//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21170 SUBJECT: GRB 170531A: Swift detection of a burst DATE: 17/05/31 20:33:44 GMT FROM: Scott Barthelmy at NASA/GSFC P.A. Evans (U Leicester), S. D. Barthelmy (GSFC), H. A. Krimm (NSF/USRA), N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and T. N. Ukwatta (LANL) report on behalf of the Swift Team: At 20:07:32 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170531A (trigger=755343). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 121.261, -14.033 which is RA(J2000) = 08h 05m 03s Dec(J2000) = -14d 01' 57" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As is typical for image triggers, there is nothing significant in the real-time light curve. We note that this trigger occurred while coming out of the SAA. The XRT began observing the field at 20:09:35.5 UT, 122.6 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 121.25380, -14.02292 which is equivalent to: RA(J2000) = 08h 05m 00.91s Dec(J2000) = -14d 01' 22.5" with an uncertainty of 4.5 arcseconds (radius, 90% containment). This location is 44 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. We cannot determine whether the source is fading at the present time. No spectrum from the promptly downlinked event data is yet available to determine the column density. The initial flux in the 2.5 s image was 2.92e-10 erg cm^-2 s^-1 (0.2-10 keV). No UVOT data are available at this time. Burst Advocate for this burst is P.A. Evans (pae9 AT star.le.ac.uk). 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: 21171 SUBJECT: GRB 170531B: Swift detection of a burst DATE: 17/05/31 22:23:52 GMT FROM: David Palmer at LANL P.A. Evans (U Leicester), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), A. Cholden-Brown (PSU), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Swift Team: At 22:02:09 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170531B (trigger=755354). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 286.895, -16.426 which is RA(J2000) = 19h 07m 35s Dec(J2000) = -16d 25' 34" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of at least 50 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~6 sec after the trigger. The XRT began observing the field at 22:04:30.1 UT, 140.9 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source with an enhanced position: RA, Dec 286.8835, -16.4196 which is equivalent to: RA(J2000) = 19h 07m 32.03s Dec(J2000) = -16d 25' 10.4" with an uncertainty of 2.3 arcseconds (radius, 90% containment). This location is 45 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 consistent with the Galactic value of 1.41 x 10^21 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 2.73e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 152 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. The 8'x8' region for the list of sources generated on-board 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 region. No correction has been made for the expected extinction corresponding to E(B-V) of 0.19. Burst Advocate for this burst is P.A. Evans (pae9 AT star.le.ac.uk). 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: 21172 SUBJECT: GRB 170531A: Swift/UVOT Observations DATE: 17/05/31 23:04:56 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and P. A. Evans (U Leicester) report on behalf of the Swift/UVOT team: UVOT took a finding chart exposure of 150 seconds with the White filter starting 3522 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. The typical 3-sigma upper limit has been about 19.6 mag. The coverage of the XRT error circle by the 8'x8' region for the list of sources generated on-board is uncertain because the large number of sources filled the available telemetry. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.09. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21173 SUBJECT: GRB 170531B: MASTER Net OT detection DATE: 17/05/31 23:19:01 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, N.Tyurina, E.Gorbovskoy, D.Kuvshinov, A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory N.M.Budnev, O.Gres, O. Ershova Irkutsk State University A.Gabovich, V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, Argentina H. Levato, C. Saffe Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina MASTER-Kislovodsk robotic telescope (2x4 square degrees, MASTER-Net: http://observ.pereplet.ru) was pointed to the GRB170531B (Evans et al., GCN #21171) 12 sec after notice time and 452 sec after trigger time on 2017-05-31 22:09:44 UT. There is marginally seen optical transient at the position 19h 07m 32.03s -16d 25' 10.4" with m_OT~19.0+-0.5 The 5-sigma upper limit is about 18.5mag The message may