TITLE: GCN CIRCULAR
NUMBER: 38890
SUBJECT: GRB 250101A: CMO RC-500 optical observations
DATE: 25/01/10 12:36:46 GMT
FROM: Nicolai Pankov at HSE, IKI RAS <colinsergesen(a)gmail.com>
N. Pankov (HSE, IKI RAS), A. Pozanenko (IKI RAS), A. Tarasenkov (INASAN), A. Moskvitin (SAO RAS)
report on behalf of a larger collaboration:
We performed optical observations of the field of GRB 250101A (Page et. al, GCN 38752; Li et. al, GCN 38753; Mohan et. al, GCN 38754; Zhu et. al, GCN 38755; …
[View More]Budnev et. al, GCN 38756; Wu et. al, GCN 38758; Zhu et. al, GCN 38759; Goad et. al, GCN 38761; Moskvitin et. al, GCN 38762; Odeh et. al, GCN 38763; Hu et. al, GCN 38764; Moskvitin et. al, GCN 38765; D'Avino et. al, GCN 38768; Escudero-Coca et. al, GCN 38769; Leonini et. al, GCN 38771; Dichiara et. al, GCN 38773; Zhang et. al, GCN 38774; Siegel, GCN 38775; Li et. al, GCN 38776; Komesh et. al, GCN 38777; Ghosh et. al, GCN 38779; Moskvitin et al., GCN 38780; Krimm et. al, GCN 38782; Komesh et. al, GCN 38790; Méndez-Lapido et. al, GCN 38810; Gupta et. al, GCN 38818; Ferro et. al, GCN 38831; Lin et. al, GCN 38837; Pankov et. al., GCN 38869) in the R filter with the 0.5-meter RC-500 telescope located at the Caucasus Mountain Observatory (CMO). The observations began on 2025-01-01 14:40:56 UT, i.e. ~1.28 hours since trigger. The preliminary light curve of the optical afterglow is available at http://grb.rssi.ru/GRB250101A/GRB250101A_RC50_KGO.png. After a typical power-law decay, the afterglow light curve demonstrates a re-brightening occurring at ~5 hr since burst, initially reported by Moskvitin et. al, GCN 38765.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38890.
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TITLE: GCN CIRCULAR
NUMBER: 38889
SUBJECT: EP250109a / GRB 250109A: refined EP-WXT analysis and EP-FXT follow-up observation
DATE: 25/01/10 09:43:01 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
R.-Z. Li (YNAO, CAS), X.-L. Chen (YNU), K. Chatterjee (YNU), Y.-L. Hua (PMO, CAS), H. Sun and Y. Liu (NAO, CAS) report on behalf of the Einstein Probe team:
Since 2025-01-09 06:17:58 (UTC, T0), EP250109a (Li et al., GCN 38864) has been detectable with high significance using the WXT …
[View More]onboard the EP, peaking about 60 seconds post-trigger. The observed peak flux in the 0.5–4 keV range is about 2.5 x 10^-9 erg/s/cm^2. The flux then rapidly decayed to background levels within 200 seconds post-trigger. The average 0.5-4 keV WXT spectrum can be fitted with an absorbed power law with a photon index of 2.9 +/- 1.0 (with a fixed Galactic equivalent hydrogen column density of 3.04 x 10^21 cm^-2). The derived lower limit of the intrinsic column density is 5.0 (-0.3, +0.4) x 10^21 cm^-2 when the redshift is fixed at 0. The derived average unabsorbed 0.5-4 keV flux is 2.5 (-1.2, +4.6) x 10^-9 erg/s/cm^2.
In addition to the follow-up observation, we conducted a follow-up observation of EP241217a using the FXT onboard the EP. The observation began at 2025-01-09T08:06:40 (UTC, 1.8 hours post-trigger), with an exposure time of approximately 4.2 ks. The average 0.5–4 keV FXT spectrum can be modeled with an absorbed power law, featuring a photon index of 1.9 (-0.7, +1.9) and a fixed Galactic equivalent hydrogen column density of 3.04 x 10^21 cm^-2). The derived lower limit of the intrinsic column density is about 3 x 10^20 cm^-2 when the redshift is fixed at 0. The estimated average unabsorbed 0.5–4 keV flux is about 4.9 (-1.2, +2.0) x 10^13 erg/s/cm^2.
The detection of EP-WXT/FXT (GCN 38864) and Fermi-GBM (GCN 38873 and GCN 38887), combined with the non-detection by Swift-XRT (GCN 38867), indicates that the flux of this transient has decreased very rapidly.
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38889.
