//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16415 SUBJECT: GRB 140619A: Swift detection of a burst with a possible optical counterpart DATE: 14/06/19 11:56:35 GMT FROM: David Burrows at PSU/Swift M. De Pasquale (INAF-IASFPA), D. N. Burrows (PSU), S. B. Cenko (GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU), F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA), K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (MSU) report on behalf of the Swift Team: At 11:38:35 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140619A (trigger=602080). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 27.092, -39.261 which is RA(J2000) = 01h 48m 22s Dec(J2000) = -39d 15' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As is usual with an image trigger, the available BAT light curve shows no significant structure. The XRT began observing the field at 11:40:54.9 UT, 139.1 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 27.1084, -39.2586 which is equivalent to: RA(J2000) = +01h 48m 26.02s Dec(J2000) = -39d 15' 31.0" with an uncertainty of 4.8 arcseconds (radius, 90% containment). This location is 46 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 2.5 s image was 5.85e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 98 seconds with the White filter starting 147 seconds after the BAT trigger. There is a weak 20.5 mag source near the XRT position. No aspect UVOT aspect solution is available because of the paucity of stars. Confirmation of the afterglow will require the full data set. No correction has been made for the expected extinction corresponding to E(B-V) of 0.01. Burst Advocate for this burst is M. De Pasquale (mdp AT ifc.inaf.it). 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: 16416 SUBJECT: GRB 140619A: Enhanced Swift-XRT position DATE: 14/06/19 19:11:16 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 2297 s of XRT Photon Counting mode data and 3 UVOT images for GRB 140619A, 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 = 27.10849, -39.25934 which is equivalent to: RA (J2000): 01h 48m 26.04s Dec (J2000): -39d 15' 33.6" with an uncertainty of 1.8 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 was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16417 SUBJECT: GRB 140619A: Swift-XRT refined Analysis DATE: 14/06/19 23:56:04 GMT FROM: Phil Evans at U of Leicester M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA) and M. De Pasquale report on behalf of the Swift-XRT team: We have analysed 7.3 ks of XRT data for GRB 140619A (De Pasquale et al. GCN Circ. 16415), from 129 s to 30.3 ks after the BAT trigger. The data comprise 112 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 16416). The late-time light curve (from T0+5.1 ks) can be modelled with a power-law decay with a decay index of alpha=0.93 (+/-0.09). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 0.67 (+/-0.05). The best-fitting absorption column is 1.9 (+/-0.4) x 10^21 cm^-2, in excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.09 (+0.15, -0.14) and a best-fitting absorption column of 2.5 (+/-0.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.4 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.5 (+/-0.5) x 10^21 cm^-2 Galactic foreground: 1.6 x 10^20 cm^-2 Excess significance: 7.7 sigma Photon index: 2.09 (+0.15, -0.14) If the light curve continues to decay with a power-law decay index of 0.93, the count rate at T+24 hours will be 0.031 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-12 (1.6 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00602080. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16418 SUBJECT: GRB 140619A: Swift/UVOT Observations DATE: 14/06/20 00:27:09 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU), F. E. Marshall (NASA/GSFC), J. Linevsky (PSU), and M. De Pasquale (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140619A 147 s after the BAT trigger (De Pasquale et al., GCN Circ. 16415). We confirm a faint afterglow consistent with the XRT position is detected in the initial UVOT exposures. We have corrected the positions in the 2.7' x 2.7’ UVOT sub-image by comparing positions with the Digital Sky Survey. The UVOT afterglow is located at: RA (J2000) = 01:48:26.15 = 27.10896 (deg.) Dec (J2000) = -39:15:32.6 = -39.25906 (deg.) with an estimated uncertainty of 1.0 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (fc) 147 245 96 20.39+-0.24 white 5112 5312 196 >21.05 b 11745 12179 422 >20.65 u 10833 11740 885 >20.82 uvw1 5933 6133 196 >19.77 uvm2 5727 5927 196 >19.59 uvw2 5317 5517 196 >19.87 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16423 SUBJECT: GRB 140619A: Swift-BAT refined analysis DATE: 14/06/20 12:24:35 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), M. De Pasquale (INAF-IASFPA) T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+421 sec from the recent telemetry downlink, we report further analysis of BAT GRB 140619A (trigger #602080) (De Pasquale, et al., GCN Circ. 16415). The BAT ground-calculated position is RA, Dec = 27.096, -39.249 deg which is RA(J2000) = 01h 48m 23.2s Dec(J2000) = -39d 14' 57.1" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 41%. The mask-weighted light curve shows a complex structure with multiple peaks. The main visible structure starts with roughly two long weaker pulses from ~T+20 s to T+150 s. The two weak pulses were followed by the major bright structure lasting until ~T+260 s, and it consists of many sub-pulses. Afterward there is another weaker long pulse lasting until ~T+350 s. T90 (15-350 keV) is 233.9 +- 13.4 sec (estimated error including systematics). Note that the main structure of the burst happened at ~150 s after the original image trigger, and was not described in the first circular (De Pasquale, et al., GCN Circ. 16415). The time-averaged spectrum from T+32.3 to T+340.4 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.45 +- 0.14, and Epeak of 117.8 +- 46.2 keV (chi squared 54.23 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 2.1 +- 0.04 x 10^-5 erg/cm2 and the 1-sec peak flux measured from T+219.52 sec in the 15-150 keV band is 4.6 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.71 +- 0.03 (chi squared 64.34 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/602080/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16443 SUBJECT: Konus-Wind observation of GRB 140619A DATE: 14/06/23 16:41:20 GMT FROM: Dmitry Svinkin at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lyssenko, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 140619A (Swift-BAT trigger #602080: De Pasquale, et al., GCN Circ. 16415, Palmer, et al., GCN Circ. 16423) was detected by Konus-Wind in the waiting mode. The burst light curve shows a single multipeak episode started at ~T0(BAT)+35 s with a duration of ~340 s. The K-W light curve of this burst is available at http://www.ioffe.ru/LEA/GRBs/GRB140619A/ As observed by Konus-Wind, the burst had a fluence of 5.4(-0.5,+0.2)x10^-5 erg/cm2 and a 2.944-s peak energy flux, measured from ~T0(BAT)+191 s, of 1.5(-0.3,+0.2)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+35 s to T0(BAT)+374 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = -1.3 ± 0.1, and Ep = 236 (-27,+33) keV. All the quoted errors are estimated at the 1 sigma confidence level. All the presented results are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17850 SUBJECT: GRB 1406194: Swift ToO observations DATE: 15/05/21 18:05:21 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/GBM GRB 1406194. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/ToO_GRBs/00020386 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/GBM event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team.