GRB 240514B
GCN Circular 36469
Subject
GRB 240514B: Fermi GBM Final Real-time Localization
Date
2024-05-14T04:14:13Z (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 04:03:45 UT on 14 May 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240514B (trigger 737352230.039954 / 240514169).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 341.9, Dec = -1.3 (J2000 degrees, equivalent to J2000 22h 47m, -1d 18'), with a statistical uncertainty of 43.6 degrees.
The angle from the Fermi LAT boresight is 161.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240514169/quicklook/glg_skymap_all_bn240514169.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/bn240514169/quicklook/glg_healpix_all_bn240514169.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240514169/quicklook/glg_lc_medres34_bn240514169.gif
GCN Circular 36472
Subject
Fermi GRB 240514B: Global MASTER-Net observations report
Date
2024-05-14T06:31:25Z (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-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) started inspect of the Fermi GRB 240514B ( Fermi GBM team, GCN 36469) errorbox 186 sec after notice time and 220 sec after trigger time at 2024-05-14 04:07:25 UT, with upper limit up to 17.8 mag. Observations started at twilight. The observations began at zenith distance = 76 deg. The sun altitude is -15.4 deg.
The galactic latitude b = -51 deg., longitude l = 70 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2455691
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
250 | 2024-05-14 04:07:25 | MASTER-SAAO | (23h 53m 26.24s , +31d 15m 52.3s) | C | 60 | 17.3 |
250 | 2024-05-14 04:07:25 | MASTER-SAAO | (23h 51m 19.62s , +31d 29m 09.8s) | C | 60 | 17.6 |
330 | 2024-05-14 04:08:44 | MASTER-SAAO | (00h 02m 55.69s , +31d 14m 48.8s) | C | 60 | 17.0 |
330 | 2024-05-14 04:08:44 | MASTER-SAAO | (00h 00m 49.32s , +31d 28m 06.8s) | C | 60 | 17.4 |
525 | 2024-05-14 04:11:59 | MASTER-SAAO | (23h 48m 56.98s , +27d 26m 04.0s) | C | 60 | 17.5 |
525 | 2024-05-14 04:11:59 | MASTER-SAAO | (23h 46m 54.69s , +27d 39m 27.5s) | C | 60 | 17.8 |
604 | 2024-05-14 04:13:19 | MASTER-SAAO | (00h 11m 01.46s , +29d 21m 22.9s) | C | 60 | 16.8 |
604 | 2024-05-14 04:13:19 | MASTER-SAAO | (00h 08m 57.25s , +29d 34m 47.3s) | C | 60 | 17.3 |
684 | 2024-05-14 04:14:39 | MASTER-SAAO | (00h 20m 12.77s , +29d 20m 15.5s) | C | 60 | 16.7 |
684 | 2024-05-14 04:14:39 | MASTER-SAAO | (00h 18m 08.63s , +29d 33m 39.6s) | C | 60 | 17.0 |
927 | 2024-05-14 04:18:42 | MASTER-SAAO | (23h 51m 33.13s , +27d 41m 18.0s) | C | 60 | 17.0 |
927 | 2024-05-14 04:18:42 | MASTER-SAAO | (23h 53m 35.76s , +27d 27m 56.6s) | C | 60 | 16.8 |
1007 | 2024-05-14 04:20:02 | MASTER-SAAO | (00h 02m 43.28s , +27d 26m 54.1s) | C | 60 | 16.5 |
1007 | 2024-05-14 04:20:02 | MASTER-SAAO | (00h 00m 40.74s , +27d 40m 16.4s) | C | 60 | 16.7 |
1590 | 2024-05-14 04:29:44 | MASTER-SAAO | (00h 02m 55.61s , +31d 15m 34.3s) | C | 60 | 14.4 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 36481
Subject
GRB 240514B: Fermi GBM Detection
Date
2024-05-14T22:49:03Z (a year ago)
From
Oliver J Roberts at USRA/NASA <oliver.roberts@nasa.gov>
Via
Web form
O.J. Roberts (USRA-NASA/MSFC) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 04:03:45.04 UT on 14 May 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 240514B (trigger 737352230/240514169).
The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 5.1, Dec = 44.5 (J2000 degrees, equivalent to J2000 22h 47m, -1d 19'),
with a statistical uncertainty of 4.0 degrees. There is additionally a
systematic error which we have characterized as a core-plus-tail model,
with 90% of GRBs having a 3.7 deg error and a small tail suffering a
larger than 10 deg systematic error (Connaughton et al. 2015, ApJS, 216, 32).
This is an improved localization that replaces the Final Position notice
GCN sent out earlier (Fermi GBM Team, 2021, GCN 36469).
The angle from the Fermi LAT boresight is 111 degrees.
The GBM light curve shows two bright peaks with a duration (T90)
of about 1.7 s (50-300 keV). The time-averaged spectrum
from T0-0.06 to T0+0.70 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.75 +/- 0.07 and the cutoff energy,
parameterized as Epeak, is 957 +/- 130 keV.
The event fluence (10-1000 keV) in this time interval is
(2.7 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.32 s in the 10-1000 keV band is 16 +/- 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/"
GCN Circular 36484
Subject
GRB 240514B: GRBAlpha detection
Date
2024-05-15T13:00:41Z (a year ago)
From
Jakub Ripa <ripa.jakub@gmail.com>
Via
Web form
J. Ripa, M. Dafcikova, 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.
The short-duration GRB 240514B (Fermi/GBM detection: GCN 36481; INTEGRAL/SPI-ACS peak detection at 2024-05-14 ~04:03:45 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 detection was confirmed at the peak time 2024-05-14 04:03:44.7 UTC. The T90 duration measured by GRBAlpha is 1.0 s and the overall significance during T90 reaches 6.1 sigma.
