TITLE: GCN CIRCULAR
NUMBER: 39424
SUBJECT: GRB 250221A: Mondy optical observations
DATE: 25/02/22 12:25:53 GMT
FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com>
N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunlo (ISTP), A. Volnova
(IKI) report on behalf of IKI GRB FuN:
We observed the optical afterglow (Francile et al., GCN 39395; Watson et
al., GCN 39397; Melandri et al., GCN 39406; Shilling et al., GCN 39409; Guo
et al., GCN 39412; Muenter et al., GCN 39417; …
[View More]Palmerio et al., GCN 39418;
Pankov et al., GCN 39422) of the Swift GRB 250221A (Caputo et al., GCN
39396) with AZT-33IK telescope of Mondy observatory starting on 2025-02-21
(UT) 12:25:52 in R filter.
The afterglow is clearly detected. Preliminary photometry of the afterglow
in the stacked image is the following
Date UT start t-T0 Exp. Filter OT Err. UL(3sigma)
2025-02-21 12:25:52 0.38490 23x60 R 20.30 0.05 22.5
The photometry is based on nearby USNO-B1.0 (R2) stars.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39424.
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TITLE: GCN CIRCULAR
NUMBER: 39423
SUBJECT: Konus-Wind detection of GRB 250221A
DATE: 25/02/22 12:13:42 GMT
FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru>
D. Frederiks, A.Lysenko, A. Ridnaya, D. Svinkin, A. Tsvetkova,
M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report
GRB 250221A (Swift detection: Caputo et al., GCN 39396)
was detected by Konus-Wind (KW) in the waiting mode.
A Bayesian block analysis of the KW waiting mode data in the 20-400 keV …
[View More]band
reveals a ~12 sigma count-rate increase in the interval
from T0-1.5 s to T0+4.4 s where T0 = T0(BAT) = 03:34:37 UT.
The KW light curve of this burst is available
at http://www.ioffe.ru/LEA/GRBs/GRB250221A/
Modeling the time-integrated spectrum of the burst
by a power law with exponential cutoff (CPL) model
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.05 (-0.12, + 0.12) and Ep = 242(-22,+26) keV.
In the 10 keV -10 MeV band, standard for the KW analysis,
the burst fluence is (1.67 ± 0.09)x10^-6 erg/cm^2
and the 2.944 s peak energy flux is (2.97 ± 0.17)x10^-7 erg/cm^2/s.
Assuming the redshift z=0.768 (Palmerio et al., GCN 39418)
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 burst isotropic energy release E_iso to (2.8 ± 0.2)x10^51 erg,
the isotropic peak luminosity L_iso to (8.6 ± 0.5)x10^50 erg/s, and
the rest-frame peak spectral energy Ep,z to (428 ± 44) keV.
With the obtained estimates, GRB 250221A is a hard-spectrum outlier
(lies outside 90% prediction bands) of both 'Amati' and 'Yonetoku' relations 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/GRB250221A/GRB250221A_rest_frame.pdf
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/39423.
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TITLE: GCN CIRCULAR
NUMBER: 39422
SUBJECT: GRB 250221A: Assy optical observations
DATE: 25/02/22 11:10:50 GMT
FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com>
N. Pankov (HSE, IKI), V. Kim (FAI), M. Krugov (FAI), Y. Aimuratov (FAI),
A. Volnova(IKI), A. Pozanenko (IKI) report on behalf of IKI GRB FuN:
We observed the optical afterglow (Francile et al., GCN 39395; Watson et
al., GCN 39397; Melandri et al., GCN 39406; Shilling et al., GCN 39409; Guo
et al., GCN 39412; …
[View More]Muenter et al., GCN 39417; Palmerio et al., GCN 39418)
of the Swift GRB 250221A (Caputo et al., GCN 39396) with AZT-20 telescope
of Assy-Turgen observatory starting on 2025-02-21 (UT) 15:25:09.55 in r'
filter.
The afterglow is clearly detected. Preliminary photometry of the OT in the
stacked image is the following
Date UT start t-T0 Exp. Filter OT Err. UL(3sigma)
2025-02-21 15:25:09 0.50385 30x60 r' 20.90 0.05 22.8
The photometry is based on nearby PS1 stars.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39422.
