- vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 42607] GRB 260506A: Fermi GBM Final Real-time Localization
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44481 SUBJECT: GRB 260506A: Fermi GBM Final Real-time Localization DATE: 26/05/06 06:39:24 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply(a)GIOC.nsstc.nasa.gov> The Fermi GBM team reports the detection of a likely SHORT GRB At 06:28:48 UT on 6 May 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260506A (trigger 799741733.38117 / 260506270). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 145.7, Dec = 76.1 (J2000 degrees, equivalent to J2000 09h 42m, 76d 05'), with a statistical uncertainty of 7.2 degrees. The angle from the Fermi LAT boresight is 18.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506270/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506270/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506270/… View this GCN Circular online at https://gcn.nasa.gov/circulars/44481. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42606] GRB 260503A: GECAM-B observation of a burst
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44480 SUBJECT: GRB 260503A: GECAM-B observation of a burst DATE: 26/05/06 05:19:05 GMT FROM: Xinghao Luo at IHEP <2952704891(a)qq.com> Xing-Hao Luo, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team: GECAM-B was triggered in-flight by GRB 260503A, at 2026-05-03T20:40:18.050 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #44451). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of multiple pulses with a duration (T90) of 21 +4/-3 s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260503A.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/44480. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42605] IceCube Alert 260505A: Global MASTER-Net observations report
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44479 SUBJECT: IceCube Alert 260505A: Global MASTER-Net observations report DATE: 26/05/05 22:26:33 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-Kislovodsk robotic telescope [1] located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the IceCube Alert 260505A (trigger No 58544625,16h 27m 57.60s , +54d 52m 12.0s, R=0.67) errorbox 1 days 3353 sec after notice time and 1 days 3411 sec after trigger time at 2026-05-05 22:08:12 UT, with upper limit up to 19.2 mag. The observations began at zenith distance = 13 deg. The sun altitude is -29.0 deg. The galactic latitude b = 42 deg., longitude l = 84 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3293437 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 89842 | 2026-05-05 22:08:12 | MASTER-Kislovodsk | (16h 26m 24.62s , +55d 13m 07.6s) | C | 60 | 13.2 | 89842 | 2026-05-05 22:08:12 | MASTER-Kislovodsk | (16h 26m 52.94s , +54d 49m 59.4s) | C | 60 | 19.1 | 89940 | 2026-05-05 22:09:50 | MASTER-Kislovodsk | (16h 26m 58.23s , +54d 48m 57.5s) | C | 60 | 19.1 | 90036 | 2026-05-05 22:11:26 | MASTER-Kislovodsk | (16h 26m 12.84s , +55d 11m 17.5s) | C | 60 | 13.3 | 90037 | 2026-05-05 22:11:27 | MASTER-Kislovodsk | (16h 26m 52.47s , +54d 47m 56.7s) | C | 60 | 19.1 | 90125 | 2026-05-05 22:12:56 | MASTER-Kislovodsk | (16h 26m 24.80s , +55d 12m 02.6s) | C | 60 | 13.6 | 90125 | 2026-05-05 22:12:56 | MASTER-Kislovodsk | (16h 26m 56.65s , +54d 48m 13.7s) | C | 60 | 19.2 | 90215 | 2026-05-05 22:14:25 | MASTER-Kislovodsk | (16h 26m 17.07s , +55d 12m 10.3s) | C | 60 | 12.9 | 90215 | 2026-05-05 22:14:25 | MASTER-Kislovodsk | (16h 26m 52.12s , +54d 49m 38.8s) | C | 60 | 19.2 | 90303 | 2026-05-05 22:15:54 | MASTER-Kislovodsk | (16h 26m 16.58s , +55d 10m 30.3s) | C | 60 | 13.1 | 90303 | 2026-05-05 22:15:54 | MASTER-Kislovodsk | (16h 26m 51.53s , +54d 48m 00.8s) | C | 60 | 19.1 | 90391 | 2026-05-05 22:17:21 | MASTER-Kislovodsk | (16h 26m 20.13s , +55d 12m 14.8s) | C | 60 | 12.7 | 90391 | 2026-05-05 22:17:21 | MASTER-Kislovodsk | (16h 26m 54.99s , +54d 49m 43.2s) | C | 60 | 19.0 | 90479 | 2026-05-05 22:18:50 | MASTER-Kislovodsk | (16h 26m 12.86s , +55d 11m 27.4s) | C | 60 | 12.7 | 90479 | 2026-05-05 22:18:50 | MASTER-Kislovodsk | (16h 26m 47.70s , +54d 48m 56.2s) | C | 60 | 19.2 | 90568 | 2026-05-05 22:20:18 | MASTER-Kislovodsk | (16h 26m 47.19s , +54d 49m 56.1s) | C | 60 | 19.2 | 90656 | 2026-05-05 22:21:46 | MASTER-Kislovodsk | (16h 26m 19.15s , +55d 11m 26.0s) | C | 60 | 12.7 | 90656 | 2026-05-05 22:21:46 | MASTER-Kislovodsk | (16h 26m 53.95s , +54d 48m 57.0s) | C | 60 | 19.2 | 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/44479. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42604] GRB 260430B: Glowbug gamma-ray detection
