January 2026 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 41439] The EP-WXT trigger 01709251112 is likely a flaring star
by GCN Circulars 07 Jan '26

07 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43348 SUBJECT: The EP-WXT trigger 01709251112 is likely a flaring star DATE: 26/01/07 10:53:44 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> H. Y. Ren (NAOC), Q.-C. Liu (THU), R.-Z. Li (YNAO, CAS) and H. Sun (NAOC) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709251112 at the time of 2026-01-07T10:12:47, is likely a stellar flare associated with PM J08310+4012. The estimated flux of the flare is around 8e-11 erg/s/cm^2 in 0.5-4.0 keV. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). View this GCN Circular online at https://gcn.nasa.gov/circulars/43348. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41438] Fermi GRB 260105A: Global MASTER-Net observations report
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43347 SUBJECT: Fermi GRB 260105A: Global MASTER-Net observations report DATE: 26/01/07 03:45:50 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) started inspect of the Fermi GRB 260105A ( Fermi GBM team, GCN 43335) errorbox 42914 sec after notice time and 42952 sec after trigger time at 2026-01-06 10:43:04 UT, with upper limit up to 19.2 mag. Observations started at twilight. The observations began at zenith distance = 35 deg. The sun altitude is -12.9 deg. MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 260105A errorbox 1 days 4422 sec after notice time and 1 days 4460 sec after trigger time at 2026-01-07 00:01:32 UT, with upper limit up to 17.2 mag. The observations began at zenith distance = 48 deg. The sun altitude is -50.2 deg. The galactic latitude b = 4 deg., longitude l = 150 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3096780 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 42983 | 2026-01-06 10:43:04 | MASTER-Tunka | (04h 46m 35.26s , +57d 50m 19.5s) | C | 60 | 19.2 | 42983 | 2026-01-06 10:43:04 | MASTER-Tunka | (04h 47m 41.61s , +57d 41m 18.4s) | C | 60 | 18.7 | 49648 | 2026-01-06 12:34:09 | MASTER- | (04h 54m 01.68s , +56d 22m 44.2s) | C | 60 | 17.3 | 49648 | 2026-01-06 12:34:09 | MASTER- | (04h 52m 23.46s , +56d 56m 52.2s) | C | 60 | 17.2 | 50074 | 2026-01-06 12:41:15 | MASTER- | (04h 24m 20.56s , +60d 44m 34.6s) | C | 60 | 17.0 | 50074 | 2026-01-06 12:41:15 | MASTER- | (04h 26m 06.14s , +60d 10m 24.1s) | C | 60 | 17.5 | 50393 | 2026-01-06 12:46:34 | MASTER- | (04h 53m 57.37s , +56d 22m 05.4s) | C | 60 | 17.6 | 50393 | 2026-01-06 12:46:34 | MASTER- | (04h 52m 21.16s , +56d 56m 07.4s) | C | 60 | 17.2 | 50819 | 2026-01-06 12:53:40 | MASTER- | (04h 26m 00.27s , +60d 10m 01.0s) | C | 60 | 17.5 | 50819 | 2026-01-06 12:53:40 | MASTER- | (04h 24m 16.25s , +60d 44m 10.6s) | C | 60 | 17.0 | 51136 | 2026-01-06 12:58:57 | MASTER- | (04h 53m 56.14s , +56d 21m 50.3s) | C | 60 | 17.3 | 51136 | 2026-01-06 12:58:58 | MASTER- | (04h 52m 21.74s , +56d 55m 48.1s) | C | 60 | 16.9 | 51568 | 2026-01-06 13:06:09 | MASTER- | (04h 26m 02.40s , +60d 10m 25.4s) | C | 60 | 16.5 | 51568 | 2026-01-06 13:06:09 | MASTER- | (04h 24m 20.55s , +60d 44m 28.7s) | C | 60 | 15.9 | 51886 | 2026-01-06 13:11:28 | MASTER- | (04h 53m 50.30s , +56d 22m 14.7s) | C | 60 | 15.8 | 51886 | 2026-01-06 13:11:28 | MASTER- | (04h 52m 17.69s , +56d 56m 07.6s) | C | 60 | 15.6 | 52310 | 2026-01-06 13:18:31 | MASTER- | (04h 25m 59.19s , +60d 10m 12.1s) | C | 60 | 15.8 | 52310 | 2026-01-06 13:18:31 | MASTER- | (04h 24m 19.17s , +60d 44m 11.3s) | C | 60 | 15.4 | 61752 | 2026-01-06 15:55:53 | MASTER-Tunka | (04h 32m 04.80s , +60d 25m 18.6s) | C | 60 | 17.8 | 61752 | 2026-01-06 15:55:53 | MASTER-Tunka | (04h 30m 52.16s , +60d 33m 07.6s) | C | 60 | 17.1 | Coadd 90891 | 2026-01-07 00:01:32 | MASTER-Kislovodsk | (04h 53m 24.59s , +56d 38m 40.5s) | C | 60 | 17.3 | 102412 | 2026-01-07 03:13:34 | MASTER-Kislovodsk | (04h 39m 35.25s , +56d 05m 19.5s) | C | 60 | 16.3 | 102412 | 2026-01-07 03:13:34 | MASTER-Kislovodsk | (04h 32m 17.01s , +56d 24m 49.6s) | C | 60 | 16.8 | 102515 | 2026-01-07 03:15:16 | MASTER-Kislovodsk | (04h 31m 43.02s , +57d 59m 37.8s) | C | 60 | 16.5 | 102515 | 2026-01-07 03:15:16 | MASTER-Kislovodsk | (04h 24m 00.92s , +58d 19m 01.2s) | C | 60 | 16.9 | 102662 | 2026-01-07 03:17:43 | MASTER-Kislovodsk | (04h 23m 11.61s , +59d 52m 00.8s) | C | 60 | 16.7 | 102662 | 2026-01-07 03:17:44 | MASTER-Kislovodsk | (04h 15m 06.89s , +60d 11m 20.5s) | C | 60 | 17.0 | 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/43347. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41437] GRB 260105B: Fermi GBM Detection
