////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Sat 29 Mar 03 11:38:41 UT NOTICE_TYPE: HETE S/C_Alert TRIGGER_NUM: 2652, Seq_Num: 1 GRB_DATE: 12727 TJD; 88 DOY; 03/03/29 GRB_TIME: 41834.67 SOD {11:37:14.67} UT TRIGGER_SOURCE: Trigger on the 6-120 keV band. GAMMA_RATE: 0 [cnts/s] on a 0.000 [sec] timescale SC_LONG: 242 [deg East] SUN_POSTN: 7.69d {+00h 30m 46s} +3.32d {+03d 19' 13"} MOON_POSTN: 334.86d {+22h 19m 27s} -15.92d {-15d 54' 58"} MOON_ILLUM: 10 [%] COMMENTS: No s/c ACS pointing info available yet. COMMENTS: Definitely not a GRB. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Sat 29 Mar 03 11:39:59 UT NOTICE_TYPE: HETE S/C_Last TRIGGER_NUM: 2652, Seq_Num: 2 GRB_DATE: 12727 TJD; 88 DOY; 03/03/29 GRB_TIME: 41834.67 SOD {11:37:14.67} UT TRIGGER_SOURCE: Trigger on the 6-120 keV band. GAMMA_RATE: 0 [cnts/s] on a 0.000 [sec] timescale SC_LONG: 242 [deg East] SUN_POSTN: 7.69d {+00h 30m 46s} +3.32d {+03d 19' 13"} MOON_POSTN: 334.86d {+22h 19m 27s} -15.92d {-15d 54' 58"} MOON_ILLUM: 10 [%] COMMENTS: No s/c ACS pointing info available yet. COMMENTS: Definitely not a GRB. COMMENTS: There is no position known for this trigger at this time. COMMENTS: Burst_Invalidity flag is true. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Sat 29 Mar 03 12:50:24 UT NOTICE_TYPE: HETE Ground Analysis TRIGGER_NUM: 2652, Seq_Num: 3 GRB_DATE: 12727 TJD; 88 DOY; 03/03/29 GRB_TIME: 41834.67 SOD {11:37:14.67} UT TRIGGER_SOURCE: Trigger on the 6-120 keV band. GAMMA_RATE: 0 [cnts/s] on a 0.000 [sec] timescale SC_-Z_RA: 0 [deg] SC_-Z_DEC: 0 [deg] SC_LONG: 242 [deg East] SXC_CNTR_RA: 161.203d {+10h 44m 49s} (J2000), 161.247d {+10h 44m 59s} (current), 160.526d {+10h 42m 06s} (1950) SXC_CNTR_DEC: +21.479d {+21d 28' 44"} (J2000), +21.462d {+21d 27' 43"} (current), +21.742d {+21d 44' 31"} (1950) SXC_MAX_SIZE: 4.00 [arcmin] diameter SXC_LOC_SN: 20 sig/noise (pt src in image) SUN_POSTN: 7.69d {+00h 30m 46s} +3.32d {+03d 19' 13"} SUN_DIST: 144.16 [deg] MOON_POSTN: 334.86d {+22h 19m 27s} -15.92d {-15d 54' 58"} MOON_DIST: 171.80 [deg] MOON_ILLUM: 10 [%] GAL_COORDS: 217.07,60.68 [deg] galactic lon,lat of the burst ECL_COORDS: 154.47,12.51 [deg] ecliptic lon,lat of the burst COMMENTS: Definite GRB. COMMENTS: SXC error box is circular; not rectangular. COMMENTS: Burst_Validity flag is true. COMMENTS: SXC data refined since S/C_Last Notice. ////////////////////////////////////////////////////////////////////// TITLE: GCN/HETE BURST POSITION NOTICE NOTICE_DATE: Sat 29 Mar 03 12:50:24 UT NOTICE_TYPE: HETE Ground Analysis TRIGGER_NUM: 2652, Seq_Num: 3 GRB_DATE: 12727 TJD; 88 DOY; 03/03/29 GRB_TIME: 41834.67 SOD {11:37:14.67} UT TRIGGER_SOURCE: Trigger on the 6-120 keV band. GAMMA_RATE: 0 [cnts/s] on a 0.000 [sec] timescale SC_-Z_RA: 0 [deg] SC_-Z_DEC: 0 [deg] SC_LONG: 242 [deg East] SXC_CNTR_RA: 161.203d {+10h 44m 49s} (J2000), 161.247d {+10h 44m 59s} (current), 160.526d {+10h 42m 06s} (1950) SXC_CNTR_DEC: +21.479d {+21d 28' 44"} (J2000), +21.462d {+21d 27' 43"} (current), +21.742d {+21d 44' 31"} (1950) SXC_MAX_SIZE: 4.00 [arcmin] diameter SXC_LOC_SN: 20 sig/noise (pt src in image) SUN_POSTN: 7.69d {+00h 30m 46s} +3.32d {+03d 19' 13"} SUN_DIST: 144.16 [deg] MOON_POSTN: 334.86d {+22h 19m 27s} -15.92d {-15d 54' 58"} MOON_DIST: 171.80 [deg] MOON_ILLUM: 10 [%] GAL_COORDS: 217.07,60.68 [deg] galactic lon,lat of the burst ECL_COORDS: 154.47,12.51 [deg] ecliptic lon,lat of the burst COMMENTS: Definite GRB. COMMENTS: SXC error box is circular; not rectangular. COMMENTS: Burst_Validity flag is true. COMMENTS: SXC data refined since S/C_Last Notice. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1985 SUBJECT: GRB 030329: Optical afterglow candidate DATE: 03/03/29 13:27:28 GMT FROM: Paul Price at RSAA, ANU B.A. Peterson and P.A. Price (RSAA, ANU) reports: We have observed the error-circle of GRB 030329 with the SSO 40-inch telescope in R-band. We identify a source that is not present on archival images at approximate coordinates: RA: 10:44:49.5 Dec: +21:31:23 (J2000) This position is preliminary, with an estimated error of 5 arcsec. Further observations are planned. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1986 SUBJECT: GRB 030329: OT candidate DATE: 03/03/29 13:43:32 GMT FROM: Ken ichi Torii at RIKEN K. Torii (RIKEN) report: The entire error region of GRB 030329 (HETE trigger 2652) was observed by the automated system at RIKEN (0.25-m f/6.8 reflector equipped with unfiltered CCD AP6E). The observatin started at 2003 Mar. 29 12:52:09 UT and 60-s intergration is repeated. We find a new bright source at position (R.A., Dec.) = (10 44 50.0, +21 31 18) (J2000) (preliminary values with a formal error of 6 arcseconds in each coordinate). The object is about 13 mag (USNO-A2.0 red magnitude). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1987 SUBJECT: GRB 030329: Optical afterglow candidate DATE: 03/03/29 13:59:38 GMT FROM: Paul Price at RSAA, ANU P.A. Price and B.A. Peterson (RSAA, ANU) report: A refined position for the optical afterglow candidate of GRB 030329 is: RA: 10:44:50.0 Dec: 21:31:17.8 (J2000) with an estimated error of 0.5 arcsec in each axis. We estimate the afterglow candidate to be R ~ 12.4 mag (!!!). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1988 SUBJECT: GRB 030329 follow-up DATE: 03/03/29 14:15:40 GMT FROM: Paul Price at RSAA, ANU P.A. Price (RSAA, ANU) reports: Identification of the afterglow of GRB 030329 was performed through clouds, with thunderstorms surrounding the mountain. Consequently, it will not be possible to obtain a spectrum of this bright afterglow from Australia. Perth observatory is also experiencing thunderstorms. We encourage observations by Northern observatories to track the afterglow lightcurve. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1989 SUBJECT: GRB 030329: Optical afterglow fading DATE: 03/03/29 14:31:43 GMT FROM: Makoto Uemura at U. of Kyoto, Astro. M. Uemura (Kyoto University) reports: We have started observations of the field of GRB 030329 at 12:53:41 UT, and confirmed the bright afterglow candidate reported in GCN 1985 and 1986. We use 30-cm and 25-cm SC telescopes and unfiltered CCDs at Kyoto, Japan. In this one hour observation, our perliminary analysis revealed a rapid fading of the object. From 12:53:41 UT to 13:51:01, the object faded about 0.53 mag, which establishes that the bright candidate is a genuine optical afterglow of GRB 030329. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1994 SUBJECT: GRB 030329: precise position from Kyoto images DATE: 03/03/29 17:19:44 GMT FROM: Hitoshi Yamaoka at Kyushu U., VSNET-GRB collab. M. Uemura (Kyoto U.), H. Yamaoka (Kyushu U.), R. Ishioka, and T. Kato (Kyoto U.) report on behalf of VSNET-GRB collaboration: The precise position for the optical afterglow candidate of GRB 030329 (GCN 1985, 1986, 1987, 1689) was derived from Kyoto images (GCN 1689) as (with mean error of measurements of nine images): R.A.= 10h44m50s.030 +/- 0s.005, Decl. = +21d31'18".15 +/- 0".07. On the DSS 2 B, R, and I images, there is no distinct source down to the limiting magnitudes, which indicates the parent galaxy is more than 8-9 mag dimmer of the OT at 76 minutes after explosion. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1995 SUBJECT: GRB 030329: Optical Afterglow Observations DATE: 03/03/29 17:35:46 GMT FROM: Eli Rykoff at Univ. of Michigan/ROTSE Rykoff, E. S. and Smith, D. A. on behalf of the ROTSE collaboration report: We have observed the full error box of GRB 030329 (HETE trigger 2652), using the ROTSE-3A 0.45 meter telescope at Siding Springs Observatory, Australia, starting March 29, 13:05:19 UT (1.46 hours after the burst). Due to partly cloudy skies, our first usable image was taken at 13:08:45 UT. We initiated a sequence of 90 one-minute exposures, interrupted by a brief spell of light rain. We identify the bright counterpart reported by Price (1985) and Torii (GCN 1986), at the following coordinates: RA: 10 44 50.0 Dec: 21:31:17.8 Some of our detections (unfiltered, calibrated to USNO A2.0 R-band) are: UT (start) Mag (USNO R-band) 13:08:48 12.88 +/- 0.01 13:19:15 12.96 +/- 0.02 13:35:25 13.11 +/- 0.01 15:34:38 13.90 +/- 0.02 15:45:16 14.05 +/- 0.03 We continued to follow the transient until it dropped below our elevation cut. A preliminary ROTSE lightcurve can be found at: http://www.rotse.net/transients/grb030329/grb030329_lc0.ps Please note that our magnitude errors fluctuated as clouds drifted through the field of view. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1996 SUBJECT: RXTE detection of GRB 030329 afterglow DATE: 03/03/29 19:37:01 GMT FROM: Frank Marshall at GSFC Marshall, F.E. and Swank, J.H. (NASA/GSFC) report: RXTE detected the X-ray afterglow of GRB 030329 (HETE trigger 2652) during a 27 minute observation that began about 4h51m after the burst at 16:28 UT on March 29 . The flux was about 1.4e-10 ergs/s/cm**2 in the 2-10 keV band or about 0.007 times as bright as the Crab Nebula. This is one of the brightest afterglows ever detected with RXTE. The spectrum is well fit by a power law model with a photon index of 2.0 and an upper limit on absorption of 1e22 Nh/cm**2. The X-ray flux was about 20% lower during a second observation starting at 17:32 UT. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1997 SUBJECT: GRB030329 (=H2652): A Long, Extremely Bright GRB Localized by the HETE WXM and SXC DATE: 03/03/29 19:53:03 GMT FROM: Don Lamb at U.Chicago R. Vanderspek, G. Crew, J. Doty, J. Villasenor, 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; T. Donaghy, M. Suzuki, Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, Y. Nakagawa, D. Takahashi, 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 11:37:14.67 UTC (41834.67 s UT) on 29 Mar 2003, the HETE FREGATE, WXM, and SXC instruments detected event H2652, a long, extremely bright GRB. The burst triggered FREGATE in the 6-120 keV energy band. The burst occurred outside of the effective FOV of the WXM Y-camera. Ground analysis of the SXC data produced a localization that was reported in a GCN Notice at 12:50:24 UT, 73 minutes after the burst. The SXC ground localization SNR was 20. Further ground analysis of the SXC data has provided an SXC localization that can be expressed as a 90% confidence circle that is 2 arcminutes in radius and is centered at SXC-Ground: RA = +10h 44m 50s, Dec = +21d 30' 54" (J2000). The SXC localization is dominated by systematic errors, which are larger than usual because the burst occurred at the edge of the SXC FOV. (The error circle radius of 2 arcminutes reported in the GCN Notice for H2652 did not include the larger systematic errors.) Ground analysis of the WXM data produced a WXM localization. The WXM ground localization SNR is > 20. The WXM localization can be expressed as a 90% confidence rectangle that is 12 arcminutes in width and 2.25 degrees in length. The center of the rectangle lies at WXM-Ground: RA = +10h 44m 24.7, Dec = +23d 20' 20" (J2000), and its corners lie at RA = +10h 44m 39.6s, Dec = +23d 29' 20", RA = +10h 43m 53.5s, Dec = +23d 26' 35", RA = +10h 44m 09.8s, Dec = +21d 11' 38", RA = +10h 44m 55.9s, Dec = +21d 14' 17" (J2000). The width of the WXM localization is dominated by systematic errors, which are larger than usual because the burst occurred at the edge of the WXM FOV. The WXM localization is a long, narrow strip because the burst occurred at the edge of the WXM FOV in a region of the sky that would have been viewed by the YB-camera, which is not operational. The burst duration in the 30-400 keV band was > 25 s. The fluence of the burst was ~1 x 10-4 ergs cm-2 and the peak flux over 1.2 s was > 7 x 10-6 ergs cm-2 s-1 (i.e., > 100 x Crab flux) in the same energy band. A light curve and skymap for GRB030329 is provided at the following URL: http://space.mit.edu/HETE/Bursts/GRB030329 [GCNOPS NOTE (29mar03): The "...on 28 Mar 2003,..." in the first line was corrected to "...on 29 Mar 2003,...".] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1998 SUBJECT: GRB030329: Upper limits from recent and historical observations. DATE: 03/03/29 20:28:22 GMT FROM: Michael Wood-Vasey at UC Berkeley/LBNL/SNfactory GRB030329: Upper limits from recent and historical observations. W. M. Wood-Vasey, P. Nugent, and B. C. Lee, 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), report recent and historical upper limits for the optical transient for GRB 20030329 (GCN #1985, 1986, 1987) using the position of Uemura et. al (GCN #1949) from images taken with the Palomar Oschin 1.2-m and Haleakala MSSS 1.2-m telescopes during the previous two years: Limiting Unfiltered Mag UT Date ( @ S/N = 3) Telescope -------------------------------------------------------------------- 2001 Mar 13.60, 13.61 [ 17.58 Haleakala 2002 Jan 8.46, 8.47, 8.49 [ 20.31 Haleakala 2002 Jan 14.44, 14.45, 14.46 [ 20.26 Haleakala 2002 Jan 21.46, 21.47, 21.48 [ 21.66 Palomar 2002 Feb 3.54, 3.55, 3.57 [ 20.86 Palomar 2002 Feb 13.56, 13.57 [ 18.96 Palomar 2002 Apr 1.27, 1.29, 1.31 [ 21.57 Palomar 2003 Jan 18.50, 18.52, 18.54 [ 20.84 Palomar 2003 Feb 23.50, 23.51, 23.52 [ 20.54 Haleakala 2003 Mar 1.51, 1.52, 1.53 [ 19.89 Haleakala 2003 Mar 23.13, 23.15, 23.17 [ 21.61 Palomar Magnitudes are calibration against 300 USNO-A V1.0 R-band stars in the 0.25 sq. degree field of the images. A co-addition of these images shows nothing at this location to a combined limiting magnitude of 22.28 (S/N = 3). The co-addition is available at: http://supernova.lbl.gov/~wwoodvas/GRB/#GRB20030329 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1999 SUBJECT: GRB 030329: OT B and R photometry, decline rate DATE: 03/03/29 21:12:43 GMT FROM: Avishay Gal-Yam at Tel Aviv U, Israel A. Gal-Yam, E. O. Ofek, D. Polishook and E.M. Leibowitz (Wise observatory, TAU) report: We are observing the OT of GRB 030329 (Peterson & Price, GCN 1985) using the Wise observatory 1m telescope + SITe CCD camera, starting March 29, 17:15 UT (5.6 hours after the burst). Large number of 300 s B, 120 s V and 120 s R-band frames are being obtained under highly variable conditions, with passing clouds. We detect the OT on numerous B, V and R-band images. A rough calibration using nearby bright USNO A-1 stars gives R~14.3 and B~15 for the OT. We can also estimate the decline rate to be about 0.3 mag/hour in the R-band, from the first two hours of data. Further data acquisition and analysis are underway. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2000 SUBJECT: GRB 030329, R-band observations DATE: 03/03/29 21:28:43 GMT FROM: Sylvio Klose at TLS Tautenburg S. Klose, C. Hoegner, J. Greiner (Thueringer Landessternwarte Tautenburg) report: We observed the field of GRB 030329 (HETE trigger #2652) with the Tautenburg Schmidt telescope equipped with the prime focus CCD camera (2k x 2k). Inspite of terrible weather conditions the afterglow discovered by Peterson & Price (GCN 1985) and Torii (GCN 1986) is detected in R. Based on a comparison with the DSS2 red we can only provide a very rough estimate of the R-band magnitude of the afterglow. The brightness of the source is approximately R=14.8 +/- 0.5 mag. We do not believe that we can improve the accuracy of the photometry substantially. The quality of the images is really very bad. This information should nevertheless help observers to plan further observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2001 SUBJECT: GRB 030329: optical observations DATE: 03/03/29 21:44:47 GMT FROM: Rodion Burenin at IKI, Moscow R. Burenin, D. Denissenko, M. Pavlinsky, R. Sunyaev, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, K. Uluc, I. Khamitov (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: Error box of GRB030329 (HETE Trigger #2652) was observed with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe (TUBITAK National Observatory, Turkey) started at Mar 29.744 UT, appr. 6 hours after the burst. We confirm the presence of the optical transient (OT) reported by Peterson and Price (GCN 1985). In the beginning of our run the afterglow appear to have the following magnitudes: B=14.99, V=14.46, R=14.12, I=13.60, and is fading at a rate appr. 0.18 mag per hour in every filter. At 29.794 the OT has magnitudes: B=15.19, V=14.65, R=14.34, I=13.82. We will continue our observations as long as it will be possible. The absolute fluxes will be calibrated more accurately. The light curves will follow. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2002 SUBJECT: GRB030329:optical observations by MASTER DATE: 03/03/29 22:01:01 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs ITLE: GCN GRB OBSERVATION REPORT V. Lipunov, A.Krylov, V.Kornilov, G.Borisov, D.Kuvshinov, A.Belinski, I.Chilingarian, M.Kuznetsov, S.Potanin, V.Vitrischak, G.Antipov Sternberg Astronomical Institute, Alexsandr Krylov Observatory, Moscow We are observing the OT of GRB 030329 in R-band with MASTER system (280 mm, http://observ.pereplet.ru). We began observations at 17:15UT (~5h30m after GRB time). Optical source (about 13.6 in R) was detected at the position given in Circ 1985 in the beginning of observations. At 20:20UT (~8h40m after GRB time) magnitude became more than one magnitude fainter and it was about 14.8 in R. The OT seems to become fainter very slowly. At present we have about 100 images of the OT. These images are being processed. These are preliminary results. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2003 SUBJECT: GRB030329 optical observations DATE: 03/03/29 22:17:09 GMT FROM: Adalberto Piccioni at Astronomy, Bologna U. C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University), G. Gavazzi (Milano-Bicocca University), R. Gualandi (Bologna Astronomical Observatory) and G. Pizzichini (IASF-CNR Bologna) report: UBVRI photometry, for a total of 13 frames, of GRB030329 has been obtained from March 29.8090 to 29.8139 with the 152 cm Loiano telescope. Data analysis is in progress. A finding chart in R light can be retrieved by sftp using hostname : ermione.bo.astro.it username: publicGRB password: GRB_bo //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2004 SUBJECT: GRB 030329, R-band observations, supplement DATE: 03/03/29 22:39:34 GMT FROM: Sylvio Klose at TLS Tautenburg S. Klose, C. Hoegner (Thueringer Landessternwarte Tautenburg), J. Greiner (MPE Garching) report: We forgot to mention that our reported R-band data point refers to an observing run which was performed 19:50 - 20:00 UT. S.K. apologizes for this mistake. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2005 SUBJECT: GRB030329: Optical observations DATE: 03/03/29 23:08:58 GMT FROM: Vasilij Rumjantsev at CrAO V.Rumyantsev, E.Pavlenko, Y.Efimov, K.Antoniuk, O.Antoniuk, N.Primak (CrAO) and A.Pozanenko (IKI) report: We have observed the GRB030329 (HETE #2652) and OT of the GRB found by B.A. Peterson and P.A. Price (GCN 1985) with Cassegrain 38-cm telescope of CrAO. Several 180 sec. exposures of R (Johnson) filter were obtained. The photometry of the OT in respect to the star of USNO á2.0 - 1050-6351075 (the star A in the figure in http://grb.rssi.ru/GRB030329/030329_030329_at64.gif) is following: Star A (USNO á2.0 - 1050-6351075) RA =10 44 54.49 DEC=+21 34 29.8 R=14.00 B=14.90 JD Hel = 52728.2293 delR=0.17 .2318 delR=0.26 .2349 delR=0.23 .2397 delR=0.27 The figure of the OT can be found in http://grb.rssi.ru/GRB030329/030329_030329_at64.gif Preliminary results of photometry with AZT-11 telescope of CrAO are following: start (JD) 52728.26714 end (JD) 52728.31593 Date JD U B V R I 52728.2932 14.25 14.95 14.49 14.02 13.65 52728.2932 0.018 0.019 0.030 0.017 0.027 error CrAO telescopes will continue to monitor the OT. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2009 SUBJECT: GRB 030329: Upper limit from 5.6 hours before trigger DATE: 03/03/30 00:17:01 GMT FROM: James Wren at LANL J. Wren and W. T. Vestrand report on behalf of the RAPTOR team: While the location of HETE-2 trigger 2652 was below our horizon at the time of the GCN notice, we did obtain observations earlier in the evening of the GRB field with one of our wide-field RAPTOR sky monitors. The observation nearest to the time of the burst was taken at 05:58:39.56 UT, 5.64 hours before the event. This image does not show the optical counterpart to a 3-sigma limiting magnitude of Rc=12.8. Unfortunately, the weather degraded rapidly later in the night, preventing further observations of this field. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2010 SUBJECT: GRB 030329: visual observations DATE: 03/03/30 00:33:03 GMT FROM: Arto Oksanen at Nyrola Obs., Finland A. Oksanen (Nyrola Observatory), R. Henriksson and M. Tuukkanen (the Finnish Deep Sky section of Astronomical Association Ursa) report: We observed the optical afterglow of GRB030329 reported by Peterson and Price (GCN 1985) visually about 8 hours after the burst. M. Tuukkanen observed the OT In Pornainen, Finland with a 0.63 m Newton telescope for about one hour starting March 29, 2003 19:30 UT. He reported it as a faint starlike object seen easily with direct vision. He did not see any flickering or distinct color. R. Henriksson was observing in Orivesi, Finland with his 0.30 m Newton telescope using 200x magnification at 20:05 UT. He reported the object stellar and faint, visible only with averted vision. His scanned sketch with notes is available on web: http://archive.ermiksson.net/record.php?id=4112 Both observers estimated the visual magnitude as 14.3 by using the 14.2 magnitude GSC 1434:322 star North of OT as reference. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2011 SUBJECT: GRB 030329: Optical pre-Imaging DATE: 03/03/30 00:49:05 GMT FROM: Josh Bloom at Harvard/CFA GRB 030329: Optical pre-Imaging C. Blake (Princeton) and J. S. Bloom (CfA) report: "Using a signal-to-noise weighted stack of 50 NEAT images (taken from 1997-2002), we do not detect a counterpart at the position of the transient afterglow of GRB 030329 (Price & Peterson; GCN #1985). The images were acquired by R. Bambery, S. Pravdo, M. Hicks, and K. Lawrence (Near-Earth Asteroid Tracking Project, Jet Propulsion Laboratory). We therefore estimate the upper limit to the brightness of any host galaxy as R=23.1 (2 sigma) or R=22.5 (3 sigma). This result is consistent with the somewhat more shallow limits reported in Wood-Vasey et al. (GCN #1998). The absence of a host to such magnitude levels suggests a redshift of z >~ 0.2, despite the extreme brightness of the early afterglow. Within 7.5 arcseconds of the position of the OT, we find two sources that are marginally detected (at the R=22.5 mag level): ------------------------------------------------------------------ RA(J2000) DEC Source-->OT ------------------------------------------------------------------- A: 10:44:49.776, +21:31:16.49 3.54" East, 1.66" North d=3.91" B: 10:44:50.065 +21:31:10.77 -0.49" East, 7.38" North, d=7.40" Positional errors relative to the USNO-B1.0 catalog are 0.5". These sources are shown in an image linked from the webpage given below. Photometric calibration of the stacked image was performed using the USNO-B1.0 catalog. Some photometric secondary stars in the field are listed below: RA(J2000) DEC R B mag mag ----------------------------------------------------- 10:44:55.17 +21:28:11.3 17.69 18.48 10:44:43.40 +21:27:58.4 18.41 19.46 10:44:44.06 +21:27:18.5 18.52 20.47 10:44:53.61 +21:30:11.6 17.45 18.41 10:45:04.39 +21:29:56.1 18.22 20.37 10:44:55.67 +21:31:22.2 19.08 19.95 10:44:54.97 +21:31:42.7 18.51 20.36 10:44:48.68 +21:31:39.8 18.95 19.30 10:44:42.00 +21:32:31.7 15.08 18.18 10:44:50.44 +21:32:05.8 16.61 17.99 10:44:59.44 +21:31:43.9 18.07 19.84 ------------------------------------------------------- Finally, we note an object at (J2000) 10:44:55 +21:31:05.9, which appeared in the DSS-II image, and is listed in the USNO-B1.0 as being R=19.60, was detected at only R=21.9 in our stacked image." A stacked image from NEAT that includes the WCS in the header may be found at: http://astro.princeton.edu/~cblake/030329.html This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2012 SUBJECT: GRB 030329: still bright DATE: 03/03/30 03:03:17 GMT FROM: Krzysztof Z. Stanek at CfA P. Martini (OCIW), P. Berlind, K. Z. Stanek (CfA) and P. Garnavich (Notre Dame): We imaged the optical afterglow of GRB 030329 (Peterson & Price: GCN 1985; Torii: GCN 1986) with the Magellan 6.5-m Clay telescope and LDSS2 imaging/spectrograph on March 30 UT 01:15 (13.6 hours after the burst). We also obtained imaging data with the FLWO 1.2-m telescope. The R-band magnitude is estimated to be 15.1 assuming star "A" is R=16.2 (see http://cfa-www.harvard.edu/~kstanek/grb030329.ps). Thus the OT continues to be very bright. We should note that the several fairly bright objects closest to the OT are clearly resolved in our images and should not be used for relative photometry. "A" and "B" appear to be stellar at ~1.3'' seeing. The foreground reddening from Schlegel et al. (1998) is E(B-V)=0.025. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2013 SUBJECT: GRB 030329, optical spectroscopy DATE: 03/03/30 03:19:19 GMT FROM: Peter Garnavich at U of Notre Dame P. Martini (OCIW), P. Garnavich (Notre Dame) and K.Z. Stanek (CfA) Spectra of the optical afterglow of GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) were obtained with the Magellan 6.5-m Clay telescope and LDSS2 imaging/spectrograph starting at March 30.06 (UT). The spectra cover the wavelength range of 4000 to 9000 Ang. with a resolution of 13 Ang. FWHM. Preliminary analysis of the spectum of this bright GRB afterglow shows a smooth blue continuum with no significant absorption features. The only obvious feature is an unresolved emission line at 5852 Ang. If this is [OII] emission from the host galaxy, then the redshift is z=0.57. Further analysis is continuing. This message may be cited. [GCN OPS NOTE(02apr03): The date int he first line was corrected from "GRB 030328" to "GRB 030329".] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2014 SUBJECT: GRB 030329: Radio Observations DATE: 03/03/30 03:35:26 GMT FROM: Edo Berger at Caltech E. Berger, A. M. Soderberg (Caltech) and D. A. Frail (NRAO) report on behalf of a larger collaboration: "We observed the position of the optical afterglow (GCN 1985) of GRB 030329 (GCN 1997) with the VLA on March 30.06 UT. We detect a 3.5 mJy source at 8.46 GHz coincident with the OT. This is the brightest radio afterglow detected to date, consistent with the unusual brightness of the optical (e.g. GCNs 1986 & 1987) and X-ray (GCN 1996) counterparts, as well as the prompt emission (GCN 1997)" This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2015 SUBJECT: GRB030329: optical spectroscopy with the TNG DATE: 03/03/30 05:56:08 GMT FROM: Angelo Antonelli at Obs. Astro. di Roma R. Della Ceca, T. Maccacaro (INAF-OABrera), D. Fugazza, M. Pedani, M. Cecconi (TNG), F. Fiore, L.A. Antonelli (INAF-OAR), S. Covino (INAF-OABrera), E. Pian (INAF-OATs), N. Masetti (IASF-CNR) report: "Starting on March 30 2003 00:43:40 UT we have obtained low resolution (R~1000) spectra of the optical afterglow of GRB030329 (Peterson & Price GCN #1985, Torii, GCN #1986) using DOLORES at TNG. Observations consisted of two exposures of 15 min each the second obtained at 2.75hh after the first, and cover the full spectral range 3800-8000 Angstrom, in relatively good seeing conditions (1.5"). At the time of the observations the afterglow magnitude was R~15-16 (e.g. Martini et al. GCN #2012). A preliminary analysis of the spectra reveals no strong absorption features. A more detailed analysis is needed to search for faint absorption lines. A faint emission line at 5846 Angstrom (see Martini et al. GCN# 2013) is present in the later spectra, when the afterglow emission was less strong. If this is [OII] emission from the host galaxy, then the redshift is z=0.568. We detect a strong spectral variability between the first spectrum, when the afterglow was extremely blue, and the second spectrum, obtained starting from 03:25:35 UT. We are particularly grateful to the TNG staff for their remarkable support to these observations. This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2016 SUBJECT: GRB030329 optical observations DATE: 03/03/30 06:34:21 GMT FROM: Gianluca Masi at Bellatrix Astronomical Obs G. Masi (University of Rome " Tor Vergata" and ESO), F. Mallia, U. Tagliaferri (Osservatorio Astronomico di Campo Catino, Italy), B. L. Jensen and J. Hjorth (University of Copenhagen), M. I. Andersen (Astrophysikalisches Institut Potsdam) report: We imaged the field around the OT located by Peterson & Price (GCN 1985) and Torii (GCN 1986), using the Campo Catino Automated Telescope (0.4-m f/8) + CCD (unfiltered, but peaking in the red part of the spectrum) on Mar 29.9621 UT. The source was bright and our astrometry provided a position in excellent agreement with that in GCN 1994 (Uemura et al.). Using the R magnitudes for the USNO SA2.0 stars in the field, we obtained a preliminary magnitude of CR = 14.5. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2017 SUBJECT: GRB 030329: Optical decay and synthesis DATE: 03/03/30 07:57:04 GMT FROM: Paul Price at RSAA, ANU P.A. Price, B.P. Peterson and B.P. Schmidt (RSAA, ANU) report: Synthesis of observations from Rykoff et al. (GCN #1995), Gal-Yam et al. (GCN #1999), Martini et al. (GCN #2012) and from the SSO 40-inch (GCN #1987) yeilds the following decay: R/mag ~ 15.8 + 2.4 log (t/days) with corresponding power-law index alpha = 0.97 +/- 0.03. Hence, though the afterglow is bright, the decay is not unusually shallow (eg, 010222 had alpha1 ~ 0.80). The spectral index, calculated from the B-I colour from Burenin et al. (GCN #2001) and Rumyantsev et al. (GCN #2005) is beta ~ 1.2. Using the measured redshift (Martini et al., GCN #2013; Della Ceca et al., GCN #2015), optical decay and spectral index, we calculate the R-band absolute magnitude of the optical afterglow for t=1 day in the source frame, M_R,1 = -26.7 mag. This is therefore the most intrinsically bright optical afterglow observed to date (with 000301C and 000418 tied for second at M_R,1 = -26.1 mag). The low redshift and the large intrinsic brightness combined to produce an optical afterglow with a large apparent brightness. The redshift of z=0.57 and measured fluence (Vanderspek et al., GCN #1997) implies an isotropic-equivalent energy release of 1.1 x 10^53 erg (30-400 keV). The Frail et al. "standard energy" result implies a jet-break time of around 4 days. At this time, the afterglow should be R ~ 17.3 mag. We encourage polarimetric observations to be made on this timescale to constrain the jet dynamics. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2018 SUBJECT: GRB 030329, optical photometry DATE: 03/03/30 08:13:11 GMT FROM: Peter Garnavich at U of Notre Dame P. Garnavich (Notre Dame), K.Z. Stanek and P. Berlind (CfA) Photometry of the GRB 030329 afterglow (Peterson & Price: GCN 1985; Torii: GCN 1986) has been obtained with the Fred L. Whipple 1.2m telescope beginning March 30.10 (UT). The R-band images show a power-law decay index of -1.9 between 14 and 18 hours after the burst. This is significantly steeper than the decay index of -0.9 derived from the photometry of Rykoff & Smith (GCN 1995) and Burenin et al. (GCN 2001) obtained within 8 hours of the burst. A break in the light curve appears to have occurred between 0.3 and 0.5 days after the burst. The post-break light curve is well fit by R=16.3+1.9*2.5*log(age in days) with the calibration based on that of Martini et al. (GCN 2013). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2019 SUBJECT: GRB030329: ROTSE network observes steepening of decay curve DATE: 03/03/30 08:29:16 GMT FROM: Don Smith at U michigan D. A. Smith reports on behalf of the ROTSE collaboration: The ROTSE-IIIb instrument at McDonald Observatory in Texas began observing the optical counterpart to GRB 030329 as soon as it was possible to do so. The first calibrated image began at 30 March 02:27:31 (UTC). Images were calibrated against the R-band magnitudes of the USNO A2.0 catalog, and the source was initially found to be at an unfiltered magnitude of 15.35+-0.06 and fading. Analysis of the first 70 images showed clearly that the rate of decay had increased when compared to the observations recorded by ROTSE-IIIa the night before (Rykoff & Smith, GCN Circ. 1995). Separate power-law fits to each instrument's data set indicated that the flux decay slope had shifted from about 1.0 (consistent with the decay slope reported by Price, et al. GCN Circ. 2017) to about 1.9 (consistent with the decay reported by Garnavich et al. GCN Circ. 2018). A plot of these decay curves along with the power-law fits can be seen at http://www.rotse.net/transients/grb030329/). An extrapolation of these curves predicts a break time of about 12.1 h after the burst. ROTSE-IIIb will continue to observe GRB 030329 as long as it is able to do so. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2020 SUBJECT: Redshift of GRB 030329 DATE: 03/03/30 09:39:08 GMT FROM: Jochen Greiner at MPI J. Greiner (MPE Garching), M. Peimbert (UNAM Mexico), C. Estaban (IAC Spain), A. Kaufer, P. Vreeswijk, A. Jaunsen, J. Smoke (all ESO), S. Klose (Thueringer Landessternwarte) and O. Reimer (Univ. Bochum) report for a larger collaboration: The optical afterglow (Peterson & Price, GCN 1985; Torii, GCN 1986) of the bright HETE (H2652) GRB 030329 was observed with the high-resolution UVES spectrograph at the VLT unit Kueyen, starting around March 30.166 UT. Quick-look analysis reveals several absorption and emission lines. In particular, we find emission lines at 5680, 5850, and 7669 A which we identify with Hbeta, [OIII]5007 and Halpha. Absorption lines are clearly seen at 3270 A and 3334 A which we identify as the MgI 2853 and MgII 2800 doubletts. Based on these identifications we determine a redshift of z=0.1685. This is nearest GRB so far (except GRB 980425/SN1998bw), consistent with the exceptional brightness of this afterglow at all wavelengths. We are highly indebted to the ESO staff at Paranal for their assistence, and K. Torii (RIKEN) for providing an early finding chart. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2021 SUBJECT: GRB 030329: Optical Decay DATE: 03/03/30 11:16:08 GMT FROM: Jules Halpern at Columbia U. J. P. Halpern, N. Mirabal, M. Bureau (Columbia U.), K. Fathi (U. Nottingham) report for the MDM Observatory follow-up team: We monitored the optical afterglow of GRB 030329 (=H2652, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the R-band with the MDM 1.3m for 7.5 hours beginning on March 30 03:05 UT, 15.5 hours after the burst. During this period, the magnitude declined from R = 15.38 to R = 16.22, referenced to star "A" of Martini et al. (GCN 2012). A fit to the 7.5 hour run yields a power-law decay slope of -1.934 +/- 0.005, in agreement with contemporaneous measurements of Garnavich et al. (GCN 2018) and Smith (GCN 2019), although it is apparent that the slope is continuing to steepen further. A graph of the preliminary differential magnitude light curve is available at http://www.astro.columbia.edu/~jules/030329_lc.ps We thank J. Kemp for providing the data reduction pipeline. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2022 SUBJECT: GRB030329, SPM optical observations DATE: 03/03/30 12:29:57 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov (OAN SPM, IA UNAM, Mexico), E. Benitez, J. Torrealba, J. Stepanian (IA UNAM, Mexico) report: We have observed the GRB030329 OT found by B.A. Peterson and P.A. Price (GCN 1985) with 1.5m and 2.1m telescopes of SPM Observatory, BC, Mexico. A set of exposures in UBVRI Bessel filters was obtained with 1.5m telescope under photometric conditions. Standard stars RU 149 and PG 1633+099 from Landolt's catalogue were used for photometric calibrations. The results of photometry are following: 30 March U B V R I UT 03:55 15.23 16.00 15.68 15.38 14.95 UT 05:55 15.44 16.25 15.92 15.61 15.19 UT 08:00 15.80 16.44 16.16 15.84 15.41 UT 10:16 15.99 16.65 16.40 16.05 15.62 Errors are about 0.02. USNO U1050_06350247 star with coordinates (AR=10 44 42; DEC=+21 32 32, J2000) can be used as the secondary standard in the OT field: B = 17.93(5); V =16.84(3); R = 16.04(2); I = 15.48(2) The continuous light curve in the R band with exposures 240 and 120 sec was obtained during 6.5h from 03:55 UT utill 10:40 UT. We estimate the decline rate to be about 0.11 mag/hour. Spectra of the optical afterglow of GRB 030329 were obtained with the 2.1-m telescope and B&Ch spectrograph (600l/mm) starting at 05:22 UT. The spectra cover the wavelength range of 3900 to 6100 AA with a resolution of 2.2A/pix. Data analysis is in progress. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2023 SUBJECT: GRB030329, BVRcIc field photometry DATE: 03/03/30 12:54:08 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 11x11 arcmin field centered at the coordinates of the optical transient (Peterson and Price, GCN 1985) for the HETE burst GRB030319 (GCN 1997) with the USNOFS 1.0-m telescope on one clear but very poor seeing night. Stars brighter than V=11.0 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/grb030329.dat The astrometry in this file is based on linear plate solutions with respect to UCAC2. The external errors are less than 100mas. Due to the poor seeing, the external photometric error is larger than normal for our calibrations. This report should be considered preliminary, with additional calibrations, including U-band, to be performed later in the week when weather conditions are better. 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: 2024 SUBJECT: GRB 030329: Light curve observed during the change of its slope. DATE: 03/03/30 15:17:40 GMT FROM: Rodion Burenin at IKI, Moscow R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, K. Uluc, I. Khamitov (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: The optical afterglow of GRB 030329 (Peterson and Price, GCN 1985) was observed with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe (TUBITAK National Observatory, Turkey). The observations started at Mar 29.744 UT, appr. 6 hours after the burst and lasted until Mar 30.061 UT, appr. 14 hours after the burst. During the night we have obtained approximately 200 images in each BVRI Bessel filter with 10-30 s exposures. The photometric conditions were good. To calibrate the OT flux from the beginning of our observations we were using the star which later was named as "A" star by Martini et al. (GCN 2012). We assume this star is R=16.20 which agree well with our mean photometric solution, obtained in previous nights. To calibrate OT flux in other filters we assume the following magnitudes of this star: B=18.22, V=17.02, I=15.42, measured using the same photometric solutions. The optical transient showed no significant variations above the gradual decline; the preliminary upper limit on short-term variability is 5%. In the first 5 hours of our run we find that the R-band flux declines as t**-1.1. During the last 2.5 hours we observed the smooth continuous change in the slope of power law flux decay. The fit of the post-break light curve reported by Garnavich et al. (GCN 2018) lies exactly on the continuation of our light curve. This suggests that we are lucky to observe in detail the major change in the slope of the light curve and measure its duration. The break occured in 12-14 hours after the burst and lasted for appr. 2-4 hours. The R magnitudes of the afterglow are: t-t0,hours R 6.199 14.10 7.049 14.26 7.899 14.38 8.749 14.52 9.599 14.64 10.449 14.75 11.299 14.84 12.149 14.96 12.999 15.06 13.849 15.16 The preliminary light curve in R can be found at http://hea.iki.rssi.ru/~br/lcl_030329_r.ps The finding chart available at http://hea.iki.rssi.ru/~br/r_030329.gif Further analysys of the lightcurve is underway. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2025 SUBJECT: GRB030329b: detection by Konus-Wind and Helicon-CoronasF DATE: 03/03/30 15:33:43 GMT FROM: Dmitry Frederiks at Ioffe Institute S.Golenetskii, E.Mazets, V.Pal'shin, and D.Frederiks on behalf of Konus-Wind and Helicon/Coronas-F teams; T.Cline on behalf of Konus-Wind team report: GRB030329b was detected by Konus-Wind at 15:34:18.824 UT and Helicon/Coronas-F at 15:34:15.347 UT We have triangulated it to a preliminary annulus centered at RA(2000) = 205.907 degrees, Decl(2000)= -13.064 degrees, and radius = 51.5 +/- 2.3 degrees (3 sigma). Analysis of Konus-Wind data from both detectors gives an ecliptic latitude of the source of -45 +/- 10 degrees. Preliminary data analysis gives the following characteristics: - fluence in 15-2000 keV range = 2.0x10-5 erg cm-2 (for 65 seconds) - peak flux in 15-2000 keV range = 1.0x10-6 erg cm-2 s-1 - Ep (at maximum intensity) = 90 keV - Ep (time integrated spectrum) = 50 keV //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2026 SUBJECT: GRB030329a: detection by Konus-Wind DATE: 03/03/30 15:49:49 GMT FROM: Dmitry Frederiks at Ioffe Institute S.Golenetskii, E.Mazets, V.Pal'shin, D.Frederiks (Ioffe Institute), and T.Cline (NASA GSFC) on behalf of Konus-Wind team report: GRB030329a (GCN 1779) was also detected by Konus-Wind at 11:37:29.354 UT Preliminary data analysis gives the following characteristics: - fluence in 15-5000 keV range = 1.6x10-4 erg cm-2 (for 35 seconds) - peak flux in 15-5000 keV range = 2.5x10-5 erg cm-2 s-1 - Ep (at maximum intensity) = 150 keV - Ep (time integrated spectrum) = 90 keV //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2028 SUBJECT: GRB030329: Optical observations DATE: 03/03/30 19:35:27 GMT FROM: Vasilij Rumjantsev at CrAO V.Rumyantsev, E.Pavlenko, O.Antoniuk (CrAO) and A.Pozanenko (IKI) report: We continue to monitor the OT of GRB030329 (GCN 2025). The OT found by Peterson and Price (GCN 1985) is clearly visible in our image taken with Cassegrain 38-cm telescope of CrAO.Several 180 sec. exposures of R (Johnson) filter were obtained. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude as Mid Time (UT) exposure OT March, 30 17:56:25 1x180 s R = 16.61 The figure image can be found in http://grb.rssi.ru/GRB030329/ Detailed calibration and observations are continuing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2029 SUBJECT: GRB 030329, optical observations DATE: 03/03/30 20:00:50 GMT FROM: Sylvio Klose at TLS Tautenburg S. Klose, C. Hoegner (Thueringer Landessternwarte Tautenburg), J. Greiner (MPE Garching) report: We observed the field of GRB 030329 (HETE trigger #2652) with the Tautenburg Schmidt telescope equipped with the prime focus CCD camera (2k x 2k). Based on the secondary standard star at RA, DEC (J2000) = 10:44:54.43, 21:34:28.6 (R=13.69, I=13.28) provided by Henden (GCN 2023), we measure for the afterglow R=16.4 at 18:54 -- 19:02 UT and I=15.9 at 18:46 -- 18:54 UT with an estimated error of 0.1 mag. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2030 SUBJECT: GRB030329: R and B observations DATE: 03/03/30 20:31:08 GMT FROM: Adriano Guarnieri at O.A.di Bologna C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University), G. Gavazzi (Milano-Bicocca University), R. Gualandi (Bologna Astronomical Observatory), G. Pizzichini and P. Ferrero (IASF-CNR, Bologna) report: By a preliminary reduction of four frames of our CCD UBVRI photometry of GRB030329 (GCN n.2003), performed with the 152 cm Loiano telescope, we obtain: mid exp. filter exposure time mag UT (seconds) Mar 29.7823 R 300 14.29 +/-.10 Mar 29.8556 R 180 14.55 +/-.03 Mar 29.7957 B 900 15.16 +/-.03 Mar 29.8493 B 300 15.38 +/-.03 Magnitude values were referred to star A (Martini et al, GCN 2012) as calibrated by Burenin et al. (GCN 2024). The uncertainties have the meaning of internal errors. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2031 SUBJECT: GRB030329 - near contemporaneous optical limits from CONCAM DATE: 03/03/30 21:34:26 GMT FROM: Avishay Gal-Yam at Tel Aviv U, Israel E. O. Ofek, A. Gal-Yam, Y. Lipkin, K. Sharon and E. Medezinski (Wise observatory, TAU) report: We searched for archival CONCAM (www.concam.net) images covering the trigger time of GRB 030329 (March 29, 11:37:14, Ricker et al. GCN 1997). This part of the night was covered by CONCAM units at Kitt Peak and Mount Wilson Observatories. Unfortunately, CONCAM images for that night from Mauna Kea Observatory in Hawaii are uavailable on the net. CONCAM images covering the exact time of the GRB trigger do not appear in the web archives of both sites (Kitt Peak and Mount Wilson). We were therefore limited to the analysis of images taken a few minutes before and after the GRB. We could not detect an OT to a conservative limiting magnitude of 3.5. The Kitt peak images are superior: four 180 s CONCAM images, taken at Mar 29, 11:29:57, 11:33:52, 11:41:46 and 11:45:42 UT were searched. The magnitude limit is shallow as the GRB location was near the horizon at Keat Peak. If the instantaneous optical display associated with GRB 030329 (z=0.1685, Greiner et al. GCN 2020) had been similar to that of GRB 990123 (z=1.6), which peaked above mag 9, then after appropriate scaling by the luminosity distance (for a flat Universe with omega=0.3, neglecting effects of extinction), we would expect GRB 030329 to be ~240 times brighter than GRB 990123. This means that an optical source with mag ~3 should have been apparent on contemporaneous CONCAM images. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2033 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/03/30 23:06:39 GMT FROM: Kevin Lindsay at Clemson.U K. Lindsay, D. H. Hartmann (Clemson University), M. Leake, M. Williams (Valdosta State University) Report on behalf of a larger collaboration: We observed the optical afterglow of GRB 030329, (=H2656, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the Johnson B-Band with the SARA 0.9m telescope at KPNO. We obtained 45, 300s exposures. Observations began at 02:55:09UT, and ended at 06:50:58UT, on March 30th. The obsevations were carried out under good seeing conditions. Aperture photometry was performed, and calibrated utilizing standards reported by Henden et al., GCN 2023. During the observational period, the afterglow faded by approximately 0.5mag. Further observations are planned. More information on the SARA Observatory can be found at http://www.saraobservatory.org/. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2034 SUBJECT: GRB030329 - Light curve flattening DATE: 03/03/30 23:27:35 GMT FROM: Eran Ofek at Tel Aviv U. Y. Lipkin, E. O. Ofek, A. Gal-Yam, Haim Mendelson (Wise observatory, TAU) report: We are observing the field of GRB 030329 (HETE trigger #2652, Ricker et al., GCN 1997) with the TEK 1K CCD mounted on the 1-meter telescope of Wise Observatory, Israel. Based on the secondary reference stars provided by Henden (GCN 2023, RA, Dec (2000) = 10:44:39 +21:30:59, and 10:44:42 +21:32:32), we measure a magnitude of R=16.40 for the OT at 17:20 UT Preliminary analysis of 75 images, obtained during three hours of observations (17.2 UT - 20.5 UT) yields a power-law decay rate (alpha) of 0.7 +/- 0.1. It appears that the OT decline rate has flattened again, after the reported break (Halpern et al. GCN 2021). [GCN OPS NOTE (30Mar03): Haim Mendelson was added to the author list.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2035 SUBJECT: GRB030329: R band light curve by MASTER DATE: 03/03/30 23:43:37 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, A. Krylov, V. Kornilov, G. Borisov, D. Kuvshinov, A. Belinski, I. Chilingarian, M. Kuznetsov, S. Potanin, V. Vitrischak, G. Antipov Sternberg Astronomical Institute, Alexsandr Krylov Observatory, Moscow report: The OT of GRB030329 (Peterson and Price, GCN 1985) was observed with MASTER system (280mm, http://observ.pereplet.ru, GCN 2002). We obtained about 200 measurements in R filter, with calibration to several tens of USNO A2.0 stars located in 15 arcmin field around the OT. Our observations started at Mar 29, 17.1 UT (5.5 hours after the GRB) and had been lasting for 8.5 hours up to Mar 30, 1.5 UT (13.9 hours after the GRB). Corresponding to our observations, R-band flux declines as t^-1.0 (sligtly differs from t^-1.1 reported by Burenin et al. GCN 2024). At the end of observations the OT's brightness began to decrease more rapidly. We had very poor transparancy at that time, so flux measurements uncertanities were quite big, therefore we can't confirm or refute -1.9 index reported by Garnavich et al. (GCN 2018). Our lightcurve based on 114 measurements available at: http://observ.pereplet.ru/images/GRB030329_R_lc.gif http://www.sai.msu.su/~chil/GRB030329_R_lc.ps Further analysis of the obtained data is underway. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2040 SUBJECT: GRB030329: Near Infrared Observations DATE: 03/03/31 04:30:27 GMT FROM: Don Lamb at U.Chicago D. Q. Lamb, D. York, J. Barentine, B. Ketzeback, J. Dembicky, R. McMillan, M. Nysewander and D. Reichart report on behalf of the ARC and UNC GRB teams of the FUN GRB collaboration: J-, H-, and K-band photometry of the optical afterglow (Peterson and Price, GCN 1985) of GRB030329 (Vanderspek et al., GCN 1997) were obtained using the ARC 3.5-m telescope and the GRIM II at APO, starting at 4.712 UT and ending at 5.651 UT on March 30. The measured J-band magnitudes of the afterglow are given below: ------------------------ UT J ------------------------ 4.712 14.230 +/- 0.047 4.961 14.307 +/- 0.077 5.425 14.596 +/- 0.119 5.570 14.501 +/- 0.075 ------------------------ Assuming a model F(nu) ~ F_0 (nu/nu_0)^alpha, the spectral slope of the flux from the J-band through the K-band at the time of the first cycle of observations is alpha = - 0.8 +/- 0.1. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2041 SUBJECT: GRB 030329, optical photometry DATE: 03/03/31 05:22:25 GMT FROM: Peter Garnavich at U of Notre Dame K.Z. Stanek (CfA), P. Martini (OCIW) and P. Garnavich (Notre Dame) Images of the GRB 030329 afterglow (Peterson & Price: GCN 1985; Torii: GCN 1986) were obtained with the Magellan 6.5-m Clay telescope beginning March 31.068 (UT). Four 30-sec exposures were taken in the R-band with the LDSS2 imaging/spectrograph. Using the calibration by Henden (GCN 2023) for "star A" (GCN 2012) at 10:44:42 +21:32:31 (2000) of R=16.06, we find the brightness of the afterglow is R=16.21 +/- 0.05. This is nearly a magnitude brighter than expected from the extrapolation of a powerlaw decay slope of -1.9 found around 16 hours after the burst by Garnavich, Stanek & Berlind (GCN 2018), Smith (GCN 2019) and Halpern et al. (GCN 2021). Apparently, a more shallow decay has reappeared as reported by Lipkin et al. (GCN 2034). We combined the Clay images, taken in 1" seeing, and subtracted the afterglow point-spread function but no evidence of the host galaxy was detected. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2042 SUBJECT: GRB 030329 RBO V Optical Observations DATE: 03/03/31 07:51:21 GMT FROM: Justin Schaefer at U of Wyoming J. Schaefer, S. Savage (University of Wyoming) Report on behalf of the University of Wyoming GRB response team and the FUN GRB collaboration: We observed the optical afterglow of GRB 030329, identified in (GCN 1986), in the Johnson V-Band with the RBO 0.6m telescope at Red Buttes Wyoming. We obtained 6, 180s exposures on March 30th UT. The observations were carried out under fair to poor conditions. Aperture photometry was performed and calibrated utilizing the standards reported by Henden et al., (GCN 2023). We initially measured the magnitude of the OT to be V=15.57 +/- 0.01 at 02:59UT which faded by 0.06 during the short observational period. Further observations are currently being undertaken, and more data for the V filter will follow. This message may be cited //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2043 SUBJECT: GRB030329 15 GHz radio observation DATE: 03/03/31 09:14:04 GMT FROM: Guy Pooley at MRAO, Cambridge, UK GRB 030329 (= H2652) (GCN 1985 and many others) was observed with the Ryle Telescope at Cambridge, UK from 2003 Mar 30 16:35 UT to 2003 Mar 31 03:30 UT. The mean flux density at 15.2 GHz was 9.8 mJy (cf 3.5 mJy at 8,46 GHz approximately 24h earlier - GCN 2014). Over the period of the observation the flux density increased from 7 to 12 mJy. A light curve may be seen at http://www.mrao.cam.ac.uk/~guy/grb/GRB030329-030330.ps //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2044 SUBJECT: GRB 030329: OT observations at Kanazawa DATE: 03/03/31 10:37:38 GMT FROM: Toshio Murikami at ISAS T. Murakami, D.Yonetoku, H.Izawa, T.Uchida, N.Hirosawa and M.Suzuki report: We observed the afterglow of GRB 030329 (HETE trigger #2652) at Kanazawa, Japan, discovered by Peterson & Price (GCN 1985) and Torii (GCN 1986). We have started observations at 13:33:34 UT. (2 hours after the burst ) until 18:55 UT, 30-s integration was repeated. The object was 13.1+/-0.1 mag preliminary (refer to USNO-A2.0 red) at the first frame with 25cm/f4.8 telescope equipped with unfiltered CCD(KAF0261E). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2045 SUBJECT: GRB030329 - OT brightens DATE: 03/03/31 11:22:57 GMT FROM: Eran Ofek at Tel Aviv U. Y. Lipkin, E. O. Ofek, A. Gal-Yam, E. M. Leibowitz, H. Mendelson (Wise observatory, TAU) report: Observations of GRB 030329 (HETE trigger #2652, Ricker et al., GCN 1997) with the TEK 1K CCD mounted on the 1-meter telescope of Wise Observatory, Israel revealed that starting approximately March 30 21:00 UT, the OT brightened. The light curve, decaying with a power-law index alpha=0.7 (Lipkin et al. GCN 2034), reached a minimum R-band magnitude of about 16.45 at approximately 21:00 UT. Over the next three hours the OT brightened, reaching R=16.25 at approximately March 31.0 UT, consistent with later observations by Stanek et al. (GCN 2041). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2046 SUBJECT: GRB 030329: further optical observations DATE: 03/03/31 11:38:58 GMT FROM: Denis Denissenko at IKI, Moscow R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, K. Uluc, I. Khamitov (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: The optical afterglow of GRB 030329 (Peterson and Price, GCN 1985) was observed with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe (TUBITAK National Observatory, Turkey; see also GCN 2001 and 2024) in the night of March 30/31. The R magnitudes of the afterglow are: t-t0,hours UT R 34.69 30.961 16.5 38.12 31.073 16.39 The magnitude of "A" star was assumed to be R=16.20. First observation was made under poor sky conditions in R filter only. Second set of four images was obtained in each of BVRI filters. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2047 SUBJECT: GRB 030329, R-band light curve DATE: 03/03/31 19:00:09 GMT FROM: Sylvio Klose at TLS Tautenburg A. Zeh, S. Klose (Thueringer Landessternwarte Tautenburg), M. Nysewander, D. Reichart (University of North Carolina at Chapel Hill), J. Greiner (MPE Garching) report: We selected from the GCN literature all available R-band data of the afterglow of GRB 030329 (including the unfiltered ROTSE data; Rykoff and Smith, GCN 1995). We fitted the afterglow light curve using the standard Beuermann equation (A&A 352, L26). The result is: alpha_1 = 0.85 +/- 0.07, alpha_2 = 1.45 +/- 0.09, t_break = 0.39 +/- 0.06 days. The substantial re-brightening reported by Lipkin et al. (GCN 2045) and Burenin et al. (GCN 2046) seems to be similar to that seen in the afterglow light curve of GRBs 000301C and 021004. A plot including a predicted supernova component and assuming a negligible contribution from an underlying host galaxy is available via anonymous ftp from ftp.tls-tautenburg.de, dir /pub/klose/10/. A multi-color plot is available at http://www.physics.unc.edu/~mnysewan/grb030329.html. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2048 SUBJECT: GRB 030329, R-band observations DATE: 03/03/31 19:56:32 GMT FROM: Sylvio Klose at TLS Tautenburg A. Zeh, S. Klose, U. Laux (Thueringer Landessternwarte Tautenburg), J. Greiner (MPE Garching) report: Recent observations with the Tautenburg Schmidt telescope indicate that the afterglow of GRB 030329 has stopped re-brightening. We measure R=16.8 +/- 0.1 on images taken at 18:43 UT. Multi-color observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2049 SUBJECT: Photometry of GRB030329 - Constant OT Magnitude DATE: 03/03/31 20:12:58 GMT FROM: Avishay Gal-Yam at Tel Aviv U, Israel Y. Lipkin, E. M. Leibowitz, E. O. Ofek, A. Gal-Yam, H. Mendelson (Wise observatory, TAU) report: We are conducting time-resolved photometry of GRB 030329 (HETE trigger #2652, Ricker et al., GCN 1997) with the TEK 1K CCD mounted on the 1-meter telescope of Wise Observatory, Israel. During 3 hours of observations, starting at March 31 17:00 UT, the OT is constant (to within 0.1 mag), with a mean magnitude of approximately R=16.8, consistent with the findings of Zeh et al (GCN 2048). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2050 SUBJECT: GRB030329: Optical observations DATE: 03/03/31 20:37:36 GMT FROM: Vasilij Rumjantsev at CrAO E.Pavlenko, V.Rumyantsev, O.Antoniuk, N.Primak (CrAO) and A.Pozanenko (IKI) report: We continue to monitor the OT of GRB030329 (GCN 2005, 2028). The OT found by Peterson and Price (GCN 1985) was imaged Cassegrain 38-cm telescope of CrAO. Several 240 sec. exposures in R (Johnson) spectral band were obtained. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude as Mid Time (UT) exposure OT March, 31 17:50:40 240 sec 16.92 +/-0.04 Taking into account R=16.8 +/- 0.1 at 18:43 obtained by A. Zeh, et al. (GCN 2048) one may suggest that light curve of OT starts new episode of re-brightening or flattering is still continuing. Detailed calibration and observations are continuing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2051 SUBJECT: GRB 030329: optical photometry DATE: 03/03/31 20:57:57 GMT FROM: Rodion Burenin at IKI, Moscow R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, K. Uluc, I. Khamitov (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: We observed the GRB 030329 afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe (TUBITAK National Observatory, Turkey). The observations started at Mar 31.724 UT. OT magnitude in all BVRI Bessel filters was constant during first 1.5 hours of our observation. We measured R=16.91 for the OT, assuming that magnitude of "A" star is R=16.20. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2052 SUBJECT: GRB 030329: fading X-ray afterglow with RXTE DATE: 03/03/31 22:56:08 GMT FROM: Frank Marshall at GSFC F.E. Marshall (NASA/GSFC), C. Markwardt (U.Md. & NASA/GSFC), and J.H. Swank (NASA/GSFC) report: RXTE re-observed GRB 030329 for a total of 3.9 ks starting at March 30.724 UT (about 1.240 days after the burst). The flux was about 0.9e-11 ergs/s/cm**2 in the 2-10 keV band or about 15 times weaker than during the RXTE observation the previous day (Marshall and Swank, GCN 1996). The total light curve is well described by a simple model in which the flux decays as t^(-1.5). More complicated models are also consistent with the sparsely sampled data. For example, a model in which the decay rate increases from t^(-1.1) at early times (Burenin et al., GCN 2024) to t^(-1.934) at late times (Garnavich et al., GCN 2018; Smith, GCN 2019; Halpern et al., GCN 2021) fits the data if the break occurs 0.54 days after the burst. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2053 SUBJECT: GRB 030329, optical spectroscopy DATE: 03/04/01 00:30:50 GMT FROM: Peter Garnavich at U of Notre Dame N. Caldwell (CfA), P. Garnavich, S. Holland (Notre Dame), T. Matheson and K.Z. Stanek (CfA) Spectra of the optical afterglow of GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) were obtained with the 6.5-m MMT and Blue-Channel spectrograph on March 30 and 31 (UT) The low-resolution spectra cover the wavelength range of 3500 to 8500 Ang. with a resolution of 7 Ang. FWHM. Analysis of the spectrum taken in good seeing on March 31 shows several narrow emission lines. The line seen at 5852 Ang. by Martini et al. (GCN 2013) and Della Ceca et al. (GCN 2015) is, in fact, [OIII] 5007 and confirms the redshift estimate of Greiner et al. (GCN 2020) of z=0.168. In a 1.25" wide slit we find the following observed fluxes: observed ID z Flux (10^-16 erg/cm^2/s) 7669.2 Halpha 6563 0.1686 4.5 5851.1 [OIII] 5007 0.1686 4.1 5795.4 [OIII] 4959 0.1687 1.6 5681.7 Hbeta 4861 0.1687 1.5 4356.1 [OII] 3727 0.1687 1.2 A narrow absorption line is detected at 3933.2 Ang. with an equivalent width of 0.4 Ang. and is probably due to CaII in our Galaxy. An estimate of the star formation rate in the 4 kpc of the host galaxy nearest the burst can be made from the [OII] luminosity (Kennicutt 1998, ARAA, 36, 189; assuming H0=72). The rate is an anemic ~0.1 Solar masses/yr. without correcting for host extinction. The Halpha/Hbeta ratio is not well determined from these data, but does not imply a large extinction. We therefore conclude that the SFR of the GRB 030329 host is very low. This message may be cited. [GCN OPS NOTE(02apr03): The SFR was corrected from "... an anemic ~0.01 ..." to "... an anemic ~0.1 ...".] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2054 SUBJECT: GRB 030329: beginning of the new fading phase in optical band DATE: 03/04/01 00:47:11 GMT FROM: Denis Denissenko at IKI, Moscow R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, K. Uluc, I. Khamitov (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: We continue observations of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe. Assuming that star "A" has R=16.20 we have measured the following magnitudes: t-t0,hours UT R 54.3 March 31.75 16.91 55.2 31.78 16.92 57.1 31.86 16.99 We see the beginning of new phase of fading of the optical afterglow. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2055 SUBJECT: IPN triangulation of GRB030329b (large error box) DATE: 03/04/01 01:55:30 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the Ulysses GRB team, D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W. Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, S.Golenetskii, E.Mazets, V.Pal'shin, and D.Frederiks on behalf of Konus-Wind and Helicon/Coronas-F teams, and T.Cline on behalf of the Ulysses and Konus-Wind teams, report: Ulysses and RHESSI also observed this burst (GCN 2025). We have triangulated it to a preliminary annulus centered at RA, Decl(2000)= 158.367, 41.226 degrees, whose radius is 89.886 +/- 0.065 degrees (3 sigma ). This annulus intersects the Konus-Helicon annulus to form two large error boxes, only one of which is in the correct ecliptic latitude band. The intersection points are: RA(2000) Dec(2000) 156.798 -48.714 156.710 -48.583 164.555 -48.558 164.440 -48.435 This error box 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: 2056 SUBJECT: GRB 030329: optical observations DATE: 03/04/01 02:11:50 GMT FROM: Jerome A. Orosz at San Diego State U J. Brodney Fitzgerald and Jerome A. Orosz (San Diego State University) report: We have observed the field of GRB 030329 (Peterson & Price, GCN 1985) with the 1 meter telescope at the Mount Laguna Observatory (located 45 miles east of downtown San Diego at a dark site in the Cleveland National Forest at an altitude of 6100 feet or 1859 meters) on the nights of 2003 March 30 and 31 (UT). We used a Loral 2048 x 2048 CCD (binned 2 x 2) and Bessell B, V, R, and I filters. Both nights were photometric. The instrumental time series were obtained using Stetson's programs DAOPHOT, ALLSTAR, and DAOMASTER. The instrumental magnitudes were placed on the standard scales using Hendon's (GCN 2023) calibration. Our observations are summarized in the 4 tables below. The errors quote include only the DAOPHOT errors, and do not include errors in the zero points (estimated to be a few percent). The CCD images of the GRB field and some Landolt fields are available upon request to orosz@sciences.sdsu.edu. Further observations are planned for the night of April 1 (UT). We also report the discovery of a possible eclipsing binary in the field. The J2000 coordinates are 10:44:36.81, +21:26:58.8 (taken from Hendon's list given in GCN 2023). The star was at a minimum brightness around March 31 at 4:30 UT. Over the next three hours it brightened by about 0.6 magnitudes in all the filters. The brightness level was roughly constant between about 8:10 UT and 11:00 UT. The star was apparently constant on the night of March 30, although this conclusion is somewhat weak owing to the fact that it was saturated in many of our images. The following table gives the extreme magnitudes observed: Filter Min Mag Max Mag ----------------------------- B 14.36 13.77 V 14.00 13.41 R 13.78 13.11 I 13.60 13.00 Our GRB observations follow: Table 1: B Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-03-30T04:39:56.10 600.000 16.263 0.008 2003-03-30T05:19:08.50 480.000 16.321 0.010 2003-03-30T06:21:03.50 480.000 16.415 0.006 2003-03-30T07:24:03.20 480.000 16.510 0.004 2003-03-30T08:01:23.30 480.000 16.577 0.004 2003-03-30T08:50:07.70 480.000 16.648 0.004 2003-03-30T09:38:09.20 480.000 16.712 0.005 2003-03-30T10:38:02.00 480.000 16.889 0.013 2003-03-31T03:49:47.10 240.000 17.060 0.008 2003-03-31T04:09:46.30 240.000 17.087 0.009 2003-03-31T04:53:02.80 300.000 17.112 0.008 2003-03-31T05:16:57.30 300.000 17.140 0.008 2003-03-31T05:39:42.70 300.000 17.172 0.008 2003-03-31T06:17:01.30 300.000 17.191 0.008 2003-03-31T06:41:33.10 300.000 17.239 0.006 2003-03-31T07:17:46.30 300.000 17.246 0.009 2003-03-31T07:40:25.90 300.000 17.243 0.007 2003-03-31T08:03:53.90 300.000 17.285 0.009 2003-03-31T08:09:22.40 300.000 17.293 0.008 2003-03-31T08:48:31.90 300.000 17.296 0.007 2003-03-31T09:10:50.10 300.000 17.309 0.007 2003-03-31T09:33:07.30 300.000 17.327 0.007 2003-03-31T09:55:57.70 300.000 17.361 0.010 2003-03-31T10:42:17.30 300.000 17.374 0.012 2003-03-31T11:05:04.70 300.000 17.385 0.014 Table 2: V Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-03-30T04:39:56.10 600.000 15.8732 0.011 2003-03-30T05:19:08.50 480.000 15.9492 0.007 2003-03-30T06:21:03.50 480.000 16.0532 0.007 2003-03-30T07:24:03.20 480.000 16.1452 0.004 2003-03-30T08:01:23.30 480.000 16.1642 0.041 2003-03-30T08:50:07.70 480.000 16.2722 0.004 2003-03-30T09:38:09.20 480.000 16.3632 0.005 2003-03-30T10:38:02.00 480.000 16.4142 0.007 2003-03-31T03:54:27.10 240.000 16.6532 0.006 2003-03-31T04:15:22.50 240.000 16.6672 0.011 2003-03-31T04:59:11.40 300.000 16.7222 0.006 2003-03-31T05:22:35.30 300.000 16.7522 0.007 2003-03-31T05:45:20.50 300.000 16.7572 0.008 2003-03-31T06:23:02.00 300.000 16.7942 0.006 2003-03-31T06:47:19.40 300.000 16.8242 0.007 2003-03-31T07:23:20.20 300.000 16.8622 0.006 2003-03-31T07:46:01.50 300.000 16.8722 0.006 2003-03-31T08:14:56.30 300.000 16.8802 0.007 2003-03-31T08:20:24.00 300.000 16.8702 0.007 2003-03-31T08:54:07.40 300.000 16.9002 0.006 2003-03-31T09:16:24.00 300.000 16.9002 0.007 2003-03-31T09:38:42.50 300.000 16.9172 0.007 2003-03-31T10:01:27.30 300.000 16.9292 0.008 2003-03-31T10:06:57.80 300.000 16.4682 0.010 2003-03-31T10:12:26.00 300.000 16.9592 0.009 2003-03-31T10:48:07.50 300.000 16.9402 0.012 2003-03-31T11:10:40.10 300.000 16.9662 0.014 Table 3: R Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-03-30T04:39:56.10 600.000 15.402 0.006 2003-03-30T05:19:08.50 480.000 15.524 0.007 2003-03-30T06:21:03.50 480.000 15.694 0.009 2003-03-30T07:24:03.20 480.000 15.801 0.004 2003-03-30T08:01:23.30 480.000 15.841 0.005 2003-03-30T08:50:07.70 480.000 15.917 0.004 2003-03-30T09:38:09.20 480.000 16.004 0.006 2003-03-30T10:38:02.00 480.000 16.048 0.006 2003-03-31T03:59:42.40 240.000 16.277 0.009 2003-03-31T04:20:13.10 240.000 16.313 0.024 2003-03-31T05:04:46.90 300.000 16.356 0.006 2003-03-31T05:28:31.20 300.000 16.378 0.005 2003-03-31T05:50:50.80 300.000 16.392 0.007 2003-03-31T06:29:05.50 300.000 16.421 0.006 2003-03-31T06:52:51.60 300.000 16.459 0.005 2003-03-31T07:28:53.20 300.000 16.479 0.006 2003-03-31T07:51:53.40 300.000 16.487 0.007 2003-03-31T08:26:10.70 300.000 16.516 0.022 2003-03-31T08:31:42.00 300.000 16.509 0.006 2003-03-31T08:59:40.10 300.000 16.536 0.007 2003-03-31T09:21:55.50 300.000 16.535 0.006 2003-03-31T09:44:13.50 300.000 16.539 0.008 2003-03-31T10:18:09.40 300.000 16.560 0.007 2003-03-31T10:29:22.00 300.000 16.555 0.009 2003-03-31T10:53:41.70 300.000 16.577 0.007 2003-03-31T11:16:11.50 300.000 16.583 0.015 Table 4: I Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-03-30T04:39:56.10 600.000 15.0006 0.009 2003-03-30T05:19:08.50 480.000 15.1076 0.012 2003-03-30T06:21:03.50 480.000 15.2816 0.007 2003-03-30T07:24:03.20 480.000 15.3916 0.004 2003-03-30T08:01:23.30 480.000 15.4266 0.027 2003-03-30T08:50:07.70 480.000 15.5186 0.005 2003-03-30T09:38:09.20 480.000 15.6376 0.008 2003-03-30T10:38:02.00 480.000 15.7036 0.011 2003-03-31T04:04:32.10 240.000 15.8716 0.008 2003-03-31T04:25:02.80 240.000 15.8926 0.010 2003-03-31T05:10:34.50 300.000 15.9396 0.006 2003-03-31T05:34:03.50 300.000 15.9596 0.006 2003-03-31T05:56:25.90 300.000 15.9946 0.006 2003-03-31T06:35:53.60 300.000 16.0276 0.007 2003-03-31T06:58:26.10 300.000 16.0536 0.006 2003-03-31T07:34:51.90 300.000 16.0826 0.008 2003-03-31T07:58:11.70 300.000 16.0746 0.008 2003-03-31T08:37:12.10 300.000 16.0836 0.008 2003-03-31T08:42:40.70 300.000 16.1066 0.006 2003-03-31T09:05:09.40 300.000 16.1026 0.007 2003-03-31T09:27:28.10 300.000 16.1196 0.008 2003-03-31T09:49:53.50 300.000 16.1346 0.009 2003-03-31T10:23:41.20 300.000 16.1386 0.009 2003-03-31T10:35:00.70 300.000 16.1716 0.013 2003-03-31T10:59:14.40 300.000 16.1476 0.012 2003-03-31T11:21:45.60 300.000 16.1626 0.019 References: Hendon, A., et al. 2003, GCN 2023 Landolt, A. U. 1992, AJ, 104, 340 Peterson, B, A. & Price, P. 2003, GCN 1985 Stetson, P. B. 1987, PASP, 99, 191 ------------------------------------------------------------------------- Jerome A. Orosz Assistant Professor of Astronomy, San Diego State University 5500 Campanile Drive, San Diego, CA 