TITLE: GCN CIRCULAR
NUMBER: 40351
SUBJECT: GRB 250504A: SVOM/VT upper limit
DATE: 25/05/05 14:53:47 GMT
FROM: SVOM_group <svomgroup(a)bao.ac.cn>
L. P. Xin, Y. L. Qiu, H. L. Li, C. Wu, Z. H. Yao, Y. N. Ma, D.H. Zhao, X. H. Han, Y. Xu, J. Wang, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. S. Deng, J. Y. Wei (NAOC) report on behalf of the SVOM/VT Instrument Center:
SVOM/VT conducted ToO follow-up observations of GRB 250504A detected by Fermi (Fermi/GBM team, GCN 40342;…
[View More] Bala et al., GCN 40346) and Swift (Moss et al., GCN 40343). The observation started on 2025-05-05T01:11:01 UT, 2025 May 05, ~1.75 hr after the burst.
Our preliminary analysis shows no detection of an optical counterpart in VT_B-band stacked images (3975 s total effective exposure) at both the de Wet et al. (GCN 40347) position and the enhanced XRT position (4.0 arcsec error radius; Osborne et al. GCN 40345), with a 3 sigma upper limit of VT_B > 22.0 mag (AB) at 2.74 hr post-burst.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC),CAS.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40351.
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TITLE: GCN CIRCULAR
NUMBER: 40350
SUBJECT: GRB 250504A: REM optical/NIR observations
DATE: 25/05/05 10:35:35 GMT
FROM: Riccardo Brivio at INAF-OAB <riccardo.brivio(a)inaf.it>
R. Brivio, M. Ferro, P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team:
We observed the field of GRB 250504A detected by Fermi/GBM (Fermi GBM team, GCN 40342) and Swift/BAT (Moss et al., GCN 40343) with the REM 60 cm robotic telescope located at the ESO observatory of La Silla (…
[View More]Chile). The observations were carried in the g, r, i, z, J, H, and K bands, started on 2025 May 05 at 01:09:20 UT (i.e. 1.7 hr after the burst), and lasted for about 1 hour.
From preliminary inspection, we do not detect any counterpart at the position of the optical afterglow (de Wet et al., GCN. 40347) down to the following 3sigma limits:
r > 19.3 (AB; calibrated against the SkyMapper catalogue),
at a mid-time of 2.2 hours after the trigger;
H > 15.7 (Vega; calibrated against the 2MASS catalogue),
at a mid-time of 2.1 hours after the trigger.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40350.
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TITLE: GCN CIRCULAR
NUMBER: 40349
SUBJECT: GRB 250502A: REM optical/NIR observations
DATE: 25/05/05 10:33:25 GMT
FROM: Riccardo Brivio at INAF-OAB <riccardo.brivio(a)inaf.it>
R. Brivio, M. Ferro, P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team:
We observed the field of GRB 250502A detected by SVOM/ECLAIRs (Wang et al., GCN 40313) with the REM 60 cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried …
[View More]in the g, r, i, z, J, H, and K bands, started on 2025 May 02 at 22:59:17 UT (i.e. 14.2 hr after the burst), and lasted for about 1 hour.
From preliminary inspection, we do not detect any counterpart at the position of the optical afterglow (Rakotondrainibe et al., GCN. 40315; An et al., GCN 40319; Li et al., GCN 40320; Ghosh et al, GCN 40322; de Ugarte Postigo et al., GCN 40328; Pérez-Fournon et al., GCN 40330; Odeh et al., GCN 40331; Bochenek & Perley, GCN 40333; Corcoran et al., GCN 40334; Leonini et al., GCN 40337; Zheng et al., GCN 40338; Pankov et al., GCN 40339) down to the following 3sigma limits:
r > 19.8 (AB; calibrated against the Pan-STARRS catalogue),
at a mid-time of 14.7 hours after the trigger;
H > 16.0 (Vega; calibrated against the 2MASS catalogue),
at a mid-time of 14.2 hours after the trigger.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40349.
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TITLE: GCN CIRCULAR
NUMBER: 40347
SUBJECT: GRB 2050504A: MeerLICHT optical afterglow detection
DATE: 25/05/05 08:04:54 GMT
FROM: Simon de Wet at DTU Space <simdewet(a)gmail.com>
S. de Wet (DTU Space), P.M. Vreeswijk (Radboud) and P.J. Groot (Radboud/UCT/SAAO) report on behalf of the MeerLICHT consortium:
The 0.6 m wide-field MeerLICHT optical telescope located in Sutherland, South Africa, obtained a repeating series of 60 s exposures in the q,u,g,r,i,z bands of GRB 250504A …
[View More]following the Swift detection (Moss et al., GCN 40343). Observations started at 23:29:27 UT on 2025 May 5 (210 seconds post-trigger) and continued for a further 3 hours, following the filter sequence quqgqrqiqz.
