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

[vsnet-grb-info 36468] Fermi Gamma-ray Burst Monitor trigger 755277791/241207641 is not a GRB
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38471 SUBJECT: Fermi Gamma-ray Burst Monitor trigger 755277791/241207641 is not a GRB DATE: 24/12/08 20:43:36 GMT FROM: Lorenzo Scotton at UAH <lscottongcn(a)outlook.com> L. Scotton (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "The Fermi Gamma-ray Burst Monitor (GBM) trigger 755277791/241207641 at 15:23:06.19 UT on 07 December 2024, tentatively classified as a GRB, is in fact not due to a GRB. This trigger is likely due to SGR 1E 1841-045 / Kes 73." View this GCN Circular online at https://gcn.nasa.gov/circulars/38471. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36467] GRB 241201A: AstroSat CZTI detection
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38470 SUBJECT: GRB 241201A: AstroSat CZTI detection DATE: 24/12/08 16:18:02 GMT FROM: Varun Bhalerao at IIT Bombay <varunb(a)iitb.ac.in> J. Joshi (IUCAA), G. Waratkar (IITB), 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 data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of GRB 241201A which was also detected by Fermi/GBM (Fermi-GBM Team, GCN Circ. 38403), and GRBAlpha (Dafcikova et al., GCN Circ. 38437). The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed two peaks of emission with the strongest peak at 2024-12-01 14:55:59.35 UTC. The measured peak count rate associated with the burst is 599 (+82, -62) counts/s above the background in the combined data of all quadrants, with a total of 1960 (+359, -389) counts. The local mean background count rate was 1849 (+16, -8) counts/s. We measure a T90 of 7.6 (+0.8, -0.6) s from the cumulative Veto light curve. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project. CZTI GRB detections are reported regularly on the payload site at: http://astrosat.iucaa.in/czti/?q=grb View this GCN Circular online at https://gcn.nasa.gov/circulars/38470. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36466] GRB 241206A: DDOTI Upper Limit on the Afterglow
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38469 SUBJECT: GRB 241206A: DDOTI Upper Limit on the Afterglow DATE: 24/12/08 16:02:20 GMT FROM: Rosa L. Becerra at Tor Vergata, Roma <rosa.becerra(a)roma2.infn.it> Rosa L. Becerra (Tor Vergata, Roma), Alan M. Watson (UNAM), Eleonora Troja (Tor Vergata, Roma), Camila Angulo Valdez (UNAM), Nat Butler (ASU), Simone Dichiara (Penn State University), Tsvetelina Dimitrova (ASU), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), Océlotl López (UNAM), and Margarita Pereyra (UNAM) report: We observed the field of the GRB 241206A detected by Fermi/GBM (Fermi GBM Team, GCN 38447) and Swift/BAT-GUANO (DeLaunay et al., GCN 38453) with the DDOTI/OAN wide-field imager at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir (http://ddoti.astroscu.unam.mx) on 2024-12-08 from 09:51 to 13:14 UTC (45.7 to 49.2 hrs after the event), obtaining a total of 1.7 hours of exposure in the w filter down to a 10-sigma limiting magnitude of w = 20.5. Comparing our observations to the USNO-B1 and PanSTARRS PS1 DR2 catalogues, we detect no uncatalogued sources within the observed field to our 10-sigma limit within the error radius reported by Fermi/GBM (Fermi GBM Team, GCN 38447). We thank the DDOTI technical team and the staff of the Observatorio Astronómico Nacional. View this GCN Circular online at https://gcn.nasa.gov/circulars/38469. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36465] AT2024adec: X-ray Upper Limits from EP-FXT Observation
