//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19979 SUBJECT: GRB 161004A: Swift detection of a burst with a possible optical counterpart DATE: 16/10/04 13:10:14 GMT FROM: Scott Barthelmy at NASA/GSFC P.A. Evans (U Leicester), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), A. A. Breeveld (UCL-MSSL), D. N. Burrows (PSU), A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), B. Mingo (U Leicester), K. L. Page (U Leicester), P. Romano (INAF-IASFPA), T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU) and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team: At 12:58:28 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 161004A (trigger=715084). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 263.171, -0.928, which is RA(J2000) = 17h 32m 41s Dec(J2000) = -00d 55' 41" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a couple of peaks with a total duration of about 5 sec. The peak count rate was ~1800 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 12:59:49.3 UT, 80.7 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 263.15298, -0.94831 which is equivalent to: RA(J2000) = 17h 32m 36.72s Dec(J2000) = -00d 56' 53.9" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 97 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.88 x 10^21 cm^-2, Willingale et al. 2013), with an excess column of 4.1 (+3.92/-2.99) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 85 seconds after the BAT trigger. There is a candidate afterglow in the list of sources generated on-board at RA(J2000) = 17:32:36.59 = 263.15244 DEC(J2000) = -00:57:02.2 = -0.95061 with a 90%-confidence error radius of about 1.10 arc sec. This position is 6.6 arc sec. from the center of the XRT error circle. The estimated magnitude is 19.03. No correction has been made for the expected extinction corresponding to E(B-V) of 0.25. 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: 19980 SUBJECT: GRB 161004A: TSHAO optical observations DATE: 16/10/04 17:44:41 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 161004A (Evans et al., GCN 19979) with Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. We obtained several images in R filter starting on Oct. 04 (UT) 13:36:52. In the XRT error circle we do not detect any new object. Wa do not detect also candidate afterglow (Evans et al., GCN 19979). Preliminary photometry of a combined image is following Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2016-10-04 13:36:52 0.04321 R 15*180 n/d n/d 21.9 Photometry is based on nearby SDSS-DR9 stars (Lupton transformations): SDSS-DR9_id R(Lupton) J173243.09-005731.3 17.04 J173250.91-005842.7 16.77 J173251.94-005803.2 15.75 J173253.88-005801.6 15.62 J173253.02-005938.3 16.02 J173232.00-005640.3 16.34 J173227.11-005646.8 16.41 J173227.04-005816.8 16.51 J173227.48-005856.9 16.62 J173236.27-010018.1 16.96 J173241.54-005823.1 16.26 A finding chart can be found at http://grb.rssi.ru/GRB161004A/GRB161004A_TSHAO_161004_XRT_UVOT.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19981 SUBJECT: GRB 161004A: Bassano Bresciano Observatory upper limit DATE: 16/10/04 19:14:38 GMT FROM: Ulisse Quadri at Bassano Bresciano Obs U.Quadri, L.Strabla and R.Girelli report: We imaged the field of GRB 161004A detected by SWIFT(trigger 715084) with the robotic telescope of (IAU station 565) Bassano Bresciano Observatory, Italy. Member of: AAVSO - American Association of Variable Star Observers. ISSP - Italian Supernovae Search Project. UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili. The observations started 4.90 hour after the GRB trigger, at the end of twilight, with our Newton telescope D=250 mm F/D=4.8. Weather conditions were good. We co-added 3 series of 10 exposures of 60 sec each. Start T0+ End T0+ Vlim 4.9 hour 5.5 hour 18 We did not found any optical counterpart in the error box of the XRTcandidate. P.A. Evans (U Leicester), S. D. Barthelmy (GSFC), et al. Magnitudes were estimated with the UCAC4 cat. and are not corrected for galactic dust extinction. Reference: http://www.osservatoriobassano.org/GRB.asp The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19983 SUBJECT: GRB 161004A: Enhanced Swift-XRT position DATE: 16/10/04 20:50:17 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 4971 s of XRT Photon Counting mode data and 10 UVOT images for GRB 161004A, 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 = 263.15236, -0.95067 which is equivalent to: RA (J2000): 17h 32m 36.57s Dec (J2000): -00d 57' 02.4" with an uncertainty of 1.6 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: 19984 SUBJECT: GRB 161004A: Swift/UVOT