TITLE: GCN CIRCULAR
NUMBER: 39375
SUBJECT: Konus-Wind detection of GRB 250215A / EP250215a
DATE: 25/02/19 15:45:03 GMT
FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru>
D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova,
A. Lysenko, A. Ridnaia, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 250215A / EP250215a
(Fermi-GBM detection: The Fermi GBM team, GCN 39327;
Scotton and Meegan, GCN 39342;
EP-WXT detection: Wang et al., GCN 39329;
…
[View More]INTEGRAL-SPI-ACS detection: Barria et al., GCN 39331;
AstroSat-CZTI detection: Tembhurnikar et al., GCN 39334;
SVOM/GRM detection: Zheng et al., GCN 39335)
triggered Konus-Wind at T0=09130.387 s UT (02:32:10.387).
The burst light curve shows a multipeaked structure
which starts at ~T0-14 s and has a total duration of ~22 s.
The emission is seen up to ~1 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB250215_T09130/
As observed by Konus-Wind, the burst
had a fluence of 8.33(-1.97,+2.51)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.054 s,
of 5.12(-1.37,+1.66)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
Since a major part of the burst emission was detected
before the trigger time and the burst shows a minor spectral evolution,
we use the spectrum measured from T0 to T0+8.448 s
to estimate the total burst fluence.
This spectrum is best fit in the 20 keV - 20 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.03(-0.54,+0.69),
the high energy photon index beta = -2.31(-1.22,+0.30),
the peak energy Ep = 130(-36,+80) keV
(chi2 = 80/97 dof).
The spectrum near the maximum count rate
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.14(-0.74,+3.47),
the high energy photon index beta = -2.35(-0.68,+0.29),
the peak energy Ep = 118(-51,+53) keV
(chi2 = 18/17 dof).
Assuming the redshift z=4.61 (Sanchez-Ramirez et al., GCN 39343)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is 3.35(-0.79,+1.01)x10^53 erg,
the peak luminosity L_iso is 1.15(-0.31,+0.37)x10^54 erg/s,
the rest-frame peak energy of the time-averaged spectrum
Ep,i,z is 660(-250,+298) keV.
With the obtained estimates, GRB 250215A is inside 68% prediction band for
the 'Amati' and 90% - for the 'Yonetoku' relations derived for the sample of >300 long
KW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),
see http://www.ioffe.ru/LEA/GRBs/GRB250215_T09130/GRB250215A_rest_frame.pdf
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/39375.
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TITLE: GCN CIRCULAR
NUMBER: 39374
SUBJECT: SVOM/sb25021804: COLIBRÍ/DDRAGO Confirmation of Variability
DATE: 25/02/19 14:04:46 GMT
FROM: Alan Watson at UNAM <alan(a)astro.unam.mx>
Damien Dornic (CPPM), Antonio de Ugarte Postigo (LAM), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Dalya Akl (AUS), Camila Angulo (UNAM), Sarah Antier (OCA), Jean-Luc Atteia (IRAP), Rosa L. Becerra (U Roma), Nathaniel R. Butler (ASU), Jean-Grégoire Ducoin (CPPM), Francis …
[View More]Fortin (IRAP), Noémie Globus (UNAM), Kin Ocelotl López (UNAM), Francesco Magnani (CPPM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), and Benjamin Schneider (LAM) report:
We imaged the field of SVOM/ECLAIRs trigger sb25021804 (Wang et al., GCN 39363) with the DDRAGO wide-field imager on the COLIBRÍ telescope at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir in Mexico.
We observed from 2025-02-19 06:23 to 09:00 UTC (23.1 to 25.7 hours after the trigger) and obtained 100 minutes of exposure in the r filter. The data were coadded with custom software and analyzed in STDWeb/STDPipe (Karpov 2021), with photometric calibration against Pan-STARRS DR1. Our photometry is in the AB system and is not corrected for Galactic extinction.
