December 2024 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 36518] GRB 241128A: CrAO ZTSh and Mondy AZT-33IK optical observations
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38519 SUBJECT: GRB 241128A: CrAO ZTSh and Mondy AZT-33IK optical observations DATE: 24/12/10 09:57:54 GMT FROM: Nicolai Pankov at HSE, IKI RAS <colinsergesen(a)gmail.com> A. Volnova (IKI), N. Pankov (HSE, IKI), A. Pozanenko (IKI), V. Rumyantsev (CrAO), E. Klunko (ISTP) report on behalf of IKI-GRB-FuN: We continued observations of the GRB 241128A (Brivio et al., GCN 38367; Page, GCN 38368) with 2.6-meter ZTSh telescope of CrAO observatory and 1.5-… [View More]

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[vsnet-grb-info 36517] GRB 241209D: AstroSat CZTI detection
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38518 SUBJECT: GRB 241209D: AstroSat CZTI detection DATE: 24/12/10 09:10:32 GMT FROM: Gaurav Waratkar at IIT Bombay <gauravwaratkar(a)iitb.ac.in> M. Tembhurnikar (IUCAA), G. Waratkar (IITB), A. Dasgupta (BITS Pilani, Hyderabad), J. Joshi (IUCAA), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI … [View More]

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[vsnet-grb-info 36516] GRB 241209A: EP-FXT follow-up observations
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38517 SUBJECT: GRB 241209A: EP-FXT follow-up observations DATE: 24/12/10 08:36:26 GMT FROM: Yu-Han Yang at University of Rome Tor Vergata <yyang(a)roma2.infn.it> E. Troja (U Rome), Y. L. Wang (NAO, CAS), Y. Wang (PMO, CAS), H. L. Peng (NNU), W. D. Zhang (NAO,CAS), Y. -H. Yang (U Rome), R. L. Becerra (U Rome) report on behalf of the Einstein Probe team: We performed a follow-up observation of the short GRB 241209A detected by Fermi/GBM (GCN 38474) and … [View More]

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[vsnet-grb-info 36515] GRB 241209B: SVOM/VT afterglow detection
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38516 SUBJECT: GRB 241209B: SVOM/VT afterglow detection DATE: 24/12/10 07:47:55 GMT FROM: Chao Wu at NAOC <cwu(a)nao.cas.cn> SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, L. P. Xin, C. Wu, X. H. Han, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. Deng, L. Lan, X. M. Lu, R. S. Zhang, D. H. Zhao (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO), C. Plasse (CEA) SVOM JSWG: Jian-Yan … [View More]Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (IHEP), Bing Zhang (UNLV) report on behalf of the SVOM team: The GRB 241209B (Xie et al., GCN 38478) was observed by on-board VT after the automatic slew of the platform. The VT conducted observations in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously. Revisit observation (TOO-EX mode) was also operated ~ 10 hr after the trigger. An uncatalogued optical source was detected in VT_B and VT_R band images within the errorbox of source #1 reported by Swift team (GCN 38494), which is 5.7 arcmin to the center of ECLAIRs localization, and further confirmed with the data from revisit observation. The source is located at RA, Dec = 194.63406, +76.17617 which is equivalent to: RA (J2000) : 12h 58m 32.17s Dec (J2000): +76d 10' 34.2" with an uncertainty of 0.5 arcsec. Its brightness was fading for ~1 magnitude in both of VT_B and VT_R images in the initial 10 hours. The magnitude was VT_B= 23.20 +/-0.20 mag and VT_R= 21.75 +/-0.05 mag in AB magnitude at 2024-12-09T05:04:49 UT, about 1.14 hr post the trigger. We proposed that this source is the optical counterpart of the burst. 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/38516. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L… [View Less]