Detection DATE: 16/10/04 21:15:33 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL) 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 161004A 85 s after the BAT trigger (Evans et al., GCN Circ. 19979). A source consistent with the enhanced XRT position (Beardmore et al., GCN Circ. 19983) is detected in the initial UVOT exposures in the white and u filters only. The preliminary UVOT position is: RA (J2000) = 17:32:36.54 = 263.15224 (deg.) Dec (J2000) = -00:57:02.7 = -0.95075 (deg.) with an estimated uncertainty of 0.56 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 early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 85 235 147 19.47 ± 0.16 v 627 6121 432 >20.1 b 552 10926 1144 >21.8 u 297 547 246 19.55 ± 0.29 w1 848 6531 413 >20.2 m2 4690 6326 393 >20.3 w2 602 12506 1063 >20.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.25 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19985 SUBJECT: GRB 161004A: Swift-XRT refined Analysis DATE: 16/10/04 21:47:28 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), A.P. Beardmore (U. Leicester), S.L. Gibson (U. Leicester), A. D'Ai (INAF-IASFPA) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.1 ks of XRT data for GRB 161004A (Evans et al. GCN Circ. 19979), from 84 s to 18.2 ks after the BAT trigger. The data comprise 112 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN Circ. 19983). The late-time light curve (from T0+4.3 ks) can be modelled with a power-law decay with a decay index of alpha=1.3 (+0.5, -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 (+0.11, -0.09). The best-fitting absorption column is consistent with the Galactic value of 1.9 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.59 (+0.18, -0.16) and a best-fitting absorption column of 2.2 (+0.9, -0.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.6 x 10^-11 (5.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.2 (+0.9, -0.4) x 10^21 cm^-2 Galactic foreground: 1.9 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 1.59 (+0.18, -0.16) If the light curve continues to decay with a power-law decay index of 1.3, the count rate at T+24 hours will be 1.1 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.9 x 10^-14 (5.9 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00715084. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19986 SUBJECT: GRB 161004A: SAO RAS optical upper limit DATE: 16/10/04 23:02:45 GMT FROM: Moskvitin Alexander at SAO RAS A. Moskvitin (SAO RAS), A. Volnova (IKI), and A. Pozanenko (IKI) report on behalf of the larger GRB follow-up team. We observed the field of GRB 161004A (Evans et al., GCN 19979) with Zeiss-1000 - the 1-meter telescope of Special Astrophysical Observatory of Russian Academy of Sciences. We obtain several images with filter Rc starting on October, 4 (UT) 15:44:35. In the refined XRT error circle (Beardmore et al., GCN 19983) we do not detect the optical counterpart (Breeveld and Evans, GCN 19984). Preliminary photometry of a combined image is following Date UT start t-T0 Filter Exp. OT UL (mid, days) (s) 2016-10-04 15:44:35 0.1396 Rc 12*300 n/d 22.4 Photometry is based on nearby SDSS-DR9 stars reported by Mazaeva et al. (GCN 19980). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19987 SUBJECT: GRB 161004B: Swift detection of a burst DATE: 16/10/04 23:18:17 GMT FROM: David Palmer at LANL A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 23:07:59 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 161004B (trigger=715246). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 112.157, -39.895 which is RA(J2000) = 07h 28m 38s Dec(J2000) = -39d 53' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single FRED peak with substructure and a duration of about 20 sec. The peak count rate was ~12000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 23:09:12.7 UT, 73.4 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 112.15290, -39.89858 which is equivalent to: RA(J2000) = 07h 28m 36.70s Dec(J2000) = -39d 53' 54.9" with an uncertainty of 3.6 arcseconds (radius, 90% containment). This location is 17 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 5.23e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 82 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 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. 