////////////////////////////////////////////////////////////////////// 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. Esteban (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. [GCN OPS NOTE(11jan13): Per author's request, "Estaban" was changed to "Esteban".] //////////////////////////////////////////////////////////////////////// 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 32.2 +- 0.9 mJy 43 GHz 53.9 +- 2.9 mJy 90 GHz 80.4 +- 5.6 mJy We will continue monitoring if the weather condition permits. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2090 SUBJECT: GRB030329 - more 15 GHz radio data DATE: 03/04/04 11:20:41 GMT FROM: Guy Pooley at MRAO, Cambridge, UK Two further 15.2-GHz observations of GRB030329 with the Ryle Telescope yield the following flux densities: 2003 Apr 03.07 20 mJy 2003 Apr 04.11 28 mJy //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2091 SUBJECT: GRB030329: final R-band light curve by MASTER DATE: 03/04/04 13:41:38 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 by MASTER system (Lipunov et al., GCN 2002, GCN 2035). Here we represent pre-final light curve of the OT. We used more than 200 direct images to obtain field photometry. Several groups of images were summarized to achieve better S/N ratio and smaller uncertanities of measurements. As the final result, we represent 64 points. Magnitude calibration was made according to the data, presented in GCN 2023 (A. Henden). 4 stars were used to do the calibration. Big uncertanities of magnitude measurements are caused by weather conditions. First points were made just after sunset on the blue sky, last points were made through cirruses near the horizont. From these data we obtained new power law flux decreasing during 8 hours of observations (t-t0 from 5.2h to 13.5h): F ~ t^(-alpha), alpha=1.22+-0.03 Rmag = 15.8 + 1.2*2.5*log(age in days) New light curve plots available at old locations: http://observ.pereplet.ru/images/GRB030329_R_lc.gif http://www.sai.msu.su/~chil/GRB030329_R_lc.ps date UT t-t0,hrs R errR 03/29/2003 16:51:49 5.24691 13.744 0.417 03/29/2003 16:54:27 5.29080 13.934 0.409 03/29/2003 17:02:12 5.41997 13.702 0.226 03/29/2003 17:07:36 5.50997 14.012 0.211 03/29/2003 17:12:04 5.58441 13.708 0.164 03/29/2003 17:14:29 5.62469 13.854 0.151 03/29/2003 17:19:18 5.70497 13.983 0.097 03/29/2003 17:34:11 5.95302 14.118 0.172 03/29/2003 17:36:19 5.98858 13.908 0.103 03/29/2003 17:40:01 6.05024 13.972 0.101 03/29/2003 17:42:44 6.09552 14.043 0.079 03/29/2003 17:46:24 6.15663 14.004 0.081 03/29/2003 17:49:09 6.20247 14.007 0.078 03/29/2003 17:52:18 6.25497 13.971 0.083 03/29/2003 17:55:22 6.30608 13.943 0.073 03/29/2003 17:59:49 6.38024 14.092 0.085 03/29/2003 18:11:56 6.58219 14.007 0.125 03/29/2003 18:21:10 6.73608 14.126 0.111 03/29/2003 18:40:45 7.06247 14.180 0.083 03/29/2003 18:43:29 7.10802 14.145 0.085 03/29/2003 18:46:06 7.15163 14.090 0.083 03/29/2003 18:48:46 7.19608 14.169 0.085 03/29/2003 18:51:23 7.23969 14.147 0.087 03/29/2003 18:54:06 7.28497 14.128 0.085 03/29/2003 18:56:48 7.32997 14.254 0.088 03/29/2003 18:59:29 7.37469 14.175 0.084 03/29/2003 19:02:06 7.41830 14.231 0.089 03/29/2003 19:04:48 7.46330 14.141 0.080 03/29/2003 19:07:29 7.50802 14.325 0.098 03/29/2003 19:12:54 7.59830 14.216 0.101 03/29/2003 19:15:32 7.64219 14.261 0.098 03/29/2003 19:18:10 7.68608 14.070 0.088 03/29/2003 19:21:27 7.74080 14.168 0.121 03/29/2003 19:52:30 8.25830 14.395 0.108 03/29/2003 19:55:12 8.30330 14.375 0.105 03/29/2003 19:58:05 8.35136 14.450 0.101 03/29/2003 20:00:50 8.39719 14.431 0.110 03/29/2003 20:03:42 8.44497 14.336 0.094 03/29/2003 20:08:30 8.52497 14.499 0.097 03/29/2003 20:11:15 8.57080 14.318 0.100 03/29/2003 20:14:05 8.61802 14.463 0.100 03/29/2003 20:16:50 8.66386 14.324 0.093 03/29/2003 20:19:28 8.70774 14.432 0.099 03/29/2003 20:24:45 8.79580 14.440 0.061 03/29/2003 20:36:35 8.99302 14.541 0.075 03/29/2003 20:41:20 9.07219 14.515 0.075 03/29/2003 20:45:58 9.14941 14.437 0.074 03/29/2003 20:51:17 9.23802 14.514 0.080 03/29/2003 20:56:44 9.32886 14.644 0.092 03/29/2003 21:01:30 9.40830 14.578 0.092 03/29/2003 21:07:22 9.50608 14.458 0.087 03/29/2003 21:17:37 9.67691 14.557 0.079 03/29/2003 21:28:18 9.85497 14.604 0.079 03/29/2003 21:39:07 10.03524 14.740 0.078 03/29/2003 21:49:59 10.21636 14.616 0.065 03/29/2003 22:03:48 10.44663 14.698 0.070 03/29/2003 22:16:04 10.65108 14.493 0.068 03/29/2003 22:26:44 10.82886 14.719 0.080 03/29/2003 22:41:42 11.07830 14.632 0.089 03/29/2003 23:03:55 11.44858 14.854 0.113 03/29/2003 23:35:46 11.97941 14.905 0.117 03/30/2003 00:04:04 12.45108 14.859 0.090 03/30/2003 00:23:25 12.77358 14.837 0.129 03/30/2003 00:52:04 13.25108 15.064 0.162 03/30/2003 01:12:16 13.58774 15.002 0.161 03/30/2003 01:35:52 13.98108 15.594 0.413 We thank Sergey M. Bodrov (general director of optical company "Ochkarik") for financial and equipment support of MASTER research project. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2092 SUBJECT: GRB030329, cessation of fading DATE: 03/04/04 15:07:27 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO), B. Canzian (USNO), H. Harris (USNO) and T. Tilleman (USNO) report on behalf of the USNO GRB team: We have acquired time-series UBVRcIc photometry of the optical transient (Peterson and Price, GCN 1985) for the HETE burst GRB030329 (GCN 1997) with the USNOFS 1.0m and 1.3m telescopes on all nights since the burst. Photometric accuracy has been typically 0.01-0.02mag in all colors (nice to have a bright OT!). On the last two nights, 030403 and 030404 UT, the transient has ceased fading, with mean magnitude on 030403 of V=18.16 and on 030404 of V=18.13. This unusual behavior may be the beginning of the supernova bump predicted by Zeh et al. (GCN 2081), though there has not been strong color evolution. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2093 SUBJECT: GRB 030329, nearby galaxies DATE: 03/04/04 23:20:33 GMT FROM: Peter Garnavich at U of Notre Dame K. Krisciunas (OCIW/CTIO), T. Matheson, K.Z. Stanek (CfA), and P. Garnavich (Notre Dame) We obtained spectra of four bright galaxies within 90 arcseconds of the afterglow of GRB 030329 using the Magellan 6.5-m Clay telescope and LDSS2 image/spectrograph. The data were taken April 2 and 3 (UT). Emission lines of Halpha, [OIII] and [OII] were detected in all four galaxies and their redshifts are: Galaxy RA (2000) Dec Sep. from GRB z A 10:44:50.5 +21:32:05 47" 0.136 B 10:44:48.7 +21:31:39 28" 0.136 C 10:44:47.9 +21:31:04 33" 0.137 D 10:44:53.6 +21:30:11 84" 0.057 The three observed galaxies closest to the burst appear to form a small group at z=0.136 which is slightly foreground to the host at z=0.168 (Greiner et al., GCN 2020; Caldwell et al. GCN 2053). A finder chart for these galaxies can be found at: http://www.nd.edu/~pgarnavi/grb030329_galaxies.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2094 SUBJECT: GRB 030329, Optical observations DATE: 03/04/05 00:11:28 GMT FROM: Irek Khamitov at TUG I. Khamitov, Z. Aslan, O.Golbasi, M.Parmaksizoglu (TUG) I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko (IKI); U. Kiziloglu, A. Alpar, A. Baykal (METU); 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. Star "A" has been used with magnitude Rc=16.06 (Henden, GCN 2082). We have measured the following magnitudes: t-t0,hours UT R Rerr 150.3 April 4.73 18.06 0.04 Afterglow continues to be bright. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2095 SUBJECT: SDSS 0.5m PT observations of GRB030329 DATE: 03/04/05 01:02:21 GMT FROM: Brian Lee at LBL B. C. Lee, D. Q. Lamb, D. L. Tucker and S. Kent on behalf of the SDSS GRB team, report: The optical transient associated with GRB 030329 (Peterson and Price, GCN 1985; K. Torii, GCN 1986) was observed with the SDSS 0.5m "Photometric Telescope" (PT) at two epochs, starting March 31.181 UT and April 01.153 UT. The preliminary r-band magnitude at March 31.181 UT was observed to be 16.60 +/- 0.02, and the u g r i z data on that date is well fit by a flux power law of approximately nu^-0.94, or nu^-1.0 if a reddening of E(B-V)=0.025 is applied (Bloom, GCN 2011 and Schlegel et al. 1998). The April 01 UT images are still being processed. Our ugriz photmetric catalog of other objects in the field will be made available upon request; please email bclee@lbl.gov or visit the follwing web page: http://supernova.lbl.gov/~bclee/grb/ This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2096 SUBJECT: SDSS 0.5m PT observations of GRB030329 (correction) DATE: 03/04/05 01:23:33 GMT FROM: Brian Lee at LBL B. C. Lee, D. Q. Lamb, D. L. Tucker and S. Kent on behalf of the SDSS GRB team, report: The optical transient associated with GRB 030329 (Peterson and Price, GCN 1985; K. Torii, GCN 1986) was observed with the SDSS 0.5m "Photometric Telescope" (PT) at two epochs, starting March 31.181 UT and April 01.153 UT. The preliminary r-band magnitude at March 31.181 UT was observed to be 16.60 +/- 0.02, and the u g r i z data on that date is well fit by a flux power law of approximately nu^-0.94, or nu^-0.85 if a reddening of E(B-V)=0.025 is applied (Bloom, GCN 2011 and Schlegel et al. 1998). The April 01 UT images are still being processed. Our ugriz photmetric catalog of other objects in the field will be made available upon request; please email bclee@lbl.gov or visit the follwing web page: http://supernova.lbl.gov/~bclee/grb/ This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2097 SUBJECT: GRB030329: Optical observations DATE: 03/04/05 01:39:57 GMT FROM: Vasilij Rumjantsev at CrAO E.Pavlenko, V.Rumyantsev, O.Antoniuk, N.Primak (CrAO) and A.Pozanenko (IKI) report: The OT found by Peterson and Price (GCN 1985) was imaged Cassegrain 38-cm telescope of CrAO. Several 300 sec. exposures in R (Johnson) obtained during Apr. 4. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude: Mid time exposure R (UT) Apr 4.7686 4x300c 18.12 +/-0.11 4.8236 5x300Ó 18.32 +/-0.10 4.8412 5x300c 18.04 +/-0.07 After nearly flat period between end of 030402 and end of 030403 (GCN 2083,2084,2092) the OT definitely start a new fading phase. A power-law index between Apr 3.8160 and Apr 4.8049 can be estimated as alpha ~1.7 A 10x180 sec. exposure image obtained on April 04.8012 can be found in http://grb.rssi.ru/GRB030329/030329_030404_at64.gif This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2098 SUBJECT: GRB 030329, BVRI photometry DATE: 03/04/05 02:50:20 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 (CrAO), G.Beskin (SAO) on behalf of large collaboration 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. Several BVRI Bessel images were obtained on April, 3. Based on star filed photometry by A. Henden (GCN 2023) we refined the estimation reported in GCN 2084 and report new measurements: UT, Apr 3 filter exposure, s mag err 15:31:56 R 300 17.842 0.018 15:38:12 R 600 17.853 0.013 18:40:49 R 600 17.787 0.027 18:52:27 R 600 17.830 0.015 19:03:13 R 600 17.766 0.013 19:14:07 B 600 18.483 0.015 19:25:11 V 600 18.126 0.015 19:35:55 R 600 17.832 0.014 19:46:45 I 600 17.299 0.020 19:58:36 B 600 18.577 0.018 20:09:46 V 600 18.109 0.016 20:20:26 R 600 17.801 0.014 20:31:14 I 600 17.333 0.023 20:41:54 R 600 17.805 0.018 20:52:38 R 600 17.806 0.014 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2099 SUBJECT: GRB030329, fading resumes DATE: 03/04/05 15:55:16 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO) reports on behalf of the USNO GRB team: We previously reported (GCN 2092) a cessation of fading. As Pavlenko et al. (GCN 2097) recently reported, this standstill has ended. Our data from last night (030405UT) indicates a typical V magnitude of 18.7 and the light curve now fits on the power law from nights prior to the standstill. The standstill was approximately 0.4mag deviant from the power law, the one of the largest bumps so far for this afterglow. Due to the shortness of the standstill and the lack of color evolution, this was not likely to have been the predicted SNe bump. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2100 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/05 18:45:06 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 02:42:47UT, and ended at 05:13:30UT, on April 4th. The obsevations were carried out under good seeing 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: 2101 SUBJECT: GRB 030329: SARA Optical Observations DATE: 03/04/05 19:01:07 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 30, 300s exposures. Observations began at 03:03:38UT, and ended at 05:32:40UT, on April 5th. The obsevations were carried out under good seeing conditions. Aperture photometry is being carried out, and further observations are planned. We thank SARA Observatory director Dr. Jim Webb, and FIU graduate student Emily Howard for making part of their 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: 2102 SUBJECT: GRB 030329: BV photographic observations DATE: 03/04/06 02:18:40 GMT FROM: V.G.Metlov at Moscow State U V.Metlov (Crimean Laboratory of the Sternberg Astronomical Institute, Moscow State University) report: I have made photographic observations of the GRB030329 OT found by B.A.Peterson and P.A.Price (GCN 1985) with 50-cm Maksutov telescope in Crimea. Exposures: 60 minutes and 50 minutes in B and V filters accordingly. Based on filed photometry presented in GCN 2023 by A.Henden (12 stars were used to do the calibration) I estimate the OT magnitudes: UT, Apr 2 filter mag err 19:33:00 - 20:33:00 B 18.15 0.15 20:45:00 - 21:35:00 V 18.10 0.25 This message may be cited. Yours sincerely, V.G.Metlov [GCN OPS NOTE (05apr03): This circular was delayed 35 hours due to no entry in the valid list.