be cited. ==================================================================== The observations made on zenit distance = 64 degrees, galaxy latitude b = -11 degree. The moon (44 % bright part) below the horizon (The Moon altitude is -6 degree). The sun altitude is -22.7 degree. The object can be observed till sunrise at 2017-06-01 01:30:50 . The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21174 SUBJECT: GRB 170531B: CrAO confirmation of the afterglow DATE: 17/06/01 00:11:21 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), D. Chestnov (ISON), A. Novichonok (ISON), A. Mokhnatkin (ISON) report on behalf of larger GRB follow-up collaboration: We observed the field of the GRB 170531B (Evans et al.,GCN 21171) with with Zeiss-1000/Koshka telescope starting on May 31 (UT) 22:32:32, i.e. ~30 minutes after burst onset. We took several images in filter R with exposures of 180 s. Near the border of XRT error circle (Evans et al.,GCN 21171) we detect the source in coordinates (J2000) 19:07:31.67 -16:25:09.3 with uncertainity of 0.5 arcsec in both coordinates. The source is probably coincedent with the object reported by (Lipunov et al., GCN 21172). The source is fading from R=19.1 at (UT) 22:32:32 down to R=19.5 at (UT) 23:30:56. Most probably the source is an afterglow of GRB 170531B. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21175 SUBJECT: GRB 170531B: Enhanced Swift-XRT position DATE: 17/06/01 00:59:47 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 1160 s of XRT Photon Counting mode data and 2 UVOT images for GRB 170531B, 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 = 286.88369, -16.41911 which is equivalent to: RA (J2000): 19h 07m 32.09s Dec (J2000): -16d 25' 08.8" 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: 21176 SUBJECT: GRB 170531A: ePESSTO NTT observations DATE: 17/06/01 01:29:05 GMT FROM: Paolo D'Avanzo at INAF-OAB G. Pignata (Univ. Andres Bello), L. Wang (CASSACA), P. D'Avanzo (INAF-OAB), D. Malesani (Dark/NBI), L. Izzo (IAA-CSIC), S. Campana (INAF OAB), J. Anderson (ESO), R. Cartier (Southampton), L. Galbany (Univ. de Chile), C. Inserra (QUB), E. Kankare (QUB), K. Maguire (ESO), S. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), O. Yaron (Weizmann), D. Young (QUB), I. Manulis (Weizmann) We observed GRB 170531A (Evans et al., GCN 21170) under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ). The observations were performed on the ESO New Technology Telescope at La Silla with the EFOSC2 instrument in imaging mode starting from 2017-05-31 at 23:12:07 UT (i.e. 3.1 hours from the burst). We obtained two consecutive images each one lasting 150s with the r filter. No optical afterglow is detected in the coadded image within the XRT error circle (http://www.swift.ac.uk/xrt_positions/) down to a limiting magnitude of r > 23 (AB; 3sigma c.l.). The photometric calibration was carried out assuming r=17.07 (AB) for the star at RA(J2000), Dec(J2000) = 08:05:00.30, -14:01:21.3, as reported in the PANSTARRS catalogue. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21177 SUBJECT: GRB 170531B: Redshift from GTC/OSIRIS DATE: 17/06/01 06:34:45 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), L. Izzo (IAA-CSIC), D.A. Kann (IAA-CSIC), C.C. Thoene (IAA-CSIC), Z. Cano (IAA-CSIC), J.P.U. Fynbo (DARK/NBI), D. Garcia Alvarez (GTC, IAC), D. Perez Valladares (GTC), A. Nuñez (GTC), M. Huertas (GTC) report on behalf of a larger collaboration: We observed the afterglow of GRB 170531B (Evans et al. GCN 21171, Lipunov et al. GCN 21173, Pozanenko et al. GCN 21174) using OSIRIS at the 10.4 m GTC telescope in La Palma (Spain). Observation consisted in 3x900s exposures using the R1000B grism, covering the range between 3700 and 7880 AA. The mean epoch of the combined spectrum is 03:09:29 UT (5.12 hr after the GRB onset). Additionally, g, r, i, and z-band observations were obtained. We note that the coordinates of the afterglow are 19:07:32.09, -16:25:05.8 (J2000 +/-0.5¿), which places the GRB approximately 5¿ away from those of the source identified by Lipunov et al. (GCN 21173) and Pozanenko et al. (GCN 21174). The afterglow can be also detected in the early Swift/UVOT images. In the acquisition image we measure a magnitude of r_AB = 21.9 for the afterglow, as compared to PANSTARRS catalogue field stars. The afterglow spectrum shows continuum throughout the wavelength range and several strong absorption features corresponding to Lyman-alpha, SiII, OI, CII, SiIV, CIV, AlII and AlII at a common redshift of 2.366, which we identify as the redshift of the GRB. [GCN OPS NOTE(01jun17): Per author's request, authors DPV, AN, & MH were added to the list.