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

[vsnet-grb-info 36438] GRB 241204A: DDOTI Upper Limits on the Afterglow
by GCN Circulars 05 Dec '24

05 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38442 SUBJECT: GRB 241204A: DDOTI Upper Limits on the Afterglow DATE: 24/12/05 11:40:03 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 241204A detected by Fermi/LAT (Bissaldi et al., GCN [38436](https://gcn.nasa.gov/circulars/38436)) and Fermi/GBM (Godwin et al., GCN 38441) with the DDOTI/OAN wide-field imager at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir (http://ddoti.astroscu.unam.mx) on 2024-12-05 from 02:29 to 03:54 UTC (22.83 to 24.25 hrs after the event), obtaining a total of 48 minutes of exposure in the w filter down to a 10-sigma limiting magnitude of w = 20.6. 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/LAT (Bissaldi et al., GCN 38436). 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/38442. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36437] GRB 241204A: Fermi GBM Observation
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38441 SUBJECT: GRB 241204A: Fermi GBM Observation DATE: 24/12/04 21:07:30 GMT FROM: Matt Godwin <msg0028(a)uah.edu> Matt Godwin (UAH), E. Bissaldi (Politecnico and INFN Bari), and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 03:39:22.51 UT on 04 December 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241204A (trigger 754976367/241204152). which was also detected by Fermi-LAT (E. Bissaldi et al. 2024, GCN 38436). The Fermi GBM on-ground location is consistent with the Fermi-LAT position. The angle from the Fermi LAT boresight is 26 degrees. The GBM light curve consists of two peaks with a duration (T90) of about 0.8 s (50-300 keV). The time-averaged spectrum from T0-0.4 to T0+1.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.31 +/- 0.04 and the cutoff energy, parameterized as Epeak, is 3453 +/- 1070 keV. The event fluence (10-1000 keV) in this time interval is (2.22 +/- 0.09)E-06 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.64 s in the 10-1000 keV band is 41 +/- 2 ph/s/cm^2. 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/38441. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36436] Fermi GRB 241204A: Global MASTER-Net observations report
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38440 SUBJECT: Fermi GRB 241204A: Global MASTER-Net observations report DATE: 24/12/04 16:30:42 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-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 GRB 241204A ( E. Bissaldi et al., GCN 38436) errorbox 39000 sec after notice time and 40326 sec after trigger time at 2024-12-04 14:51:28 UT, with upper limit up to 19.8 mag. Observations started at twilight. The observations began at zenith distance = 41 deg. The sun altitude is -13.4 deg. The galactic latitude b = -26 deg., longitude l = 53 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2695247 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 40356 | 2024-12-04 14:51:28 | MASTER-Kislovodsk | (21h 05m 11.61s , +06d 39m 14.6s) | C | 60 | 17.3 | 40617 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.85s , +06d 36m 35.4s) | C | 60 | 17.7 | 40677 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.85s , +06d 36m 35.3s) | C | 180 | 18.4 | Coadd 41157 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.84s , +06d 36m 35.4s) | C | 1140 | 19.8 | Coadd 40697 | 2024-12-04 14:57:09 | MASTER-Kislovodsk | (21h 05m 17.71s , +06d 36m 52.8s) | C | 60 | 17.8 | 40776 | 2024-12-04 14:58:28 | MASTER-Kislovodsk | (21h 05m 13.79s , +06d 38m 06.3s) | C | 60 | 17.7 | 40856 | 2024-12-04 14:59:48 | MASTER-Kislovodsk | (21h 05m 14.85s , +06d 36m 37.2s) | C | 60 | 17.8 | 40976 | 2024-12-04 14:59:48 | MASTER-Kislovodsk | (21h 05m 14.85s , +06d 36m 37.1s) | C | 300 | 19.0 | Coadd 40966 | 2024-12-04 15:01:08 | MASTER-Kislovodsk | (21h 05m 17.13s , +06d 38m 07.3s) | C | 120 | 18.4 | 41105 | 2024-12-04 15:03:27 | MASTER-Kislovodsk | (21h 05m 12.10s , +06d 37m 15.1s) | C | 120 | 18.5 | 41245 | 2024-12-04 15:05:47 | MASTER-Kislovodsk | (21h 05m 11.16s , +06d 38m 11.1s) | C | 120 | 18.4 | 41365 | 2024-12-04 15:05:47 | MASTER-Kislovodsk | (21h 05m 11.16s , +06d 38m 11.1s) | C | 360 | 19.2 | Coadd 41385 | 2024-12-04 15:08:07 | MASTER-Kislovodsk | (21h 05m 18.09s , +06d 37m 07.3s) | C | 120 | 18.5 | 41525 | 2024-12-04 15:10:27 | MASTER-Kislovodsk | (21h 05m 11.35s , +06d 36m 04.7s) | C | 120 | 18.5 | 41665 | 2024-12-04 15:12:47 | MASTER-Kislovodsk | (21h 05m 18.32s , +06d 36m 12.3s) | C | 120 | 18.6 | 41725 | 