//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1668 SUBJECT: GRB021104: possible optical afterglow DATE: 02/11/04 11:00:27 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS Weidong Li, R. Chornock, S. Jha, and A. V. Filippenko (UCB) report: "We have observed the localization of GRB021104 (HETE Trigger #2434) with the Katzman Automatic Imaging Telescope (KAIT) for several images (with exposure time 20s to 300s unfiltered) starting at 3 Nov 2002 09:47 UT, about 167 minutes after the trigger. Inspection of the images reveals a new object that is not present in DSS II red image of the region. The coordinates of the object are: RA 03:53:47.89 +37:54:28.2 (J2000) The magnitude of the object is about 19.9. We suggest that this object is the possible afterglow of GRB020813." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1669 SUBJECT: GRB021104: Candidate present in DSS DATE: 02/11/04 11:16:47 GMT FROM: Paul Price at RSAA, ANU at CIT D.W. Fox and P.A. Price (Caltech) report on behalf of a larger collaboration: We note that the candidate optical afterglow reported by Li et al. (GCN #1668) is visible on the DSS 2 N-emulsion plate. Hence we do not consider it a likely candidate for the afterglow of the GRB. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1670 SUBJECT: GRB021104: optical observations DATE: 02/11/04 11:53:14 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS Weidong Li, R. Chornock, S. Jha, and A. V. Filippenko (UCB) report: "Analyses of the images of the GRB021104 field taken by KAIT from 4 Nov 2002 09:47 UT to 11:18 UT showed that the possible afterglow reported in GCN #1668 did not vary in brightness, thus confirmed the finding by Fox and Price in GCN #1669. Corrigendum: in GCN #1668, the observation time should be "4 Nov 2002", also, the last sentence 'GRB020813' should be 'GRB021104'. Thanks to Jean-Luc Atteia of LAOMP, Observatoire Midi-Pyrenees (France) for the quick alert to these mistakes." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1671 SUBJECT: GRB021104: Optical observations DATE: 02/11/04 14:46:54 GMT FROM: Derek Fox at CIT D.W. Fox and P.A. Price (Caltech) report: "We have observed the full WXM error box of the GRB021104 (HETE #2434) with the Oschin 48-inch telescope + unfiltered NEAT camera, with our first observations occurring at 09:49 UT, 2:48 after the burst. Visual comparison of our earliest individual exposures with archival (DSS-2) images reveals several asteroids but no new stationary objects within the error box. Image-differencing analysis of the summed image from two sets of (3x120s) triplet exposures, the first with mean epoch 10:12 UT and the second with mean epoch 12:37 UT, also fails to reveal any variable sources that are not present in archival images. We estimate the limiting R-band magnitude of each of these two unfiltered searches to be R >~ 21 mag." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1675 SUBJECT: GRB021104(=H2434): A Long, X-Ray-Rich GRB Localized by HETE DATE: 02/11/05 03:59:54 GMT FROM: Don Lamb at U.Chicago T. Tamagawa, Y. Shirasaki, C. Graziani, M. Matsuoka, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy, Y. Nakagawa, D. Takahashi, M. Suzuki, R. Satoh, and Y. Urata, on behalf of the HETE WXM Team; G. Ricker, J-L Atteia, N. Kawai, D. Lamb, and S. Woosley on behalf of the HETE Science Team; N. Butler, G. Crew, J. Doty, G. Prigozhin, R. Vanderspek, J. Villasenor, T. Cline, J. G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Azzibrouck, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC Teams; M. Boer, J-F Olive, J-P Dezalay, C. Barraud and K. Hurley on behalf of the HETE FREGATE Team; write: At 07:01:02.93 UTC (25262.93 s UT) on 4 Nov 2002, the HETE FREGATE and WXM instruments detected event H2434, a long, X-ray-rich GRB. Ground analysis of the WXM data for the burst produced a location, which was reported in a GCN Position Notice at 9:47 UT, 166 minutes after the burst. The WXM localization SNR was 5. The WXM location can be expressed as a 90% confidence rectangle that is approximately 24 arcminutes in width and 42 arcminutes in length. The corners of the rectangle lie at the following J2000 coordinates: RA = 3h 52m 40.3s, Dec = 38o 19' 26" RA = 3h 54m 44.6s, Dec = 38o 17' 10" RA = 3h 54m 56.2s, Dec = 37o 34' 59" RA = 3h 52m 52.6s, Dec = 37o 37' 12". The burst duration in the 8-40 keV band was ~26s. A total of 2120 counts were detected during that interval, corresponding to a fluence of ~4 x 10-7 ergs cm-2 . The peak flux was >3 x 10-8 ergs cm-2 s-1 (i.e., >1 x Crab flux). A light curve for GRB021104 is provided at the following URL: http://space.mit.edu/HETE/Bursts/GRB021104/ This message is citable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1676 SUBJECT: IPN triangulation of GRB021104 (annulus) DATE: 02/11/06 00:34:34 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley and T. Cline, on behalf of the Ulysses and HETE teams, and G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R. Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R. Manchanda, G. Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on behalf of the HETE GRB team, report: Ulysses and HETE-FREGATE (H2436) observed this GRB at 32792 seconds. As observed by Ulysses, it had a duration of approximately 10 seconds and a 25-100 keV fluence of approximately 1.0E-06 erg/cm2. We have triangulated it to a preliminary annulus centered at RA, Decl(2000) = 0.042, -35.331 degrees, whose radius is 84.393 +/- 0.083 degrees (3 sigma ). This annulus may be constrained and/or 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: 1677 SUBJECT: GRB021104: Optical Observations DATE: 02/11/06 23:37:49 GMT FROM: Michael Bradshaw at SuperLOTIS M. Bradshaw, G. Williams (Steward Observatory), D. Hartmann (Clemson University) and H.S. Park report on behalf of the Super-LOTIS collaboration: Starting on Nov 4.456 UT the Super-LOTIS automated telescope imaged the entire error box for GRB021104 (GCNC #1675; HETE trigger #2434) in the R-band. Observations started 3.93 hours after the burst. A total of 57 images at 60 second integration were analyzed. We find no optical transients to the DSS limit in the coadded image. We also coadded three sets of 19 images and find no fading sources which are not present in the DSS. This report may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1724 SUBJECT: GRB 021104, GRB 021112 and GRB 021113 - Milagro GeV/TeV Observations DATE: 02/12/06 18:41:04 GMT FROM: Julie McEnery at UMBC/GSFC Julie McEnery on behalf of the Milagro collaboration reports: Milagro searched for GeV/TeV gamma-ray emission from GRB 021104 (GCN 1675), GRB 021112 (GCN 1682) and GRB 021113 (GCN 1686) during the burst durations reported by the HETE WXM (26, 5 and 20 seconds respectively). No evidence for prompt GeV/TeV emission was found from any of these bursts. A preliminary analysis (assuming a differential photon spectral index of -2.4) gives an upper limit on the fluence at the 99.9% confidence level of: J(E 0.2-20 TeV) < 3.4 * 10^(-6) erg cm^(-2) for GRB 021104 and, J(E 0.2-20 TeV) < 2.6 * 10^(-6) erg cm^(-2) for GRB 021112 and, J(E 0.2-20 TeV) < 2.8 * 10^(-6) erg cm^(-2) for GRB 021113