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38468 SUBJECT: AT2024adec: X-ray Upper Limits from EP-FXT Observation DATE: 24/12/08 11:37:27 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> C. Y. Wang (THU), Y.-H. I. Yin (NJU), D. H. Zhao, H. W. Pan, D. Xu (NAO,CAS) report on behalf of the Einstein Probe team: Following the detection of the optical transient AT2024adec (ZTF24abvevzs, TNS AstroNote 2024-357, M. Fulton et. al), we performed an X-ray ToO observation with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. No X-ray emission from this source has been found in the observation. The observation started at 2024-12-07T01:59:31 (UTC), with an exposure time of 16.8 ks. By analysing the FXT data, we found no significant X-ray emisssion associated with AT2024adec. The upper limits of the count rate are calculated using the method provided by Ruiz et al. 2022 [1]. Assuming an absorbed power-law model with a column density of the Galactic value 2.53 x 10^20 cm^-2 and a photon index of 2, the flux upper limits in the 0.5-10 keV and 0.5-2 keV bands are obtained as ~ 9.7 x 10^-15 erg/s/cm^2 and ~ 6.5 x 10^-15 erg/s/cm^2, respectively, at the 90% confidence level, largely consistent with the sensitivity estimation given by Zhang et al. (2022 [2]). 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). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES. References: [1] Ruiz, A., et al. "The RapidXMM upper limit server: X-ray aperture photometry of the XMM-Newton archival observations." Monthly Notices of the Royal Astronomical Society 511.3 (2022): 4265-4284. [2] Zhang, Juan, et al. "Estimate of the background and sensitivity of the follow-up X-ray telescope onboard Einstein Probe." Astroparticle Physics 137 (2022): 102668. View this GCN Circular online at https://gcn.nasa.gov/circulars/38468. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36464] AT2024adec: X-ray Upper Limits from EP-FXT Observation
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38467 SUBJECT: AT2024adec: X-ray Upper Limits from EP-FXT Observation DATE: 24/12/08 11:36:29 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> C. Y. Wang (THU), Y.-H. I. Yin (NJU), D. H. Zhao, H. W. Pan, D. Xu (NAO,CAS) report on behalf of the Einstein Probe team: Following the detection of the optical transient AT2024adec (ZTF24abvevzs, TNS AstroNote 2024-357, M. Fulton et. al), we performed an X-ray ToO observation with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. No X-ray emission from this source has been found in the observation. The observation started at 2024-12-07T01:59:31 (UTC), with an exposure time of 16.8 ks. By analysing the FXT data, we found no significant X-ray emisssion associated with AT2024adec. The upper limits of the count rate are calculated using the method provided by Ruiz et al. 2022 [1]. Assuming an absorbed power-law model with a column density of the Galactic value 2.53 x 10^20 cm^-2 and a photon index of 2, the flux upper limits in the 0.5-10 keV and 0.5-2 keV bands are obtained as ~ 9.7 x 10^-15 erg/s/cm^2 and ~ 6.5 x 10^-15 erg/s/cm^2, respectively, at the 90% confidence level, largely consistent with the sensitivity estimation given by Zhang et al. (2022 [2]). 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). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES. References: [1] Ruiz, A., et al. "The RapidXMM upper limit server: X-ray aperture photometry of the XMM-Newton archival observations." Monthly Notices of the Royal Astronomical Society 511.3 (2022): 4265-4284. [2] Zhang, Juan, et al. "Estimate of the background and sensitivity of the follow-up X-ray telescope onboard Einstein Probe." Astroparticle Physics 137 (2022): 102668. View this GCN Circular online at https://gcn.nasa.gov/circulars/38467. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36463] EP241206a: BOOTES Global Network optical limits
