0.160 [sec] timescale SC_-Z_RA: 110 [deg] SC_-Z_DEC: 11 [deg] SC_LONG: 246 [deg East] WXM_CNTR_RA: 122.228d {+08h 08m 55s} (J2000), 122.268d {+08h 09m 04s} (current), 121.560d {+08h 06m 14s} (1950) WXM_CNTR_DEC: +6.735d {+06d 44' 05"} (J2000), +6.726d {+06d 43' 33"} (current), +6.882d {+06d 52' 54"} (1950) WXM_MAX_SIZE: 28.00 [arcmin] diameter WXM_LOC_SN: 19 sig/noise (pt src in image) WXM_IMAGE_SN: X= 12.5 Y= 15.0 [sig/noise] WXM_LC_SN: X= 25.5 Y= 25.5 [sig/noise] SUN_POSTN: 258.30d {+17h 13m 12s} -23.00d {-23d 00' 08"} SUN_DIST: 134.73 [deg] MOON_POSTN: 350.36d {+23h 21m 26s} -9.86d {-09d 51' 30"} MOON_DIST: 132.35 [deg] MOON_ILLUM: 48 [%] GAL_COORDS: 215.73,20.28 [deg] galactic lon,lat of the burst ECL_COORDS: 122.94,-13.10 [deg] ecliptic lon,lat of the burst COMMENTS: Probable GRB. COMMENTS: WXM error box is circular; not rectangular. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Wed 11 Dec 02 11:22:12 UT NOTICE_TYPE: HETE S/C_Last TRIGGER_NUM: 2493, Seq_Num: 4 GRB_DATE: 12619 TJD; 345 DOY; 02/12/11 GRB_TIME: 40714.03 SOD {11:18:34.03} UT TRIGGER_SOURCE: Trigger on the 25-400 keV band. GAMMA_RATE: 287 [cnts/s] on a 0.160 [sec] timescale SC_-Z_RA: 110 [deg] SC_-Z_DEC: 11 [deg] SC_LONG: 246 [deg East] WXM_CNTR_RA: 122.228d {+08h 08m 55s} (J2000), 122.268d {+08h 09m 04s} (current), 121.560d {+08h 06m 14s} (1950) WXM_CNTR_DEC: +6.735d {+06d 44' 05"} (J2000), +6.726d {+06d 43' 33"} (current), +6.882d {+06d 52' 54"} (1950) WXM_MAX_SIZE: 28.00 [arcmin] diameter WXM_LOC_SN: 19 sig/noise (pt src in image) WXM_IMAGE_SN: X= 12.5 Y= 15.0 [sig/noise] WXM_LC_SN: X= 25.5 Y= 25.5 [sig/noise] SUN_POSTN: 258.30d {+17h 13m 12s} -23.00d {-23d 00' 08"} SUN_DIST: 134.73 [deg] MOON_POSTN: 350.36d {+23h 21m 26s} -9.86d {-09d 51' 30"} MOON_DIST: 132.35 [deg] MOON_ILLUM: 48 [%] GAL_COORDS: 215.73,20.28 [deg] galactic lon,lat of the burst ECL_COORDS: 122.94,-13.10 [deg] ecliptic lon,lat of the burst COMMENTS: Probable GRB. COMMENTS: WXM error box is circular; not rectangular. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Wed 11 Dec 02 13:29:31 UT NOTICE_TYPE: HETE Ground Analysis TRIGGER_NUM: 2493, Seq_Num: 5 GRB_DATE: 12619 TJD; 345 DOY; 02/12/11 GRB_TIME: 40714.03 SOD {11:18:34.03} UT TRIGGER_SOURCE: Trigger on the 25-400 keV band. GAMMA_RATE: 287 [cnts/s] on a 0.160 [sec] timescale SXC_RATE: 26 [cnts/s] SC_-Z_RA: 110 [deg] SC_-Z_DEC: 11 [deg] SC_LONG: 246 [deg East] WXM_CNTR_RA: 122.270d {+08h 09m 05s} (J2000), 122.309d {+08h 09m 14s} (current), 121.602d {+08h 06m 24s} (1950) WXM_CNTR_DEC: +6.678d {+06d 40' 41"} (J2000), +6.669d {+06d 40' 09"} (current), +6.825d {+06d 49' 31"} (1950) WXM_MAX_SIZE: 10.00 [arcmin] diameter WXM_LOC_SN: 67 sig/noise (pt src in image) WXM_IMAGE_SN: X= 13.1 Y= 16.8 [sig/noise] WXM_LC_SN: X= 16.0 Y= 2.2 [sig/noise] SXC_CNTR_RA: 122.250d {+08h 09m 00s} (J2000), 122.290d {+08h 09m 09s} (current), 121.581d {+08h 06m 20s} (1950) SXC_CNTR_DEC: +6.739d {+06d 44' 20"} (J2000), +6.730d {+06d 43' 49"} (current), +6.886d {+06d 53' 10"} (1950) SXC_MAX_SIZE: 4.00 [arcmin] diameter SXC_LOC_SN: 23 sig/noise (pt src in image) SUN_POSTN: 258.30d {+17h 13m 12s} -23.00d {-23d 00' 08"} SUN_DIST: 134.71 [deg] MOON_POSTN: 350.36d {+23h 21m 26s} -9.86d {-09d 51' 30"} MOON_DIST: 132.37 [deg] MOON_ILLUM: 48 [%] GAL_COORDS: 215.74,20.30 [deg] galactic lon,lat of the burst ECL_COORDS: 122.96,-13.09 [deg] ecliptic lon,lat of the burst COMMENTS: Probable GRB. COMMENTS: WXM error box is circular; not rectangular. COMMENTS: SXC error box is circular; not rectangular. COMMENTS: Burst_Validity flag is true. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1731 SUBJECT: HETE 2493: Optical candidate DATE: 02/12/11 12:11:51 GMT FROM: Paul Price at RSAA, ANU at CIT D.W. Fox and P.A. Price (Caltech) report: We have observed the error circle of HETE trigger #2493 with the Palomar 48-inch + NEAT unfiltered CCD camera. We find a point source at approximate J2000 coordinates: 8:08:59.883 6:43:37.88 that is not present on the DPOSS F plate. The source appears stationary, and appears to be fading. Further observations are planned. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1732 SUBJECT: HETE 2493: Optical observations DATE: 02/12/11 12:46:10 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price and D.W. Fox (Caltech) report: A finding chart for the optical afterglow candidate reported in GCN #1731 is available from http://darkalf.caltech.edu/~pap/hete2493.ps The star marked "Offset1" is at approximate coordinates: 8:08:58.387 6:43:25.83 J2000 and the offset to the afterglow candidate is 22.29" E and 12.72" N. At this stage in analysis, we estimate that the afterglow was R ~ 19 mag at Dec 11, 11:39 UT, and fading. No spectroscopy can be done with Keck or Palomar 200-inch. We encourage any other observers to obtain spectroscopic observations with available resources. Further imaging observations are underway. