//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19029 SUBJECT: GRB 160220B: Swift detection of a burst DATE: 16/02/20 11:22:29 GMT FROM: Kim Page at U.of Leicester J. R. Cummings (NASA/UMBC), A. Y. Lien (GSFC/UMBC), D. Malesani (DARK/NBI) and K. L. Page (U Leicester) report on behalf of the Swift Team: At 11:10:53 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 160220B (trigger=674734). Swift did not slew immediately due to an observing constraint. The BAT on-board calculated location is RA, Dec 259.854, -18.123 which is RA(J2000) = 17h 19m 25s Dec(J2000) = -18d 07' 22" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 30 sec. The peak count rate was ~6000 counts/sec (15-350 keV), at ~6 sec after the trigger. Due to an observing constraint, Swift will not slew until T0+46.5 minutes. There will be no XRT or UVOT data until this time. Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19033 SUBJECT: GRB160220B: Enhanced Swift-XRT position DATE: 16/02/20 19:20:32 GMT FROM: Kim Page at U.of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team: Using 4686 s of XRT Photon Counting mode data and 8 UVOT images, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 259.86518, -18.12401 which is equivalent to: RA (J2000): 17 19 27.64 Dec (J2000): -18 07 26.5 with an uncertainty of 1.5 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19036 SUBJECT: GRB 160220B: Swift-XRT refined Analysis DATE: 16/02/20 20:21:46 GMT FROM: Sarah Gibson at U.of Leicester J. R. Cummings (NASA/UMBC) reports on behalf of the Swift-XRT team: We have analysed 6.0 ks of XRT data for GRB 160220B (Cummings et al. GCN Circ. 19029), from 3.3 ks to 16.9 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. Using 4686 s of PC mode data and 8 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 = 259.86518, -18.12401 which is equivalent to: RA (J2000): 17h 19m 27.64s Dec(J2000): -18d 07' 26.5" with an uncertainty of 1.5 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=1.37 (+0.18, -0.17). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.17 (+0.25, -0.23). The best-fitting absorption column is 4.3 (+1.2, -1.1) x 10^21 cm^-2, in excess of the Galactic value of 2.6 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (6.3 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 4.3 (+1.2, -1.1) x 10^21 cm^-2 Galactic foreground: 2.6 x 10^21 cm^-2 Excess significance: 2.5 sigma Photon index: 2.17 (+0.25, -0.23) If the light curve continues to decay with a power-law decay index of 1.37, the count rate at T+24 hours will be 2.7 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.7 x 10^-14 (1.7 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/00674734. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19037 SUBJECT: GRB160220B: Swift/UVOT observations DATE: 16/02/20 21:42:50 GMT FROM: Massimiliano de Pasquale at IASF-Palermo M. De Pasquale (MSSL-UCL) and J. Cummings (GSFC/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 160220B 3.33 ks after the BAT trigger (Cummings et al., GCN Circ. 19029). No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 19033) is detected in the UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the summed UVOT exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 3735 5370 393 >21.0 v 4145 10454 1082 >20.1 b 3530 5165 393 >20.4 u 4882 16950 451 >20.1 w1 4555 16884 1504 >20.9 m2 4350 11207 933 >20.7 w2 5499 32840 1170 >20.9 We note the presence of an uncatalogued source of magnitude 20.2 +/- 0.20 in white filter, at coordinates RA = 17h 19m 28.07, Dec = -18d 07m 25.5s (J2000), which is 5" from the enhanced XRT position. The magnitudes above are not corrected for the substantial Galactic extinction due to the reddening of E(B-V) = 0.32 in the direction of the burst (Schlegel et al. 1998). -- Dr. Massimiliano De Pasquale Research associate - Swift UVOT scientist Mullard Space Science Laboratory, University College London //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19042 SUBJECT: GRB 160220B: GROND Observations DATE: 16/02/21 11:49:59 GMT FROM: Philip Wiseman at MPE/Swift P. Wiseman, J. Greiner (both MPE Garching) report on behalf of the GROND team: We observed the field of GRB 160220B (Swift trigger 674734; Cummings et al., GCN #19029) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 07:12 UT on 2016-02-21, ~20 hrs after the GRB trigger. They were performed at an average seeing of 1.5" and at an average airmass of 1.8. We detect a single point source at the southern edge of the 1.5" enhanced Swift-XRT error circle reported by Evans et al. (GCN #19033), at the position RA, Dec (J2000) = 259.86531, -18.12433, which is equivalent to: RA =17h 19m 27.67s Dec =-18d 07m 27.6s, with an uncertainty of 0.3" in each coordinate. Based on 72.00 min of total exposures at a mid-time of 07:54 UT, we estimate a preliminary magnitude (AB system) of: r' = 20.0 +/- 0.1 No statement about the variability of this source can be made at this time. The given magnitude is calibrated against GROND zeropoints and is not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.25 mag in the direction of the burst (Schlafly & Finkbeiner 2011). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19043 SUBJECT: GRB 160220B: Swift-BAT refined analysis DATE: 16/02/21 14:37:58 GMT FROM: Hans Krimm at NASA-GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 160220B (trigger #674734) (Cummings, et al., GCN Circ. 19029). The BAT ground-calculated position is RA, Dec = 259.851, -18.123 deg which is RA(J2000) = 17h 19m 24.2s Dec(J2000) = -18d 07' 21.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 38%. The mask-weighted light curve shows a double-peaked structure from T-10 to T+40 seconds. The spacecraft slewed away from the burst location at ~T+145 sec due to a pre-planned maneuver. T90 (15-350 keV) is 31.4 +- 2.6 sec (estimated error including systematics). The time-averaged spectrum from T-7.58 to T+37.54 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.75 +- 0.20, and Epeak of 168.7 +- 56.3 keV (chi squared 39.67 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 7.0 +- 0.2 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+6.46 sec in the 15-150 keV band is 6.6 +- 0.4 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.20 +- 0.05 (chi squared 56.26 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/674734/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19045 SUBJECT: Konus-Wind observation of GRB 160220B DATE: 16/02/21 21:03:08 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 160220B (Swift-BAT trigger #674734: Cummings et al., GCN 19029; Lien et al., GCN 19043) triggered Konus-Wind at T0=40259.435 s UT (11:10:59.435). The burst light curve shows a single pulse started at ~T0-12.8 s with a total duration of ~33.3 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB160220_T40259/ As observed by Konus-Wind, the burst had a fluence of 1.49(-0.11,+0.11)x10^-5 erg/cm2, and a 16-ms peak flux, measured from T0+0.896 s, of 4.32(-1.91,+1.92)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+16.640 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.84 (-0.22,+0.25) and Ep = 197 (-20,+26) keV (chi2 = 47/62 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.4 (chi2 = 47/61 dof) The spectrum near the maximum count rate (measured from T0+0.256 to T0+8.448 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.65 (-0.21,+0.24) and Ep = 208 (-19,+23) keV (chi2 = 57/61 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.5 (chi2 = 57/60 dof) All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19051 SUBJECT: Further Swift/UVOT observations of GRB 160220B DATE: 16/02/22 13:52:57 GMT FROM: Massimiliano de Pasquale at IASF-Palermo M. De Pasquale, A.A. Breeveld (MSSL-UCL) and J. Cummings (GSFC/UMBC) report on behalf of the Swift/UVOT team: Following the detection of a source at the southern edge of the 1.5'' Swift-XRT error circle (Evans et al. GCN circ. 19033) by GROND (Wiseman and Greiner, GCN Circ. 19042) we have re-analysed our UVOT observations We caution that the anlysis is complicated by a crowded field and large noise. About at the sourthern edge of the XRT error circle we detect a source RA = 17h 19m 27.64s (259.86517) Dec = -18d 07m 30 s (-18.12500) with an error of ~1''. The position of this source is copatible with that of the oject detected by GROND. Magnitudes of this source are given in the table below. Filter T_start(s) T_stop(s) Exp(s) Mag v 4145 10454 1082 18.7 +/- 0.2 b 3530 5165 393 19.4 +/- 0.2 The same source is detected in successive exposures: v 39730 62085 1072 18.7 +/- 0.2 b 44464 45371 885 19.4 +/- 0.2 As the source does not seem to have changed in brightness, we do not think it is the optical afterglow of GRB160220B. Magnitudes above are given in the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373). [GCN OPS NOTE(22feb16): Per Circ 19053, the Subject-line has been corrected from "20A" to "20B".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19052 SUBJECT: GRB 160220B: Further GROND Observations DATE: 16/02/22 14:04:03 GMT FROM: Philip Wiseman at MPE/Swift P. Wiseman, J. Bolmer and J. Greiner (all MPE Garching) report on behalf of the GROND team: We once again observed the field of GRB 160220B (Swift trigger 674734; Cummings et al., GCN #19029) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla Observatory (Chile). Based on 36.00 min of total exposures in r', at a mid-time of 08:55 UT on 2016-02-22, ~1.9 days after the trigger, we do not detect any fading in the source reported by Wiseman et al. (GCN #19042), placing a limit on any magnitude change to < 0.1 mag in 24 hrs, in agreement with UVOT observations ( De Pasquale et al., GCN #19051). We therefore agree that this source is likely not the afterglow of GRB 160220B. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19053 SUBJECT: Correction to the title of Swift GCN 19051 DATE: 16/02/22 14:05:01 GMT FROM: Massimiliano de Pasquale at IASF-Palermo M. De Pasquale report on behalf of the Swift/UVOT team: The title of the previous GCN Circ. 19051 should be "Further Swift/UVOT observations of GRB 160220B". We apologize for the mistake.