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TITLE: GCN CIRCULAR
NUMBER: 38888
SUBJECT: EP250108a: EP-FXT follow-up observation
DATE: 25/01/10 07:45:32 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
R.-Z. Li (YNAO, CAS), X.-L. Chen (YNU), K. Chatterjee (YNU), Y.-L. Hua (PMO) and Y. Liu (NAOC) report on behalf of the Einstein Probe team:
We performed a follow-up observation of EP250108a using the FXT onboard the EP. The observation began at 2025-01-09T10:42:46 (UTC, about 22.2 hours post-trigger), with an exposure time …
[View More]of about 6 ks. No new uncatalogued X-ray sources were detected within the EP-WXT error circle (GCN 38861). The 5-sigma upper limit flux is about 3 x 10^-14 erg/s/cm^2 in the 0.5–10 keV range.
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38888.
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TITLE: GCN CIRCULAR
NUMBER: 38887
SUBJECT: GRB 250109A: Fermi GBM Observation
DATE: 25/01/10 06:40:17 GMT
FROM: Utkarsh Pathak at IIT Bombay <utkarshpathak.07(a)gmail.com>
U. Pathak (IITB) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 06:17:08.60 UT on 09 January 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 250109A (trigger 758096233/250109262).
which was also detected by EP-WXT and EP-FXT (Li et al. 2025, GCN …
[View More]38864).
The Fermi GBM on-ground location is consistent with the EP-FXT position.
A possible optical counterpart was also detected by SVOM/VT (Qiu et al. 2025, GCN 38872).
The angle from the Fermi LAT boresight is 72 degrees.
The GBM light curve consists of multiple weak spikes from a single emission episode
with a duration (T90) of about 15 s (50-300 keV). The time-averaged spectrum
from T0-8.2 to T0+9.2 s is best fit by a power law function.
The power law index is -1.57 +/- 0.05.
The event fluence (10-1000 keV) in this time interval is
(1.9 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.9 s in the 10-1000 keV band is 1.3 +/- 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/38887.
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TITLE: GCN CIRCULAR
NUMBER: 38886
SUBJECT: The EP-WXT trigger 01709130111 is likely a flaring star
DATE: 25/01/10 05:17:40 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
R.-Z. Li (YNAO, CAS), X.-L. Chen, K. Chatterjee (YNU) and H. Q. Cheng, Z. X. Ling (NAOC, CAS) report on behalf of the Einstein Probe team:
The EP-WXT trigger (ID 01709130111) on 2025-01-10 04:52:13 (UTC) is likely a stellar flare associated with a Low-mass Star RX J0429.3-3124. The estimated flux of the …
[View More]flare is around 1.6 x 10^-10 erg/s/cm^2 in 0.5-4.0 keV, corresponding to an X-ray luminosity of around 5.5 x 10^30 erg/s.
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38886.
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TITLE: GCN CIRCULAR
NUMBER: 38885
SUBJECT: EP250108a: NOT optical observations
DATE: 25/01/10 04:55:01 GMT
FROM: Dong Xu at NAOC/CAS <dxu(a)nao.cas.cn>
Z.P. Zhu, X. Liu, S.Y. Fu, S.Q. Jiang, J. An, D. Xu (NAOC) report on behalf of large collaboration:
We observed the field of EP250108a (Li et al., GCN 38861) using the Nordic Optical Telescope (NOT) equipped with ALFOSC. The observations were carried out in the g-/r-/i-/z- bands, starting at 22:16:55 UT on 2025-01-09, i.e., 1.4 …
[View More]days after the EP/WXT trigger.
The previously reported likely optical counterpart by LT (Eyles-Ferris et al., GCN 38878) is clearly detected in NOT individual images, and it has brightened from g = 20.79 +/- 0.05 at ~1.31 days post-trigger to g = 20.05 +/- 0.03 at ~ 1.44 days post-trigger.
The SED from g-/r-/i-/z- bands is opposite to the typical GRB optical afterglow, i.e., non-thermal power-law decay. Instead, it appears as quasi-thermal.
The quick brightening and the quasi-thermal SED make this source unlikely a conventional GRB afterglow. It would be more consistent with early behaviors of Fast Blue Optical Transients (FBOT) or novel Fast X-ray Transients by EP, if it is indeed associated with EP250108a.
In addition, we performed image subtraction on the stacked NOT g-/r- band images using Legacy Survey images as templates, and only the LT source is credible in the differencing images, down to limiting magnitudes of g > 22.7 and r > 23.2.
We acknowledge the excellent support from the NOT staff, in particular Samuel Grund Sorensen.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38885.
