//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 32950 SUBJECT: GRB 221119A: Fermi GBM Final Real-time Localization DATE: 22/11/19 15:13:22 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 15:02:53 UT on 19 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221119A (trigger 690562978.639846 / 221119627). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 147.0, Dec = -12.9 (J2000 degrees, equivalent to J2000 09h 48m, -12d 54'), with a statistical uncertainty of 1.2 degrees. The angle from the Fermi LAT boresight is 89.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221119627/quicklook/glg_skymap_all_bn221119627.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221119627/quicklook/glg_healpix_all_bn221119627.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221119627/quicklook/glg_lc_medres34_bn221119627.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 32951 SUBJECT: LAT GRB221119.63: Global MASTER-Net observations report DATE: 22/11/20 12:55:23 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D.Cheryasov, Ya.Kechin (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev (Irkutsk State University, API), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational State University) MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the LAT GRB221119.63 (trigger No 690562978,09h 38m 24.00s , -14d 30m 00.0s, R=0.599833) errorbox 27555 sec after trigger time at 2022-11-19 22:42:08 UT, with upper limit up to 19.1 mag. The observations began at zenith distance = 78 deg. The sun altitude is -38.3 deg. The galactic latitude b = 28 deg., longitude l = 249 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2162046 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 27586 | 2022-11-19 22:42:08 | MASTER-SAAO | (09h 39m 34.49s , -15d 55m 59.7s) | C | 60 | 15.7 | 28167 | 2022-11-19 22:51:49 | MASTER-SAAO | (09h 32m 02.18s , -15d 56m 16.0s) | C | 60 | 18.1 | 28428 | 2022-11-19 22:56:11 | MASTER-SAAO | (09h 34m 23.11s , -14d 01m 15.4s) | C | 60 | 17.8 | 28508 | 2022-11-19 22:57:31 | MASTER-SAAO | (09h 42m 38.85s , -14d 00m 02.0s) | C | 60 | 16.4 | 28689 | 2022-11-19 23:00:32 | MASTER-SAAO | (09h 39m 34.36s , -15d 54m 17.9s) | C | 60 | 17.8 | 28831 | 2022-11-19 23:01:53 | MASTER-SAAO | (09h 47m 12.99s , -13d 08m 12.7s) | C | 180 | 17.6 | 29074 | 2022-11-19 23:06:57 | MASTER-SAAO | (09h 32m 01.53s , -15d 55m 21.5s) | C | 60 | 18.6 | 29335 | 2022-11-19 23:11:18 | MASTER-SAAO | (09h 34m 23.91s , -14d 02m 22.2s) | C | 60 | 18.4 | 29415 | 2022-11-19 23:12:38 | MASTER-SAAO | (09h 42m 43.45s , -14d 01m 55.6s) | C | 60 | 18.1 | 29675 | 2022-11-19 23:16:58 | MASTER-SAAO | (09h 39m 30.36s , -15d 55m 13.3s) | C | 60 | 18.3 | 29906 | 2022-11-19 23:19:48 | MASTER-SAAO | (09h 47m 09.48s , -13d 08m 40.4s) | C | 180 | 18.9 | 30477 | 2022-11-19 23:30:19 | MASTER-SAAO | (09h 38m 07.52s , -12d 08m 28.8s) | C | 60 | 18.6 | 30969 | 2022-11-19 23:37:31 | MASTER-SAAO | (09h 47m 10.15s , -13d 06m 54.3s) | C | 180 | 19.0 | 31539 | 2022-11-19 23:48:02 | MASTER-SAAO | (09h 38m 12.55s , -12d 06m 46.7s) | C | 60 | 19.0 | 32575 | 2022-11-20 00:05:18 | MASTER-SAAO | (09h 38m 13.03s , -12d 08m 44.0s) | C | 60 | 19.1 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 32952 SUBJECT: GRB 221119A: Fermi-LAT detection DATE: 22/11/20 14:15:17 GMT FROM: Francesco Longo at U of Trieste,INFN Trieste Longo F. (University and INFN Trieste), Pillera R. (Politecnico and INFN, Bari) and Palatiello M. (University of Udine and INFN Trieste) report on behalf of the Fermi-LAT team: On November, 19, 2022 Fermi-LAT detected high-energy emission from GRB 221119A, which was also detected by Fermi-GBM (trigger 221119627 / 690562978, GCN 32950) at 15:02:53 UT . The best LAT on-ground location is found to be RA, Dec = 144.6, -14.5 (J2000) with an error radius of 0.6 deg (90 % containment, statistical error only). This was at 85 deg from the LAT boresight at the time of the trigger. The GRB entered in the LAT field of view only after 3.5 ks from the trigger time. The 100 MeV - 1 GeV photon flux in the time interval 3500-5000 s after the GBM trigger is (2.1 +/- 0.8) E-06 ph/cm2/s. The estimated integrated photon index above 100 MeV is -1.9 +/- 0.3. The highest-energy photon is a 2.6 GeV event with 99% probability which is observed around 4600 seconds after the GBM trigger. A Swift ToO has been requested for this burst. The Fermi-LAT point of contact for this burst is Michele Palatiello (michele.palatiello@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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 32953 SUBJECT: GRB 221119A: Detection by GRBAlpha DATE: 22/11/20 15:07:20 GMT FROM: Andras Pal at Konkoly Observatory A. Pal (Konkoly Observatory), J. Ripa, M. Dafcikova, N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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. The long-duration GRB 221119A (Fermi/GBM detection: GCN Circ. 32950; GECAM-B detection at 2022-11-19 15:02:54.65 UT, trigg. num. 72; also detected by INTEGRAL/SPI-ACS) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020). The first double-peaked signal, acquired with a 1-second cadence was confirmed with a ~14 sigma detection at the peak times of 2022-11-19 15:02:55 and 15:02:58 UTC, respectively. In addition, the presence, duration and amplitude of the second peak is also confirmed by the GRBAlpha light curve 40-50 seconds after the double peaks. The T90 duration of this GRB is 54 seconds and the overall significance during T90 reaches 23.5. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB221119A_GCN.pdf GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the on-board data acquisition software stack. The ground segment is also supported by the radio amateur community, and it takes advantage of the SatNOGS network for increased data downlink volume, also allowing us the retrieval with a small latency. We would like to thank the support of the operators of the individual receiver stations as well as the maintenance of the network itself. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 32954 SUBJECT: GRB 221119A: Fermi GBM detection DATE: 22/11/20 16:31:02 GMT FROM: Suraj Poolakkil at UAH S. Poolakkil (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 15:02:53.64 UT on 19 November 2022, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 221119A (trigger 690562978 / 221119627) which was also detected by the Fermi-LAT (Longo et al. 2022, GCN 32952). The Fermi GBM Final Real-time Localization (GCN 32950) is consistent with the LAT position. The angle from the Fermi LAT boresight at the GBM trigger time is 90 degrees. The GBM light curve consists of multiple peaks followed by some extended emission with a duration (T90) of about 66 s (50-300 keV). The time-averaged spectrum from T0 s to T+74.75 s is best fit by Band function, with Epeak = 132 +/- 11 keV, alpha = -1.18 +/- 0.04 and beta = -1.97 +/- 0.04. The event fluence (10-1000 keV) in this time interval is (4.02 +/- 0.07)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+3.84 s in the 10-1000 keV band is 18.0 +/- 0.3 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/"