2024-12-04 15:12:47 | MASTER-Kislovodsk | (21h 05m 18.32s , +06d 36m 12.3s) | C | 240 | 19.0 | Coadd 41774 | 2024-12-04 15:15:06 | MASTER-Kislovodsk | (21h 05m 14.44s , +06d 37m 37.2s) | C | 60 | 18.0 | 41854 | 2024-12-04 15:16:26 | MASTER-Kislovodsk | (21h 05m 15.52s , +06d 36m 04.1s) | C | 60 | 18.0 | 41934 | 2024-12-04 15:17:46 | MASTER-Kislovodsk | (21h 05m 18.53s , +06d 37m 41.4s) | C | 60 | 18.0 | 42114 | 2024-12-04 15:17:46 | MASTER-Kislovodsk | (21h 05m 18.51s , +06d 37m 41.2s) | C | 420 | 19.5 | Coadd 42073 | 2024-12-04 15:19:05 | MASTER-Kislovodsk | (21h 05m 12.75s , +06d 36m 52.9s) | C | 180 | 18.8 | 42273 | 2024-12-04 15:22:25 | MASTER-Kislovodsk | (21h 05m 11.88s , +06d 37m 48.3s) | C | 180 | 18.8 | 42473 | 2024-12-04 15:25:45 | MASTER-Kislovodsk | (21h 05m 18.89s , +06d 36m 44.0s) | C | 180 | 18.8 | 43655 | 2024-12-04 15:46:27 | MASTER-Kislovodsk | (20h 46m 30.15s , +05d 04m 06.4s) | C | 60 | 17.7 | 44775 | 2024-12-04 16:05:07 | MASTER-Kislovodsk | (20h 54m 32.68s , +05d 03m 31.1s) | C | 60 | 17.5 | 44855 | 2024-12-04 16:06:27 | MASTER-Kislovodsk | (20h 46m 28.95s , +05d 04m 25.4s) | C | 60 | 17.8 | 44935 | 2024-12-04 16:07:47 | MASTER-Kislovodsk | (20h 54m 29.51s , +05d 02m 58.9s) | C | 60 | 17.7 | 45014 | 2024-12-04 16:09:06 | MASTER-Kislovodsk | (20h 46m 31.91s , +05d 04m 23.6s) | C | 60 | 17.8 | 45154 | 2024-12-04 16:10:26 | MASTER-Kislovodsk | (20h 58m 42.92s , +03d 10m 49.9s) | C | 180 | 18.2 | 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/38440. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36435] GRB 241130A: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38439 SUBJECT: GRB 241130A: CALET Gamma-Ray Burst Monitor detection DATE: 24/12/04 13:47:11 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> S. Ricciarini (U of Florence), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii,Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 241130A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 38405; Fermi GBM Detection: Sharma et al., GCN Circ. 38421; EIRSAT-1 GMOD Detection: McDermott et al., GCN Circ. 38423; IPN triangulation: Ridnaia et al., GCN Circ. 38424; Konus-Wind detection: Frederiks et al., GCN Circ. 38429) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:13:45.911 UTC on 30 November 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1417043611/index.html). The burst signal was seen by all CGBM detectors. Because of a problem with the ground alert processing script, the GCN notice was not distributed automatically for this event. The burst light curve shows a single pulse that starts at T-0.4 sec, peaks at T+0.1 sec, and ends at T+5.9 sec. The T90 and T50 durations measured by the SGM data are 5.4 +/- 0.8 sec and 2.4 +/- 0.5 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1417043611 The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/38439. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36434] GRB 241130A: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38439 SUBJECT: GRB 241130A: CALET Gamma-Ray Burst Monitor detection DATE: 24/12/04 13:47:11 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> S. Ricciarini (U of Florence), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii,Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 241130A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 38405; Fermi GBM Detection: Sharma et al., GCN Circ. 38421; EIRSAT-1 GMOD Detection: McDermott et al., GCN Circ. 38423; IPN triangulation: Ridnaia et al., GCN Circ. 38424; Konus-Wind detection: Frederiks et al., GCN Circ. 38429) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:13:45.911 UTC on 30 November 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1417043611/index.html). The burst signal was seen by all CGBM detectors. Because of a problem with the ground alert processing script, the GCN notice was not distributed automatically for this event. The burst light curve shows a single pulse that starts at T-0.4 sec, peaks at T+0.1 sec, and ends at T+5.9 sec. The T90 and T50 durations measured by the SGM data are 5.4 +/- 0.8 sec and 2.4 +/- 0.5 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1417043611 The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/38439. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36433] GRB 241128A : RAPAS follow-up observations