For the X-ray bright QSO WISEA J130010.60+280749.7, suggested by Eyles-Ferris et al. (GCN Circ. 39372) as a possible counterpart of the ECLAIRs source, we measure a magnitude of
r = 19.95 +/- 0.01
In our observation on the previous night, reported in de Ugarte Postigo et al. (GCN Circ. 39364), we measure
i = 19.98 +/- 0.04
Our magnitudes are about 0.3 magnitudes above the mean magnitudes reported in SDSS DR6 and PanSTARRS DR1. This confirms the excess reported by Eyles-Ferris et al. (GCN Circ. 39372) and strengthens their suggestion that this QSO might be related to the SVOM trigger.
We warmly thank the COLIBRÍ and DDRAGO engineering teams and the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39374.
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TITLE: GCN CIRCULAR
NUMBER: 39373
SUBJECT: GRB 250217C: Swift-XRT observations
DATE: 25/02/19 13:51:26 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR), B.
Sbarufatti (INAF-OAB), C. Salvaggio (INAF-OAB), J.A. Kennea (PSU), D.N.
Burrows (PSU), M. A. Williams (PSU), J.P. Osborne (U. Leicester) and
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up …
[View More]observations of the IPN-detected
burst GRB 250217C in a series of observations tiled on the sky. The
total exposure time is 3.5 ks, distributed over 7 tiles; the maximum
exposure at a single sky location in the tiling was 1.2 ks. The data
were collected between T0+69.9 ks and T0+98.0 ks, and are entirely in
Photon Counting (PC) mode.
No uncatalogued X-ray sources have been detected. The 3-sigma upper
limit in the field (not including the regions where the tiles overlap)
ranges from ~0.01 to ~0.03 ct s^-1, corresponding to a 0.3-10 keV
observed flux of 5.3e-13 to 1.3e-12 erg cm^-2 s^-1 (assuming a typical
GRB spectrum).
Three previously-catalogued X-ray sources have been detected, however
their status as catalogued objects makes them unlikely to be the
afterglow.
The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00133.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39373.
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TITLE: GCN CIRCULAR
NUMBER: 39372
SUBJECT: SVOM/sb25021804: QSO variability in Liverpool Telescope observations
DATE: 25/02/19 11:37:18 GMT
FROM: Rob Eyles-Ferris at U of Leicester <raje1(a)leicester.ac.uk>
R. A. J. Eyles-Ferris, P. T. O’Brien and R. L. C. Starling (U of Leicester) report on behalf of a larger collaboration:
We observed the field of the SVOM/ECLAIRs transient sb25021804 (Wang et al., GCN 39363) in four pointings covering ~87% of the error area using the IO:O …
[View More]on the 2m Liverpool Telescope. We obtained 4x150s exposures per pointing in the SDSS g’ filter starting at 2025-02-19 04:59:09 UT, approximately 21.7 hours after the SVOM/ECLAIRs detection.
We performed image subtraction on the stacked images using reference images from Pan-STARRS. We identify a residual at RA, Dec 195.044, 28.130 which corresponds to the X-ray bright QSO WISEA J130010.60+280749.7, about 3.4 arcmin from the SVOM ECLAIRs position reported by Wang et al., GCN 39363. We performed PSF photometry on the stacked image and find g’ = 20.09 +/- 0.11 calibrated to Pan-STARRS and not corrected for Galactic extinction. This is ~0.5 mag brighter than the magnitude catalogued in Pan-STARRS DR2 and we suggest sb25021804 is related to this variability.
We find no other obvious residuals in the subtracted images to a 3-sigma limiting magnitude of ~21.5.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39372.