We find a new transient candidate in our first q-band exposure at the following coordinates:
RA (J2000) = 17:58:28.38 (269.61827d)
Dec (J2000) = -40:21:59.58 (-40.36655d)
calibrated against Gaia DR2. The astrometric uncertainty is ~0.3" in each coordinate. This position is outside the initial XRT error circle reported by Moss et al. (GCN 40343) but within the updated XRT error circle reported by Osborne et al. (GCN 40345). We regard this object as the optical afterglow to GRB250504A. We report the following AB magnitudes and non detections from our first exposures:
q = 19.32 +/- 0.05 at 23:29:59 UT
u > 19.34 (3sigma) at 23:31:20 UT
g = 19.69 +/- 0.10 at 23:34:04 UT
r = 19.52 +/- 0.11 at 23:36:48 UT
i = 19.32 +/- 0.13 at 23:39:31 UT
z = 18.85 +/- 0.20 at 23:42:14 UT
MeerLICHT is built and run by a consortium consisting of Radboud University, University of Cape Town, the South African Astronomical Observatory, the University of Oxford, the University of Manchester and the University of Amsterdam.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40347.
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TITLE: GCN CIRCULAR
NUMBER: 40346
SUBJECT: GRB 250504A: Fermi GBM Observation
DATE: 25/05/05 08:00:47 GMT
FROM: Elisabetta Bissaldi at Politecnico and INFN Bari <elisabetta.bissaldi(a)ba.infn.it>
S. Bala (USRA) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 23:25:54.78 UT on 04 May 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 250504A (trigger 768093959/250504976),
which was also detected by Swift BAT (M. J. Moss …
[View More]et al. 2025, GCN 40343).
The Fermi GBM on-ground location is consistent with the Swift BAT position.
The angle from the Fermi LAT boresight is 111 degrees.
The GBM light curve consists of multiple peaks with a duration (T90)
of about 49 s (50-300 keV). The time-averaged spectrum
from T0+0.003 to T0+59.393 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.06 +/- 0.08 and the cutoff energy,
parameterized as Epeak, is 621 +/- 130 keV.
The event fluence (10-1000 keV) in this time interval is
(1.20 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+10 s in the 10-1000 keV band is 3.6 +/- 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/"
View this GCN Circular online at https://gcn.nasa.gov/circulars/40346.
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TITLE: GCN CIRCULAR
NUMBER: 40345
SUBJECT: GRB 250504A: Enhanced Swift-XRT position
DATE: 25/05/05 07:32:59 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 940 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 250504A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the …
[View More]USNO-B1 catalogue): RA, Dec = 269.61806, -40.36676 which is equivalent
to:
RA (J2000): 17h 58m 28.34s
Dec (J2000): -40d 22' 00.3"
with an uncertainty of 4.0 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40345.
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TITLE: GCN CIRCULAR
NUMBER: 40343
SUBJECT: GRB 250504A: Swift detection of a burst
DATE: 25/05/04 23:44:16 GMT
FROM: David Palmer at LANL <palmer(a)lanl.gov>
M. J. Moss (GSFC), C. Gronwall (PSU), R. Gupta (NASA GSFC),
J. A. Kennea (PSU), D. M. Palmer (LANL) and M. H. Siegel (PSU) report
on behalf of the Neil Gehrels Swift Observatory Team:
At 23:25:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 250504A (trigger=1310284). Swift slewed immediately to the …
[View More]burst.
The BAT on-board calculated location is
RA, Dec 269.612, -40.349 which is
RA(J2000) = 17h 58m 27s
Dec(J2000) = -40d 20' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of about 60 sec. The peak count rate
was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 23:27:15.3 UT, 77.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 269.61691,
-40.36642 which is equivalent to:
RA(J2000) = 17h 58m 28.06s
Dec(J2000) = -40d 21' 59.1"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.12
x 10^21 cm^-2 (Willingale et al. 2013).
UVOT took a finding chart exposure of 250 seconds with the U filter starting
137 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. Because of the density of catalogued stars, further analysis
is required to report an upper limit for any afterglow in the sub-image. The
8'x8' region for the list of sources generated on-board covers 0.00% of the XRT
error circle. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.191.
Burst Advocate for this burst is M. J. Moss (mikejmoss3 AT gmail.com).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
View this GCN Circular online at https://gcn.nasa.gov/circulars/40343.
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