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[vsnet-grb-info 36514] LIGO/Virgo/KAGRA S241210cw: Identification of a GW compact binary merger candidate
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38515 SUBJECT: LIGO/Virgo/KAGRA S241210cw: Identification of a GW compact binary merger candidate DATE: 24/12/10 06:44:31 GMT FROM: Pan Guo at KAGRA <panguocas(a)gmail.com> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241210cw during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo … [View More]Observatory (V1) at 2024-12-10 06:06:06.873 UTC (GPS time: 1417845984.873). The candidate was found by the cWB [1], cWB BBH [2], GstLAL [3], MBTA [4], and PyCBC Live [5] analysis pipelines. S241210cw is an event of interest because its false alarm rate, as estimated by the online analysis, is 6.3e-10 Hz, or about one in 50 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241210cw After parameter estimation by RapidPE-RIFT [6], the classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), NSBH (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [7] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [7] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [8], distributed via GCN notice about 29 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [8], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 1002 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1910 +/- 521 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004 [2] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018 [3] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [4] Aubin et al. CQG 38, 095004 (2021) doi:10.1088/1361-6382/abe913 [5] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a [6] Rose et al. (2022) arXiv:2201.05263 and Pankow et al. PRD 92, 023002 (2015) doi:10.1103/PhysRevD.92.023002 [7] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [8] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38515. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L… [View Less]

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[vsnet-grb-info 36513] EP241208a: Global MASTER-Net observations report
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38514 SUBJECT: EP241208a: Global MASTER-Net observations report DATE: 24/12/10 06:27:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.… [View More]Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), 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 (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP241208a ( EP Team et al., GCN 38513) errorbox 466 sec after trigger time at 2024-12-09 14:53:48 UT, with upper limit up to 20.0 mag. The observations began at zenith distance = 50 deg. The sun altitude is -52.9 deg. The galactic latitude b = 37 deg., longitude l = 171 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2702991 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 496 | 2024-12-09 14:53:48 | MASTER-Tunka | (08h 31m 35.90s , +49d 01m 28.2s) | C | 60 | 15.8 | Coadd 4633 | 2024-12-09 16:02:44 | MASTER-Tunka | (08h 31m 52.94s , +49d 02m 06.3s) | C | 60 | 17.3 | 4686 | 2024-12-09 16:02:44 | MASTER-Tunka | (08h 31m 52.95s , +49d 02m 06.3s) | C | 165 | 17.7 | Coadd 4696 | 2024-12-09 16:03:55 | MASTER-Tunka | (08h 31m 53.09s , +49d 02m 08.0s) | C | 45 | 16.7 | 4761 | 2024-12-09 16:04:53 | MASTER-Tunka | (08h 31m 51.16s , +49d 01m 47.8s) | C | 60 | 16.7 | 4833 | 2024-12-09 16:06:05 | MASTER-Tunka | (08h 31m 54.45s , +49d 03m 30.3s) | C | 60 | 16.6 | 4893 | 2024-12-09 16:06:05 | MASTER-Tunka | (08h 31m 54.45s , +49d 03m 30.3s) | C | 180 | 17.3 | Coadd 4908 | 2024-12-09 16:07:20 | MASTER-Tunka | (08h 31m 48.74s , +49d 02m 47.3s) | C | 60 | 16.4 | 4980 | 2024-12-09 16:08:32 | MASTER-Tunka | (08h 31m 48.76s , +49d 03m 49.2s) | C | 60 | 16.9 | 5120 | 2024-12-09 16:10:52 | MASTER-Tunka | (08h 31m 53.59s , +49d 02m 50.0s) | C | 60 | 16.9 | 5180 | 2024-12-09 16:10:52 | MASTER-Tunka | (08h 31m 53.59s , +49d 02m 50.0s) | C | 180 | 17.7 | Coadd 5193 | 2024-12-09 16:12:05 | MASTER-Tunka | (08h 31m 48.05s , +49d 01m 52.6s) | C | 60 | 17.0 | 5352 | 2024-12-09 16:14:44 | MASTER-Tunka | (08h 31m 52.44s , +49d 03m 55.3s) | C | 60 | 17.1 | 5410 | 2024-12-09 16:15:57 | MASTER-Tunka | (08h 31m 52.49s , +49d 02m 11.4s) | C | 30 | 16.9 | 5455 | 2024-12-09 16:15:57 | MASTER-Tunka | (08h 31m 52.51s , +49d 02m 11.0s) | C | 120 | 17.9 | Coadd 5453 | 2024-12-09 16:16:39 | MASTER-Tunka | (08h 31m 56.58s , +49d 04m 02.0s) | C | 30 | 16.7 | 5511 | 2024-12-09 16:17:22 | MASTER-Tunka | (08h 31m 48.88s , +49d 03m 08.3s) | C | 60 | 17.3 | 5585 | 2024-12-09 16:18:37 | MASTER-Tunka | (08h 31m 49.32s , +49d 04m 11.3s) | C | 60 | 17.5 | 5645 | 2024-12-09 16:18:37 | MASTER-Tunka | (08h 31m 49.31s , +49d 04m 11.3s) | C | 180 | 19.6 | Coadd 7406 | 2024-12-09 16:48:57 | MASTER-Tunka | (08h 31m 51.91s , +49d 04m 15.3s) | C | 60 | 19.3 | 7635 | 2024-12-09 16:52:46 | MASTER-Tunka | (08h 31m 52.57s , +49d 03m 30.6s) | C | 60 | 19.3 | 7905 | 2024-12-09 16:57:17 | MASTER-Tunka | (08h 31m 56.64s , +49d 03m 57.5s) | C | 60 | 19.1 | 7965 | 2024-12-09 16:57:17 | MASTER-Tunka | (08h 31m 56.64s , +49d 03m 57.5s) | C | 180 | 19.9 | Coadd 8062 | 2024-12-09 16:59:54 | MASTER-Tunka | (08h 31m 53.95s , +49d 05m 50.7s) | C | 60 | 19.1 | 8298 | 2024-12-09 17:03:50 | MASTER-Tunka | (08h 31m 59.92s , +49d 04m 19.1s) | C | 60 | 19.4 | 8457 | 2024-12-09 17:06:29 | MASTER-Tunka | (08h 31m 56.97s , +49d 04m 26.4s) | C | 60 | 19.3 | 8517 | 2024-12-09 17:06:29 | MASTER-Tunka | (08h 31m 56.98s , +49d 04m 26.4s) | C | 180 | 20.0 | Coadd 8615 | 2024-12-09 17:09:06 | MASTER-Tunka | (08h 31m 53.41s , +49d 06m 13.9s) | C | 60 | 19.6 | 8843 | 2024-12-09 17:12:55 | MASTER-Tunka | (08h 32m 00.08s , +49d 04m 47.0s) | C | 60 | 19.8 | 9113 | 2024-12-09 17:17:25 | MASTER-Tunka | (08h 32m 01.68s , +49d 06m 21.5s) | C | 60 | 19.5 | 9173 | 2024-12-09 17:17:25 | MASTER-Tunka | (08h 32m 01.68s , +49d 06m 21.5s) | C | 180 | 19.9 | Coadd 9269 | 2024-12-09 17:20:00 | MASTER-Tunka | (08h 32m 00.12s , +49d 05m 43.8s) | C | 60 | 19.1 | 9501 | 2024-12-09 17:23:52 | MASTER-Tunka | (08h 31m 57.98s , +49d 06m 53.6s) | C | 60 | 18.9 | 11246 | 2024-12-09 17:52:57 | MASTER-Tunka | (08h 31m 55.43s , +49d 06m 03.0s) | C | 60 | 19.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/38514. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L… [View Less]