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1733 SUBJECT: HETE 2493: Optical observations DATE: 02/12/11 14:36:49 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price and D.W. Fox (Caltech) report: We observed the afterglow of GRB 021211 (HETE trigger #2493) with the Palomar 48-inch telescope + NEAT unfiltered camera over the course of approximately 1.3 hours, commencing 20 minutes after the GRB. Rough analysis yields an approximate magnitude for the afterglow during the first observation of R ~ 18.2 mag. The source faded with an approximate power-law index of alpha ~ 0.97 over the course of our exposures. Further multicolour observations are underway. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1734 SUBJECT: GRB021211 (=H2493): A Bright, Long GRB Localized by HETE-2 in Near-Real Time DATE: 02/12/11 14:52:49 GMT FROM: Don Lamb at U.Chicago GRB021211 (=H2493): A Bright, Long GRB Localized by HETE-2 in Near-Real Time G. Crew, J. Villasenor, R. Vanderspek, J. Doty, G. Monnelly, N. Butler, T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, G. Azzibrouck, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC Teams; G. Ricker, J-L Atteia, N. Kawai, D. Lamb, and S. Woosley on behalf of the HETE Science Team; Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, and T. Donaghy, Y. Nakagawa, D. Takahashi, M. Suzuki, R. Satoh, and Y. Urata, on behalf of the HETE WXM Team; M. Boer, J-F Olive, J-P Dezalay, C. Barraud and K. Hurley on behalf of the HETE FREGATE Team; write: At 11:18:34.03 UTC (40714.03 s UT) on 11 Dec 2002, the HETE FREGATE, WXM, and SXC instruments detected event H2493, a bright, long GRB. The WXM flight localization was correct and was reported in a GCN Position Notice at 11:18:56 UT, 22 sec after the beginning of the burst. Ground analysis of the WXM data for the burst produced a refined location, which was reported in a GCN Notice at 13:29:31 UT, 131 minutes after the burst. The WXM localization SNR was 21. The WXM location can be expressed as a 90% confidence circle that is 5 arcminutes in radius and is centered at RA = +08h 09m 04.8s, Dec = 06d 40'41" (J2000). The uncertainty in the WXM localization is due entirely to systematic error. Ground analysis of the SXC data for the burst produced a further refinement in the location, which was reported in the same GCN Notice at 13:29:31 UT. The SXC localization SNR was 23. The SXC location can be expressed as a 90% confidence circle that is 2 arcminutes in radius and is centered at RA = +8h 09m 00s, Dec = +06d 44' 20" (J2000). The SXC localization may be improved. The location of the optical afterglow candidate reported in GCN 1731 (D. W. Fox and P. A. Price) is offset by 3.2 arcmin from the center of the WXM error circle and 42 arcsec from the center of the SXC error circle. The location of the optical afterglow candidate is therefore fully consistent with the WXM and SXC localizations for GRB021211. The burst duration in the 8-40 keV band was > 5.7 sec. A total of 8310 counts were detected during that interval, corresponding to a fluence of ~1 x 10-6 ergs cm-2 . The peak flux was >8 x 10-7 ergs cm-2 s-1 (i.e., > 20 x Crab flux) in 5msec. A light curve and skymap for GRB021211 is provided at the following URL: http://space.mit.edu/HETE/Bursts/ This message is citable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1736 SUBJECT: GRB021211 (HETE2493), OT at 143 sec DATE: 02/12/11 18:53:47 GMT FROM: Hye-Sook Park at LLNL H.S. Park, G. Williams, S. Barthelmy report on behalf of Super-LOTIS collaboration: Super-LOTIS observed GRB021211 (HETE2493) in real-time. The image taken at 143 sec after burst shows a bright OT at the location reported by Fox et al (GCNC 1731). Approximate R magitude is ~15.2. Further analysis on accurate photometry and the light curve from the later images are in progress. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1737 SUBJECT: GRB021211, OT at 108 s DATE: 02/12/11 21:13:01 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li, A. V. Filippenko, R. Chornock, S. Jha (UCB) report: "The Katzman Automatic Imaging Telescope (KAIT) observed GRB021211 (HETE Trigger #2493) in real time. Four batches of observations (a total of 60 images) were taken during the first three hours after the burst. The image taken at 108 s after burst (11:20:22 UT) shows a bright OT at the location reported by Fox et al. (GCN #1731), with an unfiltered magnitude about 14.8 (USNO-A2.0 calibrations). The OT faded to mag about 15.3 in an image taken at 171 s after burst, and was at mag about 15.8 in an image taken at 202 s after burst. Photometry of subsequent images is in progress." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1738 SUBJECT: GRB021211 - Upper limits from recent and historical observations DATE: 02/12/12 00:49:08 GMT FROM: Michael Wood-Vasey at UC Berkeley/LBNL/SNfactory W. M. Wood-Vasey, Lawrence Berkeley National Laboratory, using images obtained by R. Bambery, S. Pravdo, M. Hicks, and K. Lawrence (Near-Earth Asteroid Tracking project, Jet Propulsion Laboratory), reports upper limits for previous observations at the location of the object identified by Fox et al. (GCN 1731) as the optical counterpart to GRB 20021211 from unfiltered observations with the 1.2m MSSS telescope at Haleakala and the Oschin 48" telescope at Palomar Observatory (the same instrument as used by Fox et al.). A co-addition of Haleakala images from 5 January, 11 January, 16 January, 1 December (all dates 2002 UT) shows no source visible at this location to a limiting unfiltered magnitude of 21.6 (calibrated to USNO R-band stars on the image frame) at a S/N of 3. Palomar images from 9 December 2002, taken under non-ideal conditions, show no source visible at this location to a limiting unfiltered magnitude of 18.4 (calibrated to USNO R-band stars on the image frame) at a S/N of 3. The Haleakala co-added image is available at http://supernova.lbl.gov/~wwoodvas/GRB/#GRB20021201 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1739 SUBJECT: GRB 021211, R- and I-band observations DATE: 02/12/12 01:18:11 GMT FROM: Sylvio Klose at TLS Tautenburg S. Klose, J. Eisloeffel, D. Froebrich, A. Zeh, S. Richter, C. Hoegner (TLS Tautenburg) & H. Voss (DLR Berlin) report: The stellar field containing the afterglow of the HETE burst GRB 021211 (HETE 2493; Fox et al., GCN 1731) was observed with the Tautenburg Schmidt telescope in R and I on Dec. 11, 23:00 - 23:40 UT, i.e. 12 hrs after the burst trigger. We do not detect the afterglow. We estimate that at this time the source was already fainter than R=22.7 and I=20.7. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1740 SUBJECT: GRB 021211 Milagro GeV/TeV Observations DATE: 02/12/12 15:39:25 GMT FROM: Julie McEnery at UMBC/GSFC Julie McEnery on behalf of the Milagro collaboration reports: Milagro searched for emission at GeV/TeV energies from GRB 021211 over the duration reported by the HETE WXM. No evidence for prompt GeV/TeV emission was found. A preliminary analysis (assuming a differential photon spectral index of -2.4) gives an upper limit on the fluence at the 99.9% confidence level of: J(0.2-20 TeV) < 3.8 * 10^(-6) erg cm^(-2) (over a 6 second interval) //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1742 SUBJECT: SUB-MM SEARCH FOR GRB 021211 DATE: 02/12/12 21:57:22 GMT FROM: Gerald Moriarty-Schieven at Joint Astro. Center SUB-MM SEARCH FOR GRB 021211 Jim Hoge (1), Chris Willott (2), Jennifer Grimes (3), Remo Tilanus (1), Gerald Moriarty-Schieven (1,2) (1) Joint Astronomy Centre (2) National Research Council of Canada (3) Oxford University Observations were made, on behalf of two consortia, of GRB021211 (position from GCN 1731) using the SCUBA bolometer array on the James Clerk Maxwell Telescope located on Mauna Kea, Hawaii, on December 12.49 - 12.52 UT, under excellent sky conditions. After 1800 seconds of integration, the object was not detected at 850microns (347GHz) at 2 +/- 2.5 mJy, or a 3sigma upper limit of 7.5mJy. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1744 SUBJECT: GRB021211: Optical observations DATE: 02/12/13 00:32:27 GMT FROM: Don Lamb at U.Chicago GRB021211: Optical observations D. Q. Lamb, J. C. Barentine, M. C. Nysewander, D. E. Reichart, M. Schwartz, C. Laws, D. G. York, and R. J. McMillan report, We have observed the field of GRB021211 (Crewe et al., GCN 1734) using the ARC 3.5-meter telescope at APO under excellent seeing conditions but occasional high cirrus. Pointing problems prevented us from calibrating our images using standard stars. In two 2000 second i' images of the GRB021211 field beginning at 09:19 UT on December 12, we detect an object which we estimate has i* > 23 at the position of the optical afterglow of GRB021211 (Fox and Price, GCN 1731). The object is more diffuse than the point spread function for stars that are nearby in the images, which suggests that the object may be the host galaxy of GRB021211. If so, the optical afterglow of GRB021211 was fainter than about i* = 23. Comparison with I_c images taken at Tenagra beginning 40 minutes after the burst implies that the afterglow faded in i* by more than about 4 magnitudes in the intervening 21 hours. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1745 SUBJECT: GRB 021211: Radio Observations DATE: 02/12/13 00:48:37 GMT FROM: Edo Berger at Caltech E. Berger (Caltech) and D. A. Frail (NRAO) report on behalf of a larger collaboration: "On December 12.37 UT we used the VLA at 8.46 GHz to observe the position of the optical transient (GCN 1731) of GRB 021211 (GCN 1734). We do not detect a radio source coincident with the OT down to a 3-sigma limit of about 70 microJy. Further observations are planned." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1748 SUBJECT: GRB021211: Kiso Observations DATE: 02/12/13 11:27:35 GMT FROM: Yuji Urata at RIKEN H. Mito, S. Nishiura, and Y. Urata on behalf of the Kiso GRB team: "We imaged the field of GRB021211 (Crew et al., GCN 1734) using the Kiso observatory (the University of Tokyo) 1.05m Schmidt telescope starting at December 12.638 UT. We obtained 13 frames R-band images with 300 sec exposure. We could not detect significant emission at the position of the optical afterglow of GRB021211 (Fox and Price, GCN 1731). The limiting magnitude for a combined image is R~ 21 mag. (3 sigma, compared with USNO-A2.0 red magnitudes)." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1749 SUBJECT: GRB 021211: Optical Observations DATE: 02/12/13 12:11:24 GMT FROM: Ken ichi Torii at RIKEN K. Kinugasa (Gunma Astronomical Observatory), T. Kato (Kyoto U.), H. Yamaoka (Kyushu U.), and K. Torii (RIKEN) report: Starting at 12:44 UT on December 11th, the central 11x11 square arcmin of the error region of GRB 021211 (Crew, et al., GCN 1734) was observed with the Gunma Astronomical Observatory 0.65-m telescope equipped with CCD camera AP8. Images were acquired with Rc filter (30-s and 180-s exposures) and without filter (180-s exposures). The optical transient reported by Fox and Price (GCN 1731) is detected. Preliminary analysis gives Rc ~ 21 mag at 13:24 UT. Further analysis is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1750 SUBJECT: GRB 021211, optical observations DATE: 02/12/13 15:53:08 GMT FROM: Peter Garnavich at U of Notre Dame B. McLeod (CfA), N. Caldwell, T. Grav, K. Luhman (CfA), P. Garnavich (Notre Dame), and K.Z. Stanek (CfA) We observed the afterglow of GRB 021211 (GCN 1731) with the MMT plus MiniCam imager beginning Dec. 12.3 (UT) (20.6 hours after the burst). The afterglow is well detected in B,V,R filters and the R-band magnitude is estimated to be 23.20+/-0.18 based on Landolt standards observed the previous night (although some cirrus was seen on the night the afterglow was observed). The image is consistent with a point source and is quite blue compared to stars in the field. The R-band image shows very faint emission 1" to the northeast of the afterglow which may be the host galaxy (see GCN 1744). The R-band image can be viewed at: http://www.nd.edu/~pgarnavi/grb021211.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1751 SUBJECT: GRB 021211, IR observations DATE: 02/12/13 16:09:16 GMT FROM: Peter Garnavich at U of Notre Dame D. Bersier, J. Bloom, P. Challis, and P. Garnavich (Notre Dame) We observed the position of the afterglow of GRB 021211 (Fox et al. GCN 1731) with the Magellan Baade telescope and ClassiCam IR imager beginning Dec. 12.18 (UT). A point source is well detected at the positon of the afterglow and we estimate a brightness of J=21.76+\-0.11 based on a number of Persson IR standards obtained during the night. A second set of J-band images centered at Dec. 12.33 (UT) provides a magnitude of J=21.73+\-0.12 and combined with the observations of McLeod et al. (GCN 1750) gives a color of R-J=1.5, implying an absence of a strong Lyman break between the R and J bands. Thus, the Lyman break is likely shortward of 600nm, placing a limit on the redshift of about z<4 for GRB 021211. This message my be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1752 SUBJECT: GRB021211: Optical observations in CrAO DATE: 02/12/13 16:25:23 GMT FROM: Vasilij Rumjantsev at CrAO V.Rumyantsev (CrAO) and A.Pozanenko (IKI) report: We have observed the afterglow field (GCN 1731) of GRB021211 (HETE 2493; GCN 1734) with 0.64-m Richter-Slefogt telescope of Crimean Astrophysical Observatory. Several unfiltered images with exposure 30-180 sec were taken on Dec. 11 20:39 - 22:46(UT). We do not find OT at the position reported by D.Fox, et al (GCN 1731). The limiting magnitude (3 sigma) for two images are 20:39 (UT) - 18 22:39 (UT) - 19.5 Further analysis of combined image is underway. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1753 SUBJECT: GRB021211, BVRI field photometry DATE: 02/12/13 19:35:30 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO) reports on behalf of the USNO GRB team: We have acquired BVRcIc all-sky photometry for a 20x20 arcmin field centered at the coordinates for the optical transient (Fox and Price, GCN 1731) associated with the HETE burst GRB021211 (Crew et al., GCN 1734) with the USNOFS 1.0-m telescope on one photometric night. Stars brighter than V=13.5 are saturated and should be used with care. We have placed the photometric data on our anonymous ftp site: ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb021211.dat The astrometry in this file is based on linear plate solutions with respect to UCAC2. The external errors are less than 100mas. This calibration will be extended with additional nights to ensure against a systematic zeropoint error, but current weather forecasts indicate that this may be a week or two. We will not be performing U-band calibration unless requested. As always, you should check the dates on the .dat file prior to final publication to get the latest photometry. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1754 SUBJECT: GRB 021211: early break in light curve DATE: 02/12/13 20:34:27 GMT FROM: Ryan Chornock at UC Berkeley R. Chornock, W. Li, A. V. Filippenko, and S. Jha, University of California, Berkeley report: We have further analysed the unfiltered KAIT dataset (GCN 1737) for the afterglow associated with GRB 021211 (GCN 1731). The data show a steeply declining light curve, falling from magnitude 14.8 to mag 19.0 in the first half hour after the burst. It is apparent that the light curve underwent an early break. A fit to our first nine data points, spanning the time interval of 2.2-6.5 minutes after the GRB, shows a decay with a power-law index of -1.60 +/- 0.02. The light curve then shows a break at about 12 minutes after the burst. A fit to later data, taken 20 to 150 minutes after the GRB, gives a slope of -0.96 +/- 0.04, consistent with the decay seen in concurrent observations by Price and Fox (GCN 1733). This break from a steep initial decline to a shallow later decline is reminiscent of the early behavior of GRB 990123 (Akerlof et al. 1999, Nature, 398, 400). The early emission in that object is believed to be due to the reverse shock, while the later emission is ascribed to the normal forward shock (Sari and Piran 1999, ApJ, 517, L109). We hypothesize that our data for GRB 021211 show a similar evolution for this object, but it is substantially fainter (~5 mags) than 990123 at similar epochs. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1755 SUBJECT: IPN triangulation of GRB021211B (two large error boxes) DATE: 02/12/13 21:25:39 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the Ulysses GRB team, E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, and T. Cline, on behalf of the Konus and Ulysses GRB teams, report: Ulysses and Konus-Wind observed this GRB at 69205 seconds. As observed by Ulysses, it had a duration of approximately 15 seconds, a 25-100 keV fluence of approximately 1.8E-6 erg/cm2, and a peak flux of approximately 4.5E-07 erg/cm2 s over 0.50 seconds. We have triangulated it to a preliminary annulus centered at RA, Decl(2000)=2.928, -35.916 degrees, whose radius is 47.271 +/- 0.194 degrees (3 sigma). The Konus ecliptic latitude response constrains the arrival direction to a band between ecliptic latitudes -10 and -40 degrees, that is, to those portions of the annulus between RA, Decl= 32, +2 and 55, -21 degrees, and between RA, Decl= 306, -29 and 298, -61 degrees. This localization can be improved, but as the event was not observed by Mars Odyssey, a small error box cannot be derived for it. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1756 SUBJECT: VLT spectrum of GRB 021211 DATE: 02/12/14 00:55:14 GMT FROM: Paul Vreeswijk at ESO Paul Vreeswijk (ESO), Ingunn Burud, Andrew Fruchter (STScI) & Andrew Levan (U. of Leicester/STScI) report for the GRACE collaboration: At Dec. 13.34, 2002 UT, the afterglow (Price & Fox, GCN 1733) of GRB 021211 (Crew et al., GCN 1734) was observed in spectroscopic mode with FORS2 at unit 4 of the VLT at Paranal, Chile. The total exposure time was 30 min., and the spectra approximately cover the wavelength range 4000-9500 A. The combined spectrum (preliminary reduction) shows at least three emission lines, presumably originating in the host galaxy of GRB 021211. We have identified these lines as [OII] 3727, and [OIII] 4959, 5007 at a redshift of z=0.800 +- 0.001. The equivalent width of the [OII] 3727 emission is 37 +- 7 A rest-frame, which is fairly typical for the hosts of GRBs. We appreciate the kind assistance of the VLT staff at Paranal. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1757 SUBJECT: GRB021211: Measurement of Early Time Afterglow DATE: 02/12/14 03:51:40 GMT FROM: Tom Vestrand at LANL P. Wozniak, W.T. Vestrand, D. Starr, J. Wren, K. Borozdin, S. Brumby, D. Casperson, M. Galassi, K. McGowan and R. White report: One of our RAPTOR (RAPid Telescopes for Optical Response) telescopes at the Los Alamos National Laboratory responded to HETE trigger 2493 in real-time. Our imaging of the burst location began at 11:19:38.9 UT, 64.9 seconds after the GRB time. The first image, a 60-second exposure, shows an optical transient (OT) at the position identified by Fox and Price (GCN 1731). The OT signal was slightly blended with a nearby star. To correct for the blending we used difference image photometry with reference images obtained after the OT faded below our detection limit. Correlating our unfiltered magnitude with the USNO photometry reported by Henden (GCN 1753) we derive a Rc magnitude of 14.06+/-0.08. Assuming an afterglow flux decay with power-law index alpha=-1.6, the flux-weighted image time is 89.7 seconds after the GRB time. Our measurements are consistent