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43346 SUBJECT: GRB 260105B: Fermi GBM Detection DATE: 26/01/07 00:08:46 GMT FROM: Matt Godwin <msg0028(a)uah.edu> Matt Godwin (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 23:21:36.55 UT on 05 January 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260105B (trigger 789348101/260105973). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 259.71, Dec = 1.74 (J2000 degrees, equivalent to J2000 17h 18m, +1d 44'), with a statistical uncertainty of 2.03 degrees. (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a mixture of two Gaussians, one with a radius of 1.8 degrees (52% contribution) and one with a radius of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1]). The angle from the Fermi LAT boresight is 68 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 11 s (50-300 keV). The time-averaged spectrum from T0-1.9 to T0+12.5 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.96 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 232 +/- 2 keV. The event fluence (10-1000 keV) in this time interval is (8 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+2.4 s in the 10-1000 keV band is 156 +/- 2 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 178 +/- 2 keV, alpha = -0.83 +/- 0.01 and beta = -2.19 +/- 0.03. 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/43346. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41436] EP260105a: FTW optical observations
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43345 SUBJECT: EP260105a: FTW optical observations DATE: 26/01/06 15:03:15 GMT FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de> Malte Busmann, Jule Augustin, Mitra Maleki (LMU), Xander J. Hall, Brendan O'Connor (CMU), Daniel Gruen (LMU), and Antonella Palmese (CMU) report: We observed the 90% FXT localization of EP260105a (Zhou et al., GCNs 43327 and 43333) with the Three Channel Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the r and i-band simultaneously for 10 x 180 s starting at 2026-01-06T02:04:38 UT (0.84 days after the trigger). We performed difference imaging with templates from the DESI Legacy Surveys and did not detect any uncatalogued sources to a 3-sigma upper limit of r > 22.7 AB mag. The non-detection is consistent with the reports by Lipunov et al. (GCN 43328), Corcoran et al. (GCN 43332), and Li et al (GCN 43337). The magnitude is calibrated against the PS1 catalog and not corrected for Galactic extinction. We thank Christoph Ries from the Wendelstein Observatory for obtaining these observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/43345. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41435] EP260104: FTW optical observations
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43344 SUBJECT: EP260104: FTW optical observations DATE: 26/01/06 15:02:43 GMT FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de> Malte Busmann, Jule Augustin, Mitra Maleki (LMU), Xander J. Hall, Brendan O'Connor (CMU), Daniel Gruen (LMU), and Antonella Palmese (CMU) report: We observed the 90% WXT localization of EP260104a (Zhou et al., GCN 43330) with the Three Channel Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the r and i-band simultaneously for 10 x 180 s starting at 2026-01-06T01:09:48 UT (1.6 days after the trigger). We performed difference imaging with templates from the DESI Legacy Surveys and did not detect any uncatalogued sources to a 3-sigma upper limit of r > 21.5 AB mag. The non-detection is consistent with the report by Lipunov et al. (GCN 43331). The magnitude is calibrated against the PS1 catalog and not corrected for Galactic extinction. We thank Christoph Ries from the Wendelstein Observatory for obtaining these observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/43344. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41434] GRB 260105B: BALROG localization (Fermi Trigger 789348101 / GRB 260105973)
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43343 SUBJECT: GRB 260105B: BALROG localization (Fermi Trigger 789348101 / GRB 260105973) DATE: 26/01/06 08:43:43 GMT FROM: Jochen Greiner at MPE <jcgrog(a)mpe.mpg.de> T. Preis (University of Innsbruck) & J. Greiner (MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 789348101 at 23:21:36 on 05 Jan. 2026 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position is: RA(2000.0) = 258.7 deg Decl.(2000.0) = 7.9 deg The 1 sigma statistical error radius is 2.1 deg. We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB260105973/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB260105973/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB260105973/json View this GCN Circular online at https://gcn.nasa.gov/circulars/43343. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41433] GRB 260105A: SVOM/GRM observation