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2104 SUBJECT: GRB030329: More AAVSO VR obs DATE: 03/04/06 19:40:40 GMT FROM: AAVSO GRB Network at AAVSO A. Price, B. Monard, A. Oksanen, T. DiLapo, D. West, D. Kaiser, D. Starkey, P. Nelson, P. Pääkkönen and J. Mattei (AAVSO); T. Durig, A. L. Seifert, C. B. Norton, G.F. Garland, J.K.Cole, J.B. Cherry (University of the South); A. Henden (USRA/USNO) report on behalf of the AAVSO International GRB Network: This is a 3rd set of observations of the OT found by Peterson and Price (GCN 1985) dating from March 29th to April 6th. Included in the observations is a URL where a full report (equipment, seeing, etc.) is available. Many times the original FITS image is also available. When time series data is available we only put the first and last observation. A light curve of all AAVSO data to date has been made by B. Gary and posted at http://www.aavso.org/grb/grb030329.jpg Bruce L. Gary, .25m at Arizona, USA. Rc = 15.67 +/- 0.04 @ 2003.03.30 07:08 to Rc = 16.82 +/- 0.04 @ 2003.03.30 04:26 V = 15.89 +/- 0.06 @ 2003.03.30 07:16 to V = 16.13 +/- 0.04 @ 2003.04.01 08:38 Rc = 18.07 +/- 0.05 @ 2003.04.05 03:49 Rc = 18.78 +/- 0.12 @ 2003.04.06 03:50 exposures:64X15s,70X30s(for last obs) ftp://ftp.aavso.org/grb/GRB030329/BruceL.Gary_GRB030329_2452731.81361_.txt Arto Oksanen, .4m at Nyrola Observatory, Finland. Rc = 16.714 merr: 0.051 @ 2003.03.31 19:09 to Rc = 16.842 merr: 0.060 @ 2003.04.01 00:59 V = 17.157 merr: 0.053 @ 2003.03.31 19:48 to V = 17.297 merr: 0.077 @ 2003.04.01 00:55 Rc = 18.59 merr: 0.04 # 2003.04.05 21:35 exposures: 78x240s, 34x240s (last obs) ftp://ftp.aavso.org/grb/GRB030329/arto-030329-2nreport.txt http://nyrola.jklsirius.fi/grb/grb030329/ Tristan DiLapo, .31m at Orbit Jet Observatory, New York, USA. Rc = 16.32 err: 0.06 @ 2003.03.31 02:56 to Rc = 16.34 err: 0.06 @ 2003.03.31 04:02 exposures: 10X120s ftp://ftp.aavso.org/grb/GRB030329/TristanDiLapo_GRB030329_2452732.28043_.txt Doug West, .2m at West Skies Observatory, Kansas, USA. Unfiltered = 17.2 +/- 0.14 2003.04.02 02:08 7*30s exposures Unfiltered = 17.5 +/- 0.13 2003.04.04 02:09 14*35s exposures Unfiltered = 18.3 +/- 0.20 2003.04.05 02:11 19X35s exposures exposures: 7X30s ftp://ftp.aavso.org/grb/GRB030329/west-grb030329.txt Dan Kaiser, .35m at Crescent Moon Observatory, Indiana, USA. Rc = 17.44 @ 2003.04.02 02:13 exposures: 14X240s ftp://ftp.aavso.org/grb/GRB030329/kaiser-grb030329.txt D. T. Durig, A. L. Seifert, C. B. Norton, G.F. Garland, J.K.Cole, J.B. Cherry, .3m at Cordell-Lorenz Observatory, Tennessee, USA Rc = 17.96 @ 2003.04.02 02:36 Rc = 18.06 @ 2003.04.02 03:38 Rc = 18.36 +/- 0.2 @ 2003.04.03 03:45 Rc = 18.46 +/- 0.2 @ 2003.04.03 03:59 exposures: 4X600s ftp://ftp.aavso.org/grb/GRB030329/DrDouglasT.Durig_GRB030329_2452732.69648_.txt Donn Starkey, .36m at DeKalb Observatory, Indiana, USA. Rc = 16.06 @ 2003.04.02 04:30 Bu = 18.02 @ 2003.04.02 05:44 V = 16.85 @ 2003.04.02 04:52 ftp://ftp.aavso.org/grb/GRB030329/DonnStarkey_GRB030329_2452731.82174_.txt Peter Nelson, .32m at Ellinbank Observatory, Australia. Rc = 18.3 +/- 0.3 @ 2003.04.03 13:00 exposures: 3X300s ftp://ftp.aavso.org/grb/GRB030329/PeterNelson_GRB030329_2452734.05919_.txt Pertti Pääkkönen, .5m at Jakokoski Observatory, Finland. Rg = 18.55 +/- 0.04 @ 2003.04.05 22:12 exposures: 33X300s ftp://ftp.aavso.org/grb/PerttiPääkkönen_GRB030329_2452736.16987_.txt http://cc.joensuu.fi/seulaset/ccd/20030405/ Correction: The data below is a recalculation (based on a better comp star) of data posted earlier in GCN 2058. Berto Monard, .3m at Bronberg Observatory. South Africa Unfiltered: 13.8 @ 2003.03.29 17:15 to Unfiltered: 14.7 @ 2003.03.29 23:37 ftp://ftp.aavso.org/grb/GRB030329/monard-GRB030329mar29.txt * Durig et al., Gary, Starkey, Oksanen, West, Nelson, Pääkkönen and Kaiser used Henden et al. photometry (GCN 2023) for comparison. DiLapo used USNOA2. Monard used Tycho-2. * Pääkkönen's R filter (Rg) is a custom designed filter. Info at: http://cc.joensuu.fi/seulaset/ccd/rgbfilters.png The AAVSO International GRB network is greatful for a generous grant from the Curry Foundation and to NASA for the financial support for the High Energy Workshops for Amateur Astronomers. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2105 SUBJECT: GRB030329: RTT150 optical observation DATE: 03/04/06 19:56:47 GMT FROM: Irek Khamitov at TUG I. Khamitov, M.Parmaksizoglu (TUG); I. Bikmaev, N. Sakhibullin, V. Suleymanov, R.Gumerov, A.Ibragimov (KSU); Z. Aslan, O.Golbasi (TUG); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko (IKI); U. Kiziloglu, A. Alpar, A. Baykal (METU); report: We continue observations of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at TUG. Using stars from Henden (GCN 2082) we measured R=18.56+/-0.10 for UT= April 6.06 (182.3 hours after the burst). Observations were done under bad atmospheric conditions. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2106 SUBJECT: GRB030329: Kiso B and R band observations DATE: 03/04/07 01:38:35 GMT FROM: Yuji Urata at RIKEN Y. Urata(1), T. Miyata(1), S. Nishiura(1), T. Tamagawa(1), T. Sekiguchi(2), S. Miyasaka(3), C. Yoshizumi(4) 1; Kiso GRB team 2; National Astromical Observatory of Japan 3; Tokyo Metropolitan Government 4; Tokushima children's science museum report; "We have observed the optical afterglow (Peterson and Price GCN1985) of GRB030329 on the nights of 2003 March 29 and April 1 using the Kiso observatory (the University of Tokyo) 105 cm Schmidt telescope with B and R band filters. Our observations started at March 29 13:21:26 (1.8 hour after the burst). We have measured the B and R band magnitude using field photometry (Henden GCN2082). The results are listed below. The observations and more accurate photometry are in progress. Date start time exp band mag err 2003-03-29 14:23:50 60.0 R 13.324 0.010 2003-03-29 15:23:59 60.0 R 12.719 0.010 2003-03-29 16:21:56 120.0 R 13.754 0.010 2003-03-29 17:22:20 60.0 R 13.744 0.010 2003-03-29 17:42:16 60.0 R 13.644 0.010 2003-04-01 10:56:40 300.0 R 17.281 0.077 2003-04-01 10:41:15 300.0 B 17.943 0.063 We thank many high school students who participated in the education program at Kiso observatory in the night to collaborate with us." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2107 SUBJECT: GRB 030329: Supernova Spectrum Emerging DATE: 03/04/07 01:54:45 GMT FROM: Krzysztof Z. Stanek at CfA T. Matheson (CfA), P. Garnavich (Notre Dame), N. Hathi, R. Jansen, R. Windhorst, L. Echevarria (ASU), J. Lee (Arizona), W. Brown, N. Caldwell, P. Berlind. M. Calkins and K. Z. Stanek (CfA) report: We obtained spectra of the afterglow of GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) with the 6.5-m MMT and Blue-Channel spectrograph each night from March 30.12 to April 6.15 (UT). The spectra cover a wavelength range of 350 nm to 850 nm with a resolution of 0.6 nm (FWHM). The early spectra consist of a power-law continuum with narrow emission lines originating from HII regions in the host galaxy (Martini et al. GCN 2013; Della Ceca et al. GCN 2015; Greiner et al. GCN 2020; Caldwell et al. GCN 2053). However, our spectrum taken Apr. 6.15 (UT) shows a broad peak in flux at approximately 570 nm and another weak deviation from a power-law near 470nm that were not evident in the earlier spectra. The April 6 spectrum is well reproduced by adding a spectrum of SN 1998bw (Patat et al. 2001, ApJ, 555, 900) seven days before maximum light to a power-law distribution. We conclude that a supernova spectrum is emerging from the afterglow light. The brightness of the supernova is approximately V=22 based on the strengths of the broad features relative to a pure power-law. Further spectroscopy is planned. A plot of the spectrum compared with SN 1998bw is available at: http://cfa-www.harvard.edu/~tmatheson/grb030329_sn.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2108 SUBJECT: GRB030329: RTT150 optical observations DATE: 03/04/07 02:10:47 GMT FROM: Irek Khamitov at TUG I. Khamitov, M.Parmaksizoglu (TUG); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU); Z. Aslan, O.Golbasi (TUG); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko (IKI); U. Kiziloglu, A. Alpar, A. Baykal (METU); report: We continue the monitoring of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at TUG. Starting from 06 Apr 18:33 UT we obtained BVRI (Bessel) images of TO yet, 12 frames on each band. Using stars from Henden (GCN 2082) we measured follow magnitudes: Time, UT R Rerr 06 Apr. 18:33 18.812 0.056 18:55 18.716 0.048 19:16 18.747 0.052 19:38 18.973 0.063 20:00 18.956 0.062 20:21 18.859 0.055 20:43 18.822 0.051 21:05 18.921 0.057 21:26 18.749 0.049 21:48 18.670 0.046 22:09 18.713 0.049 Observational set is continued. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2109 SUBJECT: GRB 030329: possible color change DATE: 03/04/07 03:27:57 GMT FROM: Krzysztof Z. Stanek at CfA D. Bersier, R. Schild and K. Z. Stanek (CfA) report: We imaged the optical afterglow of GRB 030329 (Peterson & Price: GCN 1985; Torii: GCN 1986) with the FLWO 1.2-m telescope between April 5 UT 03:11 and April 6 UT 08:49 using standard BVRI filters. During that time, the color of the OT seems to have changed by ~0.15 in B-V (OT getting redder) and by ~0.1 in V-I (OT getting bluer). This seems to be consistent with the supernova signature discovered by Matheson et al. (GCN 2107). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2110 SUBJECT: GRB 030329, color evolution DATE: 03/04/07 11:36:10 GMT FROM: Sylvio Klose at TLS Tautenburg A. Henden (USRA/USNO, Flagstaff), B. Canzian (USNO), A. Zeh, S. Klose (Thueringer Landessternwarte Tautenburg), on behalf of the FUN and another collaboration report: USNO Flagstaff has been observing the optical transient of GRB 030329 starting 0.65 days after the burst with high photometric accuracy. A plot of the BVRcIc data obtained during the first 8 days after the burst reveals short-term (during a night) and long-term (over days) color fluctuations. In particular, the USNO data reveal a broad bump in the B-Ic color of the optical transient around day 5 when the afterglow shows an excess of red light compared to the earlier light curve. Before the occurrence of this bump the optical transient reddened continuously but slowly. Between day 5 and 7 the data reveal also an increase in the B-Rc color but a decline of the V-Ic and Rc-Ic colors. On day 8, however, this trend has stopped and the optical transient was considerably redder in all colors (B-V, V-Rc, Rc-Ic). More precisely, the optical transient was redder than ever before. Based on the USNO data alone one cannot decide what the reason for this color evolution is (emission lines from the underlying host galaxy, a dust echo, broad-band supernova features, intrinsic afterglow physics, etc.). If it is a supernova (Matheson et al., GCN 2107; Bersier et al., GCN 2109) then the color changes much more rapidly than predicted by the simplest model (Zeh et al., GCN 2081). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2111 SUBJECT: GRB 030329 Optical observations DATE: 03/04/07 14:15:17 GMT FROM: Evgeni Semkov at Inst.of Astronomy,Bulgaria E. Semkov (Institute of Astronomy, Sofia, Bulgaria) report: The afterglow of the HETE burst (H2652) GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) was observed with the 50/70 cm Schmidt telescope of the National Observatory Rozhen (Bulgaria) on 2, 3 and 3 April, Rc filter, 5 x 300 sec coo-added exposures. The observations were carried out under good seeing conditions. Using field photometry of Henden (GCN2082) we estimate the brightness of the optical afterglow in Rc band as follows. 2.04 (UT 21.3) R=17.66 +/-0.09 3.04 (UT 20.2) R=17.73 +/-0.11 4.04 (UT 19.5) R=18.11 +/-0.18 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2112 SUBJECT: GRB030329: BV photographic observations DATE: 03/04/07 15:09:40 GMT FROM: Vasilij Rumjantsev at CrAO V.Metlov (Crimean Laboratory of the Sternberg Astronomical Institute, Moscow State University) report: I have continued photographic observations of the GRB030329 OT found by B.A.Petrrson and P.A.Price (GCN 1985) with 50-cn Maksutov telescope at Crimean Laboratory of the Sternberg Astronomical Institute. Two 80-minute exposures have been made on Apr, 4. Based on additional filed photometry presented in GCN 2082 by A.Henden I have estimated the OT magnitudes on two new photographs, and also have made some corrections to my previous (GCN 2102) estimations. 14 stars were used to do the calibration. The results are shown in the table below. The increased uncertainties of last measurements are caused by affinity to the limiting magnitudes of our plates (19.0-19.5 in B band, 18.0-18.5 in V band). Despite of it, it was seen, that began a new fading phase. date UT filter mag err 2003-04-02 19:33:00-20:33:00 B 18.20 0.15 2003-04-02 20:45:00-21:35:00 V 18.05 0.25 2003-04-04 18:18:00-19:38:00 V >18.4 - 2003-04-04 19:48:00-21:08:00 B 18.80 0.30 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2113 SUBJECT: GRB030329: Optical observcations DATE: 03/04/07 15:25:45 GMT FROM: Vasilij Rumjantsev at CrAO V.Lyuty and V.Metlov (Crimean Laboratory of the Sternberg Astronomical Institute, Moscow State University) report: We have observed the GRB030329 OT found by B.A.Peterson and P.A.Price (GCN 1985) with 60-cm telescope at Crimean laboratory of the Sternberg Astronomical Institute. Our observations started at Mar 31, 18:00 UT. A set of 120 sec. exposures in R (Johnson) filter was obtained under poor weather conditions. We have estimated the R magnitudes of the OT using USNO U1050_06350247 star (R=16.06). The results are shown in the table below. UT R March 31.7510 17.09 31.7576 17.04 31.7604 16.84 31.7813 16.84 31.7840 16.94 31.7868 16.88 31.7931 17.04 31.7972 16.90 31.8056 17.09 31.8083 16.98 31.8167 17.12 Average: 16.98+/-0.03 It is possible that the beginning of the next phase of decrease of OT brightness took place. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2115 SUBJECT: GRB 030329, color evolution DATE: 03/04/07 18:46:09 GMT FROM: Sylvio Klose at TLS Tautenburg A. Zeh, S. Klose (Thueringer Landessternwarte Tautenburg), A. Henden (USRA/USNO) on behalf of the USNO GRB team and the FUN collaboration, and J. Greiner (MPE Garching), report: Stimulated by the recent claim of an appearing supernova (SN) component (Matheson et al. 2107; Bersier et al., GCN 2109) we have extended our numerical model (Zeh et al., GCN 2081) by the inclusion of a parameter which describes a delay, dt, between the onset of the SN and the GRB and have reanalyzed the USNO data on GRB 030329. The long-term evolution in the B-V, B-Rc, and V-Rc color of the optical transient (OT) seen in the high-precision USNO data so far can indeed be fitted very well with dt approximately 1..2 weeks prior to the burst, although we cannot reproduce the temporary reddening of the optical transient which was observed on t=8 days after the burst (Henden et al., GCN 2110). On day 9 this temporary reddening of the OT has disappeared. It is well possible that this phenomenon was related to another episode of flattening of the OTs light curve. For the sake of clarity we note that the unknown diversity of GRB-SNe does not allow us to state with certainty that a dt < 0 in our model does indeed represent a 'SN-first--GRB-later' scenario. So far, this parameter simply improves the numerical fit if SN 1998bw is used as a template. Its physical reality remains to be clarified. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2116 SUBJECT: Kiso observation of the GRB030329 at April 6 DATE: 03/04/08 03:07:43 GMT FROM: Yuji Urata at RIKEN J. Suzuki (1), T. Sekiguchi(2), S. Miyasaka(3), 1; Tokyo University of Science 2; National Astronomical Observatory of Japan 3; Tokyo Metropolitan Government T. Aoki, Y. Urata, and T. Tamagawa on behalf of the KISO GRB Team report: "We continue to observing the GRB030329 optical afterglow (Peterson and Price GCN1985) using the Kiso observatory (the University of Tokyo) 105 cm Schmidt telescope with B and R band filters. We measured the B and R band magnitude using field photometry (Henden GCN2082). The results are listed below. The observations and more accurate photometry are in progress. Start End exposure filter mag. error 2003-04-06 11:13 11:33 300s x 3 R 18.85 0.04 11:35 11:55 300s x 3 B 19.72 0.05 This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2117 SUBJECT: GRB030329: HET spectroscopic monitoring DATE: 03/04/08 03:37:04 GMT FROM: Mike Eracleous at PSU, Astro.Dept. Mike Eracleous (Penn State), Brad Schaefer, and Chris Gerardy (U. Texas) on behalf of the Hobby-Eberly Telescope GRB followup team report: We have obtained several spectra (410-900 nm, resolution 1.6 nm) of the optical counterpart of GRB030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) with the Hobby-Eberly Telescope and Marcario Low-Resolution spectrograph. Our spectra of March 31, April 2, and April 5 (UT) show the following evolution of the spectral properties: (a) the equivalent widths of the [O III] and H-alpha emission lines is increasing in a manner consistent with a constant line flux and a decline of the continuum, and (b) the spectrum of April 5 (UT) shows evidence of a broad feature underlying the [O III] lines, similar tresembling that reported by Matheson et al. (GCN 2107), who interpret it as due to an emerging SN spectrum. However, the contrast of this feature in our spectrum is not as high as in the spectrum of Matheson et al. (taken a day later than ours). As a consequence, we cannot rule out alternative interpretations, such as the emergence of a host galaxy spectrum that manifests itself as a break in the power-law continuum. Analysis of more recent spectra is under way to clarify this issue. Using the [O II] and H-alpha emission line fluxes of Caldwell et al. (GCN 2053), we estimate luminosities of 1x10^40 and 4x10^40 erg/s, respectively (for z=0.168, i.e., a luminosity distance of 880 Mpc), and infer star formation rates of 0.15 and 0.32 solar masses/yr (following Kennicutt 1998, ARAA, 36, 189). The upper limit on the host galaxy from historical images reported by Wood-Vasey et al. (GCN 1998; R > 22.28) implies a limit on the absolute magnitude of M_R > -17.4, which is comparable to that of the LMC. The [OIII]/H-beta ratio of 2.7 (Caldwell et al.; GCN 2053) corresponds to an LMC-like faint starburst galaxy (Ho, et al. 1997, ApJ, 487, 579, Figure 6; Hunter & Gallagher, 1997, ApJ, 475, 65; Hunter et al. 2001 ApJ, 553, 121), while the H-alpha luminosity is characteristic of starburst galaxies (Ho. et al. Figure 2). High-dispersion spectroscopy of these narrow lines may give more information on the nature of star formation in the host galaxy. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2118 SUBJECT: GRB030329: Near Infrared Observations at Gunma DATE: 03/04/08 05:04:46 GMT FROM: Eiji Nishihara at GAO E. Nishihara, O. Hashimoto, K. Kinugasa (Gunma Astronomical Observatory) J-, H-, and Ks-band photometry of the optical afterglow (Peterson and Price GCN 1985, Torii GCN 1986) of GRB030329 (Vanderspek et al. GCN 1997) were obtained on the nights of 2003 Apr 29 and 30 at GAO, Gunma, Japan, using the 1.5-m telescope and the IR Camera. The observation started at 13:50 UT (133 min after the GRB trigger). Our preliminary J-band magnitudes (rough estimate of typical error is 0.1 mag) of the afterglow are given below: --------------------- UT J --------------------- Apr 29 13.868 11.87 15.253 12.42 16.902 12.66 17.828 12.93 Apr 30 12.534 15.10 14.159 15.21 --------------------- This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2119 SUBJECT: GRB030329: RTT150 optical observations DATE: 03/04/08 19:05:41 GMT FROM: Irek Khamitov at TUG I. Khamitov, M. Parmaksizoglu, K.Uluc (TUG); I. Bikmaev, N. Sakhibullin, V. Suleymanov, R. Gumerov, A. Ibragimov (KSU); Z. Aslan, O.Golbasi (TUG); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko (IKI); U. Kiziloglu, A. Alpar, A. Baykal (METU); report: We continue observations of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with 1.5-m Russian-Turkish Telescope RTT150 at TUG in the Bessel BVRI-bands. We obtained 70 exposures at 06 Apr. 18:33UT - 07 Apr. 01:23UT; and 48 exposures at 07.Apr 17:55UT - 08 Apr. 01:02UT Second night observations were made under bad weather conditions. The magnitudes obtained are as follows: UT R Rerr Apr. 6.79 18.75 0.02 Apr. 6.83 18.76 0.02 Apr. 6.87 18.71 0.02 Apr. 6.92 18.68 0.02 Apr. 6.96 18.70 0.03 Apr. 6.99 18.73 0.02 Apr. 7.74 18.77 0.03 Apr. 7.77 18.78 0.02 Apr. 7.80 18.73 0.03 Apr. 7.80 18.80 0.03 Apr. 7.97 18.91 0.03 Apr. 8.01 18.83 0.03 There are no significant changes in the fluxes during two observational set in all BVRI-bands. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2120 SUBJECT: GRB 030329: Supernova Confirmed DATE: 03/04/08 20:13:40 GMT FROM: Krzysztof Z. Stanek at CfA T. Matheson (CfA), P. Garnavich (Notre Dame), E. W. Olszewski (Steward), P. Harding (Case Western), D. Eisenstein (Arizona), B. Pindor (Princeton), N. Hathi, R. Jansen, R. Windhorst, L. Echevarria (ASU), J. Lee (Arizona), W. Brown, N. Caldwell, P. Berlind, M. Calkins and K. Z. Stanek (CfA) report: Additional spectra of the afterglow of GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) were obtained with the 6.5-m MMT on Apr. 8.13 UT. The spectral features discovered by Matheson et al. (GCN 2107) and confirmed by Garnavich et al. (IUAC 8108) continue to develop. Subtracting a scaled version of the Apr. 4.27 UT power-law spectrum from the Apr. 8.13 spectrum reveals an energy distribution remarkably similar to that of the SN1998bw a week before maximum light (Patat et al. 2001, ApJ, 555, 900). This spectrum can be seen at http://cfa-www.harvard.edu/~tmatheson/compgrb.jpg The spectral similarity to SN 1998bw and other 'hypernovae' such as 1997ef (Iwamoto et al. 2000, ApJ, 534, 660) provides strong evidence that classical GRBs originate from core-collapse supernovae. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2122 SUBJECT: GRB 030329: VLT V-band photometry DATE: 03/04/09 11:49:15 GMT FROM: Daniele Malesani at SISSA-ISAS,Trieste,Italy S. Covino, G. Ghisellini (INAF, Brera, I); D. Malesani (SISSA, Ts, I); P.A. Price (Caltech, USA); D. Lazzati, E.M. Rossi (IoA, Cambridge, UK); G. Chincarini, G. Tagliaferri, F.M. Zerbi (INAF, Brera, I); S. Di Serego, M. Della Valle, A. Cimatti (INAF, Arcetri, I); F. Fiore, G.L. Israel, L. Stella (INAF, Roma, I); M. Vietri (Roma 3, Univ, I); N. Kawai (RICHEN, Japan); G.R. Ricker (MIT, USA); E. Le Floc'h, P. Goldoni, I.F. Mirabel (CEA, Sacley, F); S. Mereghetti (IASF, Mi, I); E. Costa, P. Soffitta (IASF, Roma, I); S. Ortolani (Padova Univ., Italy); A. Kaufer, A. Lopez, P.M. Vreeswijk, P. Vaisanen, A.O. Jaunsen (ESO); report: Starting on 2003 April 2.1, we observed the optical counterpart (Peterson & Price, GCN 1985; Torii, GCN 1986) of GRB 030329 (Vanderspek et al., GCN 1997). The observations were performed with the ESO VLT-UT1 (Antu) telescope equipped with FORS1, in spectropolarimetric mode. Several acquisition images were taken, under photometric sky conditions; here we report the V-band magnitudes of the OT, based on Henden's calibration (GCN 2023). Seeing was ~1". UT t-t0 (days) V mag err --------------------------------------- Apr 2.089 2.605 17.652 +- 0.015 Apr 2.128 2.644 17.696 +- 0.014 Apr 2.166 2.682 17.738 +- 0.015 The complete analysis of the spectropolarimetric dataset is underway. We thank the ESO staff at Paranal for their kind and reliable assistance. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2123 SUBJECT: GRB 030329, light curve flattens DATE: 03/04/09 17:53:47 GMT FROM: Sylvio Klose at TLS Tautenburg A. Henden (USRA/USNO, Flagstaff), B. Canzian (USNO), A. Zeh, S. Klose (Thueringer Landessternwarte Tautenburg), on behalf of the FUN and another collaboration report: Flagstaff BVRI data reveal that the light curve of the optical transient (OT) following GRB 030329 has now begun to flatten in all bands and might be entering the supernova phase. The signal which is now seen in the light curve shape looks different from all previous episodes of re-brightening. The photometric data alone do not yet allow us to state with certainty what the best fitting parameters of the underlying supernova component are (see Zeh et al., GCN 2081). The color evolution of the OT until day 8 after the burst, which was reported in GCN 2115 (Zeh et al.), seemed to prefer a delay dt between the onset of the supernova and the onset of the GRB by several days. The inclusion of the Flagstaff data obtained during the last two nights has changed this picture, however. Obviously on day 8 the OT underwent another episode of re-brightening and color change that made it difficult to fit the observed colors. After exclusion of this effect, a dt close to 0 days is preferred in the color evolution, as well as in the shape of the R and V-band light curves (-3 < dt <=0). This is in good agreement with the (stronger) finding based on spectroscopic data (Matheson et al., GCN 2120). Figures will be posted at Jochen Greiners internet GRB page. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2124 SUBJECT: GRB 030329: BVRI photometry at Asiago DATE: 03/04/09 19:50:40 GMT FROM: Daniele Malesani at SISSA-ISAS,Trieste,Italy A. Simoncelli (INAF, Brera, I), D. Malesani (SISSA, Trieste, I), A. Della Valle (INAF, Padova, I), N. Masetti (IASF, Bologna, I), L.A. Antonelli (INAF, Roma, I), S. Covino (INAF, Brera, I), E. Pian (INAF, Trieste, I), on behalf of a larger Italian collaboration, report We have obtained BVRI images of the afterglow (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN 1997), using the 182cm Copernico telescope of the Astronomical Observatory of Padova (Italy), plus BFOSC. Seeing was ~3"; the afterglow was clearly detected in all bands; we measured for it the following BVRI magnitudes, with respect to the calibration performed by Henden (GCN 2082): UT start exptime filter mag err ------------------------------------------ Apr. 4.908 600 s R 18.14 +- 0.02 Apr. 4.916 1200 s B 18.88 +- 0.02 Apr. 4.932 600 s I 17.71 +- 0.02 Apr. 4.941 600 s V 18.55 +- 0.02 Assuming a powerlaw shape for the spectrum (F_nu propto nu^-beta), the best fit to our data yields beta~1. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2129 SUBJECT: GRB 030329 VLBA Observations DATE: 03/04/10 03:32:38 GMT FROM: Greg Taylor at NRAO G. B. Taylor (NRAO), E. Berger (Caltech), D. A. Frail (NRAO), and S. R. Kulkarni (Caltech) report: "Following the detection of the radio afterglow on Mar 30 (Berger et al. GCN 2014) from the bright burst GRB 030329 (GCN 1985, 1997) we observed with the Very Long Baseline Array (VLBA) for 8 hours beginning on April 01.05 UT. The flux density measured at 8.4 GHz was 8.3 +/- 0.4 mJy. The source is unresolved by these observations with a size less than 0.5 mas (size < 1.4 pc given the redshift of 0.1685 reported by Greiner et al. in GCN 2020). Assuming typical parameters for the expansion (e.g. Frail et al. 2000, ApJ, 534, 559) we expect a size of about 1.3e17 cm (0.04 pc) at the time of the VLBA observation (t=2.7 days). The VLBA position is at ra = 10h44m49.9595s dec = +21d31'17.438" (equinox J2000) with a conservative error of 0.001 arcsec in each coordinate. This position is within 0.02 arcsec of the VLA radio position, but is 1.21 arcsec from the optical afterglow position reported by Yamaoka et al. (GCN 1994) who claim an uncertainty of 0.07 arcsec. Given that the optical and radio afterglow should be coincident, we suggest that the optical astrometric position suffers from a systematic error. High frequency VLBI observations are planned with the goal of eventually resolving the radio afterglow." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2130 SUBJECT: GRB030329, optical position DATE: 03/04/10 04:00:03 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO) reports on behalf of the USNO GRB team: The optical position in the field photometry file (GCN 2023) ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb030329.dat for the optical transient (GCN 1985) is given as 10:44:49.957 +21:31:17.46 J2000 (internal errors of 40mas) using UCAC2 as the reference frame. This is in good agreement with the recent, more precise, radio position of 10:44:49.9595 +21:31:17.438 given by Taylor et al. (GCN 2129). The NOFS optical position is also in disagreement with Yamaoka et al. (GCN 1994). Yamaoka et al. do not give their reference catalog, which might be the cause for the disagreement. The position given by Price and Peterson (GCN 1987) does not have sufficient precision in RA to ascertain whether their position matches NOFS and Taylor et al. within their quoted accuracy. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2131 SUBJECT: GRB 030329 and SN 2003dh DATE: 03/04/10 04:56:26 GMT FROM: Ryan Chornock at UC Berkeley R. Chornock, R. J. Foley, A. V. Filippenko, M. Papenkova, and D. Weisz, University of California, Berkeley, report that inspection of CCD spectra (range 310-1000 nm) of GRB 030329, obtained on Apr. 8 UT with the Shane 3-m telescope at Lick Observatory, confirms the emergence of broad bumps (especially at rest-frame 500 nm) characteristic of the peculiar type-Ic supernovae 1998bw and 2002ap at early times, as announced by Matheson et al. in GCN 2107 and GCN 2120. The association between core-collapse supernovae and at least some of the long-duration GRBs thus seems solid. We expect the supernova features to continue strengthening with time relative to the power-law continuum of the GRB afterglow. P.S. This information also appears in IAUC 8114, but has been reposted here for the benefit of those GCN subscribers who do not read the IAU Circulars. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2132 SUBJECT: Superluminal motion in GRB 030329 DATE: 03/04/10 16:44:18 GMT FROM: Arnon Dar at Technion-Israel Inst. of Tech Arnon Dar (Technion) and Alvaro De Rujula (CERN) report: We use the infamous Cannonball model (CB model) of GRBs to predict the superluminal motion of the source of the radio afterglow (AG) of GRB 030329 (GCN 1985, 1997), potentially observable with the VLBA (see, e.g. GCN 2129). The CB model has been succesful in describing GRB 030329 and its AG, in predicting the supernova (SN) contribution to the AG, and even the date at which the SN was to be convincingly seen [1]. In the CB model, the cannonballs responsible for the GRB and the AG light move superluminally in the sky, as they travel away from their projenitor SN. THIS MOTION MAY BE OBSERVABLE IN THE RADIO AG, IF ITS LOCATION IS FOLLOWED AS A FUNCTION OF TIME [2]. The SN cannot be currently seen in the radio, so that it is the motion of the radio-AG source (the CB) that one may try to observe. In the case of GRB 030329 there were two CBs, one of which dominates the AG after t ~ 1 day. Using the parameters of this CB determined in [1] (initial Lorentz factor 1477, viewing angle 2 mrad, and deceleration parameter 476 kpc) and Eqs. (30, 31, 41) of [3] we obtain the angular distances "alpha" (in mrad) of the dominant CB to the SN as a function of "t" (observer's time in days). For the current cosmology (Omega_Lambda=0.7, Omega_Matter=0.3, H_0=75 km/s/Mpc; and for z=0.1685, so that the angular distance is 0.64 Gpc) some representative results are: (t, alpha): (0,0); (1,0.22); (2.7,0.49); (5,0.74); (10,1.1); (30,1.9). This means that from day 2.7 to day 10 the radio source may have moved 0.6 mrad, and from day 10 to day 30 it may move an extra 0.8 mrad. Such motion may be observable with the VLBA. [1] Dado et al. astro-ph/0304106. [2] Dar and De Rujula, astro-ph/0008474. [3] Dado et al. 2003 A&A 401, 243. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2133 SUBJECT: Superluminal motion in GRB 030329 (Correction) DATE: 03/04/10 17:19:52 GMT FROM: Arnon Dar at Technion-Israel Inst. of Tech Arnon Dar (Technion) and Alvaro De Rujula (CERN) report: We use the infamous Cannonball model (CB model) of GRBs to predict the superluminal motion of the source of the radio afterglow (AG) of GRB 030329 (GCN 1985, 1997), potentially observable with the VLBA (see, e.g. GCN 2129). The CB model has been succesful in describing GRB 030329 and its AG, in predicting the supernova (SN) contribution to the AG, and even the date at which the SN was to be convincingly seen [1]. In the CB model, the cannonballs responsible for the GRB and the AG light move superluminally in the sky, as they travel away from their projenitor SN. THIS MOTION MAY BE OBSERVABLE IN THE RADIO AG, IF ITS LOCATION IS FOLLOWED AS A FUNCTION OF TIME [2]. The SN cannot be currently seen in the radio, so that it is the motion of the radio-AG source (the CB) that one may try to observe. In the case of GRB 030329 there were two CBs, one of which dominates the AG after t ~ 1 day. Using the parameters of this CB determined in [1] (initial Lorentz factor 1477, viewing angle 2 mrad, and deceleration parameter 476 kpc) and Eqs. (30, 31, 41) of [3] we obtain the angular distances "alpha" (in mas) of the dominant CB to the SN as a function of "t" (observer's time in days). For the current cosmology (Omega_Lambda=0.7, Omega_Matter=0.3, H_0=75 km/s/Mpc; and for z=0.1685, so that the angular distance is 0.64 Gpc) some representative results are: (t, alpha): (0,0); (1,0.22); (2.7,0.49); (5,0.74); (10,1.1); (30,1.9). This means that from day 2.7 to day 10 the radio source may have moved 0.6 mas, and from day 10 to day 30 it may move an extra 0.8 mas. Such motion may be observable with the VLBA. * mrad in GCN 2132 was corrected to mas [1] Dado et al. astro-ph/0304106. [2] Dar and De Rujula, astro-ph/0008474. [3] Dado et al. 2003 A&A 401, 243. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2136 SUBJECT: GRB 030329 Rc observations DATE: 03/04/14 15:53:59 GMT FROM: Corrado Bartolini at Universita di Bologna TITLE: GCN GRB OBSERVATION REPORT SUBJECT: GRB 030329: Rc photometry in Loiano G. Pizzichini and P. Ferrero (IASF/CNR, Bologna), C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University), A. Righini (Firenze University) and I. Bruni (Bologna Astronomical Observatory) report: We observed the optical afterglow (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN 1997), using the 152cm telescope + BFOSC of the Astronomical Observatory in Loiano (Italy), Seeing was ~ 1.5", but observing conditions were limited, due to the low angular distance to the moon and the not perfect weather conditions. We co-added the three exposures listed below: UT start exptime filter ----------------------------- Apr. 13.8783 300s Rc Apr. 13.8824 300s Rc Apr. 13.8865 300s Rc and used the following stars in Henden's photometric calibration (GCN2082): RA= 161.174977 DEC= 21.542124 RA= 161.158874 DEC= 21.562989 RA= 161.162639 DEC= 21.516308 RA= 161.166023 DEC= 21.570694 We obtain a preliminary magnitude Rc = 18.66 +/- 0.11. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2141 SUBJECT: GRB030329: VR Photometry at TNG DATE: 03/04/16 12:33:51 GMT FROM: Angelo Antonelli at Obs. Astro. di Roma V. Testa, G. Cocozza, A. Melandri, L.A. Antonelli (INAF-Roma, I), D. Malesani (SISSA, Trieste, I), A. Buzzoni, S. Di Tomaso, D. Fugazza, F. Ghinassi, J.C. Guerra (INAF-TNG), S. Covino (INAF-Merate, I), N. Masetti (IASF-CNR, Bologna, I), E. Pian (INAF-Trieste, I) on behalf of a larger Italian collaboration, report: "We have obtained VR images of the afterglow (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN 1997), with the Italian 3.6m TNG equipped with DOLORES. Observations were performed on Apr. 10,11 and 14; seeing in the R band was 1.0 arcsec during the first night, 1.2 arcsec during the second night, and 1.3 arcsec during the last night. The afterglow was detected in both bands with S/N(R,peak) = 43 (first night), 37 (second night) and 23 (third night). During the second and third nights measurements have been affected by a bright sky background, likely due to the moon being relatively close to the target (21 and 24 degrees respectively). We measured the following VR magnitudes, with respect to the calibration performed by Henden (GCN 2082): Obs._date(UT) t_exp(s) Filt. Mag Err(Mag) ---------------------------------------------- 10/4 21:38:37 240 V 19.72 0.05 10/4 21:31:28 240 R 19.34 0.05 11/4 21:35:49 240 V 19.68 0.11 11/4 22:04:56 240 R 19.45 0.09 14/4 20:33:01 240 V 20.10 0.12 14/4 20:48:30 240 R 19.71 0.11 All TNG measurements are consistent with a continuosly fading transient. This message can be cited." [GCN OPS NOTE (07Nov03): The INAF-TNG author list was changed from "F. Ghinassi, D. Fugazza, S. Di Tomaso (INAF-TNG)" to "A. Buzzoni, S. Di Tomaso, D. Fugazza, F. Ghinassi, J.C. Guerra (INAF-TNG)".] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2145 SUBJECT: OT GRB 030329: early UBVRcIc spectral evolution DATE: 03/04/17 14:09:19 GMT FROM: Timur Fatkhullin at SAO RAS T. Fatkhullin, V. Komarova, V. Sokolov (SAO RAS), V. Kurt (ASC RAS), A. Cherepashchuk (SAI MSU), K. Postnov (SAI MSU), V. Reshetnikov (AI SPBU), Alberto J. Castro-Tirado (INTA, Madrid and IAA, Granada) report: A part of the results of the UBVRcIc observations with the 1-m (Zeiss-1000) of SAO RAS at two epochs on March, 29 and the next two nights are now presented at our anonymous FTP-site: ftp://ftp.sao.ru/pub2/grb/GRB030329/ One can see the evolution of the early broad-band UBVRI spectra. In addition, comparison with the MPFS spectra (see GCN #2142) allows us to perform more precise flux calibration of these spectral data. Sorry! More correct reference quoted in GCN #2142 is E. Grassberg, V. Imshennik and D. Nadyozhin, 1971, Astroph. Space Sci., 10, 28 ////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2146 SUBJECT: GRB030329: Optical Observations DATE: 03/04/18 06:19:46 GMT FROM: Vasilij Rumjantsev at CrAO V.Rumyantsev, E. Sergeeva (CrAO), V.Doroshenko (SAI MSU), E.Pavlenko, O.Antoniuk, N.Primak (CrAO), and A.Pozanenko (IKI) report: We continue to monitor the OT of GRB030329. Observations were made on April 8, 9, 10, 2003 in R and I (Johnson) spectral band with the 70-cm and 38-cm Cassegrain telescopes of CrAO. Based on filed photometry by A. Henden (GCN 2023) we estimate the OT magnitude as following Mid time, UT telescope exposure mag err Apr.08.9284 K-380 20x300s R 19.35 0.25 Apr.09.9179 AZT-8 8x150s R 19.56 0.19 Apr.10.8462 AZT-8 10x120s R 19.80 0.22 Apr.10.8615 AZT-8 10x120s I 19.32 0.25 This message may be cited. ////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2147 SUBJECT: GRB 030329 OT position DATE: 03/04/18 07:21:37 GMT FROM: Hitoshi Yamaoka at Kyushu U., VSNET-GRB collab. H. Yamaoka (Kyushu U), T. Kato, M. Uemura and R. Ishioka (Kyoto U) report: The OT position given in GCN 1994 was obtained with respect to the USN0-A2.0 reference stars (epoch 1955.2). The large apparent proper motions of several stars or the systematic displacements were the main cause of the disagreement noticed by Taylor et al. (GCN 2129) and Henden (GCN 2130). Taking the same procedure as GCN 1994 but using the 2MASS positions, we obtain a refined position of R.A. = 10:44:49.958 +/- 0.005, Decl. = +21:31:17.51 +/- 0.07, which is in good agreement with the radio and optical positions (GCN 2129, 2130). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2156 SUBJECT: GRB030329: 444 AAVSO Measurements DATE: 03/04/20 03:21:34 GMT FROM: AAVSO GRB Network at AAVSO A. Price (AAVSO); B. Aquino (AWJ); E. Broens (BOS) & J. Hambsch (HJB) (VVS Werkgroep Veranderlijke Sterren); P. Brown (OPO01 - Brigham Young University); T. DiLapo (DLN); B. Dillon (DIL) & J. Dellinger, D. Beaver, P. Garossino, T. Garossino; N. Dunckel (DNI); T. Durig & A. L. Seifert, C. B. Norton, G.F. Garland, J.K. Cole, J.B. Cherry (CLW01 - University of the South); B. Gary (GBL); B. Granslo (GRL); A. Henden (USRA/USNO); D. Hohman (HDF); D. Kaiser (KDA); Z. Kereszty (KZX); P. Kilmartin & A. Gilmore (KPM - University of Canterbury) J. Liesmann (LJI); G. Lubcke (LBG); J. Mattei (AAVSO); B. Monard (MLF); P. Nelson (NLX); A. Oksanen (OAR) & P. Tikkanen (TPE); P. Pääkkönen (PPK); D. Starkey (SDB); A. von der Linden & T. Schrabback (XXX - IAEF, Bonn University); D. West (WJD) report on behalf of the AAVSO International GRB Network: The AAVSO has 444 measurements of of the GRB030329 OT found by Peterson and Price (GCN 1985) spanning 03:47 on March 31 to 03:09 on April 17, 2003. All observations have been rereduced using the final photometry from Henden et al. (GCN 2114) A light curve, all data plus a finder chart with the comparison and check stars used is available at this URL: http://www.aavso.org/grb/grb030329.shtml Full reports including equipment and site info are available at ftp://ftp.aavso.org/grb/GRB030329 Many of the FITS images are available there as well. The AAVSO International GRB network is grateful for a generous grant from the Curry Foundation and to NASA for the financial support for the High Energy Workshops for Amateur Astronomers. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2160 SUBJECT: GRB030329, optical observation DATE: 03/04/21 22:46:18 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (Ulugh Beg Astronomical Institute of the Uzbek Academy of Sciences), A.Pozanenko (IKI), V.Rumyantsev (CrAO), G.Beskin (SAO) on behalf of large collaboration report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) using 1.5m telescope of Mt.Maidanak High-altitude Observatory. Several BVRI Bessel images were obtained on April, 7,9,10 and 20. The seeing on Apr.7 was in range of 1-1.5 arcsec, on Apr.10 - 0.9-1 arcsec for R and in 1-1.3 arcsec for B. In Apr. 9 the weather was unfavorable and some images were obtained trough clouds. Based on filed photometry still by A. Henden (GCN 2023) we estimate the OT magnitudes: Mid time UT, Apr. exposure filter mag err 7.7819 7x600 B 19.78 0.04 7.7986 5x600 V 19.20 0.03 7.7771 8x600 R 18.84 0.03 7.8160 3x600 I 18.44 0.06 9.7653 2x600 B 20.07 0.14 9.7813 2x600 V 19.37 0.08 9.7729 4x600 R 19.10 0.06 10.7625 6x600 B 19.96 0.08 10.7792 6x600 V 19.56 0.06 10.7354 6x600 R 19.29 0.07 10.7792 4x600 I 19.11 0.08 And preliminary reduction of measurements on Apr.20 is following UT, Apr. exposure filter mag 20.6444 2x600 R 19.92 20.6604 2x600 B 21.08 With typical error of 0.15 (B) and 0.13 (R) Our measurements on Apr. 10 are consistent with TNG observation by V. Testa et al. (GCN 2141). While in Apr. 7 - 10 the brightness of OT is consistent with slow fading, we could not detect brightness change in R (within our accuracy) between observation on Apr.14 (GCN 2141) and our measurement on Apr. 20. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2161 SUBJECT: GRB 030329 3.5 and 6 cm radio observations at RTF-32 telescope DATE: 03/04/22 15:28:53 GMT FROM: Yuri Gnedin at Pulkovo Obs,Saint-Petersburg A.M.Finkelstein (IPA RAN), A.V.Ipatov(IPA RAN) and Yu.N.Gnedin (Pulkovo Observatory) report: GRB 030329 was observed at 3.5 cm with the RTF-32 telescope of the Institute of Applied Astronomy in Svetloe on 2003 Apr 11 and 12 and at 6 cm with the RTF-32 telescope of the Institute of Applied Astronomy in Zelenchuk on 2003 Apr 11,12 and 13. The observations in Svetloe have been made in both polarization modes. The 3.5 cm following flux densities: 2003 Apr 11.18.12 27.1 +/- 7.8 mJy in the right circular polarization . 7.8 +/- 4.2 mJy in the left circular polarization . 2003 Apr 11.16.47 30.4 +/- 9.7 mJy in the right circular polarization. 18.7 +/- 4.7 mJy in the left circular polarization. 2003 Apr 12.18.43 18.1 +/- 5.2 mJy in the right circular polarization . 7.8 +/- 2.8 mJy in the left circular polarization. Over the period of 6-cm observations in Zelenchuk the flux density at April 11 decreased from 179.6 +/- 4.4 mJy at 18.46 UT to 8.3 +/- 3.1 mJy at 22.48 UT. During Apr 12 and 13 the mean flux density was at the level of approximately 10 mJy. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2163 SUBJECT: GRB030329: optical polarization DATE: 03/04/22 20:50:48 GMT FROM: Antonio Pereyra at IAG-U.Sao Paulo A.M. Magalhães, A. Pereyra, T. Dominici and Z. Abraham (IAG, U. of São Paulo) report: We have obtained R band imaging polarimetry of GRB030329. The observation was performed with the IAGPOL imaging polarimeter and the IAG-USP 60cm telescope, at the Laboratório Nacional de Astrofísica site. The observation spanned the period UT 01:06 to 01:51 on 31 March, 1.519 - 1.592 days after the event, and was made through less than ideal sky conditions. The double-beam technique provided by a calcite plate analyser ensured however that useful polarimetric data could still be obtained. We have measured the following linear polarization for GRB030329: P = [1.974 +- 0.477] %, position angle = 83.2 degrees. (The position angle is already in the equatorial system, increasing from North to East.) As a comparison, we have obtained much smaller polarization for field objects. In particular, for USNO A-2.0 1050-6351075 (object 'A' in Rumyantsev et al, GCN 2005) and 1050-6349885, we have obtained the following linear polarization values: [0.58 +- 0.11] at 66deg and [0.06 +- 0.12] at 21deg, respectively. This low foreground polarization is consistent with the very low foreground reddening towards the field (E(B-V)=0.025, Schlegel et al. 1998). Dilution of the GRB intrinsic polarization by the much fainter (Blake & Bloom GCN 2011) host galaxy should be negligible. Polarization within the host galaxy interstellar medium seems unlikely due to the small internal extincion (Caldwell et al. GCN 2053); this should be settled by variability studies and spectropolarimetry. We conclude that a substantial fraction of the GRB030329 polarization is intrisic in nature. This strongly suggests that GRB030329 is non-spherically symmetric, lending further credence to the asymmetric fireball scenario (in combination with a physical process that produces polarization, such as synchtron radiation). The position angle above should be correlated with the object's beam or jet orientation on the sky. It would be interesting to see whether a similar position angle is present in forthcoming resolved radio observations of the source. This message may be cited. [GCN OPS NOTE (22Apr03): The circular was originally submitted on 14 Apr 03, but was delayed due to email address mismatch.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2164 SUBJECT: GRB 030329: wide-field photograph by R. Tamura 1 hr after the burst DATE: 03/04/23 09:07:47 GMT FROM: Taichi Kato at Kyoto U GRB 030329: wide-field photograph by R. Tamura 1 hr after the burst T. Kato (Kyoto U), R. Tamura and T. Inone (Akashi Municipal Planetarium) report: Ryuichi Tamura (Japanese amateur astronomer) incidentally took wide-field photographs around the afterglow of GRB 030329 one hour after the burst. The photographs were taken at two epochs covering 12:28-12:35 UT (starting at 51 min after the burst) and 12:35-12:42 UT. No obvious optical afterglow was detected on these images. A quick look of the first image has yielded an upper limit of about 8.5 mag. Further analysis of the images is in progress. The enlarged image around the GRB is placed at: http://www.kusastro.kyoto-u.ac.jp/vsnet/GRB/tamura1.gif This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2167 SUBJECT: GRB 030329: optical spectropolarimetry at VLT DATE: 03/04/24 18:55:20 GMT FROM: Daniele Malesani at SISSA-ISAS,Trieste,Italy S. Covino, G. Ghisellini (INAF, Brera, I); D. Malesani (SISSA, Ts, I); P.A. Price (RSAA, ANU); D. Lazzati, E.M. Rossi (IoA, Cambridge, UK); G. Chincarini, G. Tagliaferri, F.M. Zerbi (INAF, Brera, I); A. Cimatti, S. Di Serego, M. Della Valle (INAF, Arcetri, I); F. Fiore, G.L. Israel, L. Stella (INAF, Roma, I); M. Vietri (Scuola Norm. Sup., Pisa, I); N. Kawai (Tokyo Tech, Japan); G.R. Ricker (MIT, USA); P. Goldoni, E. Le Floc'h, I.F. Mirabel (CEA, Sacley, F); S. Mereghetti (IASF, Mi, I); E. Costa, P. Soffitta (IASF, Roma, I); S. Ortolani (Padova Univ., I); A.O. Jaunsen, A. Kaufer, A. Lopez, P. Vaisanen, P.M. Vreeswijk (ESO); report: Starting on 2003 April 2.1 (3.6 days after the GRB), we observed the optical counterpart (Peterson & Price, GCN 1985; Torii, GCN 1986) of GRB 030329 (Vanderspek et al., GCN 1997). The observations were performed with the ESO VLT-UT1 (Antu) telescope equipped with FORS1, in spectropolarimetric mode. At that time, the afterglow had a magnitude V ~ 17.7 (Covino et al., GCN 2122). Our spectrum spans the wavelenght range 350-850 nm. Several narrow emission lines are clearly detected (e.g. Greiner et al., GCN 2020). The polarization level is found very small, yet significantly nonzero, decreasing from (0.9+/-0.1)% in the blue to (0.5+/-0.1)% in the red part of the spectrum (1-sigma errors); the polarization angle also shows a mildly significant variation from (83+/-4) deg in the blue to (73+/-5) deg in the red. These trends are consistent with the effect of a mildly polarizing Galactic/host ISM on a intrinsically polarized afterglow. In particular, the values we obtain in correspondence of the R-band (lambda ~ 650 nm) are P = (0.5+/-0.1)% and theta = (73+/-5) deg. Comparison of our result with previous measurements (Efimov et al., GCN 2144; Magalhães et al., GCN 2163) might indicate some time variability on a few-days timescale. We thank the ESO staff at Paranal for their kind and reliable assistance. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2169 SUBJECT: GRB 030329: Spectral Evolution of SN 2003dh DATE: 03/04/25 02:57:32 GMT FROM: Krzysztof Z. Stanek at CfA D. Zaritsky (U. Arizona), M. Bolte (UCSC), P. M. Garnavich (Notre Dame), A. Z. Bonanos and K. Z. Stanek (CfA) report: Spectra of the optical afterglow of GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) and supernova 2003dh (Garnavich et al. IAUC 8114) were obtained with the 6.5-m MMT on April 24.15 (UT) and with the Keck-II telescope and ESI spectrograph on April 24.36. Preliminary analysis of the spectra show broad peaks at 560 nm, 450 nm and a sharp break in the continuum at 390 nm (all in the rest frame). The spectrum continues to closely follow the development of SN~1998bw (Patat et al. 2001, ApJ, 555, 900). The feature at 450 nm was not present on spectra of SN 2003dh taken April 6 (Matheson et al. GCN 2107) and suggests a significantly lower photospheric velocity in the current spectrum. SN 1998bw developed the 450 nm feature around maximum light and this implies SN 2003dh is now at or past its maximum. The continuum of SN 2003dh is bluer than SN 1998bw at a similar phase, which suggests that the afterglow light still contributes to the total flux. The April 24 MMT spectrum is available at: http://www.nd.edu/~pgarnavi/grb030329_apr24.jpg This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2170 SUBJECT: GRB 030329, the review of the sky area in plate archive (1950-1998) DATE: 03/04/25 08:39:25 GMT FROM: Valery Petkov at Terskol Observatory A.V. Sergeev ( IC AMER observatory, Terskol), V.V. Golovnya, T.P. Sergeeva, L.K. Pakuliak, L.N. Kizyun, S.V. Shatohina. (Main Astronomical Observatory, Kiev) We have undertaken the review of the sky area of GRB 030329 (Peterson & Price, GCN 1985) on astronegatives, collected in Ukrainian NAS Main astronomical observatory plate archive (1950-1998). All the plates, covered the area with GRB 030329, were taken for an analysis. The comprehensive investigation of these images shows nothing at this location. The most reportable results are given in the table: Y M D.UT UT M T N Prg Dim,cm 1 19820324.853230 20:28:39 15.2 DWA 34 FON 30x30 2 19820324.853230 20:28:39 15.2 DWA 35 FON 30x30 3 19900228.938966 22:32:07 14.6 DWA 1613 FON 30x30 4 19910411.813130 19:30:54 15.0 DWA 1772 FON 30x30 5 19920228.926992 22:14:52 14.6 DWA 1968 FON 30x30 6 19810226.866267 20:47:25 13.1 DWA 1893 MP 30x30 19810226.873539 20:57:54 13.1 DWA 1893 MP 30x30 19810226.879171 21:06:00 13.1 DWA 1893 MP 30x30 7 19810226.879171 21:06:00 13.2 DWA 1894 MP 30x30 19810226.879171 20:47:25 13.2 DWA 1894 MP 30x30 19810226.879171 20:57:54 13.2 DWA 1894 MP 30x30 8 19860404.842854 20:13:43 13.6 DWA 2879 MP 30x30 19860404.848484 20:21:49 13.6 DWA 2879 MP 30x30 19860404.853217 20:28:38 13.6 DWA 2879 MP 30x30 9 19860404.842915 20:13:48 13.8 DWA 2880 MP 30x30 19860404.845126 20:16:59 13.8 DWA 2880 MP 30x30 19860404.845183 20:17:04 13.8 DWA 2880 MP 30x30 10 19860408.845126 20:16:59 13.2 DWA 2883 MP 30x30 19860408.847777 20:20:48 13.2 DWA 2883 MP 30x30 19860408.850548 20:24:47 13.2 DWA 2883 MP 30x30 11 19860408.845183 20:17:04 13.2 DWA 2884 MP 30x30 19860408.847835 20:20:53 13.2 DWA 2884 MP 30x30 19860408.850605 20:24:52 13.2 DWA 2884 MP 30x30 12 19820326.833255 19:59:53 13.5 DWA 2324 AREA 30x30 19820326.847106 20:19:50 13.5 DWA 2324 AREA 30x30 13 19820326.833255 19:59:53 13.6 DWA 2325 AREA 30x30 19820326.847106 20:19:50 13.6 DWA 2325 AREA 30x30 M - limited mag. T - telescope; N - plate number; Prg - Observational Project; DWA - Double Wideangle Astrograph (D/F=40/2000, M=103"/mm) of the Ukrainian NAS Main astronomical observatory in Kiev (Marsden's number - 83); FON - Project Photographic Review of Northern Sky [3]; AREA - Projects of Special Programm of Photographic Review in areas with special sky objects [1,2]; References: 1. L.Pakulyak , N.Kharchenko, E.Izhakevich, V.Golovnya, V.Kisljuk, V.Andruk. Data base of photographic observations of celestial bodies of Golosiiv observatory. Baltic Astron. 6, 1997. 2. L.Pakulyak, N.Kharchenko, E.Izhakevich, V.Golovnya, V.Andruk, V.Kisljuk. Data base of photographic observations of celestial bodies of Golosiiv observatory in Kiev. Newsletters of IAU WG "Wide-field imaging" No 9, 1997 3. V.Kislyuk, A.Yatsenko, G.Ivanov, L.Pakuliak, T.Sergeeva. The FON Astrographic catalogue (FONAC): version1.0. Proc. of Journees 1999 and IX Lohrmann-Kolloquium "Motion of celestial bodies, astromerty and astronomical reference frames", Drezden, September 13-15,1999 This message may be cited. ----------------------------------------------------------------------------- Centre Astronomical and Medico-Ecological Researches of Academy of Sci. Observatory at peak Terskol, Russia. Phone (866-39)-71406 ----------------------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2171 SUBJECT: GRB030329, SPM optical observations DATE: 03/04/25 11:53:46 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov, G. Tovmassian, M. Richer (OAN SPM IA UNAM, Ensenada, Mexico) report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) using 1.5m telescope of OAN-SPM Observatory, BC, Mexico. A set of exposures in UBVRI Bessel filters was obtained 24 April and 25 April under photometric and good seeing conditions. Standard stars RU 149 from Landolt's catalogue were used for photometric calibrations in the each night. The results of photometry of summed images are following: 24 April Texp. Filter Mag. UT 5:50 5400sec U 21.76(12) UT 6:56 4800sec B 21.51(6) UT 5:54 2400sec V 20.73(4) UT 6:30 3300sec R 20.17(5) UT 6:10 2400sec I 19.90(5) Corresponding color indexes are U-B = 0.25(14) B-V = 0.78(7) V-R = 0.56(6) R-I = 0.27(6) 25 April Texp Filter Mag. UT 5:10 5400sec B 21.63(5) UT 7:30 3600sec V 21.72(4) UT 6:17 2400sec R 20.16(5) UT 8:00 3600sec I 20.01(5) The magnitudes no changed during those nights. The OT source looks like a point-like object. Two faint extended objects detected nearly OT position. O1: 10:44:50.03 J2000 +21:31:10 R~22.5 distance from OT is about 7" O2: 10:44:49.4 J2000 +21:31:14 R~22.9 distance from OT is about 9" This message may be cited //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2172 SUBJECT: GRB030329, SPM optical observations (Correction) DATE: 03/04/25 21:02:48 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov reports: I had a type in GNC2171. The V magnitude at 25 April UT 7:30 GNC2171 is 20.72(4). Thanks Dr. Arnon Dar and Dr. Daniele Malesani for note it. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2176 SUBJECT: GRB030329 observed as a sudden ionospheric disturbance (SID) DATE: 03/04/28 22:38:19 GMT FROM: Doug Welch at McMaster U,PhysAstro. P.W. Schnoor, D.L. Welch, G.J. Fishman and A. Price report, on behalf of the AAVSO GRB-SID Network, on the detection of GRB030329 as a sudden ionospheric disturbance (SID), observed by Peter Schnoor of Kiel, Germany. A disturbance of the Earth's ionosphere was observed coincident with the HETE detection of GRB030329. This SID was seen as an increase in the signal strength from a Low Frequency (LF) radio beacon received in Kiel, transmitted as a time signal from station HBG (75 kHz) near Geneva, 920 km from the receiver. (Note: This is not a radio detection of GRB030329; this disturbance was caused by the prompt X-rays and/or gamma-rays from GRB030329 ionizing the upper atmosphere and modifying the radio propagation properties of the Earth's ionosphere.) Due to the sub-burst longitude and latitude and the geographical distribution of LF/VLF beacons and monitoring stations, this was the only recording (positive or negative) where GRB030329 illuminated the ionosphere along a signal path. Several plots of the SID detection, including one with an overlay of the HETE X-Ray lightcurve are available at the URL http://www.qsl.net/df3lp/projects/sid/index.html Additional details of the observation are also available at this site. While this type of observation is not yet quantitative, future observations of enough GRBs may allow a quantitative measurement to be made of the prompt, total ionizing flux (X-rays and gamma-rays) incident at the Earth over an extremely broad energy range. This measurement is not now attainable with any single spacecraft and will not be, until the launch of the NASA GLAST mission in 2006. Previously, at least three other transient, high-energy sources have produced detectable ionospheric disturbances, as measured with VLF receivers: GRB830801 (Fishman and Inan, Nature v.331, p.418, 1988); XRF 020427 (GCN 1394), and the Aug. 27, 1998 super-flare from SGR 1900+14 (Inan, et al., Geophys. Res. Lett., v.26, p.3357, 1999). The AAVSO SID-GRB network is a worldwide network of observers monitoring VLF and LF beacons for SIDs of non-solar origin. The AAVSO Solar Committee has been monitoring and reporting solar-induced SIDs since the 1950's. This group intends to continue and expand this monitoring network. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2179 SUBJECT: GRB 030329 Oprical observations in Rozhen observatory DATE: 03/04/30 11:30:26 GMT FROM: Evgeni Semkov at Inst.of Astronomy,Bulgaria E. Semkov (Institute of Astronomy, Sofia, Bulgaria) report: We continue our observations of the afterglow of HETE burst (H2652) GRB 030329 (Peterson & Price, GCN 1985; Torii: GCN 1986) with the 2m RCC telescope of the National Astronomical Observatory Rozhen (Bulgaria). We obtained four 300 s exposures on 25 Apr UT 19:30 with Photometrics CCD camera and Rc filter. The observations were carried out under good seeing and atmospheric conditions. Using field photometry of Henden (GCN2082) and after co-adding of frames we estimate the brightness of the optical afterglow as Rc = 20.21 +/-0.09. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2191 SUBJECT: GRB 030329, BVRI photometry DATE: 03/05/02 01:07:12 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (UBAI), A.Pozanenko (IKI), V.Rumyantsev (CrAO), G.Beskin (SAO) on behalf of large collaboration report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) ÃÛÅÒ 1.5m telescope of Mt.Maidanak High-altitude Observatory (UBAI). Several BVRI Bessel images were obtained on April 20, 25 and 27. The seeing on Apr.25 was in range of 1-1.5 arcsec, and on Apr.27 is less than 1 arcsec for all filters. Based on filed photometry by A. Henden (GCN 2082) we estimate the OT magnitudes: Mid time exposure filter mag err UT, Apr. sec 20.664 1200 B 21.09 0.10 20.648 1200 R 19.91 0.06 25.745 2400 B 21.83 0.10 25.776 1800 V 20.76 0.08 25.723 1800 R 20.13 0.05 25.799 1800 I 20.01 0.11 27.731 2100 B 21.62 0.12 27.731 1500 V 20.94 0.11 27.731 2400 R 20.24 0.05 27.731 1500 I 19.70 0.10 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2193 SUBJECT: GRB 030329 Optical Observations DATE: 03/05/02 07:55:19 GMT FROM: Jens Hjorth at U.Copenhagen L. Kindt, H. H. Andersen and A. Jakobsen (University of Copenhagen) report: We have obtained V, R and I-band images of the error box of GRB 030329 (Peterson & Price 2003, GCN 1985) using the Danish 0.4-m Brorfelde Schmidt telescope. We compared our images with the Digitized Sky Survey and detected the optical afterglow of GRB 030329 at: RA: 10:44:50.03 Dec: +21:31:18.1 +- 0.5 arcsec (J2000) The following table contains our data for this object: Date Time(UT) Exposure time(s) Band Magnitude -------------------------------------------------------------- Mar 29 20:21 1080 R 14.54+-0.01 Mar 29 20:58 600 R 14.57+-0.01 Mar 30 19:16 360 R 16.35+-0.05 Mar 30 19:30 540 R 16.35+-0.04 Mar 31 21:18 540 R 16.80+-0.04 Apr 7 21:00 270 R 19.24+-0.29 Apr 7 21:08 540 R 19.20+-0.18 Apr 7 21:45 1620 R 18.92+-0.13 Apr 7 22:26 1800 I 18.82+-0.14 Apr 7 23:06 1800 V 19.09+-0.14 -------------------------------------------------------------- Time is measured from start of observation. The photometry of the afterglow is with respect to 11 stars from Henden (GCN 2023). The quoted errors in the I and V bands may be underestimated. We fitted a single power law to our data in the R-band. We found a power law slope of 1.31 +- 0.04. The combined images are made available at: http://www.fys.ku.dk/~kindt/bachelor/ Thanks to J. Hjorth, K. Augustesen, and H. Pedersen. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2198 SUBJECT: GRB030329: RTT150 optical observations and upper limit for a host DATE: 03/05/03 14:59:53 GMT FROM: Irek Khamitov at TUG I. Khamitov (TUG), I.Bikmaev (KSU), M.Parmaksizoglu (TUG); N. Sakhibullin, V. Suleymanov (KSU); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko, M.Gilfanov (IKI); Z. Aslan, O.Golbasi (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); report: We continue observations of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with the 1.5-m Russian-Turkish Telescope RTT150 at TUG. A set of 18 exposures by 5 min. duration each with Rc Bessell filter has been obtained on the night May 02/03, 2003, under good photometric conditions and average seeing of 1.3 arcsec. A new TE Andor CCD with Marcony back-illuminated 2048 x 2048 chip was used as the detector with the working chip temperature -60 C. We grouped exposures by 3 frames and results of Rc photometry relative to the stars from Henden (GCN 2082) are given in the Table below. We integrated all exposures and made PSF subtraction from the OT's star-like structure to find the presence of the host galaxy. No object brighter than R ~ 23.5 mag was found at the position of the afterglow. A faint extended detail is seen at 1 arcsec west side of OT position on the residual image at the brightness level of limiting magnitude. The limiting magnitude is defined by fringe structures. We confirm the presence of two bright enough sources O1 and O2 at the 7 and 9 arcsec distances from OT indicated by S.Zharikov et al (GCN 2171) and estimated their magnitudes as R = 22.1 and 22.4 correspondingly. Table of Rc photometry UT R Rerr May 2.774 20.51 0.07 May 2.786 20.65 0.07 May 2.800 20.34 0.06 May 2.813 20.62 0.08 May 2.826 20.63 0.07 May 2.838 20.61 0.07 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2203 SUBJECT: GRB 030329: all-sky CCD images by K. Shiokawa immediately after the burst DATE: 03/05/05 02:28:50 GMT FROM: Taichi Kato at Kyoto U GRB 030329: all-sky CCD images by K. Shiokawa immediately after the burst T. Ishida (Nishi-Harima Astronomical Observatory), T. Kato (Kyoto U) and K. Shiokawa (Nagoya U) report: K. Shiokawa (Nagoya U) is taking all-sky CCD images at 572.5nm for monitoring night sky light. As a preliminary inspection, we have examined four images immediately after the GRB 030329 burst time, whose exposures started at 11:27, 11:57, 12:27 and 12:57 UT, respectively. All images are taken every 30 minutes with 105 seconds exposure. No obvious optical afterglow was detected on these images. A quick look of each image has yielded an upper limit of about 6.4 mag. Observation system used are described in Shiokawa, K. et al. 1999, Earth, Planets, and Space, 51, 887-896, and Shiokawa, K. et al. 2000, Adv. Space Res., 26, 1025-1028. Further analysis of the images is in progress. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2212 SUBJECT: GRB 030329: High-Resolution Spectroscopy of the Host DATE: 03/05/07 08:27:34 GMT FROM: Josh Bloom at Harvard/CFA GRB 030329: High-Resolution Spectroscopy of the Host J. S. Bloom (CfA/Harvard), N. Morrell (Las Campanas Observatory), S. Mohanty (CfA) report: "Beginning May 7.01 UT, we observed the position of the optical transient (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN #1997) using the Magellan Inamori Kyocera Echelle (MIKE) Camera on the Baade 6.5 m at the Las Campanas Observatory. The dispersion at 7600 Angstrom (Ang) is 0.053 Ang/pixel. The narrow emission lines (Martini et al., GCN #2013; Della Ceca et al., GCN #2015; Greiner et al. #2020; Caldwell et al., GCN #2053; Eracleous et al., GCN #2117), presumably from the host galaxy, are well detected in each 1800 sec exposure. Using a fit to the H-alpha line, we find the heliocentric systemic redshift of the host galaxy is: z = 0.168541 +/- 0.000004 (statistical error). This is most precise emission line redshift of a GRB host galaxy reported to date. This redshift is consistent with the host redshift reported previously (Greiner et al., GCN #2020; Eracleous et al., GCN #2117; Caldwell et al., GCN #2053). The emission lines are resolved in the dispersion direction with a FWHM (H-alpha) of 1.44 +/- 0.02 Ang (56.1 km/s). While the core of the emission lines can be fit by a Gaussian, extended wings of emission and similar velocity substructure within the profiles are apparent. In particular, we identify a faint emission structure that is ~66 km/s to the red of the central core. The host plus OT continuum is discernible in each echelle order redward of ~7000 Ang. In ~0.4 arcsecond seeing the emission from the host plus OT is still unresolved in the spatial direction. The compactness, the relatively low mass implied by the velocity structure of the emission lines, and the faintness of the host (Blake & Bloom; GCN #2011) all continue to support the notion of the host of GRB 030329 as an intrinsically underluminous galaxy (Eracleous et al., GCN #2117). Despite the low overall star formation rate of the host (Caldwell et al., GCN #2053), given the high equivalent widths of the detected lines, the star-formation rate per unit mass may be appreciable." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2217 SUBJECT: GRB 030329: Optical limit (contemporaneous photography) DATE: 03/05/08 08:06:15 GMT FROM: Ken ichi Torii at RIKEN K. Sasaki (Japan Fireball Network), M. Tomita (Japan Fireball Network), K. Ohnishi (Nagano National College of Technology), and K. Torii (RIKEN) report: The sky area of GRB 030329 (Vanderspek, et al., GCN 1997) was contemporaneously photographed on 2003 March 29 by K. Sasaki and M. Tomita with all-sky patrol cameras. In the frames tabulated below, no significant object is found at the position of the optical afterglow (Peterson and Price, GCN 1985; Torii, GCN 1986). We derive preliminary upper limits for the optical transient by comparison with either 41 LMi (V=5.1) or 54 Leo (V=4.3) which is significantly detected. Data from KS ----------------------------- Start(UT) End(UT) Mag. ----------------------------- 10:40:00 10:59:58 >5.1 11:00:00 11:19:58 >5.1 11:20:00 11:39:58 >5.1 11:40:00 11:59:58 >5.1 ----------------------------- Data from MT ----------------------------- Start(UT) End(UT) Mag. ----------------------------- 10:30:00 10:59:00 >4.3 11:00:00 11:29:00 >4.3 11:30:00 11:59:00 >4.3 12:00:00 12:29:00 >4.3 12:30:00 12:59:00 >4.3 ----------------------------- Effective exposure for each frame, 399 s for KS and 580 s for MT, is 1/3 of the elapsed time due to a rotating shutter in front of the optics. Details of the instruments, originally designed for detecting fireballs (bright meteors), are as follows. Position of the observatory: KS Iwate, Japan 141d08m24s E, +39d28m22s N, 100m altitude Position of the observatory: MT Ishikawa, Japan 136d48m01s E, +36d55m39s N, 10m altitude The following instruments are common to the two observatories. Camera: Canon T70 with command back Optics: Canon New FD 15mm f/2.8 full-frame fish-eye lens, used at f/2.8 Filter: No Film: Kodak TMAX 400 Rotating shutter: Open fraction is 1/3 --------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2219 SUBJECT: GRB030329, BVRI photometry DATE: 03/05/08 17:05:46 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (UBAI), A.Pozanenko (IKI), V.Rumyantsev (CrAO), G.Beskin (SAO) on behalf of large collaboration report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) with 1.5m telescope of Mt.Maidanak High-altitude Observatory (UBAI). Several BVRI Bessel images were obtained on May 3, and 5 under good photometric and seeing conditions (1-1.5 arcsec). Based on filed photometry by A. Henden (GCN 2082) we estimate the OT magnitudes: Mid time exposure filter mag err UT, May. sec 03.700 2400 B 22.14 0.13 03.726 1800 V 21.29 0.10 03.670 1800 R 20.87 0.09 03.750 1800 I 20.08 0.12 05.690 3000 B 22.08 0.11 05.722 1800 V 21.33 0.08 05.655 1800 R 20.74 0.10 05.746 1800 I 20.28 0.15 Multicolor observations will be continued. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2225 SUBJECT: GRB 030329: Optical limit (contemporaneous imaging) DATE: 03/05/12 03:55:03 GMT FROM: Ken ichi Torii at RIKEN Y. Okamoto (NIFTY-Serve Space Forum), K. Ohnishi (Nagano National College of Technology), and K. Torii (RIKEN) report: The sky area of the GRB 030329 (Vanderspek, et al., GCN 1997) was contemporaneously imaged with the Yatsugatake Camera between 2003 March 29 10:00 UT (97 minutes before burst) and 14:00 UT. The Yatsugatake Camera is an ultra wide field (85 x 70 deg) video camera (focal length 3.5mm, f/1.4 lens equipped with Sony XC-75) placed at an altitude of 1000m in Yatsugatake, Japan. Images are output in NTSC format after 8-s (on-chip) integrations, stored to frame memory (MSJ SS-10), and recorded to timelapse video tape. The camera has built-in infrared-cut filter while no additional filter is used. By now, we have digitized and inspected the data between 10 minutes before and after the burst and created running mean images of four consecutive frames. In these images, a neighboring V=5.1 star (41 LMi) is clearly detected while no transient stellar object brighter than 41 LMi is seen at the position of the optical afterglow (Peterson and Price, GCN 1985; Torii, GCN 1986). We therefore derive preliminary upper limit of 5.1 mag for an optical transient associated with this GRB on continuous 32-s time bins between 2003 March 29 11:27 UT and 11:47 UT. Further analysis is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2204 SUBJECT: GRB030329: RTT150 optical observations and upper limit for a host DATE: 03/05/06 13:10:08 GMT FROM: Irek Khamitov at TUG I. Khamitov (TUG), I.Bikmaev (KSU), M.Parmaksizoglu (TUG); N. Sakhibullin, V. Suleymanov (KSU); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko, M.Gilfanov (IKI); Z. Aslan, O.Golbasi (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU); The combined 90 min image of the GRB 030329 optical afterglow (Petersonand Price, GCN 1985) obtained with the 1.5-m Russian-Turkish Telescope RTT150 at TUG in Bessell Rc filter on the night May 02/03, 2003, can be found in http://www.tug.tubitak.gov.tr/gozlemler/grb030329/grb030329.html On the web-site we present images of TO field befor and after PSF-model substraction. The PSF substracted image was used for the estimation of upper limit of host galaxy (Khamitov at. al, GCN 2198). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2220 SUBJECT: GRB030329: RTT150 optical observations DATE: 03/05/09 14:50:05 GMT FROM: Irek Khamitov at TUG I.Bikmaev (KSU), I. Khamitov (TUG); N. Sakhibullin, V. Suleymanov (KSU); R. Burenin, R. Sunyaev, D. Denissenko, M. Pavlinsky, O. Terekhov, A. Tkachenko, M.Gilfanov (IKI); Z. Aslan, O.Golbasi (TUG); U. Kiziloglu, A. Alpar, A. Baykal (METU);   report:   We continue observations of the GRB 030329 optical afterglow (Peterson and Price, GCN 1985) with the 1.5-m Russian-Turkish Telescope RTT150 at TUG.  During the nights of May 3,4,7, 2003,  series of  5 and 15 min exposures with V-filter have been obtained under good photometric conditions and average seeing of 1.3 arcsec.  ANDOR TE 2048 x 2048 CCD has been used as the detector.   Results of OT our photometry (based on Henden's list, GCN 2082 ), averaged over for each night, are as follow:     Midtime  Vmag   Verr Total Exp. sec     03.86UT  21.40  0.07 10200   04.86UT  21.33  0.07 11400   07.86UT  21.60  0.08  9300   Additional note: Probably, a moved object was found in the vicinity of the OT. This object was labeled as "O2" in Zharikov et al. (GCN 2171) and as "A" in  Blake and Bloom (GCN 2011).   We integrated all the three night  observations into one image and  estimated the magnitudes of the sources  in the afterglow vicinity as                V      Verr   O1 (B) 23.0   0.2 O2 (A) 22.6   0.1   Using the coordinates of the reference stars   from Henden's list  we have determined the positions of OT  and O1, O2 as   RA(2000.0) DEC(2000.0)   OT 10:44:49.958 21:31:17.50 O1 10:44:50.039 21:31:10.86 O2 10:44:49.373 21:31:15.02   The comparision of coordinates with those given by Blake and Bloom has shown that position of the source "A" is different by 6 arcsec while  the  the position of the source "B" is in agreement  within  0.5 arcsec positional error of Blake and Bloom.   