//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1281 SUBJECT: BeppoSAX ALERT: GRB020321, the "Springtime Burst" DATE: 02/03/21 10:54:37 GMT FROM: Giangiacomo Gandolfi at IAS/CNR Frascati BeppoSAX ALERT: GRB020321, the "Springtime Burst" On Mar. 21, 04:20:40 UT a faint GRB (GRB020321) has been detected in BeppoSAX WFC1 Refined coordinates are: R.A.(2000)= 243.27 DEC.(2000)= -83.71 The error radius is 5', due to the non-optimal attitude configuration of the satellite. Giangiacomo Gandolfi on behalf of BeppoSAX Mission Scientist //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1284 SUBJECT: GRB020321: a faint BeppoSAX detection DATE: 02/03/21 16:39:35 GMT FROM: Cristiano Guidorzi at Phys.Dept, U.of Ferrara(Italy) C. Guidorzi, E. Montanari and F. Frontera, Universita' di Ferrara, L. Amati, Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR, Bologna, Marco Corsi and G. D'Andreta, BeppoSAX Science Operation Center (SOC), Rome, Erik Kuulkers, Jean in 't Zand, Space Research Organization Netherlands (SRON) and Astronomical Institute, Utrecht University, Paul Lowes, SRON and SOC, L. Piro and G. Gandolfi, Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR, Rome. "The BeppoSAX Gamma Ray Burst Monitor (GRBM) and the Wide Field Camera (WFC) unit 1 detected GRB020321 on March 21.18102 UT. The GRB was faint and has been discovered only by ground trigger logic. The event detected by the GRBM shows an irregular single pulse profile with a time duration of about 70 s and a peak count rate of 130+- 40 c/s, as estimated with 1 s time resolution, in the 40-700 keV energy band. In the WFC, the duration is about 1.5 min and the peak flux is about 0.3 Crab (2-26 keV). The centroid position of the X-ray counterpart from the WFC image is R.A. = 16h13m05s, Dec = -83d42'35" (equinox 2000.0) with an error radius of 5' (99% CL). A follow-up observation with BeppoSAX narrow-field instruments is in progress." This message is citable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1285 SUBJECT: GRB020321: BeppoSAX/NFI Observations DATE: 02/03/21 18:02:10 GMT FROM: Giangiacomo Gandolfi at IAS/CNR Frascati GRB020321: BeppoSAX/NFI Observations A BeppoSAX TOO observation of GB020321 has started about 6 hours after the GRB. A preliminary analysis of MECS(1.6-10 keV) image of the first orbits shows a possible unknown source in the WFC error circle. The object, very faint, seems to be fading. The position is: RA = 242.76 Delta = -83.70 The error radius is 2 arcminutes. A more refined off-line analysys is required to confirm and improve the detection. G. Gandolfi //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1286 SUBJECT: GRB020321 optical observations DATE: 02/03/21 18:18:12 GMT FROM: Arne A. Henden at USNO/USRA A. Henden and P. Nelson (Ellinbank Observatory, Australia) on behalf of the AAVSO International GRB Network, report: The Ellinbank 320mm f/5 Newtonian with an ST-8E CCD were used on 020321 UT to image the BeppoSAX WFC error circle for GRB020321 (Gandolfi, GCN 1281; Guidorzi et al., GCN 1284). A total of 30 x 30 sec images in Rc were taken from 12:22 to 12:47 UT (8.2hrs after the burst), covering a 20x30 arcmin field that includes the entire BeppoSAX error circle. The ESO R and AAO R plate scans from the USNO PMM pixel database were used to blink the resultant coadded image. The limiting magnitude is estimated to be Rc=19. Two faint objects, near the limiting magnitude, do not appear on the ESO or AAO plates, and are not included in the minor planet database. These two objects are at: 16:11:30.00 -83:39:12.1 J2000 16:12:52.00 -83:40:13.9 with position errors of about 0.5arcsec. These may be artifacts of the processing, but are the only objects inside of the WFC error circle that do not also appear on the photographic plates. In particular, we find nothing new at our limiting magnitude inside the recent NFI error circle (Gandolfi, GCN 1285). The AAVSO would like to thank the Curry Foundation for supporting the AAVSO International GRB Network. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1289 SUBJECT: GRB 020321: Optical observations DATE: 02/03/22 00:54:03 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price (RSAA, ANU), B. Jones (Nottingham), B.A. Peterson (RSAA, ANU) report on behalf of a larger collaboration: We observed the refined error circle of GRB 020321 (GCN #1285) with the SSO 40-inch telescope + WFI at 2002 Mar 21.62 UT in poor seeing conditions. Our 2x600 sec observations in R band cover the entire error circle to a limiting magnitude of R ~ 20.5 mag. We do not detect any objects at the positions quoted by Henden & Nelson (GCN #1186). However, we detect one object at coordinates RA: 16:11:56.74 DEC: -83:39:57.3 J2000 (with approximate error of 0.5 arcsec) with R ~ 20 mag that does not appear to be on the DSS-2 red plate. Further observations are required to determine whether this source is the afterglow of GRB 020321. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1305 SUBJECT: GRB 020321: Optical observations DATE: 02/03/24 03:45:24 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price (RSAA, ANU), A. Dressler and P. McCarthy (OCIW) report on behalf of a larger collaboration: We have observed the error circle of GRB 020321 (GCN #1285) with the Magellan/Baade 6.5-m telescope + LDSS2 at 2002 Mar 22.28 and 23.41 UT. The limiting magnitude of our observations is approximately R ~ 24 mag. We have performed PSF-matched image subtraction to search for variable objects within the field. We do not find any afterglow candidate upon visual inspection of the subtracted image. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1308 SUBJECT: GRB 020321, Radio Observations DATE: 02/03/25 09:14:35 GMT FROM: Edo Berger at Caltech M. H. Wieringa (ATNF), E. Berger (Caltech), P. A. Price (Caltech and RSAA, ANU), S. R. Kulkarni (Caltech) and D. A. Frail (NRAO) report: "We observed the NFI error circle of GRB 020321 (GCN #1285) for 12 hours centered on 2002, Mar 21.90 UT with the Australia Telescope Compact Array (ATCA) at 4.8 and 8.7 GHz. At 8.7 GHz we detect two possible candidates within the NFI error circle above a 5-sigma flux density of 190 microJy: 1. RA=16:11:14.2, DEC=-83:41:13.8 (J2000) 2. RA=16:11:27.8, DEC=-83:40:29.5 (J2000) Further observations at both frequencies are required to establish variability, and identify one of these sources as the radio afterglow of GRB 020321. We have also searched the positions of these radio candidates in the Magellan/Baade 6.5-m telescope + LDSS2 data from 2002, Mar 22.28 and 23.41 UT (GCN 1305). We find no sources at these positions down to the limiting magnitude of R~24 mag." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1314 SUBJECT: GRB 020321: Infrared observations DATE: 02/03/28 16:09:23 GMT FROM: Evert Rol at U.Amsterdam Evert Rol (Univ. of Amsterdam), Patrick Woudt (Univ. of Cape Town), Isabel Salamanca, Lex Kaper (Univ. of Amsterdam), report on behalf of a larger collaboration: "We have observed the NFI errorbox of GRB 020321 (GCN 1281, 1842, 1285) with the 1.4m Infrared Survey Facility telescope simultaneously in J, H and K' band, at three epochs during the night of 21-22 March 2002. The log of the observations is as follows: date exptime band (days UT 2002) (seconds) March 21.79 400 J, H, K' March 21.95 400 J, H, K' March 22.13 800 J, H, K' We do not find any sources varying more than 3 sigma between the different epochs, down to 3 sigma limiting magnitudes of 19.4 (J), 19.6 (H) and 18.9 (K'). In particular, we do not find any sources in the combined images at the position of the two radio sources detected by ATCA (GCN 1308). " //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1342 SUBJECT: GRB 020321: Candidate X-ray Counterparts DATE: 02/04/08 23:44:03 GMT FROM: Derek Fox at CIT D.W. Fox (Caltech) reports on behalf of the Caltech-NRAO-CARA GRB collaboration: "We have imaged the error circle of GRB020321 (GCN 1284, 1285) with the Chandra X-ray Observatory for 20 ksec beginning at March 31.08 UT, 9.9 days after the burst. The pointing of the spacecraft was chosen to center the 2-arcmin radius BeppoSAX NFI localization (GCN 1285) on the ACIS-S3 detector. Reduction of the data using standard Ciao procedures yields the following source catalog (listed in decreasing order of significance) for this region: ID IAU Name Sig Cts HR ======================================================= 1 CXOU J161122.3-834121 37.4 80.4(90) 0.47(12) 2 CXOU J161105.1-834111 15.1 31.5(57) 0.43(16) 3 CXOU J161104.2-834124 7.9 15.7(40) 0.12(16) 4 CXOU J161048.0-834004 3.0 5.8(25) 0.09(28) 5 CXOU J160953.5-834159 2.9 5.7(25) 0.63(89) 6 CXOU J161205.3-834132 2.5 4.8(22) 0.04(19) 7 CXOU J161058.8-834343 2.0 3.8(20) 0.52(65) ======================================================= where "Sig" is the wavdetect-quoted significance of the source in the 0.3 to 7.0 keV band, "Cts" is the counts in this band over the 20.0 ks exposure, "HR" is the hardness ratio of 2.1-7.0 keV counts to 0.3-2.1 keV counts, and uncertainties in the trailing digits are indicated in parentheses. J2000 coordinates of the sources are implicit in their IAU names. No sources are detected coincident with the reported ATCA radio candidates (GCN 1308). Source 6 (CXOU J161205.3-834132) is coincident with a weak source (not a USNO star) from the Digitized Sky Survey (SES)." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1348 SUBJECT: X-ray afterglow of GRB020321 DATE: 02/04/10 12:09:39 GMT FROM: Jean int Zand at SRON J.J.M. in 't Zand, University of Utrecht and Space Research Organization Netherlands (SRON); L. Kuiper and J. Heise, SRON; L. Piro and G. Gandolfi, Istituto di Astrofisica Spaziale e Fisica Cosmica, Rome, report: "A refined analysis of the BeppoSAX Narrow Field Instruments data on GRB 020321, collected between 8.1 and 10.6 hrs after the burst, has resulted in a significance of only 3.0 for the tentative X-ray afterglow detection reported in GCN 1285. The source is also not confirmed by the XMM-Newton observation that took place between 10.3 and 24.2 hrs after the burst (see http://xmm.vilspa.esa.es/external/xmm_news/items/grb020321). Therefore, we regard this detection as marginal. We would like to point out another source which is outside the error circle of the marginal NFI source but inside the WFC error circle of the burst (GCN 1281) and which draws the attention through a comparison between the XMM-Newton EPIC-pn image and the Chandra ACIS-S3 observation (a 5.5 hr exposure starting 9.9 days after the burst; see Fox et al., GCN Circ. 1342). It concerns source No. 2 in the EPIC-pn image which is located at R.A. = 16h 12m 43.7s, Decl. = -83d 43' 13.9" (equinox 2000.0; error 4"). This source 1) is 0.9' from the WFC centroid; 2) shows a declining, though not smoothly, trend in the EPIC-pn photon count rate (see aforementioned Vilspa web page); 3) is the only EPIC-pn source covered but not detected in the ACIS-S3 image. Therefore, we propose that this is likely the X-ray afterglow and urge optical and radio observers to concentrate on this position for this 'dark' GRB. We thank P. Rodrigues, N. Schartel and M. Santos at the XMM-Newton Science Operations Centre (ESA) in Vilspa for advice on the XMM-Newton data." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1385 SUBJECT: GRB020321 : Optical observations. DATE: 02/05/06 10:43:33 GMT FROM: Isabel Salamanca at U. of Amsterdam Isabel Salamanca, Evert Rol, L. Kaper (Univ. of Amsterdam), A. J. Castro-Tirado (IAA-CSIC Granada), A. Fruchter (STScI, Baltimore), J. Greiner (MPE Garching and AI Potsdam), J. Hjorth, (Univ. of Copenhagen), E. Pian (INAF, OA Trieste), E. van den Heuvel (Univ. of Amsterdam), on behalf of GRACE report: Deep broad-band images of the NFI error box (GCN 1285 & 1348) and WFC error box (GCN 1281 & 1284) of GRB 020321 were obtained with EFOSC at the 3.6m telescope at ESO, La Silla. The log of observations follows below: Date (2000) exposure Filter lim mag (3 sigma) ========================================================== March 21/22 900 sec/each UBVR U=22.4 B=24.1 V=23.6 R=23.8 March 23/24 900 sec/each VR V=23.7 R=23.6 April 18/19 1200 sec R R=23.6 Magnitudes were calibrated by using the standard star WOLF 629 of the Landolt catalogue, observed during the first night, which was photometric. Very close to the position of the X-ray counterpart reported by in 't Zand et al. (GCN 1348) we found two objects which are not present in the DSS, with coordinates: Source RA(J2000) DEC(J000) error A 16h 12m 44.1s, -83d 43' 09.2" 0.5 arcsec B 16h 12m 44.4s, -83d 43' 15.5" 2 arcsec X-ray 16h 12m 43.7s, -83d 43' 13.9" 4 arcsec Their magnitudes at the three epochs are: (March 21.18102 BURST TRIGGER in BeppoSAX) Epoch UT(2002) Filter Source A Source B =========================================================== March 22.2814 R 20.81 +/-0.03 22.84 +/- 0.11 March 22.3179 V 21.43 +/-0.03 22.98 +/- 0.14 March 22.4260 B 22.79 +/-0.08 23.84 +/- 0.21 March 22.4378 U > 23.6 > 23.6 March 24.3958 R 20.78 +/-0.04 23.30 +/- 0.22 March 24.4076 V 21.47 +/-0.05 23.54 +/- 0.30 April 19.2908 R 20.93 +/-0.04 23.68 +/- 0.26 ------- Note: UTs are mid-exposure. Both sources are extended. Source "A" does not appear in the DSS 2 (red), although it has a magnitude similar to other stars that are barely visible in the DSS image. However, it does not show any clear fading behaviour as would be expected from a GRB optical afterglow. Source "B" consists of two 'blobs', one of which disappears at epochs 2 and 3. The decrease in magnitude is too shallow for the usual power-law behaviour of an afterglow: the index alpha would be ~0.2, while for gamma-ray afterglows alpha is usually around 1. However, this could be consistent with an OT superposed on its host-galaxy. Images in V and R for the three epochs, as well as a light curve can be found at http://zon.wins.uva.nl/~isabel/GRBs/GRB020321/grb020321.html This message can be cited.