//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1033 SUBJECT: BeppoSAX GRB ALERT: GRB010412 DATE: 01/04/13 02:43:17 GMT FROM: Luigi Piro at IAS/CNR Frascati BeppoSAX GRB ALERT: GRB010412 On Apr. 12, 21:46 U.T. a GRB has been detected simultaneously by the GRBM and WFC1 aboard BeppoSAX. Preliminary coordinates from WFC are: R.A.(2000)= 294.89 DEC.(2000)= 13.62 The error radius at this stage of analysis is 10'. We are not planning a follow-up observation of this burst, due to the on-going pointing of another TOO Luigi Piro BeppoSAX Mission Scientist //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1035 SUBJECT: GRB010412: refined positions from BeppoSAX DATE: 01/04/13 10:56:28 GMT FROM: Luigi Piro at IAS/CNR Frascati GRB010412: refined positions Refined coordinates from WFC are: R.A.(2000)= 294.913 DEC.(2000)= 13.618 The error radius is 6'. Luigi Piro BeppoSAX Mission Scientist //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1036 SUBJECT: IPN Triangulation of GRB010412 DATE: 01/04/13 16:54:08 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the Ulysses GRB team, and C. Guidorzi, E. Montanari, and F. Frontera, on behalf of the BeppoSAX GRBM team, report: Ulysses and BeppoSAX GRBM observed this burst (GCN 1035). As observed by Ulysses, it had a duration ~80 s, a 25-100 keV fluence of 9.4x10^-6 erg/cm^2, and a peak flux over 0.5 s of ~9 x 10^-7 erg/cm^2 s. These numbers are subject to more than the usual uncertainties because Ulysses is recording a solar proton event which raises its background by a factor of 2 or so. Triangulation gives an annulus centered at RA(2000), Decl(2000)=3.671, -21.012 deg., with radius 75.856 +/- 0.034 deg. (3 sigma). This intersects the WFC error circle to form an error box whose area is approximately 47 sq. arcmin. and whose corners are at RA(2000) DEC(2000) 294.842577=19 h 39 m 22.22 s 13.545103= 13 o 32 ' 42.37 " 294.929439=19 h 39 m 43.07 s 13.716716= 13 o 43 ' 0.18 " 294.906675=19 h 39 m 37.60 s 13.518189= 13 o 31 ' 5.48 " 294.990525=19 h 39 m 57.73 s 13.683762= 13 o 41 ' 1.54 " This error box can be refined by further processing. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1037 SUBJECT: GRB010412: BeppoSAX GRBM and WFC observations DATE: 01/04/13 17:49:46 GMT FROM: Lorenzo Amati at TESRE/CNR A. Paolino, BeppoSAX Scientific Operation Centre (SOC), Telespazio, Rome, R.G. Kaptein, SOC and Space Research Organisation Netherlands (SRON), Utrecht, J.J.M. in 't Zand, Astronomical Institute, Utrecht University and SRON, C. Guidorzi and F. Frontera, Phys. Dept. University of Ferrara, L. Amati, Istituto TESRE / CNR, Bologna and L. Piro, Istituto di Astrofisica Spaziale / CNR, report: "GRB010412 was triggered by the BeppoSAX Gamma Ray Burst Monitor (GRBM) on April 12.907280 U.T and was also detected by the Wide Field Camera (WFC) unit 1 onboard the same satellite. A preliminary analysis of the GRBM data shows a very complex, multi-pulse time profile. The duration is about 75 s and the peak count rate 1896 +/- 59 cts/s, corresponding to a 1 s peak flux of (1.71 +/- 0.06) x 10^(-6) erg/cm2/s in the 40-700 keV energy band. The WFC data show a duration of about 90 s and a peak flux of 2.3 Crab (2-28 keV). The position of the X-ray counterpart is R.A.= 19h 39m 39.0s, Decl.=+13d 37'06.6' (equinox 2000.0) with an error radius of 6', that includes uncertainties due to a non-optimum attitude control configuration. No follow-up observation with the BeppoSAX NFI was scheduled, due to an on-going other TOO." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1038 SUBJECT: GRB010412: Optical observations DATE: 01/04/13 20:50:31 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price, T.S. Axelrod and B.P. Schmidt (RSAA, ANU) report: "We have observed the error box of GRB 010412 (Piro et al., GCN #1033; Hurley et al., GCN #1036) with the robotic 50-inch telescope at Mount Stromlo Observatory at 2001 Apr 13.73 UT. Our 3x300 sec exposures cover the entire error box to a limiting magnitude of R ~ 20.0 mag, based on common stars with the USNO-A2.0 catalogue. We do not detect any optical transient within the error box, based on visual comparison with the Digital Palomar Sky Survey. The high stellar density and large Galactic reddening (A_V ~ 1.5 mag) at this low Galactic latitude (-4.2 deg) may, however, obscure a potential OT." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1039 SUBJECT: GRB010412: Optical observations DATE: 01/04/14 01:37:03 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price (Caltech/RSAA,ANU), P. Gorham (JPL), S.A. Yost and S.R. Kulkarni (Caltech) report on behalf of the larger Caltech/NRAO/CARA GRB collaboration: "P. Gorham observed the error box of GRB 010412 with the Palomar 60-inch telescope around 2001 Apr 13.5 UT (0.6 days after the GRB). The observations consisted of 2x450 sec integrations in I-band at each of four pointings to cover the entire original error-circle (GCN #1033). Within the IPN error-box (GCN #1036), we find no optical transient, on visual comparison with the Digital Palomar Observatory Sky Survey plates. We estimate the limiting magnitude of our images to be I ~ 20.5 mag." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1042 SUBJECT: GRB010412, field photometry DATE: 01/04/18 15:29:10 GMT FROM: Arne A. Henden at USNO/USRA A. Henden (USRA/USNO) reports on behalf of the USNO GRB team: We have acquired shallow BVRcIc all-sky photometry for an 11x11 arcmin field that covers the center of the error box for GRB010412 with the USNOFS 1.0-m telescope on one photometric night. Stars brighter than V=13.5 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/grb010412.dat The current photometry has a potential external zero-point error of about two percent. The astrometry in this file is based on linear plate solutions with respect to USNO-A2.0. The internal errors are less than 100mas. Since this is a crowded field, you should check the DSS images and only use stars for calibration that do not have neighbors. Further calibration of this field will be performed if an optical afterglow is identified.