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38438 SUBJECT: GRB 241128A : RAPAS follow-up observations DATE: 24/12/04 11:08:56 GMT FROM: Thierry Midavaine at GRANDMA <thierrymidavaine(a)sfr.fr> Thierry Midavaine on behalf of the RAPAS network reports (#3) : Cédric Latgé, Patrick Martinez [1], Pierre-Michel Bergé, Erik Guthleben, Patrick Martinez [2], Thierry Midavaine [3] observed the Gamma-Ray Burst GRB241128A (R. Brivio et al. GCN 38367, K.L. Page GCN 38368) using [1][2] ADAGIO N 820mm telescope f=3.1m at Belesta Observatory (IAU A05) equiped with a Moravian C3 CMOS camera, 1200s exposure [1],1500s exposure [2], [3] RC 500mm f=1.414m at Salvia Observatory (I73) equipped with ZWO6200MMPRO CMOS camera, 2400s exposure, [1][2][3] are equiped with RAPAS filters meeting the Gaia G, Gbp, Grp photometric bands. The FITS files are reduced with the Gaia photometric catalog in respective G, Gbp, Grp bands. The afterglow is detected RA(J2000) = 18h 14m 53.57s ; Dec(J2000) = +33° 26’ 20.4” ; ± 0.5’’ [1][2] At this location it is not detected, above the upper limit magnitude [3] MJD (mid) Gaia band mag.(Gaia) RAPAS station 60643.72986 G 20.50 ± 0.5 [1] 60644.77083 G 21.00 ± 0.5 [2] 60647.74270 G+Gbp+Grp >21. [3] RAPAS ( https://proam-gemini.fr/rapas/ ) is a new ProAm collaboration funded by Paris Observatory, delivering to a network of french amateur observatories a set of 3 filters meeting the Gaia spectral bands. This network is dedicated to deliver data in the Gaia photometric system on selected astrophysical alerts by Astro-COLIBRI ( https://astro-colibri.com/ ) or from Gaia alerts. View this GCN Circular online at https://gcn.nasa.gov/circulars/38438. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36432] GRB 241201A: GRBAlpha detection
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38437 SUBJECT: GRB 241201A: GRBAlpha detection DATE: 24/12/04 11:07:20 GMT FROM: Marianna Dafčíková at Masaryk University <500025(a)mail.muni.cz> M. Dafcikova, J. Ripa, M. Kolar (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Duriskova, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. We report a possible detection of the long-duration GRB 241201A (Fermi/GBM detection: GCN 38403) by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract). We note that GRBAlpha did not detect the initial bright peak but only the secondary one ~10 s later. The Fermi/GBM location of this burst was not occulted by the Earth or Moon at the trigger time. The non-detection of the initial peak could be due to a significantly decreased effective area caused by the variable attitude of the satellite. The detection peak time is at 2024-12-01 14:56:06.7 UTC. The T90 duration measured by GRBAlpha is 1.5 s and the overall significance during T90 reaches 7.8 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB241201A_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume. View this GCN Circular online at https://gcn.nasa.gov/circulars/38437. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36431] GRB 241204A: Fermi-LAT detection
by GCN Circulars 04 Dec '24

04 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38436 SUBJECT: GRB 241204A: Fermi-LAT detection DATE: 24/12/04 09:26:19 GMT FROM: Elisabetta Bissaldi at Politecnico and INFN Bari <elisabetta.bissaldi(a)ba.infn.it> E. Bissaldi (Politecnico and INFN Bari), A. Holzmann Airasca (UniTrento and INFN Bari) and T. Khalil (Johannesburg Univ) report on behalf of the Fermi-LAT Collaboration: On Dec 4, 2024, Fermi-LAT detected high-energy emission from GRB 241204A, which was also detected by Fermi-GBM (trigger 754976367 / 241204.152). The best LAT on-ground location is found to be: RA, Dec = 316.50, 6.55 (J2000), with an error radius of 0.5 deg (90 % containment, statistical error only). This was 26 deg from the LAT boresight at the time of the GBM trigger (T0 = 03:39:22.51 UT). The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0 - 350 s after the GBM trigger is (1.7 +/- 0.4) E-5 ph/cm2/s. The estimated photon index above 100 MeV is 2.8 +/- 0.4. The highest-energy photon is a 260 MeV event which is observed ~16 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Tamador Khalil (tamtam2030(a)gmail.com). 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/38436. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36430] EP241202b: Upper limits from Fermi-GBM Observations
by GCN Circulars 03 Dec '24

