//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22902 SUBJECT: GRB 180705A: Swift detection of a burst DATE: 18/07/05 15:55:08 GMT FROM: Scott Barthelmy at NASA/GSFC M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC), A. A. Breeveld (UCL-MSSL), A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), A. Deich (PSU), S. W. K Emery (UCL-MSSL), J.D. Gropp (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), B. Sbarufatti (PSU) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 15:41:14 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180705A (trigger=846299). Swift did not slew due to an observing constraint. The BAT on-board calculated location is RA, Dec 212.594, -11.630, which is RA(J2000) = 14h 10m 23s Dec(J2000) = -11d 37' 48" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As is typical for image triggers, the real-time light curve does not show anything significant. The image trigger significance is 7.8 sigma, therefore we have high confidence in this event. Due to an observing constraint, Swift will not slew until T0+54 minutes. There will be no XRT or UVOT data until this time. Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22903 SUBJECT: GRB 180705A: Swift-XRT observations DATE: 18/07/05 17:10:37 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), G. Tagliaferri (INAF-OAB), S. Campana (INAF-OAB), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and D.N. Burrows (PSU) report on behalf of the Swift-XRT team: The XRT began observing the field of GRB 180705A at 16:37:18.4 UT, 3363.7 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 212.61326, -11.64841 which is equivalent to: RA(J2000) = 14h 10m 27.18s Dec(J2000) = -11d 38' 54.3" with an uncertainty of 4.3 arcseconds (radius, 90% containment). This location is 94 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22904 SUBJECT: GRB 180705A: MASTER optical observation DATE: 18/07/05 18:08:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tiurina, A.Kuznetsov, V.Chazov, I. Gorbunov, D. Vlasenko, D.Zimnukhov, D.Kuvshinov, P.Balanutsa, V.Vladimirov Lomonosov Moscow State University,SAI D. Buckley, South African Astronomical Observatory (SAAO) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias (IAC) A. Tlatov, V.Senik, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory R. Podesta, F. Podesta, C. Lopez, C.Francile Observatorio Astronomico Felix Aguilar (OAFA) H.Levato, Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) O. Gres, N.M.Budnev , Yu.Ishmuhametova Irkutsk State University (ISU) A. Gabovich, V. Yurkov, Yu. Sergienko Blagoveschensk Educational State University (BSPU) MASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) , located in South African Astronomical Observatory, was pointed to the Swift GRB180705A (BAT: Stamatikos et al. GCN 22902, GRBtime: 2018-07-05 15:41:14UT; XRT : RA,Dec2000=14h 10m 27.18s -11d 38' 54.3" Kennea et al. GCN22903) at 2018-07-05 15:54:52 ( GRB Altitude: 55.90, Sun: Altitude: -3.10) at sunset. So MASTER-SAAO started GRB180705A observations at 2018-07-05 16:35:54UT (GRB altitute: 62.78, Sun: Altitude: -11.10). MASTER automatic unfiltered (W=0.2B+0.8R by USNO-B1) limits are the following T_start,UT Exp,s mlim MASTER-II 2018-07-05 16:35:54 540 18.8 WEST 2018-07-05 16:35:54 180 17.9 WEST 2018-07-05 16:35:59 540 18.3 EAST 2018-07-05 16:35:59 180 17.5 EAST 2018-07-05 16:39:32 180 18.2 WEST 2018-07-05 16:39:37 180 17.9 EAST 2018-07-05 16:44:51 180 18.7 WEST 2018-07-05 16:44:56 180 18.4 EAST 2018-07-05 16:48:21 540 19.7 WEST 2018-07-05 16:48:21 180 18.8 WEST 2018-07-05 16:48:25 540 19.5 EAST 2018-07-05 16:48:25 180 18.5 EAST 2018-07-05 16:51:52 180 19.0 WEST 2018-07-05 16:51:56 180 18.8 EAST 2018-07-05 16:55:26 180 19.0 WEST 2018-07-05 16:55:30 180 18.8 EAST 2018-07-05 16:58:59 540 19.9 WEST 2018-07-05 16:58:59 180 19.3 WEST 2018-07-05 16:59:04 540 19.7 EAST 2018-07-05 16:59:04 180 19.0 EAST 2018-07-05 17:02:29 180 19.3 WEST 2018-07-05 17:02:34 180 19.0 EAST 2018-07-05 