TITLE: GCN CIRCULAR
NUMBER: 40893
SUBJECT: Swift GRB250702.88: Global MASTER-Net observations report
DATE: 25/07/02 21:36:54 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko,
G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU),
O.Gress, N.Budnev (ISU),
C.Francile, F. Podesta, R.…
[View More]Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A.Sosnovskij (CrAO),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity),
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory)
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 Swift GRB250702.88 (trigger No 1329888,14h 11m 43.92s , +16d 41m 56.4s, R=0.05) errorbox 1057 sec after notice time and 1076 sec after trigger time at 2025-07-02 21:24:39 UT, with upper limit up to 16.9 mag. The observations began at zenith distance = 68 deg. The sun altitude is -70.5 deg.
The galactic latitude b = 68 deg., longitude l = 8 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2923573
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
1106 | MASTER-SAAO | P/ | 60 | 16.2 |
1106 | MASTER-SAAO | P\\ | 60 | 16.2 |
1185 | MASTER-SAAO | P/ | 60 | 16.8 |
1185 | MASTER-SAAO | P\\ | 60 | 16.7 |
1264 | MASTER-SAAO | P/ | 60 | 16.9 |
1264 | MASTER-SAAO | P\\ | 60 | 16.8 |
1343 | MASTER-SAAO | P/ | 60 | 13.8 |
The observation and reduction will continue.
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40893.
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TITLE: GCN CIRCULAR
NUMBER: 40891
SUBJECT: Fermi GBM Triggers 250702B, C, D and E are likely from the same source
DATE: 25/07/02 19:04:27 GMT
FROM: eliza.neights(a)gmail.com
E. Neights (GWU, NASA GSFC), O.J. Roberts (USRA, NASA MSFC), E. Burns (LSU), P. Veres (UAH) report on behalf of the Fermi-GBM Team:
At 13:09:02.03 UT, Fermi GBM triggered on GRB 250702D and was initially localized to an RA and Dec of 292.9 and 3.6 (19h, 31m, +03,33’; J2000), with an error of 14.7 deg. The light …
[View More]curve shows several peaks occurring over ~60 seconds.
Since then, an additional three bursts have triggered GBM with similar lightcurve characteristics and localizations. The trigger times and localizations are summarized as follows:
GRB Name MET (s) Time (UT) RA (deg) Dec (deg) Err (deg)
250702E 773166098 16:21:33.07 286.8 -17.7 11.6 (GCN 40890)
250702C 773160576 14:49:31.91 270.3 1.4 12.7 (GCN 40885)
250702B 773157370 13:56:05.77 286.0 -8.7 7.8 (GCN 40883)
250702D 773154547 13:09:02.03 292.9 3.6 14.7 (GCN 40886)
Despite the similar position lying close to or on the galactic plane, we observe photons in the BGO up to 1 MeV, with the majority of the photons occurring in the 50-300 keV range, which suggest the source may not be a typical galactic source and might be an ultra-long GRB or another source class. If a GRB origin is confirmed, it is 11.5 ks long, making it one of the longest ultra-long GRBs detected.
The combined GBM skymap can be found here: https://zenodo.org/records/15793558. The skymaps are all associated with each other with confidence between 89.2 and 98.5%.
There were no joint-GW detections during these triggered times.
We strongly suggest follow-up of the region to determine the nature of the source over multiple wavelengths.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40891.
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TITLE: GCN CIRCULAR
NUMBER: 40891
SUBJECT: Fermi GBM Triggers 250702B, C, D and E are likely from the same source
DATE: 25/07/02 19:04:27 GMT
FROM: eliza.neights(a)gmail.com
E. Neights (GWU, NASA GSFC), O.J. Roberts (USRA, NASA MSFC), E. Burns (LSU), P. Veres (UAH) report on behalf of the Fermi-GBM Team:
At 13:09:02.03 UT, Fermi GBM triggered on GRB 250702D and was initially localized to an RA and Dec of 292.9 and 3.6 (19h, 31m, +03,33’; J2000), with an error of 14.7 deg. The light …
[View More]curve shows several peaks occurring over ~60 seconds.
Since then, an additional three bursts have triggered GBM with similar lightcurve characteristics and localizations. The trigger times and localizations are summarized as follows:
GRB Name MET (s) Time (UT) RA (deg) Dec (deg) Err (deg)
250702E 773166098 16:21:33.07 286.8 -17.7 11.6 (GCN 40890)
250702C 773160576 14:49:31.91 270.3 1.4 12.7 (GCN 40885)
250702B 773157370 13:56:05.77 286.0 -8.7 7.8 (GCN 40883)
250702D 773154547 13:09:02.03 292.9 3.6 14.7 (GCN 40886)
Despite the similar position lying close to or on the galactic plane, we observe photons in the BGO up to 1 MeV, with the majority of the photons occurring in the 50-300 keV range, which suggest the source may not be a typical galactic source and might be an ultra-long GRB or another source class. If a GRB origin is confirmed, it is 11.5 ks long, making it one of the longest ultra-long GRBs detected.