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 0.54. Burst Advocate for this burst is A. D'Ai (antonino.dai 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: 19988 SUBJECT: GRB 161004B: Prompt enhanced Swift-XRT position DATE: 16/10/04 23:53:05 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 161004B, we find an enhanced XRT position of the afterglow: RA, Dec: 112.1514, -39.8976 which is equivalent to: RA (J2000) = 07 28 36.34 Dec (J2000) = -39 53 51.5 with an uncertainty of 2.0 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/715246. Position enhancement is 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: 19991 SUBJECT: GRB 161004B: Enhanced Swift-XRT position DATE: 16/10/05 11:55:09 GMT FROM: Phil Evans 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 3535 s of XRT Photon Counting mode data and 5 UVOT images for GRB 161004B, 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 = 112.15126, -39.89791 which is equivalent to: RA (J2000): 07h 28m 36.30s Dec (J2000): -39d 53' 52.5" with an uncertainty of 1.4 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: 19993 SUBJECT: GRB 161004A: RATIR Optical and NIR Observations DATE: 16/10/05 12:32:05 GMT FROM: Eleonora Troja at GSFC Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report: We observed the field of GRB 161004A (Evans, et al., GCN 19979) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2016/10 5.10 to 2016/10 5.22 UTC (13.49 to 16.23 hours after the BAT trigger), obtaining a total of 1.73 hours exposure in the r and i bands and 0.65 hours exposure in the Z, Y, J, and H bands. For a source within the Swift-UVOT error circle (Breeveld & Evans, GCN 19984), in comparison with the USNO-B1 and 2MASS catalogs, we obtain the following upper limits (3-sigma): r > 23.3 i > 23.2 Z > 22.4 Y > 21.8 J > 21.3 H > 19.4 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19994 SUBJECT: GRB 161004B: Swift-XRT refined Analysis DATE: 16/10/05 12:53:00 GMT FROM: Phil Evans at U of Leicester V. D'Elia (ASDC), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and A. D'Ai report on behalf of the Swift-XRT team: We have analysed 7.1 ks of XRT data for GRB 161004B (D'Ai et al. GCN Circ. 19987), from 63 s to 28.2 ks after the BAT trigger. The data comprise 77 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 Evans et al. (GCN Circ. 19988). The light curve can be modelled with an initial power-law decay with an index of alpha=0.89 (+/-0.05), followed by a break at T+2716 s to an alpha of 1.44 (+0.30, -0.22). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.99 (+0.19, -0.18). The best-fitting absorption column is 1.14 (+0.21, -0.19) x 10^22 cm^-2, in excess of the Galactic value of 3.5 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 5.1 x 10^-11 (9.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.14 (+0.21, -0.19) x 10^22 cm^-2 Galactic foreground: 3.5 x 10^21 cm^-2 Excess significance: 7.1 sigma Photon index: 1.99 (+0.19, -0.18) If the light curve continues to decay with a power-law decay index of 1.44, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-13 (2.0 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/00715246. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19995 SUBJECT: GRB 161004B: Swift-BAT refined analysis DATE: 16/10/05 13:02:02 GMT FROM: Takanori Sakamoto at AGU T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), A. D'Ai (INAF-IASFPA), N. Gehrels (GSFC), H. A. Krimm (GSFC/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-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 161004B (trigger #715246) (D'Ai, et al., GCN Circ. 19987). The BAT ground-calculated position is RA, Dec = 112.156, -39.896 deg which is RA(J2000) = 07h 28m 37.4s Dec(J2000) = -39d 53' 47.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 75%. The mask-weighted light curve shows two overlapping peaks starting at T-10 sec, peaking at T+1 sec and ending at T+40 sec. T90 (15-350 keV) is 15.9 +- 0.7 sec (estimated error including systematics). The time-averaged spectrum from T-5.16 to T+27.31 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.21 +- 0.13, and Epeak of 177 +- 73 keV (chi squared 35.21 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 8.8 +- 0.2 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+0.36 sec in the 15-150 keV band is 10.1 +- 0.4 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.47 +- 0.03 (chi squared 47.75 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/715246/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19996 SUBJECT: GRB161004B: AstroSat CZTI detection DATE: 16/10/05 14:56:42 GMT FROM: Dipankar Bhattacharya at IUCAA V. Kumar, V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed clear detection of GRB161004B (Swift BAT detection: D.Palmer et al., GCN Circ. 19987) in the 40-200 keV energy range. The light curve shows a single peak at 23:07:59.0 UT, coincident with the Swift Trigger. The measured peak count rate is 187.3 counts/sec above the background in combined data of four quadrants, with a total of 1393.0 counts. The local mean background count rate was 313.7 counts/sec. Using cumulative rates, we measure a T90 of 13.1 secs. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19997 SUBJECT: GRB 161004B: Swift/UVOT Upper Limits DATE: 16/10/05 16:23:52 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 161004B 82 s after the BAT trigger (D'Ai et al., GCN Circ. 19987). No optical afterglow consistent with the XRT position (Evans et al., GCN Circ. 19991) is detected in the initial UVOT exposures. 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 82 232 147 >20.8 u_FC 294 544 246 >19.6 white 82 1886 431 >21.2 v 624 1937 156 >19.5 b 550 1862 136 >19.6 u 294 1836 363 >19.6 w1 674 1812 136 >18.9 m2 5622 5747 123 >18.8 w2 600 1736 136 >18.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.54 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 19998 SUBJECT: GRB 161004B: Fermi GBM detection DATE: 16/10/05 16:51:33 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 23:07:54.79 UT on 04 October 2016, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 161004B (trigger 497315278 / 161004964) which was also detected by the Swift BAT (D'Ai et al. 2016, GCN 19987) The GBM on-ground location is consistent with the Swift position. The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The initial angle from the Fermi LAT boresight to the Swift location is 69 degrees. The GBM light curve consists of a single peak with a duration (T90) of about 14 s (50-300 keV). The time-averaged spectrum from T0-0.0 s to T0+18.4 s is best fit by a Band function with Epeak = 132 +/- 6 keV, alpha = -0.75 +/- 0.04, and beta = -2.4 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (1.877 +/- 0.039)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+4.7 s in the 10-1000 keV band is 15.4 +/- 0.4 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20001 SUBJECT: GRB 161004A: Swift-BAT refined analysis DATE: 16/10/06 09:03:15 GMT FROM: Takanori Sakamoto at AGU D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), P. A. Evans (U Leicester), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-61 to T+242 sec from the recent telemetry downlink, we report further analysis of BAT GRB 161004A (trigger #715084) (Evans, et al., GCN Circ. 19979). The BAT ground-calculated position is RA, Dec = 263.127, -0.947 deg which is RA(J2000) = 17h 32m 30.6s Dec(J2000) = -00d 56' 50.7" with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 92%. The mask-weighted light curve shows a single peak starting at T-0.1 sec, peaking at T+0.5 sec and ending at T+5 sec. T90 (15-350 keV) is 1.08 +- 0.21 sec (estimated error including systematics). The time-averaged spectrum from T-0.11 to T+1.06 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.26 +- 0.33. The fluence in the 15-150 keV band is 9.5 +- 1.6 x 10^-8 erg/cm2. The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band is 1.0 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Due to a low signal-to-noise of the data, the lag analysis is not possible. Therefore, it is not clear whether this burst belongs to a short GRB or not. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/715084/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20003 SUBJECT: GRB 161004B: CALET Gamma-Ray Burst Monitor detection DATE: 16/10/06 13:51:35 GMT FROM: Takanori Sakamoto at AGU Y. Yamada, A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 161004B (D'Ai et al., GCN Circ. 19987; Kumar et al., GCN Circ. 19996; Hamburg et al., GCN Circ. 19998; INTEGRAL-SPI/ACS trigger #7590) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:07:52.64 on 4 October 2016. The burst signal was seen by the SGM instrument. The light curve of the SGM shows a single peak starting at T0, peaking at T+7 sec and ending at T+15 sec. The T90 duration measured by the SGM data is 11.1 +- 0.9 sec (40-450 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1159657616/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20005 SUBJECT: Konus-Wind observation of GRB 161004B DATE: 16/10/06 16:02:46 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 161004B (Swift-BAT trigger #715246: D'Ai et al., GCN 19987; Sakamoto et al., GCN 19995; Fermi GBM detection: Hamburg & Meegan, GCN 19998; CALET Gamma-Ray Burst Monitor detection: Yamada et al., GCN 20003) triggered Konus-Wind at T0=83274.317 s UT (23:07:54.317). The burst light curve shows a single pulse with a total duration of ~18 s. The emission is seen up to ~2 MeV. As