TITLE: GCN CIRCULAR
NUMBER: 38823
SUBJECT: GRB 250103B: Swift-XRT refined Analysis
DATE: 25/01/04 18:05:05 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
J.P. Osborne (U. Leicester), T. Sbarrato (INAF-OAB), P. D'Avanzo
(INAF-OAB), M.G. Bernardini (INAF-OAB), D.N. Burrows (PSU), M. A.
Williams (PSU), S. Dichiara (PSU), K.L. Page (U. Leicester) and P.A.
Evans report on behalf of the Swift-XRT team:
We have analysed 3.5 ks of XRT data for GRB 250103B, from 144 s to …
[View More]44.7
ks after the BAT trigger. The data comprise 31 s in Windowed Timing
(WT) mode with the remainder in Photon Counting (PC) mode. The best
available XRT position (using the promptly downlinked event data, the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue) is RA, Dec = 54.66413, -33.74945 which is equivalent to:
RA (J2000): 03 38 39.39
Dec(J2000): -33 44 58.0
with an uncertainty of 1.9 arcsec (radius, 90% confidence).
The light curve can be modelled with a power-law decay with a decay
index of alpha=3.9 (+/-0.4).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 4.2 (+0.7, -0.5). The
best-fitting absorption column is 6.3 (+6.6, -4.5) x 10^20 cm^-2, in
excess of the Galactic value of 1.0 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 2.5 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1.
A summary of the WT-mode spectrum is thus:
Total column: 6.3 (+6.6, -4.5) x 10^20 cm^-2
Galactic foreground: 1.0 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index: 4.2 (+0.7, -0.5)
If the light curve continues to decay with a power-law decay index of
3.9, the count rate at T+24 hours will be 2.5 x 10^-10 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.3 x
10^-21 (1.2 x 10^-20) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01278865.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38823.
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TITLE: GCN CIRCULAR
NUMBER: 38822
SUBJECT: GRB 250103B: LCO/1m optical afterglow candidate detection
DATE: 25/01/04 15:54:30 GMT
FROM: Damien Turpin at CEA-Saclay <dturpin-astro(a)hotmail.com>
D. Turpin (CEA/Irfu), A. Saccardi (GEPI/Obs. de Paris, CEA/Irfu), S. Basa (UAR Pytheas, OHP, LAM), D. B. Malesani (DAWN/NBI and Radboud Univ.), J. T. Palmerio (CEA/Irfu, GEPI/Obs. de Paris), S. Vergani (GEPI/Obs. de Paris), E. Le Floc'h (CEA Paris-Saclay, DAp/AIM) on behalf of a larger …
[View More]collaboration.
We observed the field of GRB 250103B detected by Swift (Eyles-Ferris et al. GCN 38796) and SVOM (Bouchet et al., GCN 38797) with the LCO 1.0m telescope at the Sutherland Observatory (SAAO) equipped with the Sinistro instrument. Our observation started at 2025-01-03T20:25:20.617 (T - TGRB ~ 4.68 hr) with 5 x 120s exposure using the sdss-r filter.
We marginally detect the optical afterglow candidate seen by SVOM/VT (Qiu et al., GCN 38813) and VLT (Habeeb et al., GCN 38820) from the difference image analysis between our stacked image and the Legacy Survey DR10 template image. At the position reported by VLT, we derived the following magnitude r = 22.32 +/- 0.26 (at Tmid - T0 = 4.78 hr) calibrated with the SkyMapper DR4 catalog and not corrected from the galactic extinction E(B-V): 0.01.
This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004719.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38822.
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TITLE: GCN CIRCULAR
NUMBER: 38822
SUBJECT: GRB 250103B: LCO/1m optical afterglow candidate detection
DATE: 25/01/04 15:54:30 GMT
FROM: Damien Turpin at CEA-Saclay <dturpin-astro(a)hotmail.com>
D. Turpin (CEA/Irfu), A. Saccardi (GEPI/Obs. de Paris, CEA/Irfu), S. Basa (UAR Pytheas, OHP, LAM), D. B. Malesani (DAWN/NBI and Radboud Univ.), J. T. Palmerio (CEA/Irfu, GEPI/Obs. de Paris), S. Vergani (GEPI/Obs. de Paris), E. Le Floc'h (CEA Paris-Saclay, DAp/AIM) on behalf of a larger …
[View More]collaboration.
