GRB 240213A
GCN Circular 35718
Subject
GRB 240213A: Fermi GBM Final Real-time Localization
Date
2024-02-13T20:32:08Z (a year ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
Via
email
The Fermi GBM team reports the detection of a likely LONG GRB
At 20:11:09 UT on 13 Feb 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240213A (trigger 729547874.78288 / 240213841).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 166.4, Dec = -20.5 (J2000 degrees, equivalent to J2000 11h 05m, -20d 30'), with a statistical uncertainty of 1.6 degrees.
The angle from the Fermi LAT boresight is 112.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240213841/quicklook/glg_skymap_all_bn240213841.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240213841/quicklook/glg_healpix_all_bn240213841.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240213841/quicklook/glg_lc_medres34_bn240213841.gif
GCN Circular 35719
Subject
Fermi GRB 240213A: Global MASTER-Net observations report
Date
2024-02-13T20:46:19Z (a year ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,
G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij
(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. Gress, N.M. Budnev, O.Ershova
(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),
V. Yurkov, A. Gabovich
(Blagoveschensk Educational State University)
MASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240213A ( Fermi GBM team, GCN 35718) errorbox 547 sec after notice time and 581 sec after trigger time at 2024-02-13 20:20:50 UT, with upper limit up to 15.4 mag. The observations began at zenith distance = 83 deg. The sun altitude is -23.7 deg.
MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 240213A errorbox 564 sec after notice time and 598 sec after trigger time at 2024-02-13 20:21:08 UT, with upper limit up to 19.5 mag. The observations began at zenith distance = 53 deg. The sun altitude is -31.8 deg.
MASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 240213A errorbox 841 sec after notice time and 875 sec after trigger time at 2024-02-13 20:25:45 UT, with upper limit up to 18.8 mag. The observations began at zenith distance = 75 deg. The sun altitude is -37.2 deg.
The galactic latitude b = 36 deg., longitude l = 273 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2377781
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
641 | 2024-02-13 20:20:50 | MASTER-Amur | (11h 07m 11.98s , -20d 31m 49.5s) | C | 120 | 15.4 |
628 | 2024-02-13 20:21:08 | MASTER-SAAO | (11h 06m 57.05s , -20d 30m 53.7s) | C | 60 | 19.5 |
628 | 2024-02-13 20:21:08 | MASTER-SAAO | (11h 01m 26.58s , -20d 19m 25.9s) | C | 60 | 19.4 |
708 | 2024-02-13 20:22:27 | MASTER-SAAO | (11h 06m 56.96s , -20d 30m 52.9s) | C | 60 | 19.5 |
708 | 2024-02-13 20:22:27 | MASTER-SAAO | (11h 01m 26.50s , -20d 19m 25.2s) | C | 60 | 19.4 |
791 | 2024-02-13 20:23:10 | MASTER-Amur | (11h 07m 14.59s , -20d 30m 39.0s) | C | 140 | 15.4 |
788 | 2024-02-13 20:23:47 | MASTER-SAAO | (11h 06m 56.88s , -20d 30m 52.3s) | C | 60 | 19.3 |
788 | 2024-02-13 20:23:47 | MASTER-SAAO | (11h 01m 26.41s , -20d 19m 24.9s) | C | 60 | 19.4 |
906 | 2024-02-13 20:25:45 | MASTER-Tunka | (11h 05m 09.88s , -20d 06m 52.1s) | C | 60 | 18.4 |
966 | 2024-02-13 20:25:45 | MASTER-Tunka | (11h 05m 09.88s , -20d 06m 52.1s) | C | 180 | 18.8 | Coadd
965 | 2024-02-13 20:25:50 | MASTER-Amur | (11h 07m 07.90s , -20d 31m 27.1s) | C | 170 | 15.1 |
969 | 2024-02-13 20:26:48 | MASTER-Tunka | (11h 05m 10.00s , -20d 06m 51.6s) | C | 60 | 18.4 |
1032 | 2024-02-13 20:27:51 | MASTER-Tunka | (11h 05m 10.11s , -20d 06m 51.4s) | C | 60 | 18.3 |
1095 | 2024-02-13 20:28:55 | MASTER-Tunka | (11h 05m 10.20s , -20d 06m 50.6s) | C | 60 | 18.2 |