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44478 SUBJECT: GRB 260430B: Glowbug gamma-ray detection DATE: 26/05/05 16:06:39 GMT FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil> C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2,3], operating on the International Space Station, reports the detection of GRB 260430B, which was also detected by AstroSat/CZTI (GCN 44469) and SVOM/GRM (sb26043004). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-04-30 16:04:22.184 with a duration of 49.2 s and a total significance of about 113 sigma. The light curve comprises a complex series of peaks throughout the burst duration. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS and operated until 2024 April when it was put in safe storage on orbit. Glowbug was removed from storage and resumed operation on 2025 September 12. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Woolf, R.S. et al. 2024, Proc. SPIE, 13151, id. 1315108 Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/44478. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42603] GRB 260504B: SVOM/VT optical upper limits
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44477 SUBJECT: GRB 260504B: SVOM/VT optical upper limits DATE: 26/05/05 15:53:02 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> H. L. Li, L. P. Xin, C. Wu, Y. L. Qiu, Y. N. Ma, Z. H. Yao, J. R. Xu, X. H. Han, J. Wang, Y. Xu, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA/Irfu), Y. Wang (PMO,CAS; UCB) report on behalf of the SVOM/VT team. SVOM/VT performed observations with an automatic slew to GRB 260504B detected by SVOM/ECLAIRs (sb26050402, Saccardi et al., GCN 44454), SVOM/GRM (Wang et al., GCN 44470), GECAM-B (Wang et al., GCN 44473) and Konus-Wind (Frederiks et al., GCN 44474). The observation started at 2026-05-04T09:34:59 UTC, 220 seconds post trigger and lasted for 6 orbits (about 8 hours), in the VT_B (400-650 nm) and VT_R (650-1000 nm) channels simultaneously. No uncatalogued sources were detected within the error box of SVOM/ECLAIRs (Saccardi et al., GCN 44454) or SVOM/MXT (Maggi et al., GCN 44468), compared to the Legacy Survey. The following measurements are in the AB magnitude and are not corrected for Galactic extinction: Mid time | Band | Exposure Time | 5-sigma upper limit 670 s VT_B 18*50 s > 22.5 mag 670 s VT_R 18*50 s > 22.5 mag 2.59 h VT_B 34*100 s > 23.0 mag 2.59 h VT_R 33*100 s > 23.0 mag Our result is consistent with the results from the rapid decay in SVOM/MXT (Saccardi et al., GCN 44454), upper limit of EP-FXT (Zhou et al., GCN 44467), optical non-detections by MASTER-OAFA(Podesta et al., GCN 44455), LCO (Turpin et al., GCN 44456), AST3-2 (Sun et al., GCN 44457) and REM (Brivio et al., GCN 44460). 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. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS. View this GCN Circular online at https://gcn.nasa.gov/circulars/44477. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42602] GRB 260421B: radio observation with the VLA
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44476 SUBJECT: GRB 260421B: radio observation with the VLA DATE: 26/05/05 15:50:44 GMT FROM: Stefano Giarratana at INAF-OAB <s.giarratana(a)ira.inaf.it> S. Giarratana (INAF-OAB), M. Giroletti (INAF-IRA), G. Ghirlanda (INAF-OAB), N. Di Lalla (Stanford Univ.), N. Omodei (Stanford Univ.), O. S. Salafia (INAF-OAB), L. Nava (INAF-OAB) At 05:08:16 UT on 2026 April 22 (T_mid = 1.07 days post-burst) the Karl G. Jansky VLA observed the field of GRB 260421B (Fermi GBM team, GCN 44360, 44382; SVOM mission team, GCN 44362, GCN 44389, 44397; Insight-HXMT team, GCN 44401) at central frequencies of 6, 10 and 15 GHz. The standard 3C286 was used as bandpass and flux density calibrator, while J1239-1023 was used as phase calibrator. From a preliminary analysis, we do not detect the radio counterpart of GRB 260421B. We derive the following upper limits (UL; 3sigma): ================================================================ T_mid Freq UL r.m.s. Beam PA [days] [GHz] [uJy] [uJy/b] [arcsec^2] [deg] ================================================================ 1.07 6 24 8 0.47x0.28 11 1.07 10 24 8 0.30x0.18 11 1.07 15 27 9 0.20x0.11 -2 ================================================================ We would like to thank the staff of the VLA for approving, executing, and processing the observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. These observations were carried out as part of project SF181027, approved in the framework of the Fermi - NRAO joint program agreement. View this GCN Circular online at https://gcn.nasa.gov/circulars/44476. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42601] Konus-Wind detection of a burst from SGR 1E1841-045 on 2026 May 2
