GRB 240411A
GCN Circular 36061
Subject
GRB 240411A: Fermi GBM Final Real-time Localization
Date
2024-04-11T01:55:28Z (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 01:44:58 UT on 11 Apr 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240411A (trigger 734492703.48149 / 240411073).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 242.6, Dec = 40.6 (J2000 degrees, equivalent to J2000 16h 10m, 40d 36'), with a statistical uncertainty of 5.4 degrees.
The angle from the Fermi LAT boresight is 64.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240411073/quicklook/glg_skymap_all_bn240411073.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/bn240411073/quicklook/glg_healpix_all_bn240411073.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240411073/quicklook/glg_lc_medres34_bn240411073.gif
GCN Circular 36068
Subject
GRB 240411A: GRBAlpha detection
Date
2024-04-12T10:39:32Z (a year ago)
From
Andras Pal at Konkoly Observatory <apal@szofi.net>
Via
Web form
A. Pal (Konkoly Observatory), J. Ripa, M. Dafcikova, M. Kolar, 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.
The short-duration GRB 240411A (Fermi/GBM detection: GCN 36061; INTEGRAL/SPI-ACS peak detection at 2024-04-11 ~01:45:00 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract).
The sub-threshold detection was confirmed at the peak time 2024-04-11 01:45:00.0 UTC. The T90 duration measured by GRBAlpha is 1.0 s and the significance at the peak time reaches 4 sigma in the ~120-400 keV band.
The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240411A_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.
GCN Circular 36090
Subject
IPN triangulation of GRB 240411A
Date
2024-04-14T14:00:48Z (a year ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,
and T. Cline on behalf of the Konus-Wind team,
A. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,
E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
and
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team, report:
The long-duration GRB 240411A
(Fermi-GBM detection: The Fermi GBM team, GCN 36061;
GRBAlpha detection: Pal et al., GCN 36068)
was detected by Fermi (GBM trigger 734492703),
INTEGRAL (SPI-ACS), Swift (BAT), Konus-Wind, and GRBAlpha
at about 6298 s UT (01:44:58).
The burst was outside the coded field of view of the BAT.
We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
246.889 (16h 27m 33s) +45.010 (+45d 00' 36")
Corners:
251.205 (16h 44m 49s) +41.318 (+41d 19' 05")
251.479 (16h 45m 55s) +41.818 (+41d 49' 03")
241.660 (16h 06m 38s) +48.434 (+48d 26' 03")
241.553 (16h 06m 13s) +47.881 (+47d 52' 53")
---------------------------------------------
The error box area is 4.6 sq. deg, and its maximum
dimension is 9.8 deg (the minimum one is 29 arcmin).
The Sun distance was 111 deg.
This localization may be improved.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB240411_T06302/IPN/
The Konus-Wind time history and spectrum will be given
in a forthcoming GCN Circular.
GCN Circular 36141
Subject
GRB 240411A: Glowbug gamma-ray detection
Date
2024-04-16T21:12:57Z (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 240411A, which was also detected by Fermi/GBM (GCN 36061), GRBAlpha (GCN 36068), as well as INTEGRAL/SPI-ACS, Swift/BAT, and Konus/Wind (GCN 36090).
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-04-11 01:44:59.000 with a duration of 0.51 s and a total significance of about 25.8 sigma. The light curve comprises a single peak.
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 36156
Subject
Improved IPN triangulation of GRB 240411A
Date
2024-04-18T10:47:24Z (a year ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the MGNS/BepiColombo team,
J. Benkhoff on behalf of the BepiColombo team,
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,
and T. Cline on behalf of the Konus-Wind team,
A. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,
E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
and
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team, report:
Using the BepiColombo (MGNS) data we have improved
the previous IPN error box (Svinkin et al., GCN 36090).
The coordinates of the updated 3 sigma error box are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
248.823 (16h 35m 17s) +43.618 (+43d 37' 03")
Corners:
248.867 (16h 35m 28s) +43.236 (+43d 14' 08")
248.814 (16h 35m 15s) +43.972 (+43d 58' 19")
248.777 (16h 35m 07s) +43.999 (+43d 59' 57")
248.831 (16h 35m 20s) +43.263 (+43d 15' 47")
---------------------------------------------
The error box area is 65 sq. arcmin, and its maximum
dimension is 46 arcmin (the minimum one is 1 arcmin).
The Sun distance was 111 deg.
This box may be further improved.
Updated triangulation map and HEALPix FITS files are posted at
http://www.ioffe.ru/LEA/GRBs/GRB240411_T06302/IPN/
GCN Circular 36164
Subject
GRB 240411A: GOTO early optical upper limits
Date
2024-04-18T20:43:43Z (a year ago)
From
Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>
Via
email
B. P. Gompertz, D. Steeghs, B. Godson; R. Starling, K. Ackley; M. J. Dyer; J. Lyman; K. Ulaczyk; F. Jimenez-Ibarra; A. Kumar; D. O'Neill; D. K. Galloway; V. Dhillon; P. O'Brien; G. Ramsay; K. Noysena; R. Kotak; R. P. Breton; L. K. Nuttall; E. Pall'e and D. Pollacco report on behalf of the GOTO collaboration:
We report on observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022) in response to GRB 240411A (Fermi GBM Team, GCN 36061; Pal et al., GCN 36068; Cheung et al., 36141). Targeted observations began at 01:57:29 UT on 2024-04-11, 12 minutes after the GBM trigger. Each observation consisted of 4x90s exposures in the GOTO L-band (400-700 nm).
Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using recent survey observations of the same pointings. Source candidates were initially filtered using a classifier (Killestein et al. 2021) and cross-matched against a variety of contextual and minor planet catalogues. Human vetting was carried out in real time on any candidates that passed the above checks.
No new candidate transient events are identified within the refined IPN error box (Kozyrev et al., GCN 36156). The 5-sigma limiting magnitude of the image is L > 19.7 at 12 minutes after trigger.
Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.
GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).