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TITLE: GCN CIRCULAR
NUMBER: 38884
SUBJECT: EP-WXT trigger EP250109a:Xinglong optical follow-up observations
DATE: 25/01/10 04:52:16 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
Report on behalf of the Xinglong collaboration: Junjie-Jin(NAOC), Haiyang-Mu(NAOC), Feng-Xiao(NAOC), Pengliang-Du(NAOC), Ying-Wu(NAOC), Zhou-Fan(NAOC), Hong-Wu(NAOC), Jie-Zheng (NAOC)
We observed the field of the X-ray transient, EP 250109a by the Xinglong 2.16-m telescope
located at Xinglong, Hebei,…
[View More] China. A total of 6 x 600 s N-band exposures were taken , with a median observation time of 2025-01-09 T13:06:56, approximately 6.5 hours after the EP trigger. No optical counterpart was detected, with a 5-sigma limiting magnitude of 22.48, calibrated with Pan-STARRS sources in the field.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38884.
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TITLE: GCN CIRCULAR
NUMBER: 38883
SUBJECT: GRB 250109a: GMG Optical Upper Limit
DATE: 25/01/10 03:05:29 GMT
FROM: wangbaiting(a)ynao.ac.cn
B.-T. Wang, R.-Z. Li, F.-F. Song, J. Mao, X.-L. Zhang and J.-M. Bai (YNAO, CAS) report:
We observed the field of EP250109a (EP team, GCN 38864; Kennea et. al, GCN 38867; Kumar et. al, GCN 38868; Lipunov et. al, GCN 38871; Fermi GBM team, GCN 38873)with the GMG-2.4m telescope at the Lijiang Observatory. The observation began at 2025-01-09T13:30:50 (…
[View More]UT), about 7.2 hours after the trigger.
No new uncataloged optical counterpart was detected within the EP/FXT error circle (GCN 38864).
The preliminary photometry is as follows:
-----------------------------------------------------------------------------
UT EXP(s) filter mag
-----------------------------------------------------------------------------
2025-01-09T13:30:50 1800 sdss-z >23.0
-----------------------------------------------------------------------------
The magnitudes were calibrated using nearby stars of Pan-STARRS DR1 field and without corrections for Galactic extinction.
We acknowledge the staff at the Lijiang Observatory for conducting the observation.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38883.
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TITLE: GCN CIRCULAR
NUMBER: 38882
SUBJECT: EP250109a: Swift/UVOT non-detection
DATE: 25/01/09 23:46:29 GMT
FROM: Sam Shilling at Lancaster University <shilling.sam(a)gmail.com>
S. P. R. Shilling (Lancaster U.), S. R. Oates (Lancaster U.), A. A. Breeveld (UCL-MSSL)
and N. P. M. Kuin (UCL-MSSL) report on behalf of the Swift UVOT team:
Swift/UVOT observed the field of EP250109a (Li et al., GCN 38864) for 938 seconds
in the U-band starting at 09:22:16 UT, 3 hours after the …
[View More]detection by Einstein Probe WXT.
No optical afterglow is detected within a 5" radius of the EP FXT position (Li et al., GCN 38864)
to a preliminary 3-sigma U-band upper limit of >20.6, calculated using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373).
The non-detection reported here is consistent with the non-detections reported in other optical
observations using the GOTO (Kumar et al., GCN 38868), MASTER (Lipunov et al., GCN 38871), and
the SVOM/VT in one of the two filters (Qiu et al., GCN 38872).
View this GCN Circular online at https://gcn.nasa.gov/circulars/38882.
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TITLE: GCN CIRCULAR
NUMBER: 38881
SUBJECT: Konus-Wind detection of GRB 250107D (short/hard)
DATE: 25/01/09 22:08:34 GMT
FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru>
D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin,
A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The short GRB 250107D (IPN triangulation: Kozyrev et al., GCN 38880)
triggered Konus-Wind (KW) at T0=19411.897 s UT (05:23:31.897).
The burst light curve shows a …
[View More]single, multi-peaked emission pulse
which starts at ~T0-0.112 s and has a duration of ~0.208 s.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB250107_T19411/
As observed by Konus-Wind, the burst had
the total fluence of 2.06(-0.34,+0.62)x10^-6 erg/cm^2
and a 16-ms peak energy flux, measured from T0-0.064 s,
of 1.99(-0.32,+0.59)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).
Since a major part of the burst emission was detected before the trigger time,
the time-averaged spectral analysis was performed using the KW 3-channel light curve data.
Modeling the 3-channel time-integrated spectrum (measured from T0-0.112 s to T0+0.096 s)
by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -0.40 (-0.32, + 0.41) and Ep = 897(-203,+453) keV.
All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.
View this GCN Circular online at https://gcn.nasa.gov/circulars/38881.
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