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44475 SUBJECT: Konus-Wind detection of a burst from SGR 1E1841-045 on 2026 May 2 DATE: 26/05/05 15:28:39 GMT FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru> A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: A bright burst from SGR 1E1841-045 (IPN triangulation: Ridnaia et al., GCN 44448; SVOM-GRM detection: Zao et al., GCN 44450) triggered Konus-Wind at T0=20396.052 s UT (05:39:56.052) on 2026 May 2. The burst light curve shows a single pulse, which starts at ~T0-50 ms and has a total duration of ~96 ms. The emission is seen up to ~200 keV. The Konus-Wind light curve of this burst is available at http://www.ioffe.ru/LEA/SGRs/260502_T20396/ As observed by Konus-Wind, the burst had a fluence of 8.64(-0.45,+0.46)x10^-7 erg/cm2, and a 16-ms peak flux, measured from T0-0.004 s, of 1.93(-0.16,+0.16)x10^-5 erg/cm2/s (both in the 20 - 500 keV energy range). The spectrum of the burst (measured from T0 to T0+0.064 s) is best fit in the 20 - 500 keV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = 0.16(-0.69,+0.76) and Ep = 48(-4,+3) keV (chi2 = 12/15 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/44475. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42600] Konus-Wind detection of GRB 260504B (short/hard)
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44474 SUBJECT: Konus-Wind detection of GRB 260504B (short/hard) DATE: 26/05/05 14:25:39 GMT FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru> D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The short GRB 260504B (SVOM/ECLAIRs detection: Saccardi et al., GCN 44454; SVOM/GRM detection: Wang et al., GCN 44470; GECAM-B detection: Wang et al., GCN 44473) triggered Konus-Wind (KW) at T0=34281.198 s UT (09:31:21.198). The burst light curve shows a single pulse, which starts at ~T0-0.05 s and has a duration of ~0.21 s. The emission is seen up to ~6 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB260504_T34281/ As observed by Konus-Wind, the burst had the total fluence of (2.39 ± 0.52)x10^-6 erg/cm^2 and a 16-ms peak energy flux, measured from T0-0.032, of (2.06 ± 0.45)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+0.192 s) is best fitted in the 20 keV - 15 MeV range by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.00 (-0.12, + 0.14) and Ep = 1461(-398,+584) keV, chi^2 = 34/32 dof. Fitting this spectrum by a Band GRB function yields the same values of alpha and Ep, and only an upper limit on the high energy photon index beta of -2.1 All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary. View this GCN Circular online at https://gcn.nasa.gov/circulars/44474. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42599] GRB 260504B: GECAM-B detection
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44473 SUBJECT: GRB 260504B: GECAM-B detection DATE: 26/05/05 13:41:13 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> Chen-Wei Wang, Shao-Lin Xiong, Chao Zheng (IHEP) report on behalf of GECAM team: GECAM-B was triggered in-flight by a hard burst GRB 260504B at 2026-05-04T09:31:19.450 UTC (denoted as T0). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of a single pulse with a duration (T90) of 0.20 +0.02/-0.06 s, which is also detected by SVOM/ECLAIRs and SVOM/GRM (A. Saccardi et al., GCN # 44454). The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260504B.png The time-averaged spectrum from T0-0.07 s to T0+0.1 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.07 +0.29/-0.27 and the cutoff energy, parameterized as Epeak, is 1240 +730/-400 keV. The event fluence (10-1000 keV) in this time interval is (1.06 +0.13/-0.10)E-06 erg/cm^2. Thus GRB 260504B is consistent with Type I GRBs in the 'Amati' relation diagram, as shown at: https://www.bursthub.cn//admin/static/gecambgrb260504B_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/44473. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42598] Fermi-LAT Gamma-ray Observations of IceCube-260504A
by GCN Circulars 05 May '26

05 May '26

TITLE: GCN CIRCULAR NUMBER: 44472 SUBJECT: Fermi-LAT Gamma-ray Observations of IceCube-260504A DATE: 26/05/05 12:53:40 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 IC260504A neutrino event (GCN 44464) 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 2026-05-04 21:11:20.90 UTC (T0) with J2000 position RA = 246.99 (+0.86, -0.80) deg, Decl. = 54.87 (+0.46, -0.47) deg 90% PSF containment. One cataloged >100 MeV gamma-ray source is located within the 90% IC260504A localization error, at a distance of roughly 0.38 deg (4FGL-DR4; The Fourth Fermi-LAT catalog Data Release 4, The Fermi-LAT collaboration 2023, arXiv:2307.12546). This is the object 4FGL J1626.0+5436 associated with 87GB 162528.4+544848. Based on a preliminary analysis of the LAT data over the timescale of 1-day and 1-month prior to 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 IC260504A 90% confidence localization. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC260504A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 1.3e-10 ph cm^-2 s^-1 for ~17-years (2008-08-04 / T0), <4.6e-09 (<4.7e-08) 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 source the Fermi-LAT contact person is Leonard 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/44472. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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