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[vsnet-grb-info 36512] EP241208a: EP-FXT follow-up observations
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38513 SUBJECT: EP241208a: EP-FXT follow-up observations DATE: 24/12/10 06:17:47 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y. Wang (PMO, CAS), Y. L. Wang (NAO, CAS), H. L. Peng (NNU), W. D. Zhang (NAO,CAS) report on behalf of the Einstein Probe team: Following the detection of the fast X-ray transient EP241208a (Wang et al., GCN 38477), we performed an observation with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe mission. … [View More]

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[vsnet-grb-info 36511] LIGO/Virgo/KAGRA S241210d: Identification of a GW compact binary merger candidate
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38512 SUBJECT: LIGO/Virgo/KAGRA S241210d: Identification of a GW compact binary merger candidate DATE: 24/12/10 03:15:41 GMT FROM: ryoya(a)phys.aoyama.ac.jp The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241210d during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2024-12-10 02:33:35.191 UTC (GPS time:… [View More] 1417833233.191). The candidate was found by the GstLAL [1] and MBTA [2] analysis pipelines. S241210d is an event of interest because its false alarm rate, as estimated by the online analysis, is 4.4e-08 Hz, or about one in 8 months. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241210d After parameter estimation by RapidPE-RIFT [3], the classification of the GW signal, in order of descending probability, is BBH (97%), Terrestrial (3%), NSBH (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [4] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [4] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 4%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 29 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 4583 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 7530 +/- 2565 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [2] Aubin et al. CQG 38, 095004 (2021) doi:10.1088/1361-6382/abe913 [3] Rose et al. (2022) arXiv:2201.05263 and Pankow et al. PRD 92, 023002 (2015) doi:10.1103/PhysRevD.92.023002 [4] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [5] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38512. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L… [View Less]

