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[vsnet-grb-info 41500] Konus-Wind detection of GRB 251230A / EP251230a
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43405 SUBJECT: Konus-Wind detection of GRB 251230A / EP251230a DATE: 26/01/14 19:13:21 GMT FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru> D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia, A. Tsvetkova, M. Ulanov, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 251230A / EP251230a (Swift-BAT detection: Lanava et al., GCN 43252; Einstein Probe-WXT detection: Wang et al., GCN 43259; Wang et al., GCN 43272; Insight-HXMT/HE detection: Guo et al., GCN 43299; GECAM-B detection: Guo et al., GCN 43301) triggered Konus-Wind at T0=04927.542 s UT (01:22:07.542). The burst light curve shows a multipeaked structure which starts at ~T0-25 s and has a total duration of ~73 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB251230_T04927/ As observed by Konus-Wind, the burst had the total fluence of 2.03(-0.15,+0.17)x10^-5 erg/cm2, and the 64-ms peak flux, measured from T0-0.224 s, of 2.51(-0.71,+0.80)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+49.408 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.04(-0.14,+0.16) and Ep = 354(-47,+64) keV (chi2 = 93/98 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.2 (chi2 = 93/97 dof). The spectrum near the maximum count rate (measured from T0 to T0+0.256 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.70(-0.51,+0.72) and Ep = 350(-85,+147) keV (chi2 = 19/15 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.8 (chi2 = 18/14 dof). All the quoted errors are at the 68% confidence level. All the quoted values are preliminary. View this GCN Circular online at https://gcn.nasa.gov/circulars/43405. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41499] GRB 260114A: SVOM/GRM observation of a short burst
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43404 SUBJECT: GRB 260114A: SVOM/GRM observation of a short burst DATE: 26/01/14 17:52:21 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> SVOM/GRM team: Chen-Wei Wang, Wen-Jun Tan, Yang-Zhao Ren, Zheng-Hang Yu, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Maria-Grazia Bernardini (INAF-OAB, LUPM) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260114A (SVOM trigger reference: sb26011401) at 2026-01-14T11:40:26.400 (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43395), Swift/BAT (R. A. J. Eyles-Ferris et al., GCN #43396) and GECAM-B (Ren et al., GCN #43402). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of a single pulse with a T90 of 0.38 +0.06/-0.04 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260114A.png In addition, the position of this burst, as determined by Swift/BAT (RA = 74.602, Dec = -7.994, Error = 3.3 arcseconds, GCN #43396), is located at about 94 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. With this localization, the time-averaged spectrum from T0-0.12 to T0+0.3 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.43 +0.13/-0.11 and the cutoff energy, parameterized as Epeak, is 954 +134/-120 keV. The event fluence (10-1000 keV) in this time interval is (6.72 +0.23/-0.22)E-06 erg/cm^2. The localization of GRB 260114A in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260114A_amati.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM/GRM point of contact for this burst is: Chen-Wei Wang (IHEP) (cwwang(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43404. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41498] Swift GRB 260114A: Global MASTER-Net observations report
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43403 SUBJECT: Swift GRB 260114A: Global MASTER-Net observations report DATE: 26/01/14 17:42:32 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A.Sosnovskij (CrAO), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory) MASTER-Tunka robotic telescope [1] located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB 260114A ( R. A. J. Eyles-Ferris et al., GCN 43396) errorbox 13094 sec after notice time and 13137 sec after trigger time at 2026-01-14 15:19:23 UT, with upper limit up to 20.0 mag. The observations began at zenith distance = 60 deg. The sun altitude is -52.6 deg. The galactic latitude b = -28 deg., longitude l = 207 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3101880 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 13167 | MASTER-Tunka | C | 60 | 19.4 | 13227 | MASTER-Tunka | C | 180 | 20.0 | Coadd 13241 | MASTER-Tunka | C | 60 | 15.5 | 13241 | MASTER-Tunka | C | 60 | 19.2 | 13313 | MASTER-Tunka | C | 60 | 19.1 | 13389 | MASTER-Tunka | C | 60 | 14.9 | 13389 | MASTER-Tunka | C | 60 | 19.1 | 13449 | MASTER-Tunka | C | 180 | 19.8 | Coadd 13461 | MASTER-Tunka | C | 60 | 15.2 | 13461 | MASTER-Tunka | C | 60 | 19.2 | 13536 | MASTER-Tunka | C | 60 | 17.8 | 13536 | MASTER-Tunka | C | 60 | 19.0 | 13611 | MASTER-Tunka | C | 60 | 18.7 | 13611 | MASTER-Tunka | C | 60 | 19.3 | 14458 | MASTER-Tunka | C | 60 | 19.1 | 14458 | MASTER-Tunka | C | 60 | 18.6 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. [1] - V.M. Lipunov, V.G. Kornilov, E.S. Gorbovskoy, N.A. Tiurina & A.S.Kuznetsov, 2023, Astronomical Robotic Networks and Operative Multichanel Astrophysics, Lomonosov MSU PRESS, 591pp. http : // www.pereplet.ru/lipunov/625.html View this GCN Circular online at https://gcn.nasa.gov/circulars/43403. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41497] GRB 260114A: GECAM-B observation of a short burst