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43342 SUBJECT: GRB 260105A: SVOM/GRM observation DATE: 26/01/06 08:30:22 GMT FROM: Yue Wang <m18509381757(a)163.com> SVOM/GRM team: Yue Wang, Chen-Wei Wang, Hao-Xuan Guo, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Sebastien Guillot (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered on-ground by GRB 260105A at 2026-01-05T22:47:16.000 (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43335). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a T90 of 69 +16/-12 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260105A.png In addition, the position of this burst, as determined by Fermi/GBM (RA = 64.5, Dec = 55.5, Error = 3.3, GCN #43335), is located at about 85 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. With this localization, the time-averaged spectrum from T0-7 to T0+83 s is best fitted by a power law function. The power law index is -1.64 +0.08/-0.07. The event fluence (10-1000 keV) in this time interval is (1.85 +0.20/-0.20)E-05 erg/cm^2. 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: Yue Wang (IHEP) (yuewang(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43342. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41432] GRB 260105B: SVOM/GRM observation
by GCN Circulars 06 Jan '26

06 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43341 SUBJECT: GRB 260105B: SVOM/GRM observation DATE: 26/01/06 07:25:39 GMT FROM: Yue Wang <m18509381757(a)163.com> SVOM/GRM team: Yue Wang, Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Sebastien Guillot (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260105B (SVOM trigger reference: sb26010502) at 2026-01-05T23:21:37.000 (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43336). 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 6.8 +1.8/-1.4 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260105B.png In addition, the position of this burst, as determined by Fermi/GBM (RA = 259.7, Dec = 1.7, Error = 2.0, GCN #43336), is located at about 91 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. With this localization, the time-averaged spectrum from T0-1 to T0+7 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.61 +0.12/-0.13 and the cutoff energy, parameterized as Epeak, is 177 +15/-13 keV. The event fluence (10-1000 keV) in this time interval is (9.34+0.47/-0.44)E-06 erg/cm^2. The 1s peak spectrum, measured from T0-1.5 to T0+2.5 s, if fitted by a power law function with an exponential high-energy cutoff, the power law index is -0.81 +0.15/-0.17 and the cutoff energy, parameterized as Epeak, is 242 +45/-33 keV. The flux (10-1000 keV) in this time interval is (2.53 +0.22/-0.20)E-06 erg/cm^2/s. The localization of GRB 260105B in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260105B_amati.png The localization of GRB 260105B in the 'Yonetoku' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260105B_yonetoku.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: Yue Wang (IHEP) (yuewang(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43341. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41431] The EP-WXT trigger 01709251028 is likely a flaring star
by GCN Circulars 05 Jan '26

05 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43340 SUBJECT: The EP-WXT trigger 01709251028 is likely a flaring star DATE: 26/01/06 04:02:15 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> G. J. Yang, M. J. Liu, X. X. Sun, C. C. Jin (NAO, CAS) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709251028 at the time of 2026-01-05T18:47:36, is likely a stellar flare associated with ET Leo. The estimated flux of the flare is around 1.8e-10 erg/s/cm^2 in 0.5-4.0 keV, corresponding to an X-ray luminosity of around 2.4e+32 erg/s. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). View this GCN Circular online at https://gcn.nasa.gov/circulars/43340. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41430] FRB 20251229A: COLIBRÍ optical upper limits
by GCN Circulars 05 Jan '26

05 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43339 SUBJECT: FRB 20251229A: COLIBRÍ optical upper limits DATE: 26/01/06 04:00:53 GMT FROM: globus(a)astro.unam.mx Noémie Globus (UNAM), Jean-Luc Atteia (IRAP), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Dalya Akl (NYUAD), Camila Angulo (UNAM), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Nikos Mandarakas (LAM), Kin Ocelotl López (UNAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), Benjamin Schneider (LAM) and Antonio de Ugarte Postigo (LAM), report: We imaged the field of FRB 20251229A (Mulyk et al., GCN Circ. 43334), using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-01-06 02:08 to 02:42 UTC and obtained 29 minutes of simultaneous exposure in the r and z filters. The data were reduced and coadded with the COLIBRÍ ASU pipeline. The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and was not corrected for Galactic extinction. In the stacked image, we do not detect any new source at the uncertainty region (Mulyk et al., GCN Circ. 43334) down to the following preliminary 5-sigma limits: r > 22.99, z > 21.88. We thank the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams. COLIBRÍ is an astronomical observatory developed and operated jointly by France (AMU, CNES and CNRS) and Mexico (UNAM and SECIHTI). It is located at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, Baja California, Mexico. View this GCN Circular online at https://gcn.nasa.gov/circulars/43339. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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