92182-1221 (619) 594-7118 (office), 594-6182 (dept. secretary), 594-1413 (dept. fax) http://mintaka.sdsu.edu/faculty/orosz/web/ //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2058 SUBJECT: AAVSO V & R observations of GRB030329 DATE: 03/04/01 02:44:00 GMT FROM: AAVSO GRB Network at AAVSO A. Price (AAVSO) reports on behalf of the AAVSO International GRB Network: The AAVSO International GRB Network has obtained B, V, R, and unfiltered photometry of the afterglow to GRB030329 from numerous sources across the globe over the past 3 days. See notes for details and access to time series data. Berto Monard, South Africa Unfiltered = 14.06 @ 2003.03.29 17:15 to Unfiltered = 15.01 @ 2003.03.29 23:37 exposures: 317X45-60s Arto Oksanen, 0.4m at Nyrola Observatory, Finland R = 14.50 @ 2003.03.29 20:22:23 to R = 14.75 @ 2003.03.29 22:28:03 exposures: 10X120s (out of 148 total) Tim Schrabback and Anja von der Linden, 1.06m at Observatory Hoher List of Bonn University, Germany R = 15.0 @ 2003.03.29 22:55 exposure: 1800s Peter Brown, 0.41m at Orson Pratt Observatory, Brigham Young University, Utah USA R = 15.2 @ 2003.03.30 02:38 to R = 16.2 @ 2003.03.30 10:41 exposures: 1X300s Dan Kaiser, 0.35m at Crescent Moon Observatory, Indiana USA V = 16.62 2003.03.31 01:32:04 to V = 16.97 2003.03.31 06:18:06 R = 16.26 2003.03.31 02:10:12 to R = 16.53 2003.03.31 06:22:37 Bill Aquino, 0.3m with Buffalo Astronomical Association in New York, USA V = 16.71 @ 2003.03.31 05:33:03 exposures: 4X180s exposure Notes: * Detailed reports (observing equipment, location, conditions, etc.) and many original FITS files available at ftp://ftp.aavso.org/grb/GRB030329 or by e-mailing aavso@aavso.org. * Brown, Kaiser, Monard, and Oksanen have time series data spanning the observations posted here. Full data has already been or will be posted soon to the URL above. * Aquino, Kaiser, and Oksanen used comparison star photometry from Henden et al. (GCN 2023). Brown used comp star A described on the finder chart by Rumyantsev et al. (GCN 2005). Schrabback et al. used comp star A described on a different finder chart by Martini et al.(GCN 2012). Monard's comp star is from USNOA2, 14.0R, 3' NNE of GRB. * The decay rate in Monard's exposure varies from 0.191 CR/h in the beginning of the run to 0.103 CR/h at the end. Kaiser's time series data is fairly constant until about 5:40 when the OT begins to fade again. The CCD used by Oksanen plus other components of the AAVSO International GRB network were funded by a generous grant from the Curry Foundation. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2059 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/01 05:07:06 GMT FROM: Kevin Lindsay at Clemson.U K. Lindsay, D. H. Hartmann (Clemson University), M. Leake, M. Williams (Valdosta State University) Report on behalf of a larger collaboration: We observed the optical afterglow of GRB 030329, (=H2656, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the Johnson B-Band with the SARA 0.9m telescope at KPNO. We obtained 30, 300s exposures. Observations began at 02:58:24UT, and ended at 05:31:22UT, on March 31st. The obsevations were carried out under good seeing conditions. Aperture photometry is being carried out, and further observations are planned. More information on the SARA Observatory can be found at http://www.saraobservatory.org/. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2060 SUBJECT: GRB030329 - OT rebrightens DATE: 03/04/01 07:21:58 GMT FROM: Eran Ofek at Tel Aviv U. Y. Lipkin, E. M. Leibowitz, E. O. Ofek, S. Kaspi, A. Gal-Yam, H. Mendelson (Wise observatory, TAU) report: We continue our time-resolved photometry of GRB 030329. Following a brief standstill (Lipkin et al, GCN 2054), the OT decayed in brightness from March 31 20:00 to March 31 23:15, reaching a minimum of approximately R=16.9. At that time the trend reversed direction again and from 23:15 to 01:30 UT we detected a rebrightening of the OT by approximately 0.1 magnitude. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2062 SUBJECT: GRB030329 Further RBO Optical Observations DATE: 03/04/01 19:19:49 GMT FROM: Justin Schaefer at U of Wyoming S. Savage, J. Schaefer, D. Gibbs (University of Wyoming) Report on behalf of the University of Wyoming GRB response team and the FUN GRB collaboration: We observed the optical afterglow of GRB 030329, identified in Torii (GCN 1986), in the Johnson V filter with the RBO 0.6m telescope at Red Buttes Wyoming. We obtained 25, 300s exposures. Observations were undertaken between 02:26UT and 6:00UT, on March 31st. The observations were carried out under fair seeing conditions. Aperture photometry was performed and calibrated utilizing the standards reported by Henden et al., (GCN 2023). We initially measured the magnitude of the OT to be V=16.71, which faded by 0.15 mag during our observational period; however, there appeared to be a brightening. Errors were on average +/- 0.018. Further aperture photometry is being performed and observations are planned. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2063 SUBJECT: GRB 030329: KAIT optical photometry DATE: 03/04/01 22:15:33 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS Subject: GRB 030329: KAIT optical photometry Weidong Li, Ryan Chornock, Saurabh Jha, and Alexei V. Filippenko (UC Berkeley) report: We have observed the GRB 030329 afterglow (Peterson & Price, GCN 1985) with the Katzman Automatic Imaging Telescope (KAIT) on the nights of 2003 Mar 30 and 31 UT. 16 sets of UBVRI images were taken. Aperture photometry was performed on the afterglow and some local standard stars in IRAF, and the instrumental magnitudes were transformed to the standard BVRI system using the calibration provided by Henden (GCN 2023). We have also applied color corrections to the KAIT data based on well-measured color terms for the KAIT filters. Due to the lack of U-band calibrations, only BVRI images were reduced. Our R-band photometry is summarized in the table below. The errors quoted include both the IRAF aperture photometry error and the magnitude transformation error. Table: KAIT R-band observations t-t0 (hours) exptime mag err 16.5662 300.0 R 15.424 0.034 17.0989 150.0 R 15.448 0.032 17.4775 150.0 R 15.487 0.022 18.4173 150.0 R 15.618 0.028 18.7934 150.0 R 15.659 0.023 19.6814 300.0 R 15.724 0.023 20.1812 150.0 R 15.809 0.057 20.6912 150.0 R 15.825 0.016 21.0689 150.0 R 15.899 0.030 21.4514 150.0 R 15.907 0.035 21.8964 150.0 R 15.948 0.035 22.2831 150.0 R 15.965 0.037 22.6695 150.0 R 16.102 0.079 43.1320 300.0 R 16.560 0.031 44.6242 300.0 R 16.763 0.136 (observed under cloudy conditions) 45.9700 300.0 R 16.600 0.135 (observed under cloudy conditions) This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2064 SUBJECT: GRB 030329: fitting parameters and re-brightening DATE: 03/04/01 22:32:03 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS Weidong Li, Ryan Chornock, Saurabh Jha, and Alexei V. Filippenko (UC Berkeley) report: We selected from the GCN literature all available R-band measurements of the GRB 030329 afterglow. We fitted a smoothly broken power-law model (Beuermann et al. 1999, A&A 352, L26; Stanek et al. 2001, ApJ 563, 592) to the data within 24 hours of the burst, and obtained the following parameters: alpha_1 = -0.75 +/- 0.06, alpha_2 = -1.90 +/- 0.05, t_break = 0.44 +/- 0.04 days, and s = 5 +/- 2. Our fitting parameters are similar to those reported by Zeh et al. (GCN 2047) except for alpha_2 (ours is much steeper). A plot showing the fit can be found at http://astron.berkeley.edu/~bait/grb/grb030329.fit.ps while a table of GCN R-band photometry of GRB 030329 can be found at http://astron.berkeley.edu/~bait/grb/gcn030329.r.dat which includes citations for all the data points used in the plot. The substantial re-brightening reported by Lipkin et al. (GCN 2045) and Burenin et al (GCN 2046) is apparent in the plot. Applying the above fitting parameters to epochs after t = 24 hours, we found that the residual component brightened steeply starting from t = 22 hours and reached a peak of 16.8 mag at t = 40 hours, then declined gradually thereafter. Attempts to fit this component with the R-band light curve of the hypernova SN 1998bw all failed; thus the re-brightening may not be caused by a SN component. Analysis of the color of the GRB from KAIT photometry during this phase suggests the afterglow has a roughly constant color of (B-V) = 0.26 +/- 0.02 mag, (V-R) = 0.36 +/- 0.02 mag, and (V-I) = 0.78 +/- 0.02. (The data of Fitzgerald & Orosz, GCN 2056, suggests a constant (B-V) = 0.39 +/- 0.02 mag; there is an offset from the KAIT B photometry, perhaps due to a color term). The constant color during the phase of the re-brightening is additional evidence against a SN component explanation, in which significant color changes are expected when the SN rises to the maximum. Density inhomogeneities and extra energy sources are possible explanations for the re-brightening. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2065 SUBJECT: GRB 030329: Correction to GCN 2056 DATE: 03/04/01 22:48:20 GMT FROM: Jerome A. Orosz at San Diego State U J. Brodney Fitzgerald and Jerome A. Orosz (San Diego State University) report: We have a correction to GCN 2056 to report. Our tables of observations contained errors in the observation times for our March 30 data. The start times for the B filter were also listed in the tables for the V, R, and I filters. We give below the correct tables for the March 30 observations. The times for the March 31 observations are correct. We regret any inconvenience this error may have caused and thank Weidong Li for bringing this error to our attention. B data: 2003-03-30T04:39:56.10 600.000 16.263 0.008 2003-03-30T05:19:08.50 480.000 16.321 0.010 2003-03-30T06:21:03.50 480.000 16.415 0.006 2003-03-30T07:24:03.20 480.000 16.510 0.004 2003-03-30T08:01:23.30 480.000 16.577 0.004 2003-03-30T08:50:07.70 480.000 16.648 0.004 2003-03-30T09:38:09.20 480.000 16.712 0.005 2003-03-30T10:38:02.00 480.000 16.889 0.013 V data: 2003-03-30T04:50:46.60 600.000 15.8732 0.011 2003-03-30T05:27:41.40 480.000 15.9492 0.007 2003-03-30T06:29:52.70 480.000 16.0532 0.007 2003-03-30T07:34:17.30 480.000 16.1452 0.004 2003-03-30T08:10:09.80 480.000 16.1642 0.041 2003-03-30T08:58:43.00 480.000 16.2722 0.004 2003-03-30T10:07:14.90 480.000 16.3632 0.005 2003-03-30T10:49:03.60 480.000 16.4142 0.007 R data: 2003-03-30T04:13:44.60 600.000 15.402 0.006 2003-03-30T05:01:52.70 480.000 15.524 0.007 2003-03-30T06:38:59.40 480.000 15.694 0.009 2003-03-30T07:43:11.40 480.000 15.801 0.004 2003-03-30T08:18:47.30 480.000 15.841 0.005 2003-03-30T09:07:42.20 480.000 15.917 0.004 2003-03-30T10:16:32.90 480.000 16.004 0.006 2003-03-30T10:58:45.90 480.000 16.048 0.006 I data: 2003-03-30T04:29:03.70 600.000 15.0006 0.009 2003-03-30T05:10:35.20 480.000 15.1076 0.012 2003-03-30T06:47:29.70 480.000 15.2816 0.007 2003-03-30T07:52:23.00 480.000 15.3916 0.004 2003-03-30T08:27:17.40 480.000 15.4266 0.027 2003-03-30T09:16:35.30 480.000 15.5186 0.005 2003-03-30T10:26:31.30 480.000 15.6376 0.008 2003-03-30T11:07:31.20 480.000 15.7036 0.011 ------------------------------------------------------------------------- Jerome A. Orosz Assistant Professor of Astronomy, San Diego State University 5500 Campanile Drive, San Diego, CA 92182-1221 (619) 594-7118 (office), 594-6182 (dept. secretary), 594-1413 (dept. fax) http://mintaka.sdsu.edu/faculty/orosz/web/ //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2066 SUBJECT: GRB030329: further optical photometry and evidence for a light curve discontinuity DATE: 03/04/02 01:00:07 GMT FROM: Karl Glazebrook at Johns Hopkins J. Tober, E. Hoverstein, K. Chiu, K. Glazebrook We have observed the optical afterglow of GRB 030329 with the 20in Morris W. Offit telescope of the Maryland Space Grant Consortium Observatory. The telescope is located in downtown Baltimore, Maryland and the observations were made with a student built CCD camera on the night of March 31st / morning of April 1st with an R-band filter. Aperture photometry was made with APPHOT in a 20 arcsec diameter aperture with errors empirically estimated from the background noise. The photometry is computed by assuming the USNO reference star at RA 10 44 42.01 DEC +21 32 31.8 has constant magnitude R=16.2 but counts were consistent from run to run indicating near-photometric conditions. The GRB appeared to brighten suddenly between ~02:30 and ~03:30 by 0.5 mags and then fade slowly for the next few hours. Table 1. R-band Observations. Magnitudes and errors. Times (t) are in minutes from 02:33 UT on April 01, 2003 and refer to the middle of stacked sequences of ~25 minute exposures. t Star1 Star3 Star5 GRB 0 13.749 0.007 16.257 0.069 16.904 0.126 17.457 0.207 52 13.696 0.007 16.104 0.064 16.617 0.108 16.844 0.130 *** Jump ? 117 13.778 0.007 16.275 0.069 16.931 0.128 17.056 0.141 165 13.826 0.007 16.198 0.062 16.884 0.108 17.169 0.154 209 13.637 0.008 16.076 0.070 16.538 0.104 16.940 0.153 The error on the reference star was +/- 0.07 which should be added in quadrature to the above table. (Note star 1 is off the nominal R=14.00 value which we attribute to non-linearity in the CCD) This photometry is preliminary, further analysis is proceeding. The reference stars are indicated at: http://mrhanky.pha.jhu.edu/~kgb/GRB030329/grb-circ-finder.jpg A plot of the light curve is available from: http://mrhanky.pha.jhu.edu/~kgb/GRB030329/grbplot2.ps The Maryland Space Grant Consortium Observatory is supported by NASA's National Space Grant College and Fellowship Program. Further information is available at: http://henry.pha.jhu.edu/msgc/observatory.html //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2067 SUBJECT: GRB030329: Optical observations DATE: 03/04/02 01:25:34 GMT FROM: Vasilij Rumjantsev at CrAO E.Pavlenko, V.Rumyantsev, O.Antoniuk, N.Primak (CrAO) and A.Pozanenko (IKI) report: We continue to monitor the OT of GRB030329 (GCN 2005, 2028, 2050). The OT found by Peterson and Price (GCN 1985) was imaged Cassegrain 38-cm telescope of CrAO. Several 240 sec. exposures in R (Johnson) spectral band were obtained. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude as Mid Time (UT) exposure OT (R) Apr 1.8754 4x240 sec 17.07+/-0.05 Also we refined our estimations of OT within March 29-31. Cassegrain 38-cm (CCD SBIG ST-7): JD Hel UT V R 52728.2526 29.7526 - 14.03 +/- 0.03 52728.4934 29.9934 15.15 +/- 0.02 - 52728.5072 30.0072 15.22 +/- 0.04 - 52729.2689 30.7689 - 16.44 +/- 0.04 52729.4301 30.9301 - 16.40 +/- 0.06 52730.2435 31.7435 - 16.92 +/- 0.04 52730.3868 31.8868 - 16.90 +/- 0.08 52730.4023 31.9023 - 16.91 +/- 0.06 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2068 SUBJECT: GRB 030329: Observations with ANDICAM DATE: 03/04/02 01:47:33 GMT FROM: Josh Bloom at Harvard/CFA GRB 030329: Observations with ANDICAM J. S. Bloom (CfA), M. Buxton (Yale), C. Bailyn (Yale), P. G. Van Dokkum (Yale), S. R. Kulkarni (Caltech) report: "We observed the afterglow of GRB 030329 (GCN #1985, GCN #1997), using CTIO 1.3m + ANDICAM on 2003 April 1.15 UT in photometric conditions. The OT was well detected in BVIJH at the following brightness levels: UT Start, Int Time B = 17.671 +/- 0.031 tgrb - t = 2.6676 day (03:33:29, 600 sec) V = 17.263 +/- 0.043 tgrb - t = 2.6761 day (03:45:52, 600 sec) I = 16.482 +/- 0.056 tgrb - t = 2.6870 day (04:01:30, 600 sec) Optical photometry was calibrated to the Henden secondary standards (GCN #2023). Zeropoint systematics dominate the uncertainties. Magnitudes have not been corrected for Galactic extinction. We intend to obtain an IR zeropoint and IR secondary standards over the next few nights. Assuming a negligible change in flux between observations, we find (V - I) = 0.781 +/- 0.070, confirming the V-I color reported in Li et al. (GCN #2064). We find (B - V) = 0.408 +/- 0.053, which is inconsistent with Li et al, but consistent with the B-V color reported Fitzgerald & Orosz (GCN #2056)." A color composite image of the field may be viewed at: http://http://www-cfa.harvard.edu/~jbloom/GRB/grb030329/ More information about ANDICAM can be obtained at: http://www.ctio.noao.edu/yale/parameters.html This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2069 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/02 02:03:38 GMT FROM: Kevin Lindsay at Clemson.U M. Leake, M. Williams (Valdosta State University) K. Lindsay, D. H. Hartmann (Clemson University), Report on behalf of a larger collaboration: We observed the optical afterglow of GRB 030329, (=H2656, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the Johnson B-Band with the SARA 0.9m telescope at KPNO. We obtained 30, 300s exposures. Observations began at 03:06:49UT, and ended at 05:39:50UT, on April 1st. The obsevations were carried out under good seeing conditions. Aperture photometry is being carried out, and further observations are planned. More information on the SARA Observatory can be found at http://www.saraobservatory.org/. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2070 SUBJECT: GRB 030329: Additional Mt. Laguna Optical Observations DATE: 03/04/02 02:19:50 GMT FROM: Jerome A. Orosz at San Diego State U J. Brodney Fitzgerald and Jerome A. Orosz (San Diego State University) report: We report additional observations of the field of GRB 030329 (Peterson & Price, GCN 1985) made with the 1 meter telescope at SDSU's Mount Laguna Observatory. Images were taken in the Bessell B, V, R, and I filters on the night of 2003 April 1 (UT) in photometric conditions. The data were reduced and calibrated in the same manner as previously reported (GCN 2056). Our observations are summarized in the 4 tables below. The CCD images of the GRB field and some Landolt fields are available upon request to orosz@sciences.sdsu.edu. The eclipsing binary we reported on previously had a small secondary eclipse (about 0.1 mag deep) centered near 8:15 on April 1 (UT). If the orbit is circular and if no eclipses were missed between March 31 and April 1, then the orbital period would be about 2.3 days. Our GRB observations follow: Table 1: B Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-04-01T03:34:38.20 360.000 17.703 0.009 2003-04-01T04:02:57.00 300.000 17.719 0.009 2003-04-01T06:09:32.80 300.000 17.814 0.009 2003-04-01T06:35:53.40 300.000 17.831 0.010 Table 2: V Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-04-01T03:42:54.40 360.000 17.2512 0.009 2003-04-01T04:08:36.40 300.000 17.2642 0.008 2003-04-01T06:21:45.30 240.000 17.3562 0.011 2003-04-01T06:41:38.50 180.000 17.3622 0.012 2003-04-01T08:04:22.70 240.000 17.4552 0.012 2003-04-01T08:19:48.70 240.000 17.4252 0.011 2003-04-01T08:32:34.30 180.000 17.4332 0.014 2003-04-01T09:29:10.60 240.000 17.4402 0.014 2003-04-01T09:43:29.20 300.000 17.4732 0.014 2003-04-01T10:02:22.20 300.000 17.4702 0.018 2003-04-01T10:20:19.60 300.000 17.4572 0.027 Table 3: R Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-04-01T03:49:27.80 360.000 16.866 0.008 2003-04-01T04:14:10.50 300.000 16.861 0.007 2003-04-01T06:26:24.20 240.000 16.948 0.010 2003-04-01T06:45:24.30 180.000 16.970 0.011 2003-04-01T08:09:57.70 240.000 17.005 0.011 2003-04-01T08:24:45.80 180.000 17.001 0.011 2003-04-01T08:36:10.50 180.000 17.018 0.012 2003-04-01T09:34:02.60 240.000 17.061 0.013 2003-04-01T09:49:12.30 300.000 17.062 0.014 2003-04-01T10:08:02.00 300.000 17.082 0.017 2003-04-01T10:26:06.80 300.000 17.065 0.019 Table 4: I Observations: date-obs at start exptime mag err (sec) ------------------------------------------------- 2003-04-01T03:56:03.40 360.000 16.4346 0.009 2003-04-01T04:19:46.20 300.000 16.4386 0.011 2003-04-01T06:30:57.60 240.000 16.5396 0.013 2003-04-01T06:49:05.10 180.000 16.5636 0.013 2003-04-01T08:15:29.10 180.000 16.5816 0.015 2003-04-01T08:28:55.70 180.000 16.5746 0.016 2003-04-01T08:39:51.10 180.000 16.5726 0.015 2003-04-01T09:38:45.20 240.000 16.6346 0.019 2003-04-01T09:55:58.10 300.000 16.6586 0.020 2003-04-01T10:14:17.10 300.000 16.6826 0.027 2003-04-01T10:31:37.20 300.000 16.6636 0.025 ------------------------------------------------------------------------- Jerome A. Orosz Assistant Professor of Astronomy, San Diego State University 5500 Campanile Drive, San Diego, CA 92182-1221 (619) 594-7118 (office), 594-6182 (dept. secretary), 594-1413 (dept. fax) http://mintaka.sdsu.edu/faculty/orosz/web/ //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2071 SUBJECT: Further AAVSO V,B,R observations of GRB030329 DATE: 03/04/02 05:10:35 GMT FROM: AAVSO GRB Network at AAVSO A. Price & J. Mattei (AAVSO) report on behalf of the AAVSO International GRB Network: The AAVSO International GRB Network has obtained additional B, V, and R photometry of the afterglow to GRB030329 covering dates from March 29 to April 1. See notes for details, access to errors and time series data. Zsolt Kereszty, 0.25m at Corona Borealis Observatory, Hungary B = 15.43 @ 2003.03.29 21:44 B = 17.25 @ 2003.03.31 20:56 V = 14.93 @ 2003.03.29 21:44 V = 16.76 @ 2003.03.31 19:46 Rc = 14.53 @ 2003.03.29 21:44 Rc = 16.39 @ 2003.03.31 20:25 exposures: 13X60s Gilbert C. Lubcke, .28m at Wisconsin, USA Rc = 15.23 @ 2003.03.30 01:46 to Rc = 15.81 @ 2003.03.30 07:00 V = 15.56 @ 2003.03.30 01:46 to V = 16.08 @ 2003.03.30 07:00 exposures: 22X240s Josch Hambsch and Eric Broens, .4m at Mol, Belgium (VVS Werkgroep Veranderlijke Sterren) Rs = 16.47 @ 2003.03.30 19:42 to Rs = 16.40 @ 2003.03.30 21:55 V = 16.84 @ 2003.03.30 19:56 to V = 16.68 @ 2003.03.30 22:06 exposures: 15X300-600s Rs = 16.79 @ 2003.03.31 19:04 to Rs = 17.02 @ 2003.03.31 22:55 V = 17.18 @ 2003.03.31 19:22 to V = 17.26 @ 2003.03.31 22:53 exposures: 21X600s Bjorn H. Granslo, .25m at Haagaar Observatory, Norway. V = 16.8 @ 2003.03.30 20:49 exposures: 6X150s Peter Brown, 0.41m at Orson Pratt Observatory, Brigham Young University, Utah USA Rj = 15.14 @ 2003.03.30 02:32 to Rj = 16.12 @ 2003.03.30 10:34 V = 15.67 @ 2003.03.30 04:06 to V = 16.04 @ 2003.03.30 10:45 Dennis Hohman, .2m at Stone Edge Observatory, New York, USA Rs = 16.27 @ 2003.03.31 01:53 Rs = 16.35 @ 2003.03.31 02:12 Rs = 16.48 @ 2003.03.31 03:29 Rs = 16.28 @ 2003.03.31 04:31 V = 16.56 @ 2003.03.31 02:27 V = 16.75 @ 2003.03.31 03:47 V = 16.54 @ 2003.03.31 04:50 Rs = 16.72 @ 2003.04.01 01:45 V = 17.06 @ 2003.04.01 03:23 exposures: 9X180s Dr. D. T. Durig and C. G. Achee, .3m at Cordell-Lorenz Observatory, Tennessee, USA. Rc = 17.24 @ 2003.04.01 02:20 Rc = 17.24 @ 2003.04.01 02:40 Bill Aquino, 0.3m with Buffalo Astronomical Association in New York, USA V = 17.25 @ 2003.04.01 02:45 exposures: 3X300s * Rs is a filter designed by C. Schuler which follows Rc very closely. * Times are midpoints * Detailed reports (observing equipment, location, conditions, etc.) and many original FITS files available at ftp://ftp.aavso.org/grb/GRB030329 or by e-mailing aavso@aavso.org. * Lubcke, Hambsch et al., Granslo, Brown, Hohman, and Aquino used Henden et al. photometry (GCN 2023) for comparison. Kereszty used comp star A described on the finder chart by Rumyantsev et al. (GCN 2005) Durig et al. used comp star A described on the finder chart by Martini et al.(GCN 2012). * Lubcke, Hambsch et al. and Brown have time series data available. These observations bracket their datasets. The CCD used by Kereszty plus other components of the AAVSO International GRB network were funded by a generous grant from the Curry Foundation. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2072 SUBJECT: GRB030329: more 15GHz observations DATE: 03/04/02 08:54:51 GMT FROM: Guy Pooley at MRAO, Cambridge, UK The radio source associated with GRB030329 was observed at 15.2 GHz with the Ryle Telescope (cf GCN 2043) on 2003 Mar 31 - Apr 01 and Apr 01 - Apr 02. The flux density during each observation was almost constant; 2003 Mar 31.91 18 mJy 2003 Apr 01.98 16 mJy. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2073 SUBJECT: GRB 030329: Radio observations at GMRT DATE: 03/04/02 11:02:26 GMT FROM: D. Bhattacharya at Raman Research Inst. A. Pramesh Rao and C. H. Ishwara Chandra (National Centre for Radio Astrophysics, Pune, India), and D. Bhattacharya (Raman Research Institute, Bangalore, India) report on behalf of a larger collaboration: The GRB030329 was observed with the Giant Metrewave Radio Telescope (Khodad, India) for 8 hours on 31 March and for 5 hours on 01 April 2003. The observations were at 1288 MHz with a bandwidth of 8MHz and angular resolution of ~3.5". There was a detection of emission at the position of the GRB as shown below Date Time Flux Density rms noise 31 March 2003 14-22 UT 245 microJy 35 microJy 01 April 2003 18-22 UT 235 microJy 40 microJy It is at present unclear whether the detected flux is due to the burst or due to a background source that may or may not be associated with the burst. A GMRT map of the field can be seen in http://www.ncra.tifr.res.in/~pramesh/images/grb030329.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2074 SUBJECT: GRB030329: Optical observations at Teramo DATE: 03/04/02 16:58:34 GMT FROM: Elisabetta Maiorano at U.of Bologna,Italy M. Cantiello, M. Dolci (INAF - Obs. of Teramo), E. Maiorano (Univ. Bologna & IASF/CNR, Bologna), N. Masetti, E. Palazzi (IASF/CNR, Bologna), E. Brocato (INAF - Obs. of Teramo) report: "We have obtained BVRI images of the OT (Peterson & Price, GCN 1985) of GRB030329 (Vanderspek et al., GCN 1997) with the 0.72-m TNT telescope of the Astronomical Observatory of Teramo (Italy). The average seeing was 4 arcsec. The OT was well detected in all bands; we measure for it the following BVRI magnitudes using field stars calibrated by Henden (GCN 2023): mid-exposure exptime filter mag err time (UT) (s) ------------------------------------------------------- Apr. 1.824 1200 R 17.02 0.02 Apr. 1.911 1800 V 17.53 0.03 Apr. 1.966 2400 B 18.01 0.04 Apr. 1.989 1200 I 16.70 0.03 Apr. 2.055 1200 R 17.16 0.03 The comparison between the two R-band magnitude measurements shows that the OT has possibly faded across our observing run. This message is citeable." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2075 SUBJECT: GRB 030329 , SPM optical observations DATE: 03/04/02 23:08:34 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov (OAN SPM, IA UNAM, Mexico), E. Benitez, J. Torrealba, J. Stepanian (IA UNAM, Mexico) report: We have observed the GRB030329 OT with 1.5m and 2.1m telescopes of SPM Observatory, BC, Mexico. A set of exposures in UBVRI Bessel filters was obtained with 1.5m telescope under photometric conditions. Standard stars RU 149 from Landolt's catalogue were used for photometric calibrations. The results of photometry are following: 31 March U B V R I UT 7:00 16.62 UT 7:13 17.27 UT 7.16 16.90 UT 7:21 16.46 UT 7:26 16.11 UT 7:31 16:65 UT 7:37 17.28 UT 7:43 16.84 UT 7:49 16.08 UT 7:54 16.05 UT 8:48 16.58 UT 8:54 17.30 UT 8:59 16.92 UT 9:05 16.51 UT 9:11 16.11 UT10:08 16:59 UT10:13 17.27 UT10:19 16.83 UT10:60 16:60 UT10:31 16:22 Errors are about 0.03. Spectrum of the optical afterglow of GRB 030329 were obtained at the same night with the 2.1-m telescope and B&Ch spectrograph (600l/mm). The spectra cover the wavelength range of 6100 to 8200 AA with a resolution of about 2.2A/pix. The spectral data analysis is in progress. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2077 SUBJECT: GRB 030329, BRI photometry DATE: 03/04/03 00:39:01 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (Ulugh Beg Astronomical Institute of Uzbekistam Academy of Science), A.Pozanenko (IKI), V.Rumyantsev (on behalf of CrAO GRB team), G.Beskin (SAO) report: We have observed the OT found by Peterson and Price (GCN 1985) of GRB030329 with 1.5m telescope of High-altitude Observatory at Mt.Maidanak. The telescope is equipped with CCD SITe (2000x800). The observations were carried out under good seeing conditions (1".0). Several BRI Bessel images were obtained in April, 1. Based on star filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude: UT, Apr 1 filter exposure mag err 18:42:24 R 300 17.082 0.021 18:48:06 R 300 17.036 0.025 18:53:48 B 600 17.707 0.072 19:04:35 R 300 16.977 0.044 19:10:09 R 600 17.016 0.027 19:20:52 I 600 16.625 0.047 19:31:41 R 600 17.045 0.047 19:44:55 R 600 17.010 0.033 19:56:01 B 600 17.766 0.031 20:14:49 B 300 17.777 0.013 20:20:28 R 300 17.022 0.011 20:26:26 I 300 16.520 0.013 20:32:10 B 300 17.799 0.015 20:37:58 R 300 17.030 0.011 20:43:39 I 300 16.531 0.013 20:52:03 B 600 17.741 0.029 21:02:42 R 300 17.006 0.023 The estimation is preliminary and may be improved. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2078 SUBJECT: GRB030329: multiple re-brightening phases DATE: 03/04/03 08:56:27 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS Weidong Li, Ryan Chornock, Saurabh Jha, and Alexei V. Filippenko (UC Berkeley) report: We collected the available R-band measurements of the GRB 030329 afterglow through GCN 2077 and a table is available at http://astron.berkeley.edu/~bait/grb/gcn030329.r.dat We found that the afterglow went through at least three re-brightening phases. A figure illustrating this can be found at http://astron.berkeley.edu/~bait/grb/grb030329.p3.ps The first re-brightening, as reported by Lipkin et al. (GCN 2045) and Burenin et al (GCN 2046), occurred at about 30 hours after the burst. The second re-brightening, as reported by Lipkin et al. (GCN 2060), occurred at about 60 hours after the burst. A third re-brightening occurred at about 80 hours after the burst. The afterglow appears to decline with a power law after each re-brightening. The following power-law indices are measured for the three dashed lines in our plot: t = 16 to 30 hours: alpha = -1.70 +/- 0.04 t = 40 to 60 hours: alpha = -1.63 +/- 0.07 t = 64 to 70 hours: alpha = -2.09 +/- 0.26 A preliminary analysis of the data reported in GCN Circulars suggests that the afterglow shows the same behavior in the other bands (BVI) as well, though the re-brightening episodes were less constrained than in the R band. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2079 SUBJECT: GRB 030329: optical observations DATE: 03/04/03 10:28:40 GMT FROM: Rodion Burenin at IKI, Moscow R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, I. Khamitov, M. Parmaksizoglu (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: We observed the GRB 030329 afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe, in BVRI Bessel filters. Assuming that the magnitude of "A" star is R=16.20, we measured R=17.94 for UT= April 3.05 (109.5 hours after the burst). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2080 SUBJECT: GRB030329: optical observations at Tokyo Tech DATE: 03/04/03 11:56:51 GMT FROM: Nobuyuki Kawai at Tokyo Tech R. Sato, Y. Yatsu, M. Suzuki, and N. Kawai (Tokyo Tech) report: We have observed the afterglow (Peterson and Price GCN 1985, Torii GCN 1986) of GRB030229 (H2652, Vanderspek et al. GCN 1997) on the nights of 2003 Apr 29, 30, and 31 at Tokyo Tech, Tokyo, Japan, using a 30 cm SC telescope with unfiltered AP 6E CCD camera. The observationl started at 12:57 UT (80 min after the GRB trigger). We have estimated the R magnitude using USNO 2.0 stars U1050_06349885 (R=13.2), B:U1050_06348771 (R=14.2), and C:U1050_06351075 (R=14.0). The results are shown in the table below. The dip and rebrightening at t0+1.2d (Lipkin et al. GCN 2045) was detected in our data too. t-t0 (days) R mag err 0.0620 12.552 0.023 0.1484 13.370 0.029 0.1943 13.604 0.034 0.2373 13.799 0.043 0.2970 14.145 0.074 0.9457 15.987 0.127 1.0151 16.167 0.081 1.0936 16.504 0.125 1.2172 16.316 0.140 2.0050 17.087 0.212 2.1238 17.148 0.207 The images on the first night and our light curve can be found at http://www.hp.phys.titech.ac.jp/nkawai/030329/index_e.html. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2081 SUBJECT: GRB 030329, light curve and SN prediction DATE: 03/04/03 14:10:56 GMT FROM: Sylvio Klose at TLS Tautenburg A. Zeh, S. Klose (Thueringer Landessternwarte Tautenburg), J. Greiner (MPE Garching), report: Using the light curves of SN 1998bw (Galama et al. 1998, Nature 395, 670) as a template we have analyzed what color changes are expected to be seen in the optical transient following GRB 030329 if a supernova component would appear. Ingredients: ------------ 1) SN 1998bw: - A_V = 0.20 mag (Woosley, Eastman, & Schmidt 1999, ApJ 516, 792) - no time delay between the onset of the SN and the onset of the GRB - A_V(host) = 0.0 mag 2) The host galaxy: - z = 0.1685 (Greiner et al. 2003, GCN 2020) - a negligible host flux in BVRI (based on R>22.5; Blake & Bloom 2003, GCN 2011) - A_V(Galaxy) at (l, b) = 217.07, b = 60.68: E(B-V) = 0.025 (Schlegel, Finkbeiner, & Davis 1998, ApJ 500, 525), - R_V = 3.1 3) The GRB afterglow: - Considering published GCN R-band data, analyzed according to Beuermann et al. (1999, A&A 352, L26), we find: alpha_1 = 0.85 +/- 0.04 alpha_2 = 1.55 +/- 0.02 t_break = 0.42 +/- 0.03 days, after ignoring the several re-brightenings during the last days - colors (best fit): B-V = 0.39 mag V-R = 0.34 mag R-I = 0.47 mag - we have taken into account the latest re-brightening episode and assumed that a) alpha_2 remains constant and b) the color of the afterglow does not change Output cocktail: ---------------- - Fig. 1: the light curve - Fig. 2: the expected color evolution We note that differences in the reported value for alpha_2 (cf. Li et al. 2003, GCN 2078) can be explained by slightly different selection criteria for the data chosen to perform the numerical fit. http://www.tls-tautenburg.de/research/klose/grb.html Warning: -------- These results are based on a simple toy model. They provide only a hint about what the strength of the SN signal could be since most SN bumps found so far had a brightness of only 30-80% of SN 1998bw. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2082 SUBJECT: GRB030329, new UBVRcIc field photometry DATE: 03/04/03 16:39:38 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO) reports on behalf of the USNO GRB team: We have acquired additional UBVRcIc all-sky photometry for an 11x11 arcmin field centered at the coordinates of the optical transient (Peterson and Price, GCN 1985) for the HETE burst GRB030329 (GCN 1997) with the USNOFS 1.0-m telescope. Stars brighter than V=13.5 are saturated and should be used with care. We have replaced the photometric data with the same file name on our anonymous ftp site: ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb030329.dat The astrometry in this file is based on linear plate solutions with respect to UCAC2. The external errors are less than 100mas. The second night of photometry shows that the first night was acceptable, and that the external error is now about 0.02mag. For those of you not used to doing high-accuracy photometry, here are some comments. Star "A" of Martini et al. (GCN2012) has been used with either its USNO-A magnitude of R=16.2, or the more correct Rc=16.06, in various GCNs. This will lead to confusion when trying to fit light curves. However, the larger problem is that this star is red (B-V=1.19, V-I=1.41), while the afterglow itself is blue (B-V=0.35, V-I=0.77). Using this star as a comparison and following it over a large airmass will generally lead to fading/brightening trends that correlate with airmass due to differential color corrections unless proper transformations are made. This will be even more apparent when comparing Johnson R,I magnitudes with the Cousins Rc,Ic values reported here. You should also be aware of the nice eclipsing binary discovered by Fitzgerald and Orosz (GCN 2056), as this is the brightest object near the afterglow and might be used when performing early-time photometry or U-band photometry. Finally, as several observers have mentioned, there are not many real stars in this field; most of the objects are extended. You should look at the good-seeing finding charts that have been posted before selecting comparison stars, especially as the afterglow fades. Many extended objects are near-enough to stellar that they will appear in our field photometry file. We intend to extend this file with more nights and to fainter magnitudes as the afterglow fades. 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: 2083 SUBJECT: GRB030329, optical observation DATE: 03/04/03 18:22:36 GMT FROM: Alexei Pozanenko at IKI, Moscow E.Pavlenko, V.Rumyantsev, O.Antoniuk, N.Primak (CrAO) and A.Pozanenko (IKI) report: We continue to monitor the OT of GRB030329 (see also GCN 2005, 2028, 2050, 2067). The OT found by Peterson and Price (GCN 1985) was imaged Cassegrain 38-cm telescope of CrAO. Several 300 sec. exposures in R (Johnson) spectral band were obtained during Apr. 2. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude: Mid time exposure R (UT) 2.7648 5x300c 17.83 +/- 0.08 2.7929 5x300c 17.76 +/- 0.08 2.8436 5x300c 17.89 +/- 0.07 2.8739 5x300c 17.76 +/- 0.09 After steep decay between Apr 1. and Apr. 2 we observed a flattening of light curve which may be a start of new episode of re-brightening. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2084 SUBJECT: GRB030329, optical observation DATE: 03/04/03 18:43:00 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (Ulugh Beg Astronomical Institute of Uzbekistam Academy of Science), A.Pozanenko (IKI), V.Rumyantsev (on behalf of CrAO GRB team), G.Beskin (SAO) report: We have observed the OT found by Peterson and Price (GCN 1985) of GRB030329 with 1.5m telescope of High-altitude Observatory at Mt.Maidanak. The observation is carrying under good seeing conditions. Using star filed photometry by A. Henden (GCN2023) we obtained a prelimiary estimation of the OT magnitude: UT, Apr. 3 filter exposure mag Mid time 15:34:12 R 300 17.80 15:42:58 R 600 17.84 with a typical error ~ 0.05 Taking into account the data of R. Burenin et al. (GCN 2079) and E.Pavlenko et al. (GCN 2083) one can suggest that the re-brightening took place with a maximum early Apr. 3. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2085 SUBJECT: OT GRB light curves and SN predictions DATE: 03/04/03 18:59:04 GMT FROM: Vladimir Sokolov at SAO RAS V. Sokolov (SAO RAS) reports: A similar phenomenon of the OT reddening in a later phase of light curve, that was predicted in GCN#2081 (A. Zeh, S. Klose, J. Greiner) for OT GRB 030329 in 20-30 days after GRB, was already observed for OT GRB 970508 (Sokolov, Zharikov, Baryshev et al. 1999, A&A, 344, 43; Sokolov, astro-ph/0102492). Though then the object was much weaker than now (for the OT GRB 030329). But the peak magnitudes of Type Ib/c (or core collapse) SNe are not constant: M_B is from -16 to -20.5 (Richardson et al. 2002, AJ, 123, 745). The duration of maximum (or "red shoulder") in the light curve can be both similar to one of SN 1998bw, and longer, such as for the peculiar Type Ic SN 1997ef with lower luminosity (Iwamoto, Nakamura, Nomoto, Mazzali et al. 2000, astro-ph/9807060). So, it is crucially important to continue observing the light curve of this unique bright object OT GRB 030329 FURTHER in ALL possible (UBVRcIc) photometric bands not to miss the predicted (strong or weak) effect of the OT reddening in 20-30 days. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2086 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/03 21:00:35 GMT FROM: Kevin Lindsay at Clemson.U M. Leake, M. Williams (Valdosta State University) K. Lindsay, D. H. Hartmann (Clemson University), Report on behalf of a larger collaboration: We observed the optical afterglow of GRB 030329, (=H2656, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the Johnson B-Band with the SARA 0.9m telescope at KPNO. We obtained 30, 300s exposures. Observations began at 03:30:39UT, and ended at 06:15:07UT, on April 2nd. The obsevations were carried out under partial cloud cover and relatively windy conditions. Aperture photometry is being carried out, and further observations are planned. More information on the SARA Observatory can be found at http://www.saraobservatory.org/. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2087 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/03 21:16:43 GMT FROM: Kevin Lindsay at Clemson.U K. Lindsay (Clemson University) Report on behalf of a larger collaboration: We observed the optical afterglow of GRB 030329, (=H2656, Vanderspek et al. GCN 1997), identified by Peterson & Price (GCN 1985) and Torii (GCN 1986), in the Johnson B-Band with the SARA 0.9m telescope at KPNO. We obtained 28, 300s exposures. Observations began at 02:56:23UT, and ended at 05:16:54UT, on April 3rd. The obsevations were carried out under relatively windy conditions. Aperture photometry is being carried out, and further observations are planned. We thank SARA observer Dr. Scott Shaw for making part of his observing time available to us. More information on the SARA Observatory can be found at http://www.saraobservatory.org/. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2088 SUBJECT: GRB 030329: Sub-millimeter detection DATE: 03/04/04 04:33:29 GMT FROM: Ian Smith at Rice U Jim C. Hoge (JCMT), Rowin Meijerink (Leiden Observatory), Remo P.J. Tilanus (JCMT), and Ian A. Smith (Rice University) report on behalf of the NL JCMT collaboration: We have observed the afterglow of GRB 030329 (GCN 1985 and following) using the SCUBA sub-millimeter continuum bolometer array on the James Clerk Maxwell Telescope located on Mauna Kea, Hawaii. The observations took place on 2003 Apr 03.4 UT. Although the conditions were not very good, the source was easily detected. Preliminary calibration gives an 850 micron flux density of 30 +/- 5 mJy. Further observations are planned. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2089 SUBJECT: GRB030329 Radio 23/43/90 GHz observations at Nobeyama DATE: 03/04/04 11:04:15 GMT FROM: Nobuyuki Kawai at Tokyo Tech N. Kuno, N. Sato, and H. Nakanishi(NRO) report: We have observed the radio afterglow (GCN 2014, 2043) of GRB 030329 (GCN 1997) with the Nobeyama 45 m radio telescope, Japan from 2003 Apr 3 11:03 UT to 17:00 UT. The mean flux densities are: 23 GHz