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43402 SUBJECT: GRB 260114A: GECAM-B observation of a short burst DATE: 26/01/14 17:19:48 GMT FROM: renyz16607(a)163.com Yang-Zhao Ren, Chen-Wei Wang, Wen-Jun Tan, Zheng-Hang Yu, Shao-Lin Xiong (IHEP) report on behalf of GECAM team: GECAM-B was triggered in-flight by GRB 260114A, at 2026-01-14T11:40:26.350 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43395), and Swift/BAT (Eyles-Ferris et al., GCN #43396). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of a pulse with a duration (T90) of 0.38 +0.18/-0.08 s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260114A.png The time-averaged spectrum from T0-0.1 to T0+0.4 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.26 +0.16/-0.30 and the cutoff energy, parameterized as Epeak, is 700 +93/-96 keV. The event fluence (10-1000 keV) in this time interval is (5.03 +0.34/-0.31)E-06 erg/cm^2. The 'Amati' relation diagram of GRB 260114A is shown at: https://www.bursthub.cn//admin/static/gecambgrb260114A_amati.png Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS). View this GCN Circular online at https://gcn.nasa.gov/circulars/43402. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41496] GRB 260114A: Mondy optical observations
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43401 SUBJECT: GRB 260114A: Mondy optical observations DATE: 26/01/14 16:57:54 GMT FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com> A. Volnova (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov (HSE, IKI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 260114A (Eyles-Ferris et al., GCN 43396; Fermi GBM team, GCN 43395; Bissaldi et al., GCN 43400) with the AZT-33IK 1.5m telescope of the Mondy observatory starting on 2026-01-14 (UT) 12:17:27 in R filter. Within the Swift/XRT error circle (Eyles-Ferris et al., GCN 43396) we detect the optical counterpart (Li et al., GCN 43398). Preliminary photometry is the following: Date UT start t-T0 Exp. Filter Obj. Err. UL Site/Telescope (mid,days) (n*s) (3sigma) 2026-01-14 12:17:27 0.08360 37*120 R 20.41 0.15 21.6 The photometry is calibrated using USNO-B1.0 stars and is not corrected for the Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43401. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41495] GRB 260114A: Fermi GBM observation
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43400 SUBJECT: GRB 260114A: Fermi GBM observation DATE: 26/01/14 16:32:46 GMT FROM: Elisabetta Bissaldi at Politecnico and INFN Bari <elisabetta.bissaldi(a)ba.infn.it> E. Bissaldi (Politecnico and INFN Bari) reports on behalf of the Fermi GBM Team: "At 11:40:26.31 UT on 14 January 2026, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 260114A (trigger 790083631 / 260114486), which was also detected by the Swift/BAT (Eyles-Ferris et al. 2026, GCN 43396). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 70 degrees. The GBM light curve consists of a bright emission episode with a duration (T90) of about 320 ms (50-300 keV). The time-averaged spectrum from T0-0.064 s to T0+0.384 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.07 +/- 0.06 and the cutoff energy, parameterized as Epeak, is 583 +/- 25 keV. The event fluence (10-1000 keV) in this time interval is (4.87 +/- 0.12)E-06 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.064 s in the 10-1000 keV band is 35.9 +/- 1.4 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak = 575 +/- 29 keV, alpha = -0.06 +/- 0.06, and beta = -3.5 +/- 0.6. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/" View this GCN Circular online at https://gcn.nasa.gov/circulars/43400. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41494] GRB 260112B: GECAM-B observation
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43399 SUBJECT: GRB 260112B: GECAM-B observation DATE: 26/01/14 15:16:26 GMT FROM: guohx(a)ihep.ac.cn Hao-Xuan Guo, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team: GECAM-B was triggered on-ground by GRB 260112B, at 2026-01-12T20:45:55.000 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43380). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of multiple pulses with a duration (T90) of 15.9 +1.7/-2.2 s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260112B.png Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS). View this GCN Circular online at https://gcn.nasa.gov/circulars/43399. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41493] GRB 260114A: GMG Optical Observation