We observed the field of GRB 250103B detected by Swift (Eyles-Ferris et al. GCN 38796) and SVOM (Bouchet et al., GCN 38797) with the LCO 1.0m telescope at the Sutherland Observatory (SAAO) equipped with the Sinistro instrument. Our observation started at 2025-01-03T20:25:20.617 (T - TGRB ~ 4.68 hr) with 5 x 120s exposure using the sdss-r filter.
We marginally detect the optical afterglow candidate seen by SVOM/VT (Qiu et al., GCN 38813) and VLT (Habeeb et al., GCN 38820) from the difference image analysis between our stacked image and the Legacy Survey DR10 template image. At the position reported by VLT, we derived the following magnitude r = 22.32 +/- 0.26 (at Tmid - T0 = 4.78 hr) calibrated with the SkyMapper DR4 catalog and not corrected from the galactic extinction E(B-V): 0.01.
This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004719.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38822.
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TITLE: GCN CIRCULAR
NUMBER: 38821
SUBJECT: GRB 250103A: Bassano Bresciano Observatory upper limit
DATE: 25/01/04 13:43:22 GMT
FROM: Ulisse Quadri at Bassano Bresciano Observatory <osservatoriobassano(a)gmail.com>
U.Quadri, L.Strabla and P.Madurini (Bassano Bresciano Astronomical Observatory)
Members of:
GRB/UAI - Gamma ray Burst section of Unione Astrofili Italiani.
AAVSO - American Association of Variable Star Observers.
GAC - Gruppo Astrofili Cremonesi.
In a large …
[View More]collaboration with:
M.G. Dainotti (National Astronomical Observatory of Japan),
Y. Niino (Tokyo University, Institute of Astronomy),
K. Kalinowski (Aarhus University, Department of Physics and Astronomy),
B. De Simone (Universita' degli Studi Di Salerno)
report:
We imaged the field of GRB 250103A detected by SVOM with the robotic telescope of (IAU station 565) Bassano Bresciano Observatory, Italy.
The observations started 7h 55m after the GRB trigger with our Newton telescope D=450 mm F/D=4.5.
We co-added 2 series of 100 exposures of 20 sec each.
Start T0+ End T0+ Rc lim. Err.
7h 46m 8h 27m 20.2 +/- 0.1
8h 28m 9h10m 20.2 +/- 0.1
We did not found any optical uncatalogued object within the SVOM error circle.
Magnitudes were estimated with the pan-STARRS cat and are derived using Lupton (2005) equations.
Not corrected for galactic dust extinction.
Reference:
http://www.osservatoriobassano.org
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38821.
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TITLE: GCN CIRCULAR
NUMBER: 38820
SUBJECT: GRB 250103B: VLT/X-shooter spectroscopic redshift z = 1.416
DATE: 25/01/04 10:20:17 GMT
FROM: Andrea Saccardi at CEA/Irfu <andrea.saccardi(a)cea.fr>
N. Habeeb (Leicester), A. Saccardi (CEA/Irfu), L. Izzo (INAF/OACn and DARK/NBI), B. Schneider (LAM), D. B. Malesani (DAWN/NBI and Radboud Univ.), G. Pugliese (UvA), A. L. Thakur (INAF-IAPS), A. de Ugarte Postigo (CNRS, OCA and LAM), Z.P. Zhu, J. An, D. Xu (NAOC) report on behalf of the …
[View More]Stargate collaboration:
We observed the optical afterglow (Qiu et al., GCN 38813) of GRB 250103B (Evans et al., GCN 38796; Bouchet et al., GCN 38797) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-25000 AA, and consist of 4 exposures by 1200 s each. The observation mid time was 2025 Jan 4.1283 UT (11.341 hr after the GRB).