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TITLE: GCN CIRCULAR
NUMBER: 39371
SUBJECT: GRB 250217C: COLIBRÍ/DDRAGO Upper Limits on the Optical Counterpart
DATE: 25/02/19 07:20:09 GMT
FROM: Alan Watson at UNAM <alan(a)astro.unam.mx>
Alan M. Watson (UNAM), Antonio de Ugarte Postigo (LAM), Eleonora Troja (U Roma), Rosa L. Becerra (U Roma), Simone Dichiara (PSU), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Dalya Akl (AUS), Camila Angulo (UNAM), Sarah Antier (OCA), Jean-Luc Atteia (IRAP), Nathaniel R. Butler (ASU), …
[View More]Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), Noémie Globus (UNAM), Kin Ocelotl López (UNAM), Francesco Magnani (CPPM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), and Benjamin Schneider (LAM) report:
We imaged the IPN 3-sigma error box of GRB 250217C (Fermi GBM Team, GCN Circ. 39357, Tembhurnikar et al., GCN Circ. 39359, Kozyrev et al., GCN Circ. 39365) with the DDRAGO wide-field imager on the COLIBRÍ telescope at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir in Mexico.
We used three pointings that, combined with the 26 arcmin field of COLIBRÍ/DDRAGO, cover more than 95% of the IPN error box.
We observed from 2025-02-19 02:51 to 04:18 UTC (27.0 to 28.4 hours after the trigger) and obtained 20 minutes of exposure at each pointing in the i filter. The data were coadded with custom software and analyzed in STDWeb/STDPipe (Karpov 2021), with photometric calibration against Pan-STARRS DR1 and image subtraction against Pan-STARRS DR2. Our photometry is not corrected for Galactic extinction.
We do not detect any likely optical counterpart to a 5-sigma limit of
i > 22.7
Our non-detections are consistent with the shallower limits reported by Becerra et al. (GCN Circ. 39370) and with the lack of a bright X-ray candidate counterpart in the tiled Swift/XRT ToO observations reported by Evans et al. (GCN Circ. 39368).
We warmly thank the COLIBRÍ and DDRAGO engineering teams and the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39371.
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TITLE: GCN CIRCULAR
NUMBER: 39370
SUBJECT: GRB 250217C: DDOTI Upper Limits on the Optical Afterglow
DATE: 25/02/19 05:38:12 GMT
FROM: Rosa L. Becerra at Tor Vergata, Roma <rosa.becerra(a)roma2.infn.it>
Rosa L. Becerra (U Roma), Alan M. Watson (UNAM), Simone Dichiara (Penn State University), Eleonora Troja (U Roma), Camila Angulo Valdez (UNAM), Nat Butler (ASU), Tsvetelina Dimitrova (ASU), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), Océlotl López (UNAM), and Margarita …
[View More]Pereyra (UNAM) report:
We observed the field of GRB 250217C detected by Fermi/GBM (Fermi GBM Team et al., GCN 39357), AstroSat CZTI (Tembhurnikar et al., GCN 39359), and IPN (Kozyrev et al., GCN 39365), with the DDOTI/OAN wide-field imager at the Observatorio Astronomico Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) on the night of 2025-02-19 UTC.
DDOTI observed the whole IPN error box reported by Kozyrev et al. (GCN 39365) from 03:31 UTC to 04:37 UTC (from T+27.6 to T+28.7 hours after the event) with a total exposure of 48 minutes, down to a 5-sigma limiting magnitude of w = 21.1.
Comparing our observations to the USNO-B1 and PanSTARRS PS1 DR2 catalogues, we
detect no uncatalogued sources within the observed field to our 5-sigma limit.
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39370.
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TITLE: GCN CIRCULAR
NUMBER: 39369
SUBJECT: GRB 250217C: SVOM/GRM observation
DATE: 25/02/19 03:52:28 GMT
FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn>
SVOM/GRM team: Chen-Wei Wang, Shi-Jie Zheng, Shao-Lin Xiong, Yue Huang, Shuang-Nan Zhang (IHEP)
SVOM/ECLAIRs team: Frédéric Piron (LUPM), Nicolas Dagoneau (CEA), Maria-Grazia Bernardini (INAF-OAB), Jean-Luc Atteia, Sébastien Guillot (IRAP)
report on behalf of the SVOM team:
SVOM/GRM was triggered in-flight by a short burst …
[View More]GRB 250217C (sb25021704) at 2025-02-17T23:54:41.900 UTC (T0), which was also observed by Fermi/GBM (Fermi GBM team, GCN #39357), AstroSat (M. Tembhurnikar et al., GCN #39359), Konus-Wind, HEND/Mars and INTEGRAL SPI-ACS (A.S. Kozyrev et al., GCN #39365).
