TITLE: GCN CIRCULAR
NUMBER: 40630
SUBJECT: IPN triangulation of GRB 250404B
DATE: 25/06/05 15:32:58 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,
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,
and T. Cline on behalf of the Konus-Wind team,
E. Burns on behalf of the IPN,
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, A. Tohuvavohu,
and J. …
[View More]DeLaunay on behalf of the Swift-BAT team,
G. Waratkar, J.Joshi, V. Bhalerao, D. Bhattacharya,
and S. Vadawale, on behalf of the Astrosat-CZTI 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 250404B
(AstroSat CZTI detection: Salunke et al., GCN Circ. 40078)
was detected by Konus-Wind, Swift (BAT), AstroSat (CZTI),
and Mars-Odyssey (HEND) at about 66970 s UT (18:36:10).
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:
273.629 (18h 14m 31s) -2.251 ( -2d 15' 03")
Corners:
273.108 (18h 12m 26s) -2.676 ( -2d 40' 35")
274.127 (18h 16m 31s) -1.659 ( -1d 39' 32")
274.151 (18h 16m 36s) -1.842 ( -1d 50' 30")
273.131 (18h 12m 31s) -2.866 ( -2d 51' 58")
---------------------------------------------
The error box area is 768 sq. arcmin, and its maximum
dimension is 1.6 deg (the minimum one is 9 arcmin).
The Sun distance was 100 deg.
This localization may be improved.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB250404_T66970/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/40630.
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TITLE: GCN CIRCULAR
NUMBER: 40629
SUBJECT: IPN triangulation of GRB 250529A
DATE: 25/06/05 15:23:42 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,
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,
S. …
[View More]Barthelmy, J. Cummings, H. Krimm, D. Palmer, A. Tohuvavohu,
and J. DeLaunay on behalf of the Swift-BAT 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 long-duration GRB 250529A
(Fermi-GBM detection: Fermi GBM team, GCN 40567)
was detected by Fermi (GBM), Konus-Wind, Swift (BAT),
and Mars-Odyssey (HEND) at about 13576 s UT (03:46:16).
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:
18.193 (01h 12m 46s) +58.274 (+58d 16' 25")
Corners:
21.244 (01h 24m 58s) +56.039 (+56d 02' 19")
14.840 (00h 59m 22s) +60.456 (+60d 27' 22")
14.829 (00h 59m 19s) +60.366 (+60d 21' 57")
21.225 (01h 24m 54s) +55.944 (+55d 56' 37")
---------------------------------------------
The error box area is 1252 sq. arcmin, and its maximum
dimension is 5.6 deg (the minimum one is 4 arcmin).
The Sun distance was 48 deg.
This localization may be improved.
The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM (GCN 40567) localization.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB250529_T13600/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/40629.
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TITLE: GCN CIRCULAR
NUMBER: 40628
SUBJECT: The EP-WXT trigger 01709177837 is likely a flaring star
DATE: 25/06/05 09:41:18 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
S. Q. Jiang (NAOC), T. C. Zheng (PMO), X. Y. Zhou (PRIC), H. W. Pan (NAOC) on behalf of the Einstein Probe (EP) team:
The EP-WXT trigger 01709177837 at the time of 2025-06-05T09:24:19, is likely a stellar flare associated with RV Crt. The estimated flux of the flare is around 8e-11 erg/s/cm^2 in 0.5-4.0 keV, …
[View More]corresponding to an X-ray luminosity of around 4e32 erg/s.
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics).
View this GCN Circular online at https://gcn.nasa.gov/circulars/40628.
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TITLE: GCN CIRCULAR
NUMBER: 40627
SUBJECT: Fermi Gamma-ray Burst Monitor trigger 770470765/250601486 is not a GRB
DATE: 25/06/04 15:35:09 GMT
FROM: Joe Mangan at IJCLab <joseph.mangan(a)ijclab.in2p3.fr>
J. Mangan (IJCLab/CNRS) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:
"The Fermi Gamma-ray Burst Monitor (GBM) trigger 770470765/250601486 at 11:39:20.34 UT
on 01 June 2025, tentatively classified as a GRB, is in fact not due
to a GRB. This trigger is likely due …
[View More]to local particles."