with the suggestion by Chornock et al. (GCN 1754) that the early afterglow was fading more rapidly than the late afterglow. An animation that compares the detection image with an image taken after the object faded below our detection limit will be posted on the RAPTOR website at: www.raptor.lanl.gov This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1758 SUBJECT: GRB 021211: CTIO observations DATE: 02/12/15 13:26:17 GMT FROM: Andrew Levan at U.of Leicester Andrew Levan (U. Leicester/STScI), Andrew Fruchter (STScI), Doug Welch (McMaster), Chris Palma (Penn State), Bryan Henderson (U. Washington), Michael Siegel and Ingunn Burud (STScI) report for a larger collaboration: The optical afterglow of GRB 021211 was imaged with the CTIO 4m telescope and Mosaic imager on the 12th Dec beginning 06:15UT and 13th Dec at 06:11UT. On 12th Dec, 1440s were obtained in both R and I. On 13th Dec 2880s were obtained in R only. Each observation consisted of several shorter, dithered observations. The afterglow is clearly visible in both epochs. Using a 1" aperture we measure magnitudes in the first epoch of R=22.8, I=22.5 and in the second epoch of R=23.1, where photometry has been calibrated using the calibration of Henden (GCN 1753). The host galaxy is a clearly visible extension to the north-east of the OT. Subtraction of a point source from the position of the optical transient on its host indicates that the brightest point source present was fainter than R=23.2 at the time of the first observations (t=19 hours), and R=23.6 at t=43 hours. Implying that the host galaxy is brighter than R=24. An image of the field, showing the OT and host galaxy on the night of Dec 12th can be found at http://www.stsci.edu/~fruchter/GRB/021211/ctio/host.jpg //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1759 SUBJECT: GRB 021211, optical observations DATE: 02/12/16 01:01:57 GMT FROM: Peter Garnavich at U of Notre Dame N. Caldwell (SAO), B. McLeod (CfA), P. Garnavich (Notre Dame) and K.Z. Stanek (CfA) We have continued to observe the afterglow of GRB 021211 with the MMT plus MiniCam imager (GCN 1750). R-band images obtained Dec. 13.4 and Dec. 14.4 (UT) in 0.8" seeing clearly show the afterglow and a rapid fading. From PSF fitting photometry, we estimate the power-law decay index between Dec. 12 and Dec. 14 is 1.03+/-0.14. This is consistent with the decay rate measured by Chornock et al. (GCN 1754) beginning 12 minutes after the burst. Combining the three epochs allows a clear detection of the possible host galaxy noted on GCN 1750 (also GCN 1758). A galaxy centered 1.5" north and east of the afterglow is cleanly separated from the optical transient . It has an approximate brightness of R=24.8. This is likely the source of emission lines found by Vreeswijk et al. (GCN 1756) at a redshift of z=0.80. Another galaxy of similar brightness is detected 2.7" north of the burst. The average of all R-band images can be viewed at: http://www.nd.edu/~pgarnavi/grb021211_host.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1765 SUBJECT: GRB021211: APO optical observations DATE: 02/12/17 23:23:11 GMT FROM: Don Lamb at U.Chicago D. Q. Lamb, M. C. Nysewander, D. E. Reichart, J. C. Barentine, C. Laws, D. G. York, and R. J. McMillan report, We have calibrated our i* image of the optical transient and host galaxy of GRB021211 (Crewe et al., GCN 1734), taken with the ARC 3.5-meter telescope at APO beginning at 09:19 UT on December 12 (Lamb et al., GCN 1744). Using the photometric calibration reported by A. Henden (GCN 1753) and a 1" aperture, we measure i* = 23.0 +/- 0.20 mag for the optical afterglow. This value may be subject to some systematic error because of the presence of the host galaxy, which is visible as an extension to the northeast of the afterglow (Lamb et al., GCN 1744; McLeod et al., GCN 1750; Levan et al. GCN 1758; Caldwell et al., GCN 1759). Conservative upper limits on the brightness of the host galaxy are i* > 24.1 mag (1 sigma), > 23.4 mag (2 sigma), and > 23.0 mag (3 sigma). Second epoch observations of the GRB021211 field are planned that will enable us to refine these values. An i* image of the GRB021211 field, showing the optical afterglow and the host galaxy on the night of Dec 12th can be found at http://astro.uchicago.edu/home/web/lamb/grb021211/apo/ot_and_host.