observed by Konus-Wind, the burst had a fluence of 1.71(-0.07,+0.08)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+4.144 s, of 3.43(-0.80,+0.80)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+15.616 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 = -1.05(-0.09,+0.09), and Ep = 175(-12,+14) keV (chi2 = 56/58 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.14 (chi2 = 56/57 dof). The spectrum near the peak count rate (measured from T0 to T0+7.424 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 = -0.71(-0.10,+0.11), and Ep = 210(-13,+15) keV (chi2 = 67/58 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.12 (chi2 = 67/57 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB161004_T83274/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20011 SUBJECT: GRB 161004A: refined analysis of TSHAO optical observations DATE: 16/10/07 23:58:37 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We present a refined analysis of our observations (Mazaeva et al., GCN 19980) of the field of GRB 161004A (Evans et al., GCN 19979) with Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. We obtained several images in R filter starting on Oct. 04 (UT) 13:36:52. In a combined image of the first 30 minutes of our observations we detect the afterglow (Breeveld et al., GCN 19984). Preliminary photometry of a combined image is following Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2016-10-04 13:36:52 0.03632 R 9*180 21.65 0.25 21.7 Photometry is based on nearby SDSS-DR9 stars used in GCN 19980. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20012 SUBJECT: GRB 161004A: Maidanak optical observations DATE: 16/10/08 00:26:58 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), B. Hafizov (UBAI), A. Volnova (IKI), O. Burhonov (UBAI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 161004A (Evans et al., GCN 19979) with AZT-22 telescope of Maidanak observatory equipped with SNUCAM in R filter starting on Oct. 04 (UT) 14:25:10. We clearly detected optical afterglow (Evans et al., GCN 19979; Breeveld et al., GCN 19984; Mazaeva et al., GRB 20011). Preliminary photometry of the afterglow in a combined image is following Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2016-10-04 14:25:10 0.06981 R 15*120 22.0 0.15 22.7 Photometry is based on nearby SDSS-DR9 stars used in GCN 19980. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20053 SUBJECT: GRB161004A: Further analysis of the burst nature DATE: 16/10/16 00:06:51 GMT FROM: Amy Lien at GSFC S. D. Barthelmy (GSFC), P.A. Evans (U Leicester), N. Gehrels (GSFC), A. Y. Lien (GSFC/UMBC), J. P. Norris (BSU), P. O'Brien (U Leicester), K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC), and H. Ziaeepour report on behalf of the Swift Team: We performed further analysis of GRB161004A (trigger #715084; Evans et al., GCN Circ. 19979), to explore the possibility to clarify its short/long nature. Using the full BAT event data set from T-240 to T+962 sec, the updated T90 is 3 +/- 1.4 s (using the 1-s binned light curve). This T90 is longer than the 1.08 +- 0.21 s originally reported (Palmer et al, GCN Circ. 20001). However, we note that due to the weakness of the burst, the standard pipeline finds a T90 that varies from ~ 1.3 s to ~ 3 s when using light curves with different bin sizes. The image analysis with the BAT data in 15-150 keV finds no significant detections for extended emission within several hundred seconds after the trigger. However, the BAT image from T+250 s to T+350 s, which is the time period around the peak of the XRT flare, does show a slight increase of significance of 3.8 sigma (comparing to ~ 1 to 2 sigma detections for other periods). Therefore, it is possible that the XRT flare might be the second peak of the prompt emission, but was close to the detection limit of the BAT. The time averaged spectrum is best fit by a simple power-law model, with an index of 1.3 +/- 0.33. This value is consistent with the average value of the short GRB distribution, and slightly on the harder side of the long burst distribution, but still within the majority (Lien & Sakamoto et al. 2016). The lag analysis is still unavailable due to the weakness of the burst (Palmer et al, GCN Circ. 20001). The bright flare in the XRT light curve around T+300 s is unusual for short GRBs. However, Swift have detected short GRBs with flares before (e.g., GRB 070724A, GRB 100816A; Margutti et al., 2011, MNRAS, 417, 2144), and thus we cannot rule out the short-burst possibility base on this. Therefore, we conclude that the burst nature remains ambiguous with current information.