View this GCN Circular online at https://gcn.nasa.gov/circulars/40627.
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TITLE: GCN CIRCULAR
NUMBER: 40626
SUBJECT: GRB 250601A: PRIME H band upper limit.
DATE: 25/06/04 15:02:32 GMT
FROM: N. Passaleva at Sapienza University of Rome <niccolo.passaleva(a)uniroma1.it>
N. Passaleva (U Rome), O. Guiffreda (UMD), J. Durbak (UMD), M. Elkabir (U Rome), E. Troja (U Rome), A. S. Kutyrev (NASA/GSFC), S. B. Cenko (NASA/GSFC)
Following the Fermi Gamma-ray Burst Monitor (GBM) detection (GCN 40596), and the Swift/BAT-GUANO arcminutes localization of same event, …
[View More]we observed the transient field in H filter with PRIME ~47.5 hours after the initial Fermi detection.
Using Two Micron All Sky Survey (2MASS) for preliminary calibration we do not detect any uncatalogued source down to H>20.6 AB (3-sigma) not corrected for galactic extinction at the position of the candidates reported by Swift/XRT (Page et al. GCN 40604, Salvaggio et al., GCN 40606) and EP/FXT (Liu et al., GCN 40607).
PRIME is a 1.8m telescope with 1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South Africa at the South African Astronomical Observatory (SAAO) (Kutyrev et al. 2023, Yama et al. 2023, Durbak et al. 2024).
We thank the Osaka University observers at PRIME and the staff at SAAO for their support with these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40626.
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TITLE: GCN CIRCULAR
NUMBER: 40625
SUBJECT: GRB 250530A: SVOM/GRM analysis
DATE: 25/06/04 03:52:55 GMT
FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn>
SVOM/GRM team: Chen-Wei Wang, Chao Zheng, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP)
SVOM/ECLAIRs team: M. G. Bernardini (INAF-OAB, LUPM)
Report on behalf of the SVOM team:
SVOM/GRM detected the burst GRB 250530A at 2025-05-30T06:31:54.99 UTC (T0), which is also detected by SVOM/ECLAIRs (Wang et al., GCN #…
[View More]40576).
With the event-by-event data downloaded through the X-band ground station, we conducted the standard analysis pipeline of GRB 250530A. The GRM light curve shows that this burst consists of a single pulse with a T90 of 15.0 +3.0/-4.0 s in the 15-5000 keV band, which is consistent with the result from VHF data.
With the localization of ECLAIRs (RA=186.71, DEC=-2.5648), the time-averaged spectrum from T0 to T0+15 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.26 +0.18/-0.13 and the cutoff energy, parameterized as Epeak, is 707 +1140/-360 keV. The event fluence (10-1000 keV) in this time interval is (2.8 +/-0.4)E-06 erg/cm^2.
Thus GRB 250530A is consistent with Type I GRBs in the 'Amati' relation diagram although the duration is much longer than 2 seconds, as shown at:
https://www.bursthub.cn//admin/static/grb250530A_amati.png
Further follow-up observations are encouraged.
We note that the calibration of SVOM/GRM is undergoing thus these results are preliminary. Refined analysis will be reported later.
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. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS.
The SVOM/GRM point of contact for this burst is: Chen-Wei Wang (IHEP) (cwwang(a)ihep.ac.cn)
View this GCN Circular online at https://gcn.nasa.gov/circulars/40625.
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TITLE: GCN CIRCULAR
NUMBER: 40624
SUBJECT: GRB 250601A: PRIME J band upper limit.
DATE: 25/06/03 22:03:13 GMT
FROM: N. Passaleva at Sapienza University of Rome <niccolo.passaleva(a)uniroma1.it>
N. Passaleva (U Rome), O. Guiffreda (UMD), J. Durbak (UMD), M. Elkabir (U Rome), E. Troja (U Rome), A. S. Kutyrev (NASA/GSFC), S. B. Cenko (NASA/GSFC)
Following the Fermi Gamma-ray Burst Monitor (GBM) detection (GCN 40596), and the Swift/BAT-GUANO arcminute localization of same event, …
[View More]we observed the transient field in J filter with PRIME ~23.5 hours after the initial Fermi detection.
