//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 3552 SUBJECT: GRB 050626 - a long GRB detected with INTEGRAL DATE: 05/06/26 04:42:47 GMT FROM: Diego Gotz at IASF-CNR D. Gotz, S. Mereghetti (IASF, Milano), N. Mowlavi, S. Shaw, M. Beck, A. Neronov (ISDC, Versoix), J. Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report A 60 s long GRB has been detected in IBIS/ISGRI data by IBAS (Alert Number 2587) at 03:45:16 UT. Its coordinates (J2000) are RA: 186.7445 DEC: -63.1342 with an uncertainty of 2 arcmin (90% c.l.). The preliminary peak flux is 0.4 ph (3E-8 erg) cmsq/s, while the fluence is 8.7E-7 erg/cmsq. Both values refer to the 20-200 keV band. A preliminary spectral analysis shows that this event is X-ray rich. A light curve will be posted at http://ibas.mi.iasf.cnr.it/IBAS_Results.html This message can be cited. [GCN OPS NOTE(26jun05): Per author's request, 050625 was changed to 050626.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 3553 SUBJECT: GRB 050626 - Correction to GCN 3552 DATE: 05/06/26 12:18:00 GMT FROM: Diego Gotz at IASF-CNR D. Gotz (IASF, Milano) on behalf of the IBAS Localization Team reports: The subject of GCN 3552 should refer to GRB 050626 and not to 050625. We aplogize for the misprint. This messages can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 3564 SUBJECT: GRB 050626: Swift XRT observations DATE: 05/07/05 17:34:19 GMT FROM: David Burrows at PSU/Swift V. Mangano, T. Mineo, V. La Parola, G. Cusumano (INAF-IASF/Palermo), S. Hunsberger (PSU), D. Morris (PSU), A. Beardmore, K. Page (U. Leicester), P. Boyd (GSFC-UMBC), L. Angelini (GSFC-JHU) and D. N. Burrows (PSU) report on behalf of the Swift XRT team: Swift observed GRB 050626 (D. Gotz at al, GCN3552) with XRT in Photon Counting (PC) mode for three times starting between 2005-06-29 03:38:54 and 2005-07-01 12:10:42 and collected a total of 38.6 ks. (Observations were delayed by several days because the Integral source was initially located near the Swift orbital pole, and was within the Swift Earth avoidance angle.) The three observations were performed in manual state to avoid the automatic switching in Windowed Timing (WT) mode caused by the presence of two bright optical stars within 3 arcmin of the INTEGRAL position. Only one uncataloged X-ray source was detected within the INTEGRAL error circle, at RA(J2000) = 12h 27m 01.2s Dec(J2000) = -63:08:13.9, i.e. 20 arcsec from the INTEGRAL position. The count rate of this source has been found to be steady within errors at the average level of (1.6 +/- 0.4)E-3 counts/s, making it unlikely to be the X-ray afterglow of the GRB. No afterglow candidate was detected within the INTEGRAL error circle. We estimate 3 sigma upper limits of 7.9E-14, 6.6E-14, and 1.6E-13 erg cm-2 s-1 for the flux of the GRB afterglow in the first, second and third observations, respectively and a 3 sigma upper limit of 3.8E-14 erg cm-2 s-1 in the sum of the three observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 3565 SUBJECT: GRB 050626 optical observations DATE: 05/07/06 09:37:17 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel, A.J. Castro-Tirado, (IAA-CSIC), P. Tristam, T. Britton, Ph. Yock (Univ. of Auckland), S. Guziy, A. de Ugarte Postigo, M. Jelinek (IAA-CSIC), O. Bogdanov (Nikolaev State Univ.), report: "We have observed the error box of the INTEGRAL GRB 050626 (Gotz et al. GCN Circ. 3552). The observations were carried out ~4 hours after the gamma-ray event with the 0.6 m telescope at Mt. John Astronomical Observatory (MOA) using the MOA wide red filter (Texp=5x300s). We note the presence of Alpha Crucis (R=1.3) close to the error box, which produces a strong background gradient in our images. Thus, the deepness of the combined image ranges approximately from R~14 to R~20.5 depending on the position within the error box. Comparison with the DSS did not reveal any variable source in the INTEGRAL error box, including the position of the unlikely X-ray afterglow (Mangano et al., GCN Circ. 3564). At this X-ray source position the limiting magnitude of our combined image is approximately R~20." This message can be cited.