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TITLE: GCN CIRCULAR
NUMBER: 39421
SUBJECT: EP250220a: FTW optical and NIR observations and upper limits
DATE: 25/02/22 11:03:18 GMT
FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de>
Malte Busmann (LMU), Brendan O’Connor (Carnegie Mellon U.), Daniel Gruen (LMU) and Antonella Palmese (Carnegie Mellon U.) report:
We observed the 90% EP-FXT localization area of EP250220a (Wang et al., GCN 39387; Hu et al., GCN 39420) with the Three Channel …
[View More]Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the r, i and J band simultaneously for 59 x 180 s starting at 2025-02-20T22:20:37 UT (0.84 days after the trigger) and 2025-02-21T20:54:36 UT (1.78 days after the trigger). We performed difference imaging with templates from the DESI Legacy Surveys in the r band and templates from PS1 in the i band as well as between our two epochs. We detect no new or evolving source in the EP-FXT localization area. The three sigma mean depths of our observations in the r band are
2025-02-20: r > 25.0 mag
2025-02-21: r > 24.4 mag.
This is consistent with the non-detections by Lipunov et al. (GCN 39338), Zhang et al. (GCN 39393), Eyles-Ferris et al. (GCN 39401), Guo et al. (GCN 39402) and Bochenek and Perley (GCN 39408).
The magnitudes are calibrated against the PS1 catalog and provided in the AB system. They are not corrected for Galactic extinction.
We thank Michael Schmidt from the staff of the Wendelstein Observatory for obtaining these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39421.
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TITLE: GCN CIRCULAR
NUMBER: 39420
SUBJECT: EP250220a: EP-FXT follow-up observations
DATE: 25/02/22 08:11:55 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
D. F. Hu (PMO, CAS), Y. L. Wang (NAOC, CAS), P. Y. Han, C. X. Zhang (HUST), B. B. Zhang (BNU), Y. Liu (NAOC, CAS) report on behalf of the Einstein Probe team:
Following the detection of the fast X-ray transient EP250220a (Wang et al., GCN 39387), we performed two follow-up observations with the Follow-up X-ray Telescope (…
[View More]FXT) on board the Einstein Probe (EP) mission.
The first FXT observation started at 2025-02-20 14:59:57 (UTC), about 13 hours after the WXT detection, with an exposure of ~ 3 ks. Within the WXT error circle, one faint X-ray source was detected by one of the FXT modules, at the position of R.A. = 113.4516 deg, DEC = 39.8098 deg (J2000), with an uncertainty of 10 arcsec in radius (90% C. L. statistical and systematic). The detection is relatively weak and the spectrum is not well fitted.
The second FXT observation started at 2025-02-21 10:12:09 (UTC), about 32 hours after the WXT detection, with an exposure of ~ 7 ks. No source was detected within the WXT error circle. Assuming a photon index of 1.1 and Galactic absorption with NH = 7.13 x 10^20 cm^-2, we derive an upper limit of 1.90e-14 erg/s/cm^2 (0.5-10 keV; 90% C. L.).
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/39420.
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TITLE: GCN CIRCULAR
NUMBER: 39419
SUBJECT: GRB 250219A: NUTTelA-TAO / BSTI Optical Limits
DATE: 25/02/22 07:47:55 GMT
FROM: Toktarkhan Komesh at Nazarbayev University <toktarkhan.komesh(a)nu.edu.kz>
T. Komesh (NU), Z. Abdullayev (NU), Z. Maksut (NU), D. Berdikhan (NU), B. Grossan (UCB, NU), M. Krugov (FAI) and E. Abdikamalov (NU) report on behalf of the Energetic Cosmos Laboratory:
We imaged the field of GRB 250219A with the Nazarbayev University Transient Telescope at Assy-…
[View More]Turgen Astrophysical Observatory (NUTTelA-TAO) starting at 21:54:17 UT on 2025-02-19, 6.0 hours after the SVOM/ECLAIRs trigger (F. Daigne et al., GCN 39376). Observations were made in clear conditions. No source consistent with the XRT (J. A. Kennea et al., GCN 39379) was detected. We report the following results:
start time t-t0 (minute) end time UL g' UL r' exposure_time (s)
------------ --------------------------------------------------
21:54:17 361 21:55:17 19.29 19.09 60
21:58:38 365 22:02:38 19.57 19.49 240
t is the middle time, t0 is the SVOM/ECLAIRs trigger time, t-t0 is given in minutes. UL gives the 5 sigma upper limit sensitivity in magnitudes, for images of the given exposure time. Calibration was done with 4 Pan-STARRS catalog stars on our images. No color or other corrections were applied to the values above.