Using nearby VISTA Hemispherical Survey (VHS) we do not detect any uncatalogued source down to J>20.3 AB (3-sigma) at the position of the candidates reported by Swift/XRT (Page et al. GCN 40604, Salvaggio et al., GCN 40606) and EP/FXT (Liu et al., GCN 40607).
PRIME is a 1.8m telescope with 1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South Africa at the South African Astronomical Observatory (SAAO) (Kutyrev et al. 2023, Yama et al. 2023, Durbak et al. 2024).
We thank the Osaka University observers at PRIME and the staff at SAAO for their support with these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40624.
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TITLE: GCN CIRCULAR
NUMBER: 40623
SUBJECT: Fermi Gamma-ray Burst Monitor trigger 770675211/250603852 is not a GRB
DATE: 25/06/03 21:37:43 GMT
FROM: Lorenzo Scotton at UAH <lscottongcn(a)outlook.com>
L. Scotton (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:
"The Fermi Gamma-ray Burst Monitor (GBM) trigger 770675211/250603852 at 20:26:46.25 UT
on 03 June 2025, tentatively classified as a GRB, is in fact not due
to a GRB. This trigger is likely due to local …
[View More]particles."
View this GCN Circular online at https://gcn.nasa.gov/circulars/40623.
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TITLE: GCN CIRCULAR
NUMBER: 40622
SUBJECT: GRB 250601A: VLT/FORS2 Optical Observation
DATE: 25/06/03 19:31:34 GMT
FROM: Roberto Ricci at INAF-IRA <ricci(a)ira.inaf.it>
Roberto Ricci (U Rome), Yu-Han Yang (U Rome), Rosa L. Becerra (U Rome) and Eleonora Troja (U Rome) report on behalf of the ERC BHianca team:
We observed the field of GRB 250601A (Fermi GBM team GCN 40596; DeLaunay et al., GCN 40600) with the FORS2 imager on the ESO VLT UT1 (Antu). Observations began 29.8 hours …
[View More]after the trigger and were carried out in the R filter with an average airmass of ~2.3.
Our field covers the candidates reported by Swift/XRT (Page et al. GCN 40604, Salvaggio et al., GCN 40606) and EP/FXT (Liu et al., GCN 40607). Compared with the Legacy Survey DR10 (Dey et al. 2019) catalogue, we do not detect any uncatalogued source down to R>24 AB (3-sigma).
Further observations are planned.
We thank the staff at the VLT for the rapid execution of these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/40622.
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TITLE: GCN CIRCULAR
NUMBER: 40621
SUBJECT: GRB 250601A: Fermi GBM Observation
DATE: 25/06/03 15:42:16 GMT
FROM: Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma(a)nasa.gov>
V. Sharma (NASA-GSFC/UMBC) and C. Meegan (UAH) report on behalf of the
Fermi Gamma-ray Burst Monitor Team:
"At 17:29:35 UT on 1 Jun 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 250601A (trigger 770491780 / 250601729).
which was also detected by Swift/BAT-GUANO (J. DeLaunay et al. …
[View More]2025, GCN 40600)
and Swift/XRT (K.L. Page et al. 2025, GCN 40604).
The Fermi GBM on-ground location is consistent with the Swift/BAT-GUANO position.
The angle from the Fermi LAT boresight is 24 degrees.
The GBM light curve consists of main emission episode with a
duration (T90) of about 3 s (50-300 keV). The time-averaged
spectrum from T0-0.5 to T0+2.4 s is best fit by a power law
function with an exponential high-energy cutoff. The
power law index is -0.58 +/- 0.1 and the cutoff energy,
parameterized as Epeak, is 873 +/- 142 keV.
The event fluence (10-1000 keV) in this time interval is
(2.7 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1 s in the 10-1000 keV band is 4.9 +/- 0.2 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/"
View this GCN Circular online at https://gcn.nasa.gov/circulars/40621.
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