We estimate the color of O2 as  V-R = 0.2,  and of O1 as V-R = 0.9 (R mag estimates are taken from Khamitov et al., GCN 2198)   Taking into account the apparent magnitudes, color and considerable positional shift, we suppose that this is an object nearer to the Sun. Additional observations are encouraged.    This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2228 SUBJECT: HETE GRB030329, correction to Rc Observations in Loiano DATE: 03/05/13 18:01:31 GMT FROM: Graziella Pizzichini at IASF/CNR,Bologna G. Pizzichini and P. Ferrero (IASF/CNR, Bologna), C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University), A. Righini (Firenze University) and I. Bruni (Bologna Astronomical Observatory) report: The Rc magnitude quoted by us for the OT of GRB030329 in GCN 2136 was not correct, due to a bad subtraction of the background in conditions of nearly full moon. By coadding the three exposures listed below: -- UT start exptime filter ----------------------------- Apr. 13.8783 300s Rc Apr. 13.8824 300s Rc Apr. 13.8865 300s Rc and using the star at RA = 161.231899, DEC = 21.522793, in the new field photometry given by Henden, GCN 2082, we now find Rc = 19.53 +- 0.20 . In the following night, by coadding the exposures: - UT start exptime filter ----------------------------- Apr. 14.8879 300s Rc Apr. 14.8923 300s Rc Apr. 14.8973 300s Rc and still under very unfavorable conditions because of the moon, we find Rc = 20.27 +- 0.33. Errors quoted are 1 sigma. We thank Dr. A. Henden for promptly signalling the problem to us and Dr. E. Palazzi for useful advice. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2241 SUBJECT: GRB030329: XMM-Newton observation DATE: 03/05/22 14:29:47 GMT FROM: Sandro Mereghetti at IASF/CNR A.Tiengo (IASF-Milano), S.Mereghetti (IASF-Milano), and N.Schartel (XMM-Newton SOC, Villafranca) report: An XMM-Newton TOO observation of GRB030329 (Ricker et al. IAU Circ. 8101) has been performed on May 5, 2003 from 12:30 to 24 UT. A source positionally consistent with the optical transient of GRB030329 (Price and Peterson, GCN 1987) has been detected with the EPIC MOS and PN cameras. Its spectrum can be fit by a power law with photon index 2.0+/-0.25 and absorption smaller than 6x10^20 cm^-2. The 2-10 keV observed flux is (2.1+/-0.6)x10^-14 erg cm^-2 s^-1. Comparison with previous X-ray observations obtained with RXTE (Marshall and Swank, GCN 1996; Marshall et al., GCN 2052) indicates that the X-ray flux decay is consistent with a power law F ~ t^(-1.7). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2242 SUBJECT: GRB 030329 Optical Observations DATE: 03/05/22 14:45:48 GMT FROM: Javier Gorosabel at LAEFF-INTA, Madrid J. Gorosabel (IAA-CSIC/STScI), A. de Ugarte Postigo (IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC), A. Fruchter (STScI), A. Levan (U. Leicester/STScI), S. Guziy (IAA-CSIC), J.M. Castro Cerón (STScI), A. Guijarro (CAHA), A. Aguirre (CAHA), report: "We have imaged the field of the GRB 030329 (GCN 1997) in four optical colours with the 2.2 m (+BUSCA) telescope at the Observatorio de Calar Alto on 20.9148-20.9670 UT May 2003. Aperture photometry of the counterpart yielded Ic = 20.92 +/- 0.07. The zero point is based on the star located at R.A.(J2000) = 10:44:42, Dec(J2000) = +21:32:31.6 with I = 15.432 (GCN 2082). Further observations are planned." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2243 SUBJECT: GRB 030329: HST ACS Observations of the Host DATE: 03/05/23 18:34:25 GMT FROM: Andrew S. Fruchter at STScI A. Fruchter (STScI), A. Levan (U. Leicester/STScI), R. Hook (ST-ECF/STScI), N. Pirzkal (ST-ECF), J. Gorosabel (STScI/IAA-CSIC), P. Garnavich (Notre Dame), P. Nugent (LBNL), S. Thorsett (UCSB), A. Castro-Tirado (IAA), J.M. Castro-Ceron (STScI), C. Kouveliotou (USRA), S.T. Holland (Notre Dame), J. Hjorth (U. Copenhagen), and N. Tanvir (U. Hertfordshire) report for the GOSH collaboration: GRB 030329 has been observed at three epochs by HST: 15/16 April, 21/23 April and 12/13 May. During all epochs UV (ACS/HRC), optical (ACS/WFC) and NIR (NICMOS) images were obtained. Additionally, in the first epoch an ACS grism spectrum was taken, and in the second epoch a STIS optical spectrum, delayed from the first epoch by a gyrocope failure, was also obtained. Here we report on aspects of the imaging and grism spectroscopy which provide a unique contribution from HST: information on the nature of the host. All the ACS images show the host extending to approximately ~0."5 from the OT to the west, with a PA of approximately 230 degrees. In the most recent ACS/WFC images the OT has faded sufficiently to allow a reasonable subtraction of the OT from the host, particularly in the F435W and F606W filters where the blue color of the host provides greater contrast against the redder OT than in the F814W image. We find the magnitude of the host to be approximately V=22.7 +/- 0.3, where the uncertainty is dominated by the subtraction of the OT and the unknown contribution to the host magnitude by faint outerlying areas. This apparent magnitude corresponds to an absolute magnitude of about -16.5, very similar to that of the SMC. The host can also be seen clearly in the UV ACS/HRC F250W images taken on May 12. The OT appears to lie at the end of a bar-like structure approximately 0."25 across, which at the ~600 Mpc angular-diameter distance of the GRB corresponds to a length of about 800 pc. The separation of the host from the OT can also be discerned in the grism spectrum, where the emission lines of the host are seen to be offset from spectral continuum of the OT. Although the spatial projection of the grism makes this somewhat uncertain, the Halpha emission of the host appears to be fairly well centered on host's blue light. Images of the OT and host and the 2-d grism spectrum can be seen at http://www.stsci.edu/~fruchter/GRB/030329 //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2244 SUBJECT: GRB 030329/SN 2003dh: Possible increase in brightness DATE: 03/05/25 03:35:52 GMT FROM: Krzysztof Z. Stanek at CfA K. Z. Stanek, D. W. Latham (Harvard-Smithsonian CfA) and M. E. Everett (Planetary Sciences Institute) report: We imaged the SN 2003dh (Matheson et al. GCN 2107, 2120; Garnavich et al. IAUC 8108, 8114; Stanek et al. astro-ph/0304173) associated with the GRB 030329 with the FLWO 1.2-m telescope between May 20 UT 05:45 and May 23 UT 04:30 (51.75 and 54.7 days after the burst) using standard R filter. The transient seems to brighten during that time: UT R dR Filter Texp ---------------------------------------------------- 2003-05-20 05:45 21.575 0.07 R 4x900 sec 2003-05-21 05:00 21.689 0.11 R 4x900 sec 2003-05-22 05:45 21.429 0.08 R 4x900 sec 2003-05-23 04:30 21.321 0.09 R 5x900 sec Observations using larger telescopes, also in other bands, are strongly encouraged. Any use of these data should include proper reference to this GCN. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2245 SUBJECT: GRB030329, Optical observations DATE: 03/05/26 07:13:08 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov(OAN IA UNAM), V. Chavushyan, R. Mujica (INAOE) report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) using the 2.1m telescope of the "Guillermo Haro" Observatory in Cananea, Sonora, Mexico with the Landessternwarte Faint Object Spectrograph and Camera (LFOSC). The I image was obtained on April 26 with time of exposure 1200s. Several R band images with time of exposure 1800s were obtained on April 28,30 and May 2,5,6 and 8 under good photometric conditions. Based on filed photometry by A. Henden (GCN 2082) we estimate of OT magnitudes: Date Time(UT) Band Magnitude ---------------------------------------------- April 26 03:21 I 20.02(10) April 28 03:20 R 20.49(7) April 30 03:24 R 20.60(8) May 2 03:28 R 20.64(8) May 5 03:55 R 20.90(12) May 6 03:09 R 20.90(12) May 8 03:43 R 20.88(11) This message may be cited. //////////////////////////////////////////////////////////////////////// //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2247 SUBJECT: GRB 030329: optical photometry at various french observatories DATE: 03/05/26 12:02:10 GMT FROM: Michel Boer at CESR-CNRS A. Klotz and M. Boer (CESR France) report magnitudes of GRB 030329 obtained at TAROT-Calern, at TBL-Pic du Midi and by members of AUDE (Association des Utilisateurs de Detecteurs Electroniques - Electronic Device Users Association). All images are photometrically calibrated by Alain Klotz using the reference stars given by A. Henden (GCNC 2023). Red filtered measurements : DATE Observers Diam(mm) filter int(s) R +/- observatory day-GRB 2003-04-12T20:21:10 SD 600 R 5400 19.30 0.18 Lantelme 14.3628 2003-04-21T00:20:37 EB&al. 600 R 3000 20.25 0.75 Pic Du Midi 22.5291 2003-04-21T22:32:00 OM&YM&PM 820 R 600 19.9 0.4 Belesta 23.4537 2003-05-04T21:32:41 CC&SD 600 R 2760 22.74 0.37 Lantelme 36.4124 Infrared filtered measurements (afteglow not detected) : DATE Authors Diam(mm) filter int(s) mag +/- observatory day-GRB 2003-04-17T23:30:00 AK&CB 2000 K 3060 >18.2 Pic du Midi 19.4939 2003-04-18T01:26:00 AK&CB 2000 J 3960 >18.6 Pic du Midi 19.5745 Unfiltered measurements converted to the R band : DATE Authors Diam(mm) filter int(s) R +/- observatory day-GRB 2003-04-01T00:25:00 AK 200 C 360 16.72 0.45 Guitalens 2.5321 2003-04-04T20:30:00 TAROT 250 C 600 18.55 0.36 Calern 6.3689 2003-04-06T21:48:21 ML 318 C 2550 18.58 0.33 Dax 8.4234 2003-04-07T22:05:00 TM&BC 600 C 400 18.68 0.23 Pic du Midi 9.4349 2003-04-08T20:30:00 TAROT 250 C 600 18.81 0.44 Calern 10.3690 2003-04-21T22:05:00 OM&YM&PM 820 C 900 19.93 0.15 Belesta 23.4315 Observers AK = Alain Klotz ML = Mathieu Lahitte=20 TM&BC = Thierry Midavaine & Bernard Christophe SD = Serge Deconhiout AK&CB = Alain Klotz & Coralie Berteloite OM&YM&PM = Olivier Maury, Yves Megret, Patrick Martinez EB&al. = Eric Barbotin, Cathy Dupeyre, Alain Laffont, Audrey Cazenave CC&SD = Cyril Cavadore & Serge Deconhiout Complementary data (images) : http://www.cesr.fr/~klotz/grb030329/results.html This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2249 SUBJECT: GRB 030329: Planned XMM-Newton Observation DATE: 03/05/27 11:42:09 GMT FROM: Norbert Schartel at XMM-Newton/ESA The XMM-Newton SOC has scheduled a Target of Opportunity observation of GRB 030329 in revolution 635 (28th to 30th of May 2003). Details of the instrumental setup can be found at (Observation ID 0128531501): http://xmm.vilspa.esa.es/external/xmm_sched/sched_obs_srch_frame.shtml //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2254 SUBJECT: GRB 030329: Optical Observations DATE: 03/05/28 18:42:55 GMT FROM: Haw Cheng at UNC H. Cheng, M. Bayliss, D. Reichart, J. Moran, M. Nysewander, M. Schwartz, and P. Holvorcem report on behalf of the UNC GRB team of the FUN GRB collaboration: We observed the afterglow (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN 1997) with the 32-inch Tenagra II telescope in IcRcVIc on April 2nd and 3rd, in IcIc on April 4th and 5th, and in Ic on April 6th, 7th, 8th, 9th, and 10th. Between April 2nd and 10th, we find that the afterglow faded from Ic = 16.9 mag to Ic = 18.9 mag. Our 1-sigma error bars are typically less than 0.02 mag. Fitting a four-parameter model to the data, where the parameters are the temporal index alpha, the spectral index beta, a normalization parameter, and a parameter that measures the level of of systematic (i.e., non-statistical) fluctuations in the light curve, we find that alpha = -1.70(+0.13)(-0.14), beta = -1.38(+0.20)(-0.20), and that the fading afterglow is fluctuating at the 17.5(+3.8)(-3.5)% level at these times. We note that the measured spectral index is too steep given the measured temporal index and the post-jet break time relations of Sari, Piran, & Halpern (1999, ApJ, 519, L17). Possible explanations include: 1. The light curve had not yet reached its asymptotic temporal index, which if the afterglow is unextinguished would be alpha = -2.76 +- 0.20 if the cooling break is redward of the observed bands or alpha = -3.76 +- 0.20 if the cooling break is blueward of the observed bands; or 2. The light curve is extinguished. Although this does not appear to be the case at earlier times, this could be the case at later times if dust was destroyed within the initial opening angle of the jet, but then the jet expanded laterally behind undisturbed dust. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2255 SUBJECT: GRB 030329: Correction to GCN 2254 DATE: 03/05/28 20:26:22 GMT FROM: Haw Cheng at UNC We have noticed a minor numerical error near the end of GCN 2254. Here is a corrected (and slightly expanded) version: H. Cheng, M. Bayliss, D. Reichart, J. Moran, M. Nysewander, M. Schwartz, and P. Holvorcem report on behalf of the UNC GRB team of the FUN GRB collaboration: We observed the afterglow (Peterson & Price, GCN 1985) of GRB 030329 (Vanderspek et al., GCN 1997) with the 32-inch Tenagra II telescope in IcRcVIc on April 2nd and 3rd, in IcIc on April 4th and 5th, and in Ic on April 6th, 7th, 8th, 9th, and 10th. Between April 2nd and 10th, we find that the afterglow faded from Ic = 16.9 mag to Ic = 18.9 mag. Our error bars are typically less than 0.02 mag (1 sigma). Fitting a four-parameter model to the data, where the parameters are the temporal index alpha, the spectral index beta, a normalization parameter, and a parameter that measures the level of systematic (i.e., non-statistical) fluctuations in the light curve, we find that alpha = -1.70(+0.13)(-0.14), beta = -1.38(+0.20)(-0.20), and that the fading afterglow is fluctuating at the 17.5(+3.8)(-3.5)% level at these times. Furthermore, these fluctuations appear to be chromatic in nature. We note that the measured spectral index is too steep given the measured temporal index and the post-jet break time relations of Sari, Piran, & Halpern (1999, ApJ, 519, L17). Possible explanations include: 1. The light curve had not yet reached its asymptotic temporal index, which if the afterglow is unextinguished would be alpha = -2.76 +- 0.40 if the cooling break is redward of the observed bands or alpha = -3.76 +- 0.40 if the cooling break is blueward of the observed bands; or 2. The light curve is extinguished. Although this does not appear to be the case at earlier times, this could be the case at later times if dust was destroyed within the initial opening angle of the jet, but then the jet expanded laterally behind undisturbed dust. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2259 SUBJECT: GRB 030329/SN 2003dh: Jitter Episode DATE: 03/05/29 20:36:24 GMT FROM: Krzysztof Z. Stanek at CfA K. Z. Stanek, D. Bersier, M. Calkins, D. L. Freedman and T. Spahr (Harvard-Smithsonian CfA) report: We continued imaging of the SN 2003dh (Matheson et al. GCN 2107, 2120; Garnavich et al. IAUC 8108, 8114; Stanek et al. astro-ph/0304173) associated with the GRB 030329 with the FLWO 1.2-m telescope between May 26 UT 05:00 and May 29 UT 05:00 (57.7 and 60.7 days after the burst) using standard R_c filter. The increase in brightness by >0.3 mag observed by Stanek et al. (GCN 2244) between May 21 and May 23 UT was followed by a decay of ~0.3 mag and then by an increased scatter in the light curve: UT R dR Filter Texp ---------------------------------------------------- 2003-05-26 05:00 21.612 0.06 R 5x900 sec 2003-05-28 04:50 21.456 0.07 R 4x900 sec 2003-05-29 05:00 21.617 0.09 R 4x900 sec The figure showing the light curve since May 20 UT can be accessed at: http://cfa-www.harvard.edu/~kstanek/jitter.jpg We should stress that we have a very extensive data set for this object obtained with exactly the same instrumentation and this "jitter episode" is very unusual when compared to the whole data set and we strongly believe that it is real and it might continue. Therefore, observations using larger telescopes, also in other bands, are strongly encouraged. Any use of these data should include proper reference to this GCN. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2260 SUBJECT: GRB 030329: optical observations DATE: 03/05/31 09:07:43 GMT FROM: Rodion Burenin at IKI, Moscow R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O. Terekhov, A. Tkachenko (IKI); Z. Aslan, O.Golbasi, I. Khamitov (TUG); M.A. Alpar (SU); U. Kiziloglu, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU) report: We observed the GRB 030329 afterglow with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe, Turkey. Our data for May 20 -- 28 are consistent with constant flux of the OT. Using the photometry by Henden (GCN 2082) we measured the following R magnitudes for the OT: Date UT R err 05-20 21:45 21.65 0.28 05-21 21:20 21.41 0.06 05-22 20:30 21.60 0.08 05-24 21:15 21.40 0.10 05-28 21:10 21.55 0.06 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2265 SUBJECT: GRB030329, SPM optical observations DATE: 03/06/02 10:04:32 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov, G. Tovmassian (OAN SPM IA UNAM, Ensenada, Mexico) report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) using 1.5m telescope of OAN-SPM Observatory, BC, Mexico. A set of exposures in VR Bessel filters was obtained of 2 June under photometric and good seeing conditions. Based on field photometry by A. Henden (GCN 2082) we estimate OT (or its host galaxy?) magnitudes: 2 June Texp. Filter Mag. UT 6:00 2400sec V 21.86(10) UT 5:15 3000sec R 21.42(7) The R magnitude no changed during 20 May up to 2 June. (see Burenin et al., GCN 2260). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2268 SUBJECT: GRB030329, further radio observations at GMRT DATE: 03/06/04 10:00:26 GMT FROM: D. Bhattacharya at Raman Research Inst. A. Pramesh Rao and C. H. Ishwara Chandra (NCRA, Pune), D. Bhattacharya (RRI, Bangalore) and A.J. Castro-Tirado (IAA, Granada) report on behalf of a larger collaboration: The afterglow of GRB030329 (Peterson & Price, GCN 1985) was observed with the GMRT for about 5 hours on May 31, 2003. The observations were at 1288 MHz with a bandwidth of 12MHz and effective angular resolution of ~3.5". The flux density of the source seen at the position of the GRB on 31 March and 01 April 2003 (Rao et al, GCN 2073) has increased to 1.1 mJy confirming that the radio source is related to the GRB. The details of the GMRT measurements of GRB030329 at 1288 MHz: Date Time Flux Density 31 May 2003 14-18 UT 1100+/-150 microJy 31 March/01 April 2003 14-22 UT 330+/-100 microJy The quoted error bars are 2-sigma, and include systematic errors of calibration. Note that the flux density at 31 March/01 April epoch has been revised upwards in comparison to that reported in GCN 2073, following a better absolute flux density calibration. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2276 SUBJECT: GRB030329, SPM optical observations (Correction of GCN2075 R band) DATE: 03/06/07 04:06:02 GMT FROM: Sergej Zharikov at OAN IA UNAM S. Zharikov (IA OAN UNAM) reports: The right magnitude of GRB030329 OT in R band of 31 March, 2003 at UT 7:49 was 16.48(3). This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2282 SUBJECT: GRB030329 -- RATAN-600 data in April-May DATE: 03/06/11 17:33:39 GMT FROM: Sergei Trushkin at SAO RAS/Russia Trushkin S.A. (SAO RAS) on behalf of the SAO-IKI collaboration report: We have observed GRB 030329 during four sets with RATAN-600 radio telescope, the mean flux densities of the radio counterpart are given in the table: Frequency 3-7 Apr 13-21 Apr 1-7 May 15-31 May ------------------------------------------------- GHz mJy +- mJy +- mJy +- mJy +- ------------------------------------------------- 3.9 49 10 15 3 15 3 10 3 7.7 33 5 28 5 15 3 18 3 11.2 20 5 47 7 32 6 19 4 The spectral index varied from -0.7 to +1.1, +0.7, +0.75 respectively with rms ~0.15. The May indices are consistent with Nobeyama data (Cir.N2089). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2285 SUBJECT: GRB030329: second XMM-Newton observation DATE: 03/06/19 12:38:20 GMT FROM: Sandro Mereghetti at IASF/CNR A.Tiengo (IASF-Milano), S.Mereghetti (IASF-Milano) and N.Schartel (XMM-Newton SOC, Villafranca) report: A 24 hour long observation of GRB030329 has been obtained with XMM-Newton starting at 21 UT on May 28, 2003. After rejecting high background time intervals, the net exposure time in the EPIC instrument is about 40 ks. The X-ray afterglow is detected at a level of (7+/-3)x10^-15 erg cm^-2 s^-1 (observed flux in the 2-10 keV range). This value is consistent with the late time (t>1 day) flux evolution as a power law with index ~1.9, as reported by Tiengo et al. (astro-ph/0305564). The X-ray spectrum is well fit by a power law with photon index 2.2+/-0.4 and absorption <9x10^20 cm^-2. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2288 SUBJECT: GRB030329, optical observation in May DATE: 03/06/27 22:29:44 GMT FROM: Alexei Pozanenko at IKI, Moscow M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (UBAI), A.Pozanenko (IKI), V.Rumyantsev (CrAO), G.Beskin (SAO), I.Zolotukhin, A.Birykov (SAI MSU) report: We have observed the OT GRB030329 found by B.Peterson and P.Price (GCN 1985) with 1.5m telescope of Maidanak High-altitude Observatory (UBAI). Several VBR Bessel images were obtained in May and June 2003. Based on the field photometry by A. Henden (GCN 2082) we estimate the OT magnitudes: -------------------------------------------- Date2003 Mid UT exp fltr mag err -------------------------------------------- May 07 17:00 1800 R 20.72 0.09 May 07 17:58 3000 B 22.77 0.30 May 07 18:33 1800 V 22.20 0.31 May 13 17:07 1200 R 20.93 0.43 May 15 16:46 3300 R 21.16 0.21 May 17 16:33 2100 R 21.76 0.20 May 17 17:19 2400 B 21.86 0.27 May 19 16:32 1800 R 21.53 0.19 May 19 17:29 3600 B 22.59 0.16 May 21 17:33 600 R 20.91 0.18 May 22 17:00 2700 R 21.15 0.09 Jun 01 16:55 2400 R 21.77 0.19 Using our previous observations (GCN 2219) we can determine that within the error bars the OT brightness did not change in B filter over the period from May 3 till 19. Our data in R filter taken on May 7 and June 1 are consistent with the values reported by S.Zharikov et al. (GCN 2245, 2265). The data on May 19 are consistent with measurement by K.Stanek et al. (GCN 2244) taken 13 hrs later. Based on our "R" data set obtained with the same instrument we can conclude that the OT re-brightness took place in May 21-22. However there are apparent differences in brightness estimations in the nearest epochs of the observations obtained by the other teams in May 21-22. The magnitude on May 21 differs from that estimated 12 hours earlier (GCN 2244). The magnitude on May 22 differs from that estimated 3.5 hours later (R. Burenin et al., GCN 2260). Taking into account published brightness estimations one may suppose that during the period of May 21-22 the OT experienced brightness variations as suggested by K.Stanek et al. (GCN 2244, 2259). However, the indicated differences are marginal (3.7 sigma), and to confirm the variations cross-calibration of the data obtained by different teams on May 21-22 is necessary. If brightness variation will be confirmed, such kind of variations should be considered as the shortest ones observed to date for the late afterglows. The Maidanak data for May 21, 22 can be accessed at http://grb.rssi.ru/GRB030329/, and the file names are: 030329_030521R_UB.fits and 030329_030522R_UB.fits This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2299 SUBJECT: GRB030329: RTT150 optical observations DATE: 03/07/15 10:24:50 GMT FROM: Irek Khamitov at TUG I. Khamitov (TUG), I. Bikmaev, A.Galeev, N. Sakhibullin, V. Suleymanov (KSU); Z. Aslan, O.Golbasi(TUG), S.Ozer (AU); M.A. Alpar (SU); U. Kiziloglu, A. Baykal(METU); R. Burenin, R. Sunyaev, M. Pavlinsky, D. Denissenko, O.Terekhov, A. Tkachenko (IKI) Report: We observed the GRB 030329 target with 1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe, Turkey, in June-July, 2003, by using Andor CCD. Based on the photometry by Henden (GCN 2082) we measured the following Rc magnitudes for the target: Date t-t0 Rc dR 2003-06-02 65.322 21.65 0.07 2003-06-03 66.303 21.67 0.06 2003-06-23 86.314 21.80 0.10 2003-06-29 92.338 21.83 0.10 2003-07-02 95.334 21.83 0.17 2003-07-03 96.309 21.91: 0.28 Although there is some indication of a systematic fading, the errors are large for obvious reasons and we are already near the limiting magnitude at this high zenith distance. We will therefore discontinue the observations for this summer season. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2305 SUBJECT: GRB030329: Subaru Optical Spectroscopy DATE: 03/07/18 00:01:53 GMT FROM: George Kosugi at Subaru Telescope G. Kosugi, Y. Mizumoto, Y. Ohyama, K. S. Kawabata, and K. Aoki (Subaru Telescope, NAOJ), report: Spectra of GRB 030329 (H2656, Vanderspek et al, GCN 1997) optical transient (Peterson & Price, GCN 1985) were obtained using the Subaru 8.2m telescope and FOCAS (Faint Object Camera And Spectrograph) with the wavelength coverage of 4700 to 9400A (R=700) on June 22.3 UT (85 days after the burst). Compared with the previous data (May 8 and 9 UT : 40 days after the burst, Kawabata et al. IAUC 8133), we found that several nebular phase lines ([OI] 6300/6364, [CaII] 7291/7323, etc.) began to emerge out of the photospheric phase supernova spectrum. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2424 SUBJECT: GRB030329: radio observations at RT-22 (CrAO) DATE: 03/10/20 16:06:19 GMT FROM: Vasilij Rumjantsev at CrAO A.Volvach, I.Strepka (CrAO) on behalf of CrAO/IKI/SAO collaboration report: We have observed the radio afterglow position (E.Berger et al, GCN2014) of GRB030329 (R. Vanderspek et al, GCN1997) in June 26 at 4.8GHz, in July 8 at 22GHz, and in September at 4.8 and 8GHz with 22-m radio telescope RT-22 of Crimean Astrophysical Observatory. The radio source was detected at 22 GHz and upper limits have been obtained for other frequencies. The flux densities are: Date,UT Frequency Duration Flux density GHz hrs mJy Jun. 26 4.8 2 21.0 (3 sigma upper limit) Jul. 08 22 2 6.9 +-2.3 Sep. 23 8 2 9.0 (3 sigma) Sep. 25 4.8 3 7.5 (3 sigma) The sensitivity at 4.8 GHz was significantly improved in September with introducing in operation a cryo-radiometer. In September we detected a signal at 4.8 GHz, however the beam of RT-22 (12 arcmin) covers 3 sources found in NVSS (Condon et al. 1998, AJ, 115, 1693).The upper limit of flux density on Sep. 25 includes statistical errors and uncertainty of spectral indices of the 3 sources. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2455 SUBJECT: GRB 030329: Planned XMM-Newton Observation DATE: 03/11/27 16:24:18 GMT FROM: Norbert Schartel at XMM-Newton/ESA The XMM-Newton SOC has scheduled a Target of Opportunity observation of the field of GRB 030329 in revolution 734 (12th to 13th of December 2003). Details of the instrumental setup can be found at (Observation ID 0128531601): http://xmm.vilspa.esa.es/external/xmm_sched/sched_obs_srch_frame.shtml //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 2612 SUBJECT: GRB 030329: Rebrightening of hyperluminal ejecta. DATE: 04/06/18 06:09:43 GMT FROM: Arnon Dar at Technion-Israel Inst. of Tech S. Dado [Technion], A. Dar [Technion] and A. De Rujula [CERN] report: Taylor, Frail, Berger and Kulkarni [1] reported the discovery of a second compact radio source in the afterglow of GRB 030329 at an angular distance of 0.28 +\- 0.05 mas from the main source on day 51.3 after burst, which was not resolved in their VLBI observations at other epochs. This separation is "hyperluminal": the relative mean sky-projected-velocity is > 19c. A transient strong rebrightening of the second radio source is consistent with the reported "jitter" first seen in observations of the optical afterglow that began on day 51.75 (GCN 2224 [2], GCN 2259 [3]). At that late time, the optical afterglow of GRB 030329/SN 2003dh is expected to be dominated by the supernova. The spectroscopic resolution of the afterglow into the individual contributions of the SN and GRB [2] indicates that the GRB contribution rebrightened by a factor 2 or more. An analogous rebrightening of the second radio source may explain why it was resolved only on day 51.3. The discovery [1] of a hyperluminal compact source may pin down the origin of GRBs [5]. We encourage prompt and follow-up VLBI observations of XRFs. In the cannonball model the source separation observed by Taylor et al. is the expected one [5], and both GRBs and XRFs are produced by hyperluminal plasmoids ejected in SN explosions. Relative to GRBs, XRFs are selectively viewed at closer distances, and at viewing angles typically 3 times larger [6]. This makes them very attractive targets for radio searches of the expected hyperluminal motions, in particular promptly after the burst. [1] astro-ph/0405300: G.B. Taylor, D.A. Frail, E. Berger, S. Kulkarni [2] GCN 2224: K.Z. Stanek, D.W. Latham, M.E. Everett [3] GCN 2259: K.Z. Stanek, D. Bersier, M. Calkins, D.L. Freedman, T. Spahr [4] astro-ph/0307435: T. Matheson et al. [5] astro-ph/0406325: Dado, A. Dar, A. De Rujula [6] astro-ph/0309294: S. Dado, A. Dar, A. De Rujula