//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11429 SUBJECT: GRB 101201A detected in ground analysis of BAT data DATE: 10/12/02 00:05:45 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift GRB 101201A detected in ground analysis of BAT data J. R. Cummings (GSFC/UMBC/CRESST), H. A. Krimm (GSFC/USRA/CRESST), D. M. Palmer (LANL), S. D. Barthelmy (GSFC) on behalf of the Swift-BAT team At 10:01:48, Swift-BAT detected GRB 101201A (BAT triggers 439595-6, Fermi GBM 312890511). There was no source found onboard. A strong source was found in ground analysis at RA, Dec 1.955, -16.196, which is: RA (J2000) 00h 07m 49s Dec (J2000) -16d 11m 46s with an estimated uncertainty radius of 2 arcmin (90% containment). This point is 1.8 degrees from the GBM position, within the GBM error circle. It was about 3% coded. The burst was about 50 seconds long, with 3 overlapping peaks. The available BAT event-by-event data covers most of the second peak. A Swift TOO for XRT follow-up is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11430 SUBJECT: GRB 101201A: GROND Detection of the Optical/NIR Afterglow DATE: 10/12/02 02:49:33 GMT FROM: Patricia Schady at MPE/Swift A. Nicuesa Guelbenzu, (Tautenburg Obs.), P.Schady and J.Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 101201A (Swift trigger 439595-6, Fermi GBM 312890511; Cummings et al., GCN #11429) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile). Observations started during twilight, at 00:36 UT on 2010-12-02, 14.6 hours after the GRB trigger, and are continuing. They were performed at an average seeing of better than 0.8" and at an average airmass of 1. We found a bright, uncatalogued point source within the 2 arcmin Swift- BAT error circle at RA (J2000.0) = 00:07:52.19 s DEC (J2000.0) = -16:11: 05.42 with an uncertainty of 0.5" in each coordinate. The source is detected in all optical and NIR GROND filters and had a preliminary AB magnitude or r' = 19.67+/-0.01 10 mins after the start of our observations. The source faded by ~0.3 magnitudes within the first 1.5 hours of GROND observations, leading us to conclude that this is the afterglow of GRB101201A. The detection of the source in the reddest GROND filter puts an upper limit on the redshift of this GRB of z < ~3. Given magnitudes are calibrated against USNO zeropoints and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.02 mag in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11431 SUBJECT: GRB 101201A: Swift/UVOT Detection DATE: 10/12/02 05:00:45 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and V. Magnano (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the field of GRB101201A approximately 14 hours after the BAT detection (GCN Circ. 11429). We confirm the uncataloged source reported Guelbenzu et al. (GCN Circ. 11430). We also find evidence of fading between the two orbits. Magnitudes for the first and second orbit exposures are listed below. Filter T_start(s) T_stop(s) Exp(s) Mag white 52065 52087 21 19.90+-0.49 white 57847 58387 531 20.01+-0.11 u 51218 52058 827 19.50+-0.17 u 57000 57840 826 20.01+-0.26 The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.02 (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11433 SUBJECT: GRB 101201A: Swift-XRT refined Analysis DATE: 10/12/02 15:51:21 GMT FROM: Boris Sbarufatti at INAF-OAB/IASFPA V. Mangano (INAF/IASF Pa), B. Sbarufatti (INAF/OAB - IASF Pa) report on behalf of the Swift-XRT team: We have analysed 4.9 ks of XRT data for GRB 101201A (Cummings et al. GCN Circ. 11429), from 51.2 ks to 69.7 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. Using 3879 s of PC mode data and 3 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 1.96750, -16.18540 which is equivalent to: RA (J2000): 00h 07m 52.21s Dec(J2000): -16d 11' 07.4" with an uncertainty of 1.9 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=3.80 (+0.03, -1.25). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.4 (+0.7, -0.6). The best-fitting absorption column is 8 (+14, -6) x 10^20 cm^-2, consistent with the Galactic value of 2.2 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (4.6 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8 (+14, -6) x 10^20 cm^-2 Galactic foreground: 2.2 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.4 (+0.7, -0.6) If the light curve continues to decay with a power-law decay index of 3.80, the count rate at T+24 hours will be 4.9 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x 10^-13 (2.2 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020152. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11434 SUBJECT: GRB 101201A: Fermi GBM observation DATE: 10/12/02 16:38:38 GMT FROM: Suzanne Foley at MPE S. Foley (MPE) reports on behalf of the Fermi GBM Team: "At 10:01:49.74 UT on 01 Dec 2010, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 101201A (trigger 312890511 / 101201418) which was also detected by the SWIFT-BAT (Cummings et al. 2010, GCN 11429). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 74 degrees. The GBM light curve consists of 3 main pulses with a duration (T90) of about 79 (+/-11) s (50-300 keV). The time-averaged spectrum from T0+2.048 s to T0+81.922 s is well fit by a power law function with an exponential high energy cutoff. The power law index is -1.50 (+/-0.03) and the cutoff energy, parameterized as Epeak, is 275.70 (+37.20/-27.80) keV (CSTAT 1263.1 for 480 d.o.f.). The event fluence (10-1000 keV) over the T90 duration is (2.41 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+31.74 s in the 10-1000 keV band is 6.7 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."