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38466 SUBJECT: EP241206a: BOOTES Global Network optical limits DATE: 24/12/08 10:31:29 GMT FROM: Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct(a)iaa.es> D.-R. Xiong (Yunnan Observatories of CAS, YNAO), I. Perez-Garcia, E. Fernandez-Garcia, A. J. Castro-Tirado, S.-Y. Wu, M. D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy, G. Garcia-Segura (IAA-CSIC), Y.-D. Hu (INAF-OAB), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), Y.-F. Fan, J.-M. Bai, C.-J. Wang, Y.-X. Xin, X.-H. Zhao (YNAO), S. Jeong (ADD, Daejeon) and D. Hiriart and W. H. Lee (UNAM), on behalf of a larger collaboration, report: Following the detection of EP241206a by the Einstein Probe (Yin et al., GCNC 38457) we triggered our 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical Observatory (China) to follow-up this fast X-ray transient starting on Dec. 7 at 13:30 UT (~ 21.1 h after trigger time). No optical afterglow within the EP/WXT error box is detected in the co-added image (15 x 60 s, clear filter) down to 19.2 mag. Later epoch observations were obtained on Dec. 8 at 06:41 UT with the 0.6m BOOTES-5/JGT robotic telescope at San Pedro Martir Astronomical Observatory (Mexico). The resulting co-added frame (10 x 60s, clear filter) imposed a 20.3 mag limiting magnitude. We thank the staff at both Lijiang and San Pedro Martir observatories for their excellent support. View this GCN Circular online at https://gcn.nasa.gov/circulars/38466. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36462] GRB 241207C: MASTER optical observations
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38465 SUBJECT: GRB 241207C: MASTER optical observations DATE: 24/12/08 03:02:31 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), V.Lipunov, I.Panchenko, A.Kuznetsov, K.Zhirkov, E.Gorbovskoy, N.Tiurina,D.Vlasenko, A.Chasovnikov, V.Topolev, P.Balanutsa, G.Antipov, A.Sankovich,M.Gulyaev, Ya.Kechin, V.Senik (Lomonosov MSU), A.Sosnovskij (CrAO RAS), O.Gress, N.Budnev(ISU), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity) 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the MAXI GRB241207C error-box (trigger No 2412072220, GCN #38462, notice time 2024-12-08T00:13:03UT ) 8462 sec after trigger time at 2024-12-08 00:41:09 UT,with upper limit up to 18.6 mag. Observations started at twilight. The observations began at zenith distance = 61 deg. The sun altitude is -13.9 deg. Distance to Moon is 34deg., distance to Sun is 47deg. The galactic latitude b = -31 deg., longitude l = 21 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2700028 We obtain the following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|_________________________________|_____|_______|_______|_ 8475 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 36m 54.99s -22d 53m 32.3s) | C | 25 | 16.6 | 8500 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 36m 54.99s -22d 53m 32.3s) | C | 75 | 17.3 | Coadd 8486 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 27m 07.85s -23d 14m 22.0s) | C | 45 | 17.9 | 8531 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 27m 07.85s -23d 14m 22.0s) | C | 345 | 19.0 | Coadd 8537 | 2024-12-08 00:42:11 | MASTER-OAFA | (20h 37m 00.75s -22d 54m 33.0s) | C | 25 | 16.6 | 8547 | 2024-12-08 00:42:11 | MASTER-OAFA | (20h 27m 13.60s -23d 15m 22.0s) | C | 45 | 18.1 | 8601 | 2024-12-08 00:43:14 | MASTER-OAFA | (20h 36m 55.72s -22d 55m 33.7s) | C | 25 | 16.8 | 8611 | 2024-12-08 00:43:15 | MASTER-OAFA | (20h 27m 08.52s -23d 16m 21.9s) | C | 45 | 18.1 | 8661 | 2024-12-08 00:44:15 | MASTER-OAFA | (20h 37m 01.73s -22d 55m 30.7s) | C | 25 | 16.8 | 8672 | 2024-12-08 00:44:15 | MASTER-OAFA | (20h 27m 14.60s -23d 16m 18.7s) | C | 45 | 18.0 | 8724 | 2024-12-08 00:45:18 | MASTER-OAFA | (20h 36m 58.39s -22d 53m 48.8s) | C | 25 | 16.9 | 8734 | 2024-12-08 00:45:18 | MASTER-OAFA | (20h 27m 11.43s -23d 14m 36.5s) | C | 45 | 18.2 | 8822 | 2024-12-08 00:46:18 | MASTER-OAFA | (20h 36m 58.46s -22d 55m 16.4s) | C | 100 | 17.7 | 8792 | 2024-12-08 00:46:19 | MASTER-OAFA | (20h 27m 11.44s -23d 16m 03.0s) | C | 40 | 18.2 | 8838 | 2024-12-08 00:47:05 | MASTER-OAFA | (20h 27m 11.45s -23d 16m 03.3s) | C | 40 | 18.2 | 8884 | 2024-12-08 00:47:50 | MASTER-OAFA | (20h 27m 11.44s -23d 16m 03.5s) | C | 40 | 18.2 | 8943 | 2024-12-08 00:48:49 | MASTER-OAFA | (20h 37m 01.58s -22d 54m 05.1s) | C | 40 | 17.4 | 8953 | 2024-12-08 00:48:50 | MASTER-OAFA | (20h 27m 14.72s -23d 14m 51.6s) | C | 60 | 18.5 | 9020 | 2024-12-08 00:50:07 | MASTER-OAFA | (20h 36m 55.16s -22d 54m 38.4s) | C | 40 | 17.3 | 9031 | 2024-12-08 00:50:07 | MASTER-OAFA | (20h 27m 08.24s -23d 15m 24.4s) | C | 60 | 18.4 | Filter C is a clear (unfiltred) band. Reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/38465. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36461] Fermi trigger No 755225799: Global MASTER-Net observations report
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38464 SUBJECT: Fermi trigger No 755225799: Global MASTER-Net observations report DATE: 24/12/08 01:00:57 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.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) started inspect of the Fermi GRB241207.04 (trigger No 755225799,20h 13m 19.92s , +01d 52m 58.8s, R=27) errorbox 42443 sec after notice time and 42477 sec after trigger time at 2024-12-07 12:44:32 UT, with upper limit up to 17.4 mag. The observations began at zenith distance = 82 deg. The sun altitude is -34.0 deg. MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB241207.04 errorbox 49802 sec after notice time and 49836 sec after trigger time at 2024-12-07 14:47:11 UT, with upper limit up to 12.7 mag. Observations started at twilight. The observations began at zenith distance = 60 deg. The sun altitude is -12.6 deg. MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB241207.04 errorbox 85440 sec after notice time and 85474 sec after trigger time at 2024-12-08 00:41:09 UT, with upper limit up to 18.6 mag. Observations started at twilight. The observations began at zenith distance = 61 deg. The sun altitude is -13.9 deg. The galactic latitude b = -18 deg., longitude l = 45 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2698706 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 42508 | 2024-12-07 12:44:32 | MASTER-Tunka | (19h 11m 44.73s , +05d 08m 47.3s) | C | 60 | 17.4 | 49867 | 2024-12-07 14:47:11 | MASTER-Kislovodsk | (19h 11m 05.58s , +05d 03m 36.5s) | C | 60 | 12.7 | 54645 | 2024-12-07 16:06:50 | MASTER-Kislovodsk | (19h 11m 08.51s , +04d 59m 37.3s) | C | 60 | 12.3 | 85487 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 36m 54.99s , -22d 53m 32.3s) | C | 25 | 16.6 | 85512 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 36m 54.99s , -22d 53m 32.3s) | C | 75 | 17.3 | Coadd 85498 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 27m 07.85s , -23d 14m 22.0s) | C | 45 | 17.9 | 85543 | 2024-12-08 00:41:09 | MASTER-OAFA | (20h 27m 07.85s , -23d 14m 22.0s) | C | 135 | 18.6 | Coadd 85549 | 2024-12-08 00:42:11 | MASTER-OAFA | (20h 37m 00.75s , -22d 54m 33.0s) | C | 25 | 16.6 | 85559 | 2024-12-08 00:42:11 | MASTER-OAFA | (20h 27m 13.60s , -23d 15m 22.0s) | C | 45 | 18.1 | 85613 | 2024-12-08 00:43:14 | MASTER-OAFA | (20h 36m 55.72s , -22d 55m 33.7s) | C | 25 | 16.8 | 85623 | 2024-12-08 00:43:15 | MASTER-OAFA | (20h 27m 08.52s , -23d 16m 21.9s) | C | 45 | 18.1 | 85673 | 2024-12-08 00:44:15 | MASTER-OAFA | (20h 37m 01.73s , -22d 55m 30.7s) | C | 25 | 16.8 | 85684 | 2024-12-08 00:44:15 | MASTER-OAFA | (20h 27m 14.60s , -23d 16m 18.7s) | C | 45 | 18.0 | 85736 | 2024-12-08 00:45:18 | MASTER-OAFA | (20h 36m 58.39s , -22d 53m 48.8s) | C | 25 | 16.9 | 85746 | 2024-12-08 00:45:18 | MASTER-OAFA | (20h 27m 11.43s , -23d 14m 36.5s) | C | 45 | 18.2 | 85834 | 2024-12-08 00:46:18 | MASTER-OAFA | (20h 36m 58.46s , -22d 55m 16.4s) | C | 100 | 17.7 | 85804 | 2024-12-08 00:46:19 | MASTER-OAFA | (20h 27m 11.44s , -23d 16m 03.0s) | C | 40 | 18.2 | 85850 | 2024-12-08 00:47:05 | MASTER-OAFA | (20h 27m 11.45s , -23d 16m 03.3s) | C | 40 | 18.2 | 85896 | 2024-12-08 00:47:50 | MASTER-OAFA | (20h 27m 11.44s , -23d 16m 03.5s) | C | 40 | 18.2 | 85955 | 2024-12-08 00:48:49 | MASTER-OAFA | (20h 37m 01.58s , -22d 54m 05.1s) | C | 40 | 17.4 | 85965 | 2024-12-08 00:48:50 | MASTER-OAFA | (20h 27m 14.72s , -23d 14m 51.6s) | C | 60 | 18.5 | 86032 | 2024-12-08 00:50:07 | MASTER-OAFA | (20h 36m 55.16s , -22d 54m 38.4s) | C | 40 | 17.3 | 86043 | 2024-12-08 00:50:07 | MASTER-OAFA | (20h 27m 08.24s , -23d 15m 24.4s) | C | 60 | 18.4 | 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/38464. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36460] GRB 241207C: Tiled Swift observations
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38463 SUBJECT: GRB 241207C: Tiled Swift observations DATE: 24/12/08 00:47:51 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the MAXI GRB 241207C. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00129 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the MAXI event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38463. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36459] GRB 241207C: MAXI/GSC detection
by GCN Circulars 08 Dec '24

08 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38462 SUBJECT: GRB 241207C: MAXI/GSC detection DATE: 24/12/08 00:13:03 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> GRB 241207C: MAXI/GSC detection M. Nakajima (Nihon U.), M. Serino (AGU), W. Iwakiri (Chiba U.), H. Negoro, Y. Kudo, H. Shibui, K. Takagi, H. Takahashi, K. Tatano, H. Nishio (Nihon U.), T. Mihara, T. Kawamuro, S. Yamada, S. Wang, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, Y. Kawakubo, H. Hiramatsu, H. Nishikawa, Y. Kondo, S. Sasao, A. Yoshida (AGU), Y. Tsuboi, H. Sugai, N. Nagashima (Chuo U.), M. Shidatsu, Y. Niida (Ehime U.), I. Takahashi, M. Niwano, N. Higuchi, Y. Yatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, S. Ogawa, M. Kurihara (JAXA), Y. Ueda, Y. Okada, K. Fujiwara (Kyoto U.), M. Yamauchi, Y. Otsuki, T. Hasegawa, M. Nishio (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Sugizaki (Kanazawa U.), report on behalf of the MAXI team: The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 22:20:07 UT. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (306.821 deg, -23.399 deg) = (20 27 17, -23 23 56) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.41 deg and 0.34 deg, respectively. The roll angle of long axis from the north direction is 132.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 91 +- 22 mCrab (4.0-10.0keV, 1 sigma error). There was no significant excess flux in the previous transit at 20:47 UT and in the next transit at 23:53 UT with an upper limit of 20 mCrab for each. View this GCN Circular online at https://gcn.nasa.gov/circulars/38462. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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