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1767 SUBJECT: VLT spectra of GRB 021211 revisited DATE: 02/12/19 15:20:55 GMT FROM: Paul Vreeswijk at ESO Paul Vreeswijk (ESO), Ingunn Burud, Andrew Fruchter (STScI) & Andrew Levan (U. of Leicester/STScI) report for the GRACE collaboration: We have determined that the slit position used in the VLT service observations of GRB 021211, reported in GCN 1756, was 1 to 1.5 arcseconds East of the expected position due to the saturation of the offset star in the acquisition images. The position angle of the slit was zero degrees, i.e. aligned along the North-South direction, the seeing during the observations was 0.65", and the slit width was 1". Consequently, the object 1.5" to the North-East of the afterglow (see GCNs 1759, 1750, 1758, 1765), is by accident mostly contained within the slit, while the emission from the position of the afterglow is not or only partly. Therefore, the reported redshift most likely belongs to the galaxy 1.5" away from the transient, as suggested by Caldwell and colleagues (GCN 1759). Future observations are needed to prove or disprove that this galaxy is in fact the GRB host. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1777 SUBJECT: GRB021211, radio observations DATE: 02/12/24 17:12:17 GMT FROM: Evert Rol at U.Amsterdam E. Rol (University of Amsterdam) and R. Strom (ASTRON, UoA) report on behalf of a larger collaboration: "We observed the position of the GRB 021211 afterglow at 4.9 GHz with the Westerbork Synthesis Radio Telescope, centered at December 12.0 and December 17.0. We do not detect a radio source at the position of the optical afterglow, with 3 sigma upper limits of 0.17 and 0.12 mJy, respectively." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1781 SUBJECT: GRB 021211: Probable Host and Underlying Supernova DATE: 02/12/30 00:11:03 GMT FROM: Andrew Levan at U.of Leicester Andrew Fruchter (STScI), Andrew Levan (U. Leicester/STScI), Paul Vreeswijk (ESO), Stephen T. Holland (Notre Dame) and Chryssa Kouveliotou (MSFC) report for the GOSH collaboration: We have observed the field of GRB 021211 with the Advanced Camera for Surveys (ACS) on HST in the F435W (B), F606W (wide V) and F814W (I) filters and the NICMOS camera using the F160W (H) filter on 18 December, and again using the F606W and F814W filters on 25 and 24 December, respectively. We find that the source at the location of the optical afterglow (GCN 1731) is resolved in the ACS images with a FWHM of approximately 0."14, or approximately twice that of the native ACS resolution, suggesting that the light is primarily from the GRB's host. This is further supported by the colors of the object. In the 18 December data we find that in AB magnitudes, F435W - F606W ~ F814W - F160W ~ 0.1 mag; however, F606W - F814W = 0.95 +/- 0.1 and F606W = 25.26 +/- 0.2 (where we have used conservative errors due to uncertainties in the calibration). These colors are roughly consistent with the observation of the 4000A break in a blue galaxy at approximately z=0.8, the host may therefore be interacting with the galaxy to the North East at z=0.800 +- 0.001 (GCN 1756). However the color is also consistent with the 1216A break at around z=5. When we examine the flux within a few pixels of the peak brightness of the object (which corresponds well with the location of the afterglow in early CTIO images, GCN 1758) the flux in the F606W band falls between the two epochs by 0.07 +/- 0.03 mags, but rises in F814W by about 0.3 +/- 0.07 mags. This may suggest we are seeing the first signs of an underlying supernova, which like the galaxy, would be expected to show a break between the F606W and F814W bands if it were at approximately z=0.8. However, given its present magnitude, at maximum any underlying supernova will likely be significantly less bright than SN1998bw, and be only a fraction of the host light. Using the x-ray fluence of GCN 1734 and assuming a "standard" candle gamma-ray energy of 5e50 erg for GRB021211, we derive a beaming angle of 101 degrees at z=0.8 or, alternatively of 17 degrees at z=5. If GRB 021211 does originate from z=0.8 (which would be the case if the observed rebrightening is due to a supernova), it is likely an underluminous event in gamma-rays, similar to GRB980425. Images of the field can be found at http://www.stsci.edu/~fruchter/GRB/021211 Further HST observations are planned. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1785 SUBJECT: VLT spectroscopy of the probable host of GRB 021211 DATE: 03/01/03 21:07:37 GMT FROM: Paul Vreeswijk at ESO Paul Vreeswijk (ESO), Andrew Fruchter (STScI), Jens Hjorth (University of Copenhagen) and Chryssa Kouveliotou (MSFC) report for the GRACE collaboration: On the night of 29/30 December 2002, the field of GRB 021211 was re-observed in spectroscopic mode with FORS2 at unit-4 of ESO's VLT at Paranal, Chile. The total exposure time was 30 min in the 300V grism, covering approximately 4000-9300A with a resolution of about 12A. The slit, with a width of 1", was positioned to cover the position of the probable host galaxy, as well as the galaxy 1.5" to the North-East (see Fruchter et al., GCN 1781). The seeing during the observations was ~0.7". Preliminary reduction of these spectra confirm that the redshift of the nearby galaxy is z=0.800+-0.001 (see Vreeswijk et al., GCN 1767). Due to a reference star also being in the slit, there is no ambiguity in the identification of this galaxy as the source of