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43398 SUBJECT: GRB 260114A: GMG Optical Observation DATE: 26/01/14 13:39:46 GMT FROM: Rui-Zhi Li at Yunnan Observatories, CAS <liruizhi(a)ynao.ac.cn> R.-Z. Li, J. Mao, B.-T. Wang, F.-F. Song, Y. Wang, J.-G. Wang and B. Wang (YNAO, CAS) report: We observed the field of GRB 260114A (Eyles-Ferris et al., GCN 43396; Fermi GBM team, GCN 43395; T0 at 2026-01-14T11:40:26) using the GMG-2.4m telescope at the Lijiang Observatory. The observation began at 2026-01-14T12:18:52, about 0.64 hours after the trigger. We detected an optical source within the Swift/XRT error circle (Eyles-Ferris et al., GCN 43396). The preliminary analysis results for this source are presented below. +---------------+------------+----------+--------------+----------------+ | Tmid-T0 [h] | Exp. [s] | Filter | Mag | 5-sigma U.L. | +===============+============+==========+==============+================+ | 0.81 | 1200 | r | 21.19 ± 0.06 | 22.6 | +---------------+------------+----------+--------------+----------------+ We note that an extended galaxy (R.A., Dec. = 04:58:23.41, −08:00:49.6; r = 21.47 mag in the Pan-STARRS DR2 image) is located within the Swift/XRT error circle. Three objects within the Swift/XRT error circle have photometric redshifts of z ~ 0.5 in the DESI Legacy Surveys. Given the poor seeing conditions at the Lijiang Observatory, no additional candidate sources in our image were found within the Swift/XRT error circle. The given magnitudes are derived based on calibration against Pan-STARRS1 field stars, and are not corrected for the expected Galactic foreground extinction, corresponding to a reddening of E(B-V) = 0.0685 mag in the direction of the optical source (Schlafly & Finkbeiner 2011). View this GCN Circular online at https://gcn.nasa.gov/circulars/43398. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41492] Fermi-LAT Gamma-ray Observations of IceCube-260111A
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43397 SUBJECT: Fermi-LAT Gamma-ray Observations of IceCube-260111A DATE: 26/01/14 12:42:22 GMT FROM: Leo Pfeiffer at University of Würzburg <pfeiffer.leo(a)gmail.com> L. Pfeiffer (Univ. of Wuerzburg), S. Buson (DESY, Univ. of Wuerzburg) and S. Garrappa (Weizmann Institute of Science) on behalf of the Fermi-LAT collaboration: We report an analysis of observations of the vicinity of the high-energy IC-260111A neutrino event (GCN 43374) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 26-01-11 at 20:10:33.91 UTC (T0) with J2000 position RA = 70.88 (+1.55, -1.40) deg, Decl. = 34.59 (+0.76, -0.64 ) deg 90% PSF containment. One cataloged >100 MeV gamma-ray source is located within the 90% IC-260111A localization error, at a distance of roughly 0.3 deg (Fourth Fermi-LAT catalog, 4FGL-DR4, The Fermi-LAT collaboration 2023, arXiv:2307.12546). This is the object 4FGL J0444.6+3425 associated with the blazar of uncertain type B2 0441+34. Based on a preliminary analysis of the LAT data over the timescale of one day and one month prior T0, this object is not significantly detected at gamma-rays. We searched for the existence of intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (> 100 MeV) within the IC-260111A 90% confidence localization. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is 3.0e-10 ph cm^-2 s^-1 for ~17-years (2008-08-04 / T0), <9.3e-09 (1.6 e-07) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For this analysis, the Fermi-LAT contact person is L. Pfeiffer (leonard.pfeiffer at uni-wuerzburg.de). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. View this GCN Circular online at https://gcn.nasa.gov/circulars/43397. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41491] GRB 260114A: Swift detection of a short burst
by GCN Circulars 14 Jan '26

14 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43396 SUBJECT: GRB 260114A: Swift detection of a short burst DATE: 26/01/14 11:55:28 GMT FROM: Rob Eyles-Ferris at U of Leicester <raje1(a)leicester.ac.uk> R. A. J. Eyles-Ferris (U Leicester), J. A. Kennea (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester) and B. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift Observatory Team: At 11:40:26 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 260114A (trigger=1440319). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 74.602, -7.994 which is RA(J2000) = 04h 58m 25s Dec(J2000) = -07d 59' 37" 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 0.5 sec. The peak count rate was ~16000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 11:42:28.4 UT, 122.2 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 74.59830, -8.01433 which is equivalent to: RA(J2000) = 04h 58m 23.59s Dec(J2000) = -08d 00' 51.6" with an uncertainty of 3.3 arcseconds (radius, 90% containment). This location is 74 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 https://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 consistent with the Galactic value of 5.72 x 10^20 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 126 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 0.080. Burst Advocate for this burst is R. A. J. Eyles-Ferris (raje1 AT leicester.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/) View this GCN Circular online at https://gcn.nasa.gov/circulars/43396. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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