03 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38435 SUBJECT: EP241202b: Upper limits from Fermi-GBM Observations DATE: 24/12/03 20:18:30 GMT FROM: mariaedvige.ravasio(a)ru.nl M. E. Ravasio (Radboud Univ.), E. Burns (LSU), P.G. Jonker (Radboud Univ.), and M. Hui (NASA MSFC) report on behalf of the Fermi-GBM Team: Fermi-GBM had full spatial and temporal coverage of the EP-WXT signal of EP241202b (Zhou et al., GCN 38426). There was no Fermi-GBM onboard trigger around the EP-WXT trigger time T0=2024-12-02 15:12:55 UTC. The GBM targeted search [1], the most sensitive, coherent search for GRB-like signals, was run in the time interval [-50;+500] s from the EP trigger time, seeking signals between 64 ms and 32.768 s in duration. A transient was found, but its localization is not consistent with the EP transient’s one. No signal consistent both temporally and spatially is identified, as confirmed by visual inspection of the data. Assuming a “normal” spectral template (Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3), whose alpha value is consistent with the power law index reported by EP (Zhou et al., GCN 38426), and a duration of 8.192 s, we derive a sky-averaged upper limit of 5.2e-08 erg/cm2/s in the energy band 10-1000 keV. [1] Goldstein et al. 2019 arXiv:1903.12597 View this GCN Circular online at https://gcn.nasa.gov/circulars/38435. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36429] IceCube-241127A: No transient candidates from the Zwicky Transient Facility
by GCN Circulars 03 Dec '24

03 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38434 SUBJECT: IceCube-241127A: No transient candidates from the Zwicky Transient Facility DATE: 24/12/03 18:53:03 GMT FROM: Robert David Stein at JSI <rdstein(a)umd.edu> Robert Stein (JSI), Sven Weimann (Ruhr University Bochum), Jannis Necker (DESY), Anna Franckowiak (Ruhr University Bochum) and Jesper Sollerman (Stockholm University) report: On behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: As part of the ZTF neutrino follow up program (Stein et al. 2023), we observed the localization region of the neutrino event IceCube-241127A (Zegarelli et. al, GCN 38349) with the Palomar 48-inch telescope, equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). As a result of delays due to bad weather, we started observations in the g- and r-band beginning at 2024-11-29 10:38 UTC, approximately 44.4 hours after event time. We covered 95.5% (1.0 sq deg) of the reported localization region. This estimate accounts for chip gaps. Each exposure was 300s with a typical depth of 21.0 mag. The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019, Stein et al. 2021) was used to search the alerts database for candidates. We reject stellar sources (Tachibana and Miller 2018) and moving objects, and apply machine learning algorithms (Mahabal et al. 2019). We find one candidates lying within the 90.0% localization of the skymap. +---------------------------------------------------------------------------------+ | ZTF Name | IAU Name | RA (deg) | DEC (deg) | Filter | Mag | MagErr | +---------------------------------------------------------------------------------+ | ZTF19aasljeo | AT2022aelp | 163.5871140 | +05.9265829 | g | 19.23 | 0.14 | +---------------------------------------------------------------------------------+ ZTF19aasljeo is a nuclear source that was first detected on 2019-04-27, and has a long history of variability in ZTF. The source has a crossmatched detection as WISEA J105420.91+055535.5 at a distance of 0.25", and based on the WISE colours of the galaxy (W1-W2 = 1.07), ZTF19aasljeo is very likely an AGN. Over the past two months the source has been detected in difference imaging with a magnitude of g ~ 19.3. In historical detections over the past two years, the source was detected at a fainter level of g ~ 20. In reference science images from PS1 (Chambers et al. 2016), the source was detected at a much fainter level of g = 21.3, demonstrating that the source has brightened substantially in recent years. However, there are no indications of significant flaring on timescales of either weeks or months that coincide with the detection of IC241127A. We therefore find no strong evidence from our data to suggest that this AGN is associated with the neutrino. Observations of this field will continue as part of our standard ToO cadence for high-energy neutrinos (Stein et al. 2023). ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA; WIS, Israel; OKC, Sweden; JSI/UMd, USA; DESY, Germany; TANGO, Taiwan; UW Milwaukee, USA; LANL, USA; TCD, Ireland; IN2P3, France. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert database searches are done by AMPEL (Nordin et al. 2019). Alert filtering is performed with the nuztf (Stein et al. 2021, https://github.com/desy-multimessenger/nuztf ). View this GCN Circular online at https://gcn.nasa.gov/circulars/38434. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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