these emission lines (again [OII] and [OIII]). At the position of the probable host, we find one clear emission line at 7476A with an observed equivalent width of 66 +- 8 A (Poisson error only). The continuum level just redward of the line is similar to that on the blue side, suggesting that the line is not Lyman alpha. The most likely identification is [OII] 3727A at a redshift of z=1.006. At this redshift, other prominent emission lines such as Hbeta and [OIII] 5007A fall outside our spectral coverage. If the line were Halpha, we would have expected to see [OII] and [OIII] in the blue part of the spectra, which we do not detect. An alternative identification of the emission line is [OIII] 5007A, which would put the host at z=0.493. However, in this case we would have expected to also detect [OII] (although it would be very close to a bright sky line), assuming that its flux would be more than about half the flux of [OIII] 5007A. The [OII] at z=1.006 identification is strengthened by flux calibration of the spectra, which shows a drop of about 1 magnitude between the 8000-9000A continuum and that blueward of the emission line. This is consistent with the red HST V-I colour reported by Fruchter et al., and with the possibility that this colour is caused by the 4000A break. We are grateful for the assistence of the staff at Paranal, in particular Thomas Szeifert and Elena Mason. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1809 SUBJECT: GRB 021211: VLT spectrum DATE: 03/01/15 10:39:40 GMT FROM: Daniele Malesani at Brera Astro. Obs. M. Della Valle (INAF-OAA), S. Benetti (INAF-OAPd), D. Malesani (SISSA), E. Mason (ESO), L.A. Antonelli (INAF-OAR), G. Cocozza, (INAF-OAR), S. Covino (INAF-OABr), D. Fugazza (INAF-TNG), G. Ghisellini (INAF-OABr), G.L. Israel (INAF-OAR), L. Stella (INAF-OAR), and V. Testa (INAF-OAR), on behalf of a larger Italian collaboration, report: A low resolution spectrum of the probable host galaxy of GRB 021211 (Fox & Price, GCN 1731; Crew et al., GCN 1734) was obtained under modest sky (cirrus) and seeing (between 0.6" and 1.4") conditions, starting on 2003 Jan 8.27, with UT4 (Yepun) + FORS2 at the ESO-VLT. The spectrum covers the range of wavelengths 6000A-11000A with a resolution of about 17A (grism 150I). The total exposure time was 4h. We obtained the spectrum for both the complex afterglow+host and the nearby galaxy 1.5" NE (e.g. Caldwell et al., GCN 1759), that we confirm to be at z=0.80 (Vreeswijk et al., GCN 1756 & 1767). We clearly detect the emission line at 7472.9A already found by Vreeswijk et al. (GCN 1785). In addition we have identified three additional emissions at 9722.0A, 9954.9A and 10022.8A. We interpret the four lines as due to [OII] 3727A, Hbeta and [OIII] at 4959A and 5007A in the rest frame of the host galaxy, observed at a redshift of z=1.004+-0.002. We thank the kind assistance of the staff at Paranal, in particular Riccardo Scarpa and Andreas Kaufer. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1821 SUBJECT: GRB 021211: R-band observations at late-time DATE: 03/01/16 14:23:05 GMT FROM: Daniele Malesani at SISSA-ISAS,Trieste,Italy V. Testa (INAF-OAR), D. Fugazza (INAF-TNG), M. Della Valle (INAF-OAA), D. Malesani (SISSA), E. Mason (ESO), E. Pian (INAF-OATs), L.A. Antonelli (INAF-OAR), S. Benetti (INAF-OAPd), G. Cocozza (INAF-OAR), S. Covino (INAF-OABr), G. Ghisellini (INAF-OABr), G.L. Israel (INAF-OAR), N. Masetti (IASF-CNR), E. Palazzi (IASF-CNR), L. Stella (INAF-OAR), on behalf of a larger Italian collaboration, report: We have imaged the optical afterglow of the GRB 021211 (Fox & Price, GCN 1531; Crew et al., GCN 1734) on different epochs, using the Italian 3.6m TNG telescope, equipped with OIG, and the 8.2m ESO-VLT-UT4 (Yepun) equipped with FORS2, in the R-band filter. In the VLT images we clearly detect a point-like source at the position of the afterglow. Our results are reported in the following table: UT exposure Telescope seeing R magnitude -------------------------------------------------------- 2002 Dec 27.09 70 min 3.6m TNG 1.0" > 25.0 2003 Jan 9.30 33 min 8.2m VLT 0.6" 24.1 +- 0.2 2003 Jan 10.23 30 min 8.2m VLT 1.2" 24.5 +- 0.2 2003 Jan 14.33 15 min 8.2m VLT 0.8" 24.6 +- 0.1 The first value is a 3-sigma upper limit and it assumes a point-like source. Errors for the other observations are 1-sigma. Some cirrus were present during the Jan 9 exposure. Our dataset confirms the flattening in the light curve found by HST (Fruchter et al., GCN 1781). The VLT measurements do not indicate significant variability, and are also consistent with the HST ACS F606W measurement. We thank the ESO Director and the ESO staff at Garching for promptly considering our DDT proposal. We also thank the personnel at TNG (in particular Massimo Cecconi, Juan Carlos Guerra and Marco Pedani) and at Paranal (in particular Andreas Kaufer and Nancy Ageorges). This messagge is citeable.