The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240514B_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 36488
Subject
GRB 240514B: GOTO candidate optical counterpart
Date
2024-05-15T17:21:18Z (a year ago)
From
Amit Kumar at University of Warwick, UK <amitkundu515@gmail.com>
Via
Web form
A. Kumar, B. P. Gompertz, K. Ackley, J. Lyman, S. Belkin, A. J. Levan, R. Starling, M. J. Dyer, K. Ulaczyk, F. Jimenez-Ibarra, D. O'Neill, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Palle 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 the Fermi GBM detected GRB 240514B (Fermi GBM team, GCN 36469, Roberts et al., GCN 36481). Targeted observations were performed by GOTO-South on 2024-05-14 from 18:11:25 to 19:24:33 UT (respectively from 14.128 to 15.347 hours after trigger) distributed over five epochs. 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.
We identify AT2024ixa/GOTO24bph as a possible optical counterpart within the GBM 90% localisation region. The source is coincident with a galaxy in the GLADE+ catalogue (Dalya et al. 2021) with a photometric redshift of z=0.0579+/-0.0349. The source is seen to fade by 8.6 +/- 5.8 mags/day across 5 epochs of observations.
We find no evidence of this source prior to the GRB trigger time in previous GOTO observations, the ZTF observations provided by the Lasair broker (Smith et al. 2019), or the ATLAS forced photometry server (Shingles et al. 2021). We caution that the position has not been covered by GOTO since 2024-01-09 prior to the GBM trigger. Hence, further observations are encouraged to ascertain the nature of the candidate.
Name | RA(J2000) | Dec(J2000) | Epoch(MJD) | dt_trig(hrs) | Filter | Mag(AB)
GOTO24bph | 22:43:13.32 | -00:08:17.37 | 60444.7579 | 14.128 | L | 19.58 +/- 0.18
Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and were 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).
GCN Circular 36491
Subject
GRB 240514B: AT2024ixa/GOTO24bph is not consistent with the Fermi localisation
Date
2024-05-15T19:26:57Z (a year ago)
From
Amit Kumar at University of Warwick, UK <amitkundu515@gmail.com>
Via
Web form
A. Kumar, B. P. Gompertz, K. Ackley, J. Lyman, S. Belkin, A. J. Levan, R. Starling, M. J. Dyer, K. Ulaczyk, F. Jimenez-Ibarra, D. O'Neill, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Palle and D. Pollacco report on behalf of the GOTO collaboration:
The Gravitational-wave Optical Transient Observer (GOTO, Steeghs et al. 2022) autonomously responded to GRB 240514B, initially reported at RA = 341.9, Dec = -1.3 (J2000 degrees, equivalent to J2000 22h 47m, -1d 18') (Fermi GBM Team, GCN 36469).
Following the initial alert, the localisation was subsequently updated to RA = 5.1, Dec = 44.5, stated to be equivalent to J2000 22h 47m, -1d 19' (Roberts et al. GCN 36481). Inspection of the localisation map suggests the decimal coordinates are the correct ones, and the candidate optical counterpart identified by GOTO (Kumar et al. GCN 36488) is inconsistent with the GBM localisation.
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).
GCN Circular 36507
Subject
IPN triangulation of GRB 240514B (short)
Date
2024-05-17T17:35:13Z (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 short-duration GRB 240514B
(Fermi-GBM detection: The Fermi GBM team, GCN 36469;
Roberts and Meegan, GCN 36481;
GRBAlpha detection: Ripa et al., GCN 36484)
was detected by Fermi (GBM trigger 737352230), Swift (BAT),
INTEGRAL (SPI-ACS), GRBAlpha, and Konus-Wind, in the waiting mode,
at about 14625 s UT (04:03:45).
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:
77.510 (05h 10m 02s) +53.570 (+53o 34' 12")
Corners:
147.796 (09h 51m 11s) +57.777 (+57d 46' 37")
7.396 (00h 29m 35s) +57.580 (+57d 34' 49")
7.207 (00h 28m 50s) +47.865 (+47d 51' 55")
148.019 (09h 52m 04s) +48.062 (+48d 03' 43")
---------------------------------------------
The error box area is 816 sq. deg, and its maximum
dimension is 69 deg (the minimum one is 9.7 deg).
The Sun distance was 46 deg.
This localization may be improved.
The optical transient reported by Kumar et al., GCN 36488 is outside the IPN error box and the updated Fermi-GBM localization (glg_healpix_all_bn240514169_v02).
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB240514_T14625/IPN/
GCN Circular 36521
Subject
GRB 240514B: VZLUSAT-2 detection
Date
2024-05-20T15:21:26Z (a year ago)
From
Andras Pal at Konkoly Observatory <apal@szofi.net>
Via
Web form
A. Pal (Konkoly Observatory), M. Dafcikova, J. Ripa, N. Werner (Masaryk U.), M. Ohno (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration.
The short-duration GRB 240514B (Fermi/GBM detection: GCN 36481; GRBAlpha detection: GCN 36484; INTEGRAL/SPI-ACS peak detection at 2024-05-14 ~04:03:45 UT) was detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/).
The data acquisition was performed by the GRB detector unit no. 1. The detection was confirmed at the peak time 2024-05-14 04:03:34 UTC. The T90 duration is 1 s and the significance during T90 reaches 10 sigma.
The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB240514B_GCN_VZLUSAT2.pdf
We note that the light curve measured by VZLUSAT-2 is shifted by approximately 11 s with respect to light curves obtained by other missions. The cause of the on-board clock slip is being fixed.
All VZLUSAT-2 detections are listed at: https://monoceros.physics.muni.cz/hea/VZLUSAT-2/.
The GRB detectors on VZLUSAT-2 are a demonstration payload for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13 from Cape Canaveral.