//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22695 SUBJECT: GRB 180510A: Swift detection of a burst DATE: 18/05/10 19:47:25 GMT FROM: Boris Sbarufatti at PSU J.D. Gropp (PSU), A. Deich (PSU), J. A. Kennea (PSU), S. J. LaPorte (PSU), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), B. Sbarufatti (PSU), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 19:24:34 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180510A (trigger=831810). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 276.318, -31.911 which is RA(J2000) = 18h 25m 16s Dec(J2000) = -31d 54' 38" 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 70 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 19:26:02.5 UT, 88.3 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 276.3303, -31.9069 which is equivalent to: RA(J2000) = +18h 25m 19.27s Dec(J2000) = -31d 54' 24.8" with an uncertainty of 5.5 arcseconds (radius, 90% containment). This location is 40 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 1.09e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 96 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. Results from the list of sources generated on-board are not available at this time. No correction has been made for the expected extinction corresponding to E(B-V) of 0.26. Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu). 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: 22696 SUBJECT: GRB 180510B: Swift detection of a burst with an optical counterpart DATE: 18/05/10 21:22:21 GMT FROM: Boris Sbarufatti at PSU A. Tohuvavohu (PSU), A. Deich (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU), S. J. LaPorte (PSU), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 20:15:42 UT, the Swift Burst Alert Telescope (BAT) triggered and located possible GRB 180510B (trigger=831816). Due to an observing constraint Swift did not slew immediately to the burst. The BAT on-board calculated location is RA, Dec 77.989, -62.335 which is RA(J2000) = 05h 11m 57s Dec(J2000) = -62d 20' 05" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 20 sec. The peak count rate was ~800 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 21:04:52.4 UT, 2950.1 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 77.96962, -62.32356 which is equivalent to: RA(J2000) = 05h 11m 52.71s Dec(J2000) = -62d 19' 24.8" with an uncertainty of 3.6 arcseconds (radius, 90% containment). This location is 52 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (2.54 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.8 (+3.31/-2.67) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 2953 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 05:11:52.64 = 77.96932 DEC(J2000) = -62:19:26.3 = -62.32396 with a 90%-confidence error radius of about 0.76 arc sec. This position is 4.0 arc sec. from the center of the XRT error circle. The estimated magnitude is 18.25 with a 1-sigma error of about 0.15. No correction has been made for the expected extinction corresponding to E(B-V) of 0.03. Burst Advocate for this burst is A. Tohuvavohu (aaronb AT swift.psu.edu). 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: 22698 SUBJECT: GRB 180510B: Enhanced Swift-XRT position DATE: 18/05/11 00:21:41 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 2476 s of XRT Photon Counting mode data and 7 UVOT images for GRB 180510B, 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 = 77.96901, -62.32411 which is equivalent to: RA (J2000): 05h 11m 52.56s Dec (J2000): -62d 19' 26.8" 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 was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22700 SUBJECT: GRB 180510B: TAROT La Silla observatory optical observations DATE: 18/05/11 09:01:11 GMT FROM: Alain Klotz at IRAP-CNRS-OMP Klotz A., Noysena.K., Atteia J.L. (CNRS-OMP-IRAP), Boer, M., Eymar, L. (CNRS-ARTEMIS), Gendre B. (UWA - Univ. Western Australia) report: We imaged the field of GRB 180510B detected by SWIFT (trigger 831816) with the TAROT robotic telescope (D=25cm) located at the European Southern Observatory, La Silla observatory, Chile. The observations started 2.88h after the GRB trigger just after the dusk. The elevation of the field decreased from 38 degrees above horizon weather conditions were good. We co-added a series of exposures but we we cannot detect the OT reported by Tohuvavohu et al. (GCNC 22696) Preliminary analysis gives: start end rlim(AB) (hour) (hour) 2.88 3.62 19.0 Magnitudes were estimated with the nearby NOMAD1 stars and are not corrected for galactic dust extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22701 SUBJECT: GRB 180510B: GROND detection in all bands DATE: 18/05/11 11:12:06 GMT FROM: Patricia Schady at MPE/Swift P. Schady (MPE, Garching) reports: We observed the field of GRB 180510B (Swift trigger 831816; Tohuvavohu et al., GCN #22696) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 23:14 UT on 10th May, 3.0 hours after the GRB trigger. They were performed at an average seeing of 1.3" and at an average airmass of 1.8. A single point source is present within the 1.5" Swift-XRT error circle reported by Beardmore et al. (GCN #22698) at RA (J2000.0) = 05:11:52.66 DEC (J2000.0) = -62:19:26.4 with an uncertainty of 0.2" in each coordinate. Based on 6.6 min of total exposures in g'r'i'z' and 6 min in JHK, the estimated AB magnitudes are g' = 20.5 +/- 0.1 mag r' = 20.0 +/- 0.1 mag i' = 19.8 +/- 0.1 mag z' = 19.6 +/- 0.1 mag J = 18.8 +/- 0.1 mag H = 18.5 +/- 0.1 mag K = 18.0 +/- 0.1 mag Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.02 in the direction of the burst (Schlafly & Finkbeiner 2011). I would like to thank Markus Rabus for his excellent support from La Silla. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22702 SUBJECT: GRB 180510B: VLT/X-shooter observations DATE: 18/05/11 11:34:10 GMT FROM: Andrea Rossi at INAF J. Palmerio (IAP, Paris), A. Rossi (INAF-OAS), D. Malesani (DAWN/NBI and DARK/NBI), N. R. Tanvir (Univ. Leicester), V. D'Elia (ASI-SSDC), A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), S. D. Vergani (GEPI/Obs. Paris), D. Xu (NAOC), D. A. Kann (HETH/IAA-CSIC), J.P.U. Fynbo (DAWN/NBI), and B. Sbarufatti (PSU), report on behalf of the Stargate Consortium: We observed the optical afterglow of GRB 180510B (Tohuvavohu et al., GCN 22696; Schady et al., GCN 22701) with the ESO VLT/X-shooter spectrograph, covering the wavelength range 3000-21000 AA. The afterglow is clearly detected in the 10s acquisition images taken starting at 23:09 UT (~3.7 hours after the GRB trigger) with brightness R~19.8 (Vega), calibrated against USNO-B1 stars in the field. Spectroscopy started at 23:19 UT on 2018-05-10 (~3.9 hours after the GRB trigger) and consisted of 2 exposures of 600 s. Preliminary analysis of the spectrum reveals continuum flux down to 3600 AA, which sets an upper limit to the redshift z <~ 2 via the lack of any obvious DLA feature. In addition, we identify several absorption lines at a common redshift of z=1.305, the most prominent being ZnII/CrII, FeII, MgII, and MgI. Moreover, we also identify another absorption system at z=0.63 based on the detection of the MgII doublet. Therefore, we propose the most probable redshift of the GRB to be z=1.305, with an intervening system at 0.638. We acknowledge the excellent support from the ESO staff, particularly Boris Haeussler, Karleyne Silva and Emanuela Pompei in obtaining these observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22705 SUBJECT: GRB 180510B: Swift-BAT refined analysis DATE: 18/05/11 14:30:53 GMT FROM: Amy Lien at GSFC S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), A. Tohuvavohu (PSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180510B (trigger #831816) (Tohuvavohu et al. GCN Circ. 22696). The BAT ground-calculated position is RA, Dec = 77.965, -62.320 deg which is RA(J2000) = 05h 11m 51.6s Dec(J2000) = -62d 19' 13.0" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 41%. The mask-weighted light curve shows a weak pulse that starts at ~T-20 s and peaks at ~T+1 s. The main pulse ends at ~ T+40 s, and there is some low-level emission that lasts until ~T+140 s. T90 (15-350 keV) is 134.3 +- 48.2 sec (estimated error including systematics). The time-averaged spectrum from T-19.92 to T+137.10 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.00 +- 0.17. The fluence in the 15-150 keV band is 2.1 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.96 sec in the 15-150 keV band is 1.2 +- 0.2 ph/cm2/sec. 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/831816/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22707 SUBJECT: GRB 180510A: Swift-XRT refined Analysis DATE: 18/05/11 19:47:04 GMT FROM: Phil Evans at U of Leicester A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB) and J.D. Gropp report on behalf of the Swift-XRT team: We have analysed 4.9 ks of XRT data for GRB 180510A (Gropp et al. GCN Circ. 22695), from 77 s to 40.5 ks after the BAT trigger. The data comprise 228 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 refined XRT position is RA, Dec = 276.3314, -31.9081 which is equivalent to: RA (J2000): 18 25 19.54 Dec(J2000): -31 54 29.1 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The late-time light curve (from T0+15.8 ks) can be modelled with a power-law decay with a decay index of alpha=1.2 (+/-0.4). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.94 (+0.08, -0.07). The best-fitting absorption column is 5.2 (+/-0.5) x 10^21 cm^-2, in excess of the Galactic value of 2.1 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.01 (+0.30, -0.28) and a best-fitting absorption column of 3.5 (+1.4, -1.2) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.8 x 10^-11 (5.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.5 (+1.4, -1.2) x 10^21 cm^-2 Galactic foreground: 2.1 x 10^21 cm^-2 Excess significance: 1.9 sigma Photon index: 2.01 (+0.30, -0.28) If the light curve continues to decay with a power-law decay index of 1.2, the count rate at T+24 hours will be 0.016 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x 10^-13 (9.4 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/00831810. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22708 SUBJECT: GRB 180510B: Swift-XRT refined Analysis DATE: 18/05/11 21:22:02 GMT FROM: Phil Evans at U of Leicester B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), Z. Liu (NAOC / U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) and A. Tohuvavohu report on behalf of the Swift-XRT team: We have analysed 2.6 ks of XRT data for GRB 180510B (Tohuvavohu et al. GCN Circ. 22696), from 3.0 ks to 10.2 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN Circ. 22698). The light curve can be modelled with a power-law decay with a decay index of alpha=1.48 (+/-0.12). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.83 (+/-0.12). The best-fitting absorption column is 1.3 (+0.4, -0.3) x 10^21 cm^-2, in excess of the Galactic value of 2.5 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.3 (+0.4, -0.3) x 10^21 cm^-2 Galactic foreground: 2.5 x 10^20 cm^-2 Excess significance: 5.0 sigma Photon index: 1.83 (+/-0.12) If the light curve continues to decay with a power-law decay index of 1.48, the count rate at T+24 hours will be 9.2 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.4 x 10^-13 (4.1 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/00831816. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22709 SUBJECT: GRB 180510A: Swift/UVOT followup observations DATE: 18/05/12 07:21:32 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL), S. R. Oates (U.Warwick) and J. D. Gropp (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180510A 97 s after the BAT trigger (Gropp et al., GCN Circ. 22695). A source is detected at the edge of the refined XRT position (D’Ai et al. GCN Circ. 22707) but this is consistent with the position of a USNO-B1.0 source (at 276.332, -31.908), and it is not clear if we see any fading. 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 97 247 147 20.0 ± 0.3 white 28989 29010 21 >19.2 v 22961 23272 301 >19.4 b 28076 28983 885 20.2 ± 0.2 u 310 322 12 >17.6 uvw1 15854 16753 886 >20.6 uvw2 22055 22955 886 >20.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.26 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22722 SUBJECT: Konus-Wind observation of GRB 180510A DATE: 18/05/14 11:16:13 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 180510A (Swift detection of a burst: Gropp et al., GCN 22695; Ukwatta et al., GCN 22704) triggered Konus-Wind at T0=69881.488 s UT (19:24:41.488). The burst light curve shows a single pulse which starts at ~T0-6.4 s and has a total duration of ~23.5 s. The emission is seen up to ~1 MeV. As observed by Konus-Wind, the burst had a fluence of 1.07(-0.14,+0.21)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0-0.064 s, of 3.53(-1.13,+1.18)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+16.640 s) is best fit in the 20 keV - 1.5 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with  alpha = -1.14(-0.31,+0.38), and Ep = 237(-56,+126) keV (chi2 = 93/60 dof). Fitting by the GRB (Band) model yields alpha = -0.62(-0.66,+1.24), Ep = 150(-54,+131) keV, and an upper limit on the high energy photon index: beta < -1.90 (chi2 = 91/59 dof). The spectrum near the peak count rate (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 1 MeV range by a power law with exponential cutoff model with  alpha = -0.97(-0.30,+0.35), and Ep = 202(-34,+54) keV (chi2 = 75/50 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.37 (chi2 = 75/49 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB180510_T69881/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22730 SUBJECT: GRB 180510A: MITSuME Ishigakijima optical upper limits DATE: 18/05/15 01:02:37 GMT FROM: Ryosuke Itoh at Tokyo Institute of Tech. T. Horiuchi, H. Hanayama, M. Honma (IAO, NAOJ), R. Itoh, K. L. Murata and N. Kawai (Tokyo Tech) report on behalf of the MITSuME and OISTER collaboration: We observed the field of GRB 180510A (Gropp et al.,GCN 22695) with the optical three color (g', Rc and Ic) CCD camera attached to the Murikabushi 1m telescope of Ishigakijima Astronomical Observatory. The observation started on 2018-05-10 19:29:21 UT, (287 seconds after the burst). No new or fading source is detected within the Swift-XRT error circle. We note that there is faint (~20mag) source detected in DSS images within XRT error circle (at 18:25:19.2, -31:54:22.7) but the source did not shows temporal variability during observation (~45 min). we derive the following upper limits using UCAC-4 catalog for flux calibration. #T0+[sec] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------------------- 287 19:55:17 2700.0 >19.4 >20.4 >20.2 ------------------------------------------------------------------- T0+ : Elapsed time after the burst [hour] T-EXP: Total Exposure time [sec]