The combined GBM skymap can be found here: https://zenodo.org/records/15793558. The skymaps are all associated with each other with confidence between 89.2 and 98.5%.
There were no joint-GW detections during these triggered times.
We strongly suggest follow-up of the region to determine the nature of the source over multiple wavelengths.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40891.
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TITLE: GCN CIRCULAR
NUMBER: 40889
SUBJECT: Konus-Wind detection of GRB 250627A
DATE: 25/07/02 16:17:20 GMT
FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru>
A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin,
A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The short-duration GRB 250627A
(SVOM-GRM detection: Wang et al., GCN 40871;
Insight-HXMT detection: Wang et al., GCN 40872;
IPN triangulation: Kozyrev et al., GCN 40888)
triggered …
[View More]Konus-Wind at T0=60377.861 s UT (16:46:17.861).
The burst light curve shows a multipeaked structure
which starts at ~T0-0.3 s and has a total duration of ~1.1 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB250627_T60377/
As observed by Konus-Wind, the burst
had a fluence of 9.65(-1.16,+1.29)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.420 s,
of 2.60(-0.49,+0.52)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.31(-0.21,+0.25)
and Ep = 874(-128,+160) keV (chi2 = 73/76 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.7
(chi2 = 73/75 dof).
All the quoted errors are at the 68% confidence level.
All the quoted values are preliminary.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40889.
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TITLE: GCN CIRCULAR
NUMBER: 40888
SUBJECT: IPN triangulation of GRB 250627A (short)
DATE: 25/07/02 16:13:38 GMT
FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru>
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the HEND/Mars Odyssey team,
A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,
E. Burns on behalf of the IPN,
Y. Zhang, C. Wang, S. Xiong, J. Wei, and B. Cordier
on behalf …
[View More]of the SVOM-GRM team,
and
W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr,
and A.S. Gardner on on behalf of the GRS-Odyssey GRB team,
report:
The short-duration GRB 250627A
(SVOM-GRM detection: Wang et al., GCN 40871;
Insight-HXMT detection: Wang et al., GCN 40872)
was detected by SVOM (GRM), Insight-HXMT, Konus-Wind,
and Mars-Odyssey (HEND) at about 60378 s UT (16:46:18).
We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
90.764 (06h 03m 03s) +10.097 (+10d 05' 48")
Corners:
90.676 (06h 02m 42s) +10.618 (+10d 37' 04")
90.803 (06h 03m 13s) +9.585 ( +9d 35' 07")
90.855 (06h 03m 25s) +9.577 ( +9d 34' 37")
90.727 (06h 02m 55s) +10.609 (+10d 36' 32")
---------------------------------------------
The error box area is 185 sq. arcmin, and its maximum
dimension is 1.1 deg (the minimum one is 2.4 arcmin).
The Sun distance was 14 deg.
This localization may be improved.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB250627_T60377/IPN
The HEALPix triangulation map is the multi-order HEALPix in units of
probability density.
The Konus-Wind time history and spectrum will be given
in a forthcoming GCN Circular.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40888.
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TITLE: GCN CIRCULAR
NUMBER: 40887
SUBJECT: GRB 250702A: Fermi GBM Detection
DATE: 25/07/02 15:35:45 GMT
FROM: Christian Malacaria at INAF-OAR <cmalacaria.astro(a)gmail.com>
C. Malacaria (INAF-OAR) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 09:54:07.56 UT on 02 July 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 250702A (trigger 773142852/250702413).
The Fermi-GBM position was reported in GCN 40883 (Fermi GBM Team …
[View More]2025).
The angle from the Fermi LAT boresight is 56 degrees.
The GBM light curve consists of a single bright emission episode with a duration (T90)
of about 52.7 s (50-300 keV). The time-averaged spectrum
from T0 to T0+69 s is best fit by a Band function
with Epeak= 242 +/- 9 keV, alpha =-0.57 +/- 0.03 and beta =-2.6 +/- 0.2.
A power law function with an exponential high-energy cutoff
fits the spectrum equally well with a power law index of -0.61 +/- 0.02
and a cutoff energy, parameterized as Epeak, of 262 +/- 7 keV.
The event fluence (10-1000 keV) in this time interval is
(3.84 +/- 0.08)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.9 s in the 10-1000 keV band is 12.8 +/- 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/40887.
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