With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multi-pulses with a T90 of about 0.42 +0.07/-0.22 seconds in the 15-5000 keV.
The time-averaged spectrum from T0-0.2 to T0+0.2 s could be fit by a Band function with alpha = -0.61 +/- 0.3, beta = -1.87 +/- 0.07 and Epeak = 77 +20/-11 keV. The event fluence (10-1000 keV) in this time interval is (1.40 +/- 0.71)E-06 erg/cm^2.
The SVOM/GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb250217C.png
In addition, the position of this burst, as determined by Fermi/GBM (Fermi GBM Team, GCN #39357), is located at about 50 degrees from the SVOM optical axis, right at the edge of the ECLAIRs field of view.
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/39369.
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TITLE: GCN CIRCULAR
NUMBER: 39368
SUBJECT: GRB 250217C: Tiled Swift observations
DATE: 25/02/18 19:30:39 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a series of observations, tiled on the sky, of the
IPN GRB 250217C. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00133
Any uncatalogued X-ray sources detected in …
[View More]this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the IPN event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39368.
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TITLE: GCN CIRCULAR
NUMBER: 39367
SUBJECT: GRB 250217C: Fermi GBM Observation
DATE: 25/02/18 18:55:40 GMT
FROM: Jacob Smith at Fermi-GBM Team <jrs0118(a)uah.edu>
Jacob Smith (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:
At 23:54:41.80 UT on 17 February 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 250217C (trigger 761529286/250217996).
which was also detected by AstroSat (M. Tembhurnikar, et al. 2025, GCN 39359) and IPN …
[View More]triangulation (A.S. Kozyrev, et al. 2025, GCN 39365).
The Fermi GBM on-ground location is consistent with the IPN triangulation.
The angle from the Fermi LAT boresight is 100 degrees.
The GBM light curve consists of a double emission episode with a duration (T90)
of about 0.35 s (50-300 keV). The time-averaged spectrum
from T0-0.06 to T0+0.38 s is best fit by
a Band function with Epeak = 85 +/- 13 keV,
alpha = -0.2 +/- 0.3, and beta = -1.83 +/- 0.04.
The event fluence (10-1000 keV) in this time interval is
(1.68 +/- 0.05)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band is 62 +/- 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/39367.
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TITLE: GCN CIRCULAR
NUMBER: 39366
SUBJECT: GRB 250215A / EP250215A: Encouraging Follow-up Observations of a BdHN I with a Rest-Frame Duration 2.3 s at z=4.61
DATE: 25/02/18 17:28:03 GMT
FROM: Remo Ruffini at ICRA <ruffini(a)icra.it>
R. Ruffini, D. Berkimbayev, G. Vereshchagin, R. F. Mohideen Malik, N. Shynggyskhan, M.T. Mirtorabi, J.A. Rueda, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
GRB 250215A / EP250215A was detected by Fermi (GCN 39327), Einstein Probe (GCN …
[View More]39329), and SVOM (GCN 39333) at a redshift of z = 4.61 (GCN 39343). The burst duration is 2.3 s in the rest frame, corresponding to T_{90} = 13.4 s in the observer's frame (GCN 39342). The isotropic energy release is 3 \times 10^{53} erg, consistent with a BdHN I classification. This event shares similarities with GRB 220101A (GCN 37964), GRB 221009A (GCN 32828), and GRB 240825A (GCN 37536). Extended follow-up multi-wavelength observations are encouraged to fully characterize the BdHN I episodes: optical data for pulsar identification, X-ray observations to track the afterglow evolution, and GeV measurements to constrain the black hole energy.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39366.
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