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21178 SUBJECT: GROND observations of GRB 170531B DATE: 17/06/01 09:42:36 GMT FROM: Patricia Schady at MPE/Swift P. Schady and T. Kruehler (both MPE) report We observed the field of GRB 170531B (Swift trigger 755354; Evans et al., GCN #21171) 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 03:55 UT on 01-06-2017, 5.9 hours the GRB trigger. They were performed at an average seeing of 1.3" and at an average airmass of 1.3. We detect a point source within the 1.8" enhanced Swift/XRT error circle (Osborne et al., GCN #21175), and consistent with the afterglow position reported by Ugarte Postigo et al. (GCN #21177). Based on a total exposure of 54 min in g'r'i'z' and 45 min in JHK, we estimate preliminary magnitudes (all in AB) of g' = 22.65 +/- 0.04 r' = 22.15 +/- 0.04 i' = 21.99 +/- 0.05 z' = 21.84 +/- 0.06 J = 21.8 +/- 0.3 H = 21.5 +/- 0.3 K > 19.9 Given magnitudes are calibrated against PanSTARRS and 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.16 mag in the direction of the burst (Schlafly & Finkbeiner 2011). We acknowledge the excellent support provided by the Chilean observer at the telescope, and the support astronomer, Sam Kim, in obtaining these data. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21179 SUBJECT: GRB 170531B: MASTER Net optical counterpart refind position and magnitude DATE: 17/06/01 11:21:45 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs N.Tyurina, V. Lipunov, V.Kornilov, E.Gorbovskoy, I.Gorbunov, D.Kuvshinov, A.V.Krylov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory N.M.Budnev, O.Gres, O. Ershova Irkutsk State University A.Gabovich, V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, Argentina H. Levato, C. Saffe Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina MASTER-Kislovodsk robotic telescope (2x4 square degrees, MASTER-Net: http://observ.pereplet.ru) was pointed to the GRB170531B (Evans et al., GCN #21171) 12 sec after notice time and 452 sec after trigger time on 2017-05-31 22:09:44 UT (Lipunov et al., GCN #21173). Id Date time Exp Proc.type Limit* Tube OT Err UT sec 5sigma 1240587 2017-05-31 22:09:44 90 Alert (SWIFT) 18.3 EAST 18.3 0.5 1240589 2017-05-31 22:11:23 110 Alert (SWIFT) 18.4 EAST 18.4 0.5 1240591 2017-05-31 22:13:24 130 Alert (SWIFT) 18.5 EAST 18.4 0.5 1240593 2017-05-31 22:15:44 160 Alert (SWIFT) 18.5 EAST 18.5 0.5 1240596 2017-05-31 22:18:35 180 Alert (SWIFT) 18.5 EAST 18.5 0.5 1240652 2017-05-31 22:09:44 490 SumAlert(SWIFT) 19.1 EAST 18.3 0.2 1240597 2017-05-31 22:21:59 180 Alert (SWIFT) 18.3 EAST no - 1240599 2017-05-31 22:25:24 180 Alert (SWIFT) 18.5 EAST no - ................................................................. 1240629 2017-05-31 23:16:43 180 Alert (SWIFT) 18.5 EAST no - * - unfiltered magnitude with respect to USNO B1.0 stars reference stars m=0.2B + 0.8R We refind OT preliminary astrometric position (Lipunov et al., GCN #21173) which was done visually. Our refind position are: RA,DEC = 19 07 32.19 -16 25 06.9 3 sigma error = (+/-)2 arcsec (the source is marginaly visible). Our pixel is 2 arcsec. The offset from X-ray Swift position (Osborne at all) is 1.9 arcsec . The position of the Postigo et al. ( GCN 21177) is inside our error box (offset ~ 1.9 arcsec). The possible OT position Pozanenko et al.( GCN #21174) offset ~ 8.2 arc sec. The OT detection image is available. The message may be cited. ==================================================================== The observations made on zenit distance = 64 degrees, galaxy latitude b = -11 degree. The moon (44 % bright part) below the horizon (The Moon altitude is -6 degree). The sun altitude is -22.7 degree. The object can be observed till sunrise at 2017-06-01 01:30:50 . The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21180 SUBJECT: GRB 170531A: Swift-XRT refined Analysis DATE: 17/06/01 11:33:02 GMT FROM: Phil Evans at U of Leicester A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), S. J. LaPorte (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), V. D'Elia (ASDC) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.2 ks of XRT data for GRB 170531A (Evans et al. GCN Circ. 21170), from 254 s to 44.6 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The best available XRT position (using the promptly downlinked event data, the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue) is RA, Dec = 121.2524, -14.0227 which is equivalent to: RA (J2000): 08 05 00.57 Dec(J2000): -14 01 21.8 with an uncertainty of 3.5 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=0.62 (+0.20, -0.16). If the light curve continues to decay with a power-law decay index of 0.62, the count rate at T+24 hours will be 1.3 x 10^-3 count s^-1 The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00755343. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21181 SUBJECT: GRB 170531A: MASTER Net job DATE: 17/06/01 12:23:54 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, N.Tyurina, E.Gorbovskoy, D.Kuvshinov, A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias D.Buckley South African Astronomical Observatory A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory N.M.Budnev, O.Gres, O. Ershova Irkutsk State University A.Gabovich, V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, Argentina H. Levato, C. Saffe Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina MASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in SAAO was pointed to the GRB170531.84 25 sec after notice time and 99 sec after trigger time at 2017-05-31 20:09:15 UT. On our first (20s exposure) set we haven`t found optical transient within SWIFT error-box (ra=121.258 dec=-14.0328 r=0.05). The 5-sigma upper limit has been about 15.5mag The observations made on zenit distance = 84 degrees, galaxy latitude b = 10 degree. The moon (43 % bright part) is 19 degrees above the horizon. The distance between moon and object is 41 The sun altitude is -56.5 degree. MASTER-IAC robotic telescope (2x4 square degrees, MASTER-Net: http://observ.pereplet.ru) was pointed to the GRB170531A (Evans et al., GCN #21170; Siegel et al. GCN #21172) 895 sec after notice time and 2115 sec after trigger time on the 2017-05-31 20:42:48 UT. The observations were made on zenit distance = 74 degrees during the twilight. The sun altitude was -9.6 degree. The moon (43 % bright part) is 58 degrees above the horizon. The distance between moon and object is 41deg. On our 5-th (180s exposure) set we haven`t found optical transient within SWIFT error-box (ra=121.258 dec=-14.0328 r=0.1). The 5-sigma upper limit m~13.9mag (unfiltered) on the first image and MASTER-OAFA robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in OAFA was pointed to the GRB170531.84 15674 sec after notice time and 15751 sec after trigger time at 2017-06-01 00:30:03 UT. On our first (180s exposure) set we haven`t found optical transient within Master error-box (ra=121.25 dec=-14.0225 r=0.1). The 5-sigma upper limit has been about 18mag The message may be cited. The observations made on zenit distance = 63 degrees, galaxy latitude b = 10 degree. The moon (45 % bright part) is 38 degrees above the horizon. The distance between moon and object is 43 The sun altitude is -35.4 degree. The object can be observed till 2017-06-01 02:41:37. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21182 SUBJECT: GRB 170531B: Swift-XRT refined Analysis DATE: 17/06/01 13:55:38 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.8 ks of XRT data for GRB 170531B (Evans et al. GCN Circ. 21171), from 129 s to 52.1 ks after the BAT trigger. The data comprise 303 s in Windowed Timing (WT) mode (the first 10 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 Osborne et al. (GCN Circ. 21175). The late-time light curve (from T0+5.5 ks) can be modelled with a power-law decay with a decay index of alpha=1.18 (+0.25, -0.20). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.45 (+/-0.04). The best-fitting absorption column is 6.5 (+2.7, -2.5) x 10^21 cm^-2, at a redshift of 2.366, in addition to the Galactic value of 1.4 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.07 (+0.13, -0.12) and a best-fitting absorption column consistent with the Galactic value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.4 x 10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Galactic foreground: 1.4 x 10^21 cm^-2 Intrinsic column: 1.4 (+2.2, -0.0) x 10^21 cm^-2 at z=2.366 Photon index: 2.07 (+0.13, -0.12) If the light curve continues to decay with a power-law decay index of 1.18, the count rate at T+24 hours will be 3.3 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-13 (1.6 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/00755354. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21183 SUBJECT: GRB 170531B: LCO observations DATE: 17/06/01 15:49:04 GMT FROM: Antonino Cucchiara at UVI A. Cucchiara, D. Morris (U. of Virgin Islands), C. Guidorzi (U. Ferrara), reports on behalf of a larger collaboration: "On June 1.00 UT (T_0 +2.0h) we began observing the center of the field of GRB 170531B (Evans et al. GCN 211171) using the Las Cumbres Observatory 1m Sutherland facility. We performed a series of 10x60s observations in R and I band for a total of 10 minutes on sky in each filter. Seeing conditions were poor. We identified no optical counterpart within the center of Swift-XRT refined position (Evans et al. GCN 21175), or at the location of the identified counterpart (Lipunov et al. GCN 21173, Pozanenko et al. GCN 21174, Schady et al. GCN 21178) at the following 3-sigma limits: R > 19.9 mag I > 19.6 mag These magnitude are calibrated against nearby USNO-B1 sources, and are not corrected for Galactic extinction." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21184 SUBJECT: GRB 170531A: Swift/UVOT Upper Limits DATE: 17/06/01 16:02:44 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and P. A. Evans (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 170531A 3523 s after the BAT trigger (Evans et al., GCN Circ. 21170). No optical afterglow consistent with the XRT position (Melandri et al., GCN Circ. 21180) is detected in the initial UVOT exposures. We note that the XRT position is 3.5” away from a known USNO-B1 source, which we detect. There is no indication of a second source within the error circle. Preliminary 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 3523 3673 147 >18.1 white 3523 4292 344 >18.2 v 4502 4702 197 >17.5 b 3887 4087 197 >18.2 u 3682 3881 197 >18.0 w2 4298 4497 197 >19.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21185 SUBJECT: GRB 170531A: Swift-BAT refined analysis DATE: 17/06/01 16:17:56 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), P.A. Evans (U Leicester), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-65 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 170531A (trigger #755343) (Evans et al., GCN Circ. 21170). The BAT ground-calculated position is RA, Dec = 121.218, -14.017 deg which is RA(J2000) = 08h 04m 52.4s Dec(J2000) = -14d 00' 59.7" with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 92%. The mask-weighted light curve shows a weak pulse that starts ~T-10 s and ends at ~T+25 s. T90 (15-350 keV) is 26.74 +- 7.94 sec (estimated error including systematics). The time-averaged spectrum from T-13.24 to T+25.78 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.22 +- 0.28. The fluence in the 15-150 keV band is 7.5 +- 1.2 x 10^-7 erg/cm2. 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/755343/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21186 SUBJECT: GRB 170531B: Swift-BAT refined analysis DATE: 17/06/01 16:18:59 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), P. A. Evans (U Leicester), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU), 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 170531B (trigger #755354) (Evans et al., GCN Circ. 21171). The BAT ground-calculated position is RA, Dec = 286.901, -16.414 deg which is RA(J2000) = 19h 07m 36.3s Dec(J2000) = -16d 24' 51.6" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weighted light curve shows a multi-peaked structure that starts at ~T0 and ends at ~T+180 s. T90 (15-350 keV) is 164.13 +- 8.82 sec (estimated error including systematics). The time-averaged spectrum from T+0.55 to T+181.67 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.95 +- 0.14. The fluence in the 15-150 keV band is 2.0 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+42.71 sec in the 15-150 keV band is 0.8 +- 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/755354/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21187 SUBJECT: GRB 170531B: SMARTS optical/IR observations DATE: 17/06/01 18:25:15 GMT FROM: Bethany Cobb at GWU B. E. Cobb (GWU), reports: Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained optical/IR imaging of the error region of GRB 170531B (GCN 21171, Evans et al.) at two epochs (with mid-exposure times of 2017-06-01 04:22 UT & 08:19 UT). For each epoch, several dithered images were obtained with total summed exposure times amounting to 36 minutes in I and 30 minutes in J. No source is detected at the position of the X-ray/optical afterglow (GCN 21175, Osborne et al.; GCN 21174, Pozanenko et al.; GCN 21177, de Ugarte Postigo et al.; GCN 21178, Schady & Kruehler; GCN 21179, Tyurina et al.) to the approximate 3-sigma limiting magnitudes listed below: mid-exposure time post-burst (hours) I-limit J-limit 6.33056 >20.8 >18.5 10.27333 >21.2 >18.7 (Optical photometry is calibrated against USNO-B1.0 stars and IR photometry is calibrated against 2MASS stars in the field.