1155 | 2024-02-13 20:28:55 | MASTER-Tunka | (11h 05m 10.19s , -20d 06m 50.7s) | C | 180 | 18.8 | Coadd
1160 | 2024-02-13 20:29:00 | MASTER-Amur | (11h 07m 07.37s , -20d 30m 33.7s) | C | 180 | 14.3 |
1159 | 2024-02-13 20:29:58 | MASTER-Tunka | (11h 05m 10.31s , -20d 06m 50.4s) | C | 60 | 18.3 |
1222 | 2024-02-13 20:31:01 | MASTER-Tunka | (11h 05m 10.38s , -20d 06m 49.8s) | C | 60 | 18.3 |
1360 | 2024-02-13 20:32:19 | MASTER-Amur | (11h 07m 11.73s , -20d 31m 38.6s) | C | 180 | 14.0 |
1349 | 2024-02-13 20:33:08 | MASTER-Tunka | (11h 05m 10.60s , -20d 06m 48.8s) | C | 60 | 18.3 |
1409 | 2024-02-13 20:33:08 | MASTER-Tunka | (11h 05m 10.59s , -20d 06m 48.6s) | C | 180 | 18.7 | Coadd
1412 | 2024-02-13 20:34:11 | MASTER-Tunka | (11h 05m 10.65s , -20d 06m 48.8s) | C | 60 | 18.3 |
1559 | 2024-02-13 20:35:38 | MASTER-Amur | (11h 07m 06.10s , -20d 32m 41.8s) | C | 180 | 13.6 |
1544 | 2024-02-13 20:36:23 | MASTER-Tunka | (11h 05m 11.14s , -20d 05m 45.1s) | C | 60 | 18.1 |
1670 | 2024-02-13 20:38:29 | MASTER-Tunka | (11h 05m 11.38s , -20d 05m 44.6s) | C | 60 | 18.5 |
1733 | 2024-02-13 20:39:33 | MASTER-Tunka | (11h 05m 11.46s , -20d 05m 44.6s) | C | 60 | 18.5 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 35720
Subject
GRB 240213A: BALROG localization (Fermi Trigger / GRB 240213841)
Date
2024-02-13T20:59:44Z (a year ago)
From
Jochen Greiner at MPE <jcgrog@mpe.mpg.de>
Via
email
T. Preis, B. Biltzinger, J. Burgess & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
at 20:11:09 on 13 Feb. 2024 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) = 166.0 deg
Decl.(2000.0) = -18.3 deg
The 1 sigma statistical error radius is 3.1 deg.
We estimate an additional systematic error of 1 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB240213841/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB240213841/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB240213841/json
GCN Circular 35728
Subject
GRB 240213A: Glowbug gamma-ray detection
Date
2024-02-14T21:26:45Z (a year ago)
From
C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>
Via
Web form
C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:
The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240213A, which was also detected by Fermi/GBM (GCN 35718, 35720).
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-02-13 20:11:08.016 with a duration of 46.1 s and a total significance of about 130 sigma. The light curve comprises a multi-peaked structure similar to that observed by Fermi/GBM.
Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=1.1 and a cutoff energy ("Epeak") of 223 keV. The modeled 10-10000 keV fluence is 1.5e-05 erg/cm^2.
The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006
Distribution Statement A: Approved for public release. Distribution is unlimited.
GCN Circular 35745
Subject
GRB 240213A: GRBAlpha detection
Date
2024-02-18T08:52:14Z (a year ago)
From
Marianna Dafčíková at Masaryk University <500025@mail.muni.cz>
Via
Web form
M. Dafcikova, J. Ripa (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. Kolar, 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.
The long-duration GRB 240213A (Fermi/GBM detection: GCN 35718; Glowbug detection: GCN 35728; INTEGRAL/SPI-ACS peak detection at 2024-02-13 ~20:11:35) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048).
The detection was confirmed at the peak time 2024-02-13 20:11:48 UTC. The T90 duration measured by GRBAlpha is 44.5 s and the overall significance during T90 reaches 28 sigma.
The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240213A_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.