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[vsnet-grb-info 36510] Fermi trigger No 755485387: Global MASTER-Net observations report
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38511 SUBJECT: Fermi trigger No 755485387: Global MASTER-Net observations report DATE: 24/12/10 03:15:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, … [View More]F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), 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 (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB241210.04 (trigger No 755485387,01h 20m 36.00s , +70d 57m 36.0s, R=12.56) errorbox 671 sec after notice time and 696 sec after trigger time at 2024-12-10 01:14:39 UT, with upper limit up to 18.3 mag. The observations began at zenith distance = 53 deg. The sun altitude is -35.0 deg. The galactic latitude b = 9 deg., longitude l = 126 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2701815 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 787 | 2024-12-10 01:14:39 | MASTER-Kislovodsk | (02h 23m 37.27s , +73d 17m 39.2s) | C | 180 | 17.9 | 1186 | 2024-12-10 01:21:18 | MASTER-Kislovodsk | (02h 51m 33.92s , +73d 19m 08.5s) | C | 180 | 18.0 | 1386 | 2024-12-10 01:24:38 | MASTER-Kislovodsk | (02h 23m 37.58s , +73d 19m 27.5s) | C | 180 | 18.1 | 1786 | 2024-12-10 01:31:18 | MASTER-Kislovodsk | (02h 51m 31.76s , +73d 20m 23.6s) | C | 180 | 17.9 | 1985 | 2024-12-10 01:34:37 | MASTER-Kislovodsk | (02h 23m 36.36s , +73d 18m 13.0s) | C | 180 | 18.1 | 3649 | 2024-12-10 02:02:21 | MASTER-Kislovodsk | (02h 51m 39.75s , +73d 18m 26.3s) | C | 180 | 17.6 | 3849 | 2024-12-10 02:05:41 | MASTER-Kislovodsk | (02h 51m 34.19s , +73d 17m 08.8s) | C | 180 | 18.1 | 4049 | 2024-12-10 02:09:00 | MASTER-Kislovodsk | (02h 53m 59.19s , +73d 17m 31.6s) | C | 180 | 13.3 | 4248 | 2024-12-10 02:12:20 | MASTER-Kislovodsk | (02h 23m 37.99s , +73d 17m 44.8s) | C | 180 | 18.1 | 4448 | 2024-12-10 02:15:40 | MASTER-Kislovodsk | (02h 23m 37.59s , +73d 15m 53.3s) | C | 180 | 18.1 | 4648 | 2024-12-10 02:19:00 | MASTER-Kislovodsk | (02h 23m 41.81s , +73d 17m 22.5s) | C | 180 | 18.2 | 6303 | 2024-12-10 02:46:35 | MASTER-Kislovodsk | (02h 51m 44.54s , +73d 17m 28.6s) | C | 180 | 17.3 | 6503 | 2024-12-10 02:49:55 | MASTER-Kislovodsk | (02h 51m 37.36s , +73d 16m 35.6s) | C | 180 | 17.7 | 6703 | 2024-12-10 02:53:15 | MASTER-Kislovodsk | (02h 51m 39.50s , +73d 17m 24.6s) | C | 180 | 15.9 | 6902 | 2024-12-10 02:56:34 | MASTER-Kislovodsk | (02h 23m 48.99s , +73d 15m 15.6s) | C | 180 | 18.0 | 7103 | 2024-12-10 02:59:55 | MASTER-Kislovodsk | (02h 26m 40.49s , +73d 14m 14.8s) | C | 180 | 13.4 | 7303 | 2024-12-10 03:03:15 | MASTER-Kislovodsk | (02h 23m 51.46s , +73d 14m 17.8s) | C | 180 | 18.3 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/38511. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L… [View Less]

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[vsnet-grb-info 36509] GRB 241207B: Fermi GBM Observation
by GCN Circulars 10 Dec '24

10 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38510 SUBJECT: GRB 241207B: Fermi GBM Observation DATE: 24/12/10 01:28:08 GMT FROM: Lorenzo Scotton at UAH <lscottongcn(a)outlook.com> L. Scotton (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 20:51:01.75 UT on 07 December 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241207B (trigger 755297466/241207869) which was also detected by Swift/BAT-NITRATES (DeLaunay et al. 2024, GCN 38472)… [View More]

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