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21188 SUBJECT: GRB 170531B: Swift/UVOT Detection DATE: 17/06/02 04:27:30 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and P. A. Evans (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 170531B 152 s after the BAT trigger (Evans et al., GCN Circ. 21171). We detect a possible afterglow consistent with the position given by GTC (de Ugarte Postigo et al., GCN Circ. 21177) and MASTER (Tyurin et al., GCN CIrc. 21179). The preliminary UVOT position is: RA (J2000) = 19:07:32.10 = 286.88373 (deg.) Dec (J2000) = -16:25:05.8 = -16.41829 (deg.) with an estimated uncertainty of 0.1 arc sec. (radius, 90% confidence). This position is 3.0 arc sec away from the enhanced XRT position (Osborne et al. GCN Circ. 21175). Given the fading, detection by other observatories and lack of matching source in the DSS, we find it likely to be the GRB afterglow. Preliminary 3-sigma magnitudes 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) 152 302 147 20.50+-0.29 white 590 1532 244 >21.03 v 640 1581 116 >18.88 b 566 1508 97 >19.77 u (fc) 310 560 245 >20.07 u 713 1643 85 >19.17 uvw1 689 1630 97 >18.91 uvm2 664 1606 116 >18.88 uvw2 615 1557 116 >19.14 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.19 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21189 SUBJECT: GRB 170531B: ISON/Terskol optical observations DATE: 17/06/02 15:22:42 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Mokhnatkin (KIAM), A. Pozanenko (IKI), A. Volnova (IKI), I. Molotov (KIAM) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 170531B (Evans et al.,GCN 21171) with K-800 (0.8m) telescope of ISON/Terskol observatory starting on May, 31 (UT) 22:21:31. We obtained several unfiltered images of 40 s exposure. The optical afterglow (Lipunov et al., GCN 21173 Pozanenko et al. GCN 21174) is clearly visible in combined images. Preliminary photometry of the afterglow is following Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2017-05-31 22:21:31 0.01810 CR 18*40 18.90 0.10 21.0 2017-05-31 22:35:41 0.02949 CR 21*40 19.10 0.10 21.0 Photometry is based on nearby USNO-B1.0 stars USNO-B.1_id R2 0736-0718845 16.77 0735-0729626 17.35 0735-0729622 16.96 0735-0729439 16.59 0735-0729327 17.22 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21209 SUBJECT: GRB 170531B: WHT spectroscopy DATE: 17/06/07 09:17:35 GMT FROM: Klaas Wiersema at U Leicester K. Wiersema, N. Tanvir (Leicester), A. Levan (Warwick) report: We observed the afterglow of GRB 170531B (Evans et al. GCN 21171; Lipunov et al. GCN 21173; Pozanenko et al. GCN 21174) with the 4.2m William Herschel Telescope on La Palma, using the ACAM instrument. We obtained a spectrum, consisting of 4x900 seconds exposure time, starting at 02:55 UT on 1 June 2017. Our wavelength coverage is ~4500 - 9500 A. We detect a small number metal lines (at low S/N) at a redshift consistent with that obtained by de Ugarte-Postigo et al. (GCN 21177). We warmly thank the staff of ING, in particular Raine Karjalainen, for their assistance. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21210 SUBJECT: GRB 170531B: Zeiss-1000/CrAO optical observations DATE: 17/06/07 21:38:36 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), D. Chestnov (ISON), A. Novichonok (ISON), V. Agletdinov (KIAM), I. Nikolenko (CrAO), A. Volnova (IKI), report on behalf of larger GRB follow-up collaboration: We report refined analysis of Zeiss-1000/CrAO observations. Results reported below supersede GCN cir. 21174. We observed the field of the GRB 170531B (Evans et al., GCN 21171) with Zeiss-1000/Koshka (CrAO) telescope between May 31 (UT) 22:32:32 and June 01 (UT) 00:58:11. We took several unfiltered images with exposure of 180 s. The afterglow (Lipunov et al. GCN 21173; Pozanenko et al. GCN 21174) is clearly visible in each image in first initial images, and detected later in combined images. The finding chart of the combined image can be found at http://grb.rssi.ru/GRB170531B/GRB170531B_Koshka_170531_sources.png The coordinates of the afterglow (source A in the finding chart) are (J2000) 19:07:32.10 -16:25:06.0 with uncertainty of 0.5 arcsec in both coordinates. The coordinates are consistent with the position reported by de Ugarte Postigo et al., GCN 21177, Tyurina et al., GCN 21179, and Siegel et al., GCN 21188. Preliminary photometry of the afterglow can be found in the light curve at http://grb.rssi.ru/GRB170531B/GRB170531B_light_curve_v2.png The photometry is based on nearby USNO-B1.0 stars, calibrated against to R2 magnitudes USNO-B.1_id R2 0736-0718845 16.77 0735-0729622 16.96 0735-0729439 16.59 0735-0729327 17.22 Due to presence of sources in near vicinity to the afterglow the photometry of wide FOV telescopes might be affected by the sources. In particular our photometry reported in GCN 21189 is apparently biased by the two sources C and D (see the finding chart). We report coordinates and brightness of the nearby sources. Source coordinates(J2000) AG distance filter mag. err. C 19:07:32.34 -16:25:09.1 4.6" CR 20.46 0.04 D 19:07:31.83 -16:25:05.6 3.9" CR 20.47 0.04