//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24912 SUBJECT: GRB 190630A: Fermi GBM Final Real-time Localization DATE: 19/06/30 06:21:40 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely SHORT GRB At 06:09:58 UT on 30 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190630A (trigger 583567803.319036 / 190630257). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 307.0, Dec = -1.3 (J2000 degrees, equivalent to J2000 20h 27m, -1d 18'), with a statistical uncertainty of 7.7 degrees. The angle from the Fermi LAT boresight is 48.0 degrees. The skymap can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_skymap_all_bn190630257.png The HEALPix FITS file, including the estimated localization systematic, can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_healpix_all_bn190630257.fit The GBM light curve can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_lc_medres34_bn190630257.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24913 SUBJECT: Swift Trigger 912102: possible GRB 190630B DATE: 19/06/30 06:24:47 GMT FROM: Hans Krimm at NSF/NASA-GSFC H. A. Krimm (NSF), N. J. Klingler (PSU), K. L. Page (U Leicester) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 06:02:08 UT, the Swift Burst Alert Telescope (BAT) triggered and located possible GRB 190630B (trigger=912102). Swift slewed immediately to the location. The BAT on-board calculated location is RA, Dec 223.669, +41.521 which is RA(J2000) = 14h 54m 41s Dec(J2000) = +41d 31' 16" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 5 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. This increase in flux occurred during a rise in background due to entry to the SAA, so it is not immediately clear from the BAT data alone that this is indeed a burst rather than a noise event. The XRT began observing the field at 06:03:10.7 UT, 62.1 seconds after the BAT trigger. No source was detected in the 2.5-s promptly available image. We are waiting for the full dataset to detect and localise the XRT counterpart. UVOT took a finding chart exposure of 66 seconds with the White filter starting 65 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 25% of the BAT 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 BAT 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 0.01. Due to the high background in the BAT and the lack of immediate counterpart detection in the XRT, the Swift team will not be able to confirm or deny whether this event is a GRB without further data. Burst Advocate for this burst is H. A. Krimm (hkrimm AT nsf.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/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24918 SUBJECT: GRB 190630B, Swift-BAT refined analysis DATE: 19/06/30 16:01:10 GMT FROM: Hans Krimm at NSF/NASA-GSFC J. R. Cummings (CPI), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), F. Marshall (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+50 sec from the recent telemetry downlink, we report further analysis of BAT GRB 190630B (trigger #912102) (Krimm, et al., GCN Circ. 24913). The BAT ground-calculated position is RA, Dec = 223.729, 41.528 deg which is RA(J2000) = 14h 54m 55.0s Dec(J2000) = +41d 31' 42.4" with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows a single, weak pulse with a FRED-like shape, starting from T-3 sec, peaking at T+1 sec and fading to background by T+6 sec. We note that data is available until approximately T+250 sec. However, after T+50 sec, the background cannot be properly subtracted due to high background levels arising from Swift’s entry into the SAA. Therefore we only use data prior to T+50 sec for analysis. The raw light curve shows no sign of any burst activity after the initial pulse. T90 (15-350 keV) is 5.6 +- 0.9 sec (estimated error including systematics). The time-averaged spectrum from T-1.7 to T+4.7 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.36 +- 0.24. The fluence in the 15-150 keV band is 2.8 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.19 sec in the 15-150 keV band is 1.1 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. In the initial circular for GRB 190630B (Krimm, et al., GCN Circ. 24913), this event was reported as a possible burst. After the more complete analysis carried out here, we conclude that Swift trigger 912102 is indeed a GRB. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/912102/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24919 SUBJECT: GRB 190630B: Swift-XRT refined Analysis DATE: 19/06/30 17:37:06 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester), P.A. Evans (U. Leicester) and F.E. Marshall (NASA/GSFC) report on behalf of the Swift-XRT team: We have analysed 2.4 ks of XRT data for GRB 190630B, from 47 s to 28.2 ks after the BAT trigger. The data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. Using 307 s of PC mode data and 1 UVOT image, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 223.70024, +41.52614 which is equivalent to: RA (J2000): 14h 54m 48.06s Dec(J2000): +41d 31' 34.1" with an uncertainty of 3.1 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=1.32 (+0.08, -0.07). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 3.0 (+1.1, -0.4). The best-fitting absorption column is consistent with the Galactic value of 1.4 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 3.0 x 10^-11 (3.3 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Total column: 1 (+/-20) x 10^20 cm^-2 Galactic foreground: 1.4 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 3.0 (+1.1, -0.4) If the light curve continues to decay with a power-law decay index of 1.32, the count rate at T+24 hours will be 6.5 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x 10^-14 (2.1 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/00912102. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24927 SUBJECT: GRB 190630C: Swift detection of a burst DATE: 19/07/01 00:05:00 GMT FROM: David Palmer at LANL T. N. Ukwatta (LANL), J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 23:52:59 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190630C (trigger=912239). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 293.908, -32.751 which is RA(J2000) = 19h 35m 38s Dec(J2000) = -32d 45' 03" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 120 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 23:55:28.8 UT, 149.3 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 293.87874, -32.74273 which is equivalent to: RA(J2000) = 19h 35m 30.90s Dec(J2000) = -32d 44' 33.8" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 93 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. 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 1.02e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 157 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 0.11. This source lies within the current (Sector 13) field-of-view of TESS camera 1. Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 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/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24930 SUBJECT: GRB 190630C: Enhanced Swift-XRT position DATE: 19/07/01 03:12:27 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 195 s of XRT Photon Counting mode data and 1 UVOT images for GRB 190630C, 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 = 293.88034, -32.74405 which is equivalent to: RA (J2000): 19h 35m 31.28s Dec (J2000): -32d 44' 38.6" with an uncertainty of 1.9 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: 24931 SUBJECT: GRB 190630B: KAIT Optical Afterglow Confirmation DATE: 19/07/01 05:41:45 GMT FROM: Weikang Zheng at UC Berkeley WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to the Swift GRB 190630B (Krimm et al., GCN 24913; Cummings et al. GCN 24918) starting at 310s after the burst. Observations were performed with a sequence in the clear (roughly R), V, and I filters, and the exposure time was 60 s per image. Further analysis on our reported afterglow candidate (Zheng & Filippenko, GCN 24914) shows that the candidate position is within the enhanced XRT error circle (Page et al., GCN 24919), and its brightness faded more than 2 magnitude during our ~2 hours observing range. We therefore confirm this is the optical afterglow of GRB 190630B. A preliminary KAIT clear band light curve is available at: http://w.astro.berkeley.edu/~zwk/grb/GRB190630B/GRB190630B_kait.jpg //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24939 SUBJECT: GRB 190630C: AstroSat CZTI detection DATE: 19/07/01 13:59:57 GMT FROM: Vidushi Sharma at IUCAA V. Sharma, R. Gaikwad, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed the detection of a long GRB 190630C, which was also detected by Swift (Ukwatta T. N. et al., GCN # 24927) and Swift-XRT (Goad M. R. et al., GCN # 24930). The source was clearly detected in the 40-200 keV energy range. The light curve shows single pulse of emission with strongest peak at 23:53:01 UT. The measured peak count rate associated with the burst is 153 cts/s above the background in the combined data of four quadrants, with a total of 1301 cts. The local mean background count rate was 571 cts/s. Using cumulative rates, we measure a T90 of 21.3 s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. 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: 24941 SUBJECT: GRB 190630C: Swift-BAT refined analysis DATE: 19/07/01 14:58:51 GMT FROM: Hans Krimm at NSF/NASA-GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 190630C (trigger #912239) (Ukwatta, et al., GCN Circ. 24927). The BAT ground-calculated position is RA, Dec = 293.890, -32.759 deg which is RA(J2000) = 19h 35m 33.6s Dec(J2000) = -32d 45' 32.5" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 57%. The mask-weighted light curve shows a single FRED-shaped burst, beginning at ~T-5 sec, peaking at T+0 sec, and declining to background by ~T+40 sec. A spacecraft slew took the burst position out of the BAT field of view just before T+500 sec. T90 (15-350 keV) is 38.4 +- 9.3 sec (estimated error including systematics). The time-averaged spectrum from T-1.92 to T+50.23 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.96 +- 0.11. The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band is 2.0 +- 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/912239/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24943 SUBJECT: GRB 190630B: Swift/UVOT Upper Limits DATE: 19/07/01 17:59:50 GMT FROM: Kira Simpson at PSU GRB 190630B: Swift/UVOT Upper Limits K. K. Simpson (PSU) and F. E. Marshall (NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190630B 65 s after the BAT trigger (Krimm et al., GCN Circ. 24913). No optical afterglow consistent with the optical position (Zheng and Filippenko GCN Circ. 24914) 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 initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 65 131 65 >20.5 b 57357 57675 308 >20.69 uvm2 39177 40077 885 >20.36 u 46044 46193 145 >19.89 v 55313 55640 317 >18.87 uvw1 40084 40453 363 >20.02 uvw2 49543 49700 155 >19.09 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24944 SUBJECT: GRB 190630C: KAIT Optical Upper Limit DATE: 19/07/01 18:00:13 GMT FROM: Weikang Zheng at UC Berkeley WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to Swift GRB 190630C (Ukwatta et al., GCN 24927) starting at ~0.379 days after the burst. Observations were performed in the clear (roughly R) filters, a total of 31 images were obtained and the exposure time was 60 s per image. We do not detect any optical afterglow candidate within the Enhanced XRT position error circle (Goad et al., GCN 24930), neither in single image, nor in the co-add images. We estimate our limiting magnitude of our co-added image is ~19.0 mag calibrated to the APASS catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24945 SUBJECT: GRB 190630C: Swift/UVOT Upper Limits DATE: 19/07/01 19:32:37 GMT FROM: Kira Simpson at PSU GRB 190630C: Swift/UVOT Upper Limits K. K. Simpson (PSU) and T. N. Ukwatta (LANL) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190630C 136 s after the BAT trigger (Ukwatta et al., GCN Circ. 24927). No optical afterglow consistent with the XRT position (Goad et al. GCN Circ. 24930) 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 157 307 147 >20.5 white 157 307 147 >20.5 v 136 412 32 >18.1 w2 367 387 19 >20.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.11 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24947 SUBJECT: GRB 190630C: ISON-Castelgrande optical upper limit DATE: 19/07/01 20:07:58 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), S. Schmalz (KIAM), A. Pozanenko (IKI), A. Volnova (IKI), E. Mazaeva (IKI), I. Molotov (KIAM) report on behalf of larger GRB IKI FuN collaboration: We observed the field of GRB 190630C (Ukwatta et al., GCN 24927) with ORI-22 (22 cm) telescope of ISON-Castelgrande observatory in Clear filter starting on July 01 (UT) 00:03:42. We do not detect any object within enhanced Swift-XRT position (Goad et al., GCN 24930). Preliminary photometry of the field is following Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2019-07-01 00:03:42 0.02584 CR 53*60 n/d n/d 18.8 The photometry is based on nearby USNO-B1.0 (R2) stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24949 SUBJECT: GRB 190630B: Tien Shan and Koshka Zeiss-1000 optical upper limits DATE: 19/07/01 21:13:42 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Kusakin (FAPHI), I. Reva (FAPHI), A. Novichonok (KIAM), A. Pozanenko (IKI), E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov (KIAM) report on behalf of larger GRB IKI FuN collaboration: We observed the field of GRB 190630B (Krimm, et al., GCN 24913) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on June, 30 (UT) 18:40:21 and Koshka Observatory starting on June, 30 (UT) 20:38:42 in R-filter. We do not detect the afterglow (Zheng, et al., GCN 24914; Zheng, et al., GCN 24931). Preliminary photometry of the field is following Date UT start t-T0 Filter Exp. OT Err. UL Observatory (mid, days) (s) 2019-06-30 18:40:21 0.55999 R 6720 n/d n/d 22.3 TSHAO 2019-06-30 20:38:42 0.63060 R 3780 n/d n/d 21.9 Koshka The photometry is based on several nearby USNO-B1.0 stars. USNO-B1.0_id R2 1315-0255078 18.06 1314-0253302 17.18 1314-0253267 15.88 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24958 SUBJECT: GRB 190630C: Swift-XRT refined Analysis DATE: 19/07/02 00:05:19 GMT FROM: Phil Evans at U of Leicester M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , V. D'Elia (ASDC), B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester) and T.N. Ukwatta report on behalf of the Swift-XRT team: We have analysed 5.7 ks of XRT data for GRB 190630C (Ukwatta et al. GCN Circ. 24927), from 155 s to 57.3 ks after the BAT trigger. The data comprise 56 s 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. 24930). The light curve can be modelled with an initial power-law decay with an index of alpha=4.3 (+0.7, -0.5), followed by a break at T+310 s to an alpha of 1.06 (+0.12, -0.23). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 3.09 (+0.33, -0.29). The best-fitting absorption column is 2.7 (+/-0.7) x 10^21 cm^-2, in excess of the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.2 (+/-0.3) and a best-fitting absorption column of 2.0 (+1.0, -0.9) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.0 (+1.0, -0.9) x 10^21 cm^-2 Galactic foreground: 1.1 x 10^21 cm^-2 Excess significance: 1.7 sigma Photon index: 2.2 (+/-0.3) If the light curve continues to decay with a power-law decay index of 1.06, the count rate at T+24 hours will be 3.0 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.7 x 10^-14 (1.4 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/00912239. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24965 SUBJECT: IPN triangulation of GRB 190630A (short) DATE: 19/07/02 12:01:33 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova and K. Hurley, on behalf of the IPN, A. Goldstein, M. S. Briggs, and C. Wilson-Hodge on behalf of the Fermi GBM team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and S. Xiao, C. K. Li, X. B. Li, Y. Huang, and S. L. Xiong on behalf of the Insight-HXMT GRB team, report: The short-duration GRB 190630A was detected by Fermi (GBM trigger 583567803), INTEGRAL (SPI-ACS), and Insight (HXMT/HE) at about 22198 s UT (06:09:58). We have triangulated this GRB to a GBM-INTEGRAL annulus centered at RA(2000)=32.604 deg (02h 10m 25s) Dec(2000)=-47.005 deg (-47d 00' 16"), whose radius is 73.654 +/- 2.609 deg (3 sigma). The annulus is partially consistent with the 90% localization probability region of GW compact binary merger candidate event S190630ag (The LIGO Scientific Collaboration and the Virgo Collaboration GCN Circ. 24922). This annulus may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB190630_T22198/IPN/