17:05:58 180 19.3 WEST 2018-07-05 17:06:03 180 19.0 EAST 2018-07-05 17:09:33 540 20.0 WEST 2018-07-05 17:09:33 180 19.3 WEST 2018-07-05 17:09:37 540 19.6 EAST 2018-07-05 17:09:37 180 19.0 EAST 2018-07-05 17:13:06 180 19.3 WEST 2018-07-05 17:13:10 180 19.1 EAST 2018-07-05 17:16:51 180 19.3 WEST 2018-07-05 17:16:56 180 19.0 EAST 2018-07-05 17:20:25 180 19.3 WEST 2018-07-05 17:20:29 180 19.0 EAST The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22906 SUBJECT: GRB 180705A: Enhanced Swift-XRT position DATE: 18/07/05 19:08:58 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 1348 s of XRT Photon Counting mode data and 4 UVOT images for GRB 180705A, 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 = 212.61323, -11.64745 which is equivalent to: RA (J2000): 14h 10m 27.17s Dec (J2000): -11d 38' 50.8" 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: 22907 SUBJECT: GRB 180705A: Swift-BAT refined analysis DATE: 18/07/06 03:32:53 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), 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-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180705A (trigger #846299) (Stamatikos et al., GCN Circ. 22902). The BAT ground-calculated position is RA, Dec = 212.605, -11.640 deg which is RA(J2000) = 14h 10m 25.1s Dec(J2000) = -11d 38' 23.7" with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 36%. The mask-weighted light curve shows some weak emission that starts at ~T0 and ends at ~T+130 s. However, the burst went out of the BAT FOV from T+158 s to T+204 s due to a preplanned slew, and thus there might be additional emission when the burst was out of the FOV. The burst came back in the BAT FOV shortly during the slew period (from T0+205 s to T0+262 s), though no emission are found during this time. T90 (15-350 keV) is 123.2 +- 16.6 sec (estimated error including systematics). The time-averaged spectrum from T+0.26 to T+133.70 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.63 +- 0.22. The fluence in the 15-150 keV band is 2.0 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+3.60 sec in the 15-150 keV band is 0.7 +- 0.3 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/846299/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22911 SUBJECT: GRB 180705A: RATIR Optical Observations DATE: 18/07/06 09:19:42 GMT FROM: Alan M. Watson at Instituto de Astronomia UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 180705A (Stamatikos et al., GCN Circ. 22902) 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 2018/07 6.16 to 2018/07 6.27 UTC (12.19 to 14.82 hours after the BAT trigger), obtaining a total of 1.74 hours exposure in the r and i bands. For a source within the Swift-XRT error circle (Kennea et al., GCN Circ. 22903), in comparison with the SDSS DR9 catalog, we obtain the following 3-sigma upper limits: r > 23.20 i > 23.07 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: 22912 SUBJECT: GRB 180705A: Swift/UVOT Upper Limits DATE: 18/07/06 10:11:35 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL), S. W. K Emery (UCL-MSSL) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180705A 3368 s after the BAT trigger (Stamatikos et al., GCN Circ. 22902). No optical afterglow consistent with the enhanced XRT position (Goad et al. GCN Circ. 22906) 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 3368 3485 115 >20.2 white 3368 5327 312 >20.8 v 4103 5738 393 >18.9 b 4923 11649 311 >20.5 u 4718 11527 1082 >21.0 w1 4513 16889 483 >20.5 m2 4308 15205 647 >20.1 w2 5333 5533 197 >20.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.06 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22913 SUBJECT: GRB 180705A: TSHAO optical upper limit DATE: 18/07/06 11:29:42 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), A. Kusakin (FAPHI), I. Reva (FAPHI), A. Volnova (IKI), M. Krugov (FAPHI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 180705A (Stamatikos et al., GCN 22902) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on July 05 (UT) 16:13:52. We obtained several images in R-filter. Within enhanced XRT Swift-XRT position (Goad et al., GCN 22906) we do not detect any object. Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-07-05 16:13:52 0.04895 R 25*120 n/d n/d 21.3 The photometry is based on several nearby SDSS-DR12 stars. Ref.stars SDSS-DR12_id R(Lupton) J141030.67-113927.0 17.460 J141015.17-113809.7 17.680 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22920 SUBJECT: GRB 180705A: Swift-XRT refined Analysis DATE: 18/07/06 17:10:02 GMT FROM: Phil Evans at U of Leicester A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), V. D'Elia (ASDC) and M. Stamatikos report on behalf of the Swift-XRT team: We have analysed 5.7 ks of XRT data for GRB 180705A (Stamatikos et al. GCN Circ. 22902), from 3.4 ks to 56.6 ks after the BAT trigger. The data comprise 1.1 ks in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 22906). The light curve can be modelled with a power-law decay with a decay index of alpha=1.12 (+0.17, -0.13). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.99 (+0.32, -0.30). The best-fitting absorption column is 3.9 (+1.8, -1.5) x 10^21 cm^-2, in excess of the Galactic value of 5.8 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 3.9 x 10^-11 (6.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.9 (+1.8, -1.5) x 10^21 cm^-2 Galactic foreground: 5.8 x 10^20 cm^-2 Excess significance: 3.7 sigma Photon index: 1.99 (+0.32, -0.30) If the light curve continues to decay with a power-law decay index of 1.12, the count rate at T+24 hours will be 6.4 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.5 x 10^-13 (3.8 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/00846299. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22929 SUBJECT: GRB 180705A: RTT150 optical upper limit DATE: 18/07/08 16:42:54 GMT FROM: Rodion Burenin at IKI, Moscow I. Bikmaev, E. Irtuganov, N. Sakhibullin (KFU/AST), R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Khamitov, S. Ozdemir (TUG), E. Gogus (Sabanci Uni.) report: We observed the field of GRB 180705A (Stamatikos et al., GCN 22902) with the Russian-Turkish 1.5-m optical telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey) using the TFOSC instrument. We obtained series of Rc exposures in July 05, 2018 (6 frames x 600 sec, UT = 19:12 - 20:19), ~ 4 hours after the burst. Within enhanced Swift-XRT position (Goad et al., GCN 22906) we have not detected any object down to Rc =~ 23.5 mag in the combined image (calibrated against SDSS secondary standard stars). Our result confirms OT non-detections as published in other GCNs (Lipunov et al., GCN 22904, Watson et al., GCN 22911, Breeveld et al., GCN 22912, Mazaeva et al., GCN 22913). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22941 SUBJECT: GRB 180705A: OSN observations DATE: 18/07/11 19:25:41 GMT FROM: Alexander Kann at IAA-CSIC D. A. Kann, L. Izzo (both HETH/IAA-CSIC), and A. Sota (IAA/CSIC) report on behalf of HETH: We observed the field of GRB 180705A (Stamatikos et al., GCN #22902) with the 1.5-m OSN telescope in Granada, Spain. We obtained 20 x 300 s images in the Ic band centered at 0.262416 days (6.3 hrs) after the GRB. At the XRT position of the GRB (Goad et al., GCN #22906), there is a possible faint source, formally detected at Ic (Vega) = 23.6 +/- 0.2 mag. We note, however, that the background of the image is structured because of the proximity of the bright star HD 123921 (V ~ 9 mag), therefore the detection may be spurious. The formal 3 sigma upper limit is Ic > 24 mag, also possibly overestimated. Even if the source we detect is not real, any afterglow of this GRB is clearly very faint, in agreement with other non-detection reports (Lipunov et al., GCN #22904, Watson et al., GCN #22911, Breeveld et al., GCN #22912, Mazaeva et al., GCN #22913, Bikmaev et al., GCN #22929). The field was calibrated against SDSS secondary standard stars using the transformation of Lupton (2005).