In a 60-s acquisition image taken with the z filter (mid time Jan 4.104 UT), we clearly detect the afterglow (Qiu et al., GCN 38813). We measure the following coordinates (J2000):
RA = 03:38:39.335
Dec = -33:44:56.80
with an uncertainty of ~0.4". We measure a magnitude z = 22.5 +- 0.2 AB, calibrated against a single star in common with the Legacy Survey.
In a preliminary reduction of the spectra, we detect a continuum over the entire wavelength range. From the detection of multiple absorption features, which we interpret as due to Mg II and Fe II, we infer a common redshift of z = 1.416. At a consistent redshift, we also detect emission lines due to Halpha, [O III] 5007 AA and the [O II] 3726, 3729 AA doublet. We conclude that this is the redshift of GRB 250103B.
We note that, at the afterglow position, a faint object is seen in the Legacy survey, only confidently detected in the g band, which is likely the GRB host galaxy.
We acknowledge the expert support from the ESO observing staff at Paranal.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38820.
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TITLE: GCN CIRCULAR
NUMBER: 38819
SUBJECT: GRB 250103A: Swift-XRT observations
DATE: 25/01/04 09:24:43 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri
(INAF-OAR), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), J.A. Kennea
(PSU), D.N. Burrows (PSU), M. A. Williams (PSU) and P.A. Evans (U.
Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
…
[View More]SVOM/ECLAIRs-detected burst GRB 250103A, collecting 2.0 ks of Photon
Counting (PC) mode data between T0+24.1 ks and T0+47.2 ks.
One uncatalogued X-ray source has been detected within the estimated
3-sigma SVOM/ECLAIRs error region (454 arcsec), it is below the RASS
limit and shows no definitive signs of fading. However, it is
consistent with the position of the optical afterglow candidate (Li et
al. GCN 38795, Qiu et al. GCN 38802, Xu et al. GCN 38808). Details of
this source are given below:
Source 1:
RA (J2000.0): 22.0647 = 01:28:15.54
Dec (J2000.0): -5.0517 = -05:03:06.0
Error: 4.3 arcsec (radius, 90% conf.)
Count-rate: 0.0853 +/- 0.0076 ct s^-1
Distance: 172 arcsec from SVOM/ECLAIRs position.
Flux: (2.93 +/- 0.26)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)
The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021752.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38819.
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TITLE: GCN CIRCULAR
NUMBER: 38818
SUBJECT: GRB 250101A: 1.3m DFOT optical afterglow detection
DATE: 25/01/04 06:50:02 GMT
FROM: ANSHIKA GUPTA at ARIES <anshika05180(a)gmail.com>
Anshika Gupta, Amit K. Ror, Mamta, Kuntal Misra, and Shashi B. Pandey (ARIES) report:
We observed the field of GRB 250101A detected by Swift-BAT (GCN 38752) with the 1.3m Devasthal Fast Optical Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta Research Institute
of Observational …
[View More]Sciences (ARIES), India. The observations were started on 2025-01-01 at 17:14:04 UT, i.e., ~ 3.85 hours after the Swift-BAT trigger. We have taken multiple frames with an exposure time of 300 s in the R filter. We stacked the images after the alignment. We clearly detected optical afterglow in our stacked image within the error box of the enhanced Swift-XRT position by Goad et al. 2025 (GCN 38761). We obtained the following preliminary magnitude in the stacked image:
Date Start_UT T_start-T0 (hour) Filter Exp time (s) magnitude
==================================================================
2025-01-01 17:14:04 ~3.85 hour R 300*12 19.955+-0.003
Our detection is consistent with Page et al. 2025 (GCN 38752); Li et al. 2025 (GCN 38753); Mohan et al. 2025(GCN 38754); Zhu et al. 2025 (GCN 38755); Budnev et al. 2025 (GCN 38756); SVOM/C-GFT team 2025 (GCN 38758); Zhu et al. 2025 (GCN 38759); Moskvitin et al. 2025(GCN 38762, GCN 38765); Odeh et al. 2025 (GCN 38763); Hu et al. 2025 (GCN 39764); D'Avino et al. 2025(GCN 38768); Coca et al. 2025 (GCN 38769); Leonini et al. 2025(GCN 38771); Zhang et al. 2025 (GCN 38774); Siegel et al. 2025 (GCN 38775); Komesh et al. 2025 (GCN 38777); Ghosh et al. 2025 (GCN 38779); Moskvitin et al. 2025 (GCN 38780); Komesh et al. 2025 (GCN 38790); Bochenek et al. 2025 (GCN 38798); Lapido et al. 2025 (GCN 38810).
The magnitude is not corrected for the Galactic extinction in the direction of the burst.
Photometric calibration is performed using the standard stars from the USNO-B1.0 catalog. This circular may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38818.
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TITLE: GCN CIRCULAR
NUMBER: 38817
SUBJECT: GRB 241229A: 1.3m DFOT upper limit
DATE: 25/01/04 05:51:44 GMT
FROM: ANSHIKA GUPTA at ARIES <anshika05180(a)gmail.com>
Anshika Gupta, Amit K. Ror, Pranshu, Kuntal Mishra, and Shashi B. Pandey (ARIES) report:
We observed the field of GRB 241229A detected by SVOM (Liang et al 2024, GCN 38697) with the 1.3m Devasthal Fast Optical Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta Research Institute of Observational …
[View More]Sciences (ARIES), India. The observations were started on 2024-12-31 at 21:30:48 UT, i.e., ~ 2.89 days after the SVOM trigger. We have taken multiple frames with an exposure time of 300 s in the R filter. We stacked the images after the alignment. We could not detect the optical emission in our stacked image within the error box of SVOM/ECLAIRs (Liang et al. 2024, GCN 38697) and Swift-XRT (Williams et al. 2024, GCN 38728). We obtain the following 3-sigma upper limit in the stacked image:
Date Start_UT T_start-T0 (days) Filter Exp time (s) Magnitude
=========================================================
2024-12-31 21:30:48 ~2.89 R 300s*24 >21.4
The non-detection of the burst is consistent with the upper limits reported by Kumar et al. 2024, GCN 38705; Moskvitin et al. 2024, GCN 38731.
The magnitude is not corrected for the Galactic extinction in the direction of the burst. Photometric calibration is performed using the standard stars from the USNO-B1.0 catalogue. This circular may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38817.
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TITLE: GCN CIRCULAR
NUMBER: 38816
SUBJECT: GRB 241228B: 1.3m DFOT Optical observations
DATE: 25/01/04 05:44:27 GMT
FROM: Amit Kumar Ror at ARIES <mitturor77894(a)gmail.com>
Amit K. Ror, Anshika Gupta, Pranshu, Shashi B. Pandey, Kuntal Mishra
(ARIES) report:
We observed the field of GRB 241228B detected by the Fermi Gamma-ray Burst
Monitor (Fermi GBM team, GCN 38682), with the 1.3m Devasthal Fast Optical
Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta
…
[View More]Research Institute of Observational Sciences (ARIES), India. The
observations were started on 2024-12-30 at 17:50:12 UT, i.e., ~ 2.5 days
after the Fermi GBM trigger. We have taken multiple frames with an exposure
time of 300 s in the R filter. We stacked the images after the alignment.
We detected an optical emission in our stacked image at the position of the
optical counterpart candidate by GOTO collaboration (Amit et al. 2024, GCN
38684). We obtain the following preliminary magnitude in the stacked image:
Date Start_UT T_start-T0 (days) Filter Exp time (s) Magnitude
=========================================================
2024-12-30 17:50:12 ~2.56 R 300s*24 21.23 +/- 0.05
Our detection is consistent with Amit et al. 2024, GCN 38684; An et al.
2024, GCN 38687; Kumar et al. 2024, GCN 38691; Ortega-Casas et al. 2024,
GCN 38692; Ghosh et al. 2024, GCN 38702; An et al. 2024, GCN 38704; Volnova
et al. 2024, GCN 38709; Strobl et al. 2024, GCN 38715; Moskvitin et al.
2024, GCN 38733; Kumar et al. 2024, GCN 38739.
The magnitude is not corrected for the Galactic extinction in the direction
of the burst. Photometric calibration is performed using the standard stars
from the USNO-B1.0 catalogue. This circular may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38816.
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