-----------------------------------------------
NU = Nazarbayev University, Astana, Kazakhstan
UCB = University of California, Berkeley, USA
FAI = Fesenkov Astrophysical Institute, Kazakhstan
This research has been funded by the Science Committee of the Ministry of Science and Higher Education of the Republic of Kazakhstan (Grant No. AP26103591). The NUTTelA-TAO Team acknowledges the support of the staff of the Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazkhstan.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39419.
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TITLE: GCN CIRCULAR
NUMBER: 39418
SUBJECT: GRB 250221A: VLT/X-shooter redshift z = 0.768
DATE: 25/02/22 04:24:41 GMT
FROM: J. T. Palmerio at CEA-Saclay <jesse.palmerio(a)obspm.fr>
J. T. Palmerio (CEA/Irfu), A. Saccardi (CEA/Irfu), B. Rayson (U. Leicester), D. B. Malesani (DAWN/NBI and Radboud Univ.), A. J. Levan (Radboud and Warwick), N. R. Tanvir (U. Leicester) report on behalf of the Stargate collaboration:
We observed the optical afterglow (Francile et al., GCN 39395; Caputo …
[View More]et al., GCN 39396; Watson et al., GCN 39397; Melandri et al., GCN 39406; Shilling et al., GCN 39409; Guo et al., GCN 39412; Cotter et al. GCN 39413) of GRB 250221A (Caputo et al., GCN 39396) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-25000 AA, and consist of 4x600 s exposures. The slit’s position angle was set to cover the afterglow position as well as the nearby object to the NW (Watson et al., GCN 39397; Cotter et al. GCN 39413). The observation mid time was 2025 Feb 22.08 UT (~22.5 hr after the GRB).
In a preliminary reduction of the spectra, we detect two blended traces, corresponding to the afterglow and to the NW object. Spatially consistent with the afterglow position, we detect emission lines of H alpha, [O III] 5007, [O III] 4959, H beta, [O II] 3726/3729 at a common redshift of z = 0.768.
In the UBV arm, the trace is dominated by the afterglow continuum. Absorption features are detected corresponding to Mg II and Fe II, at a consistent redshift, which we suggest is the redshift of the burst.
We should note the presence of a possible, weak emission feature at 16,588 AA at the position of the afterglow trace. We are not able to identify this feature presently and a full reduction of the data is required to ascertain its reality.
At the position of the NW object, a faint, red continuum is detected in the VIS and NIR arms. No clear emission or absorption features are detected, and at the moment we can not provide a redshift determination for this object.
We thank Alan Watson (UNAM) for providing us with accurate coordinates of the afterglow. We acknowledge expert support from the ESO staff in Paranal, in particular Francesca Lucertini and Rodrigo Palominos.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39418.
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TITLE: GCN CIRCULAR
NUMBER: 39417
SUBJECT: GRB 250221A: GRANDMA/TAROT Detection
DATE: 25/02/22 03:00:44 GMT
FROM: Heather N. Muenter at UMN <hmuenter000(a)gmail.com>
H. Muenter (UMN), F. Magnani (CPPM), S. Antier (OCA/IJCLAB), Y. Rajabov (UBAI), C. Andrade (UMN), A. Klotz (IRAP), C. Limonta, Q. Andre, A. Durroux (OCA), M. Coughlin (UMN),S. Karpov (FZU), P. Hello (IJCLAB), P-A. Duverne (APC), T. Pradier (Unistra/IPHC), N. Guessoum (AUS) on behalf of the GRANDMA collaboration:
…
[View More]We imaged the field of GRB 250221A detected by SWIFT (GCN 39396) with the TAROT robotic telescope located at the European Southern Observatory, La Silla observatory, Chile.
The first image was taken 45 s post T0 and without filter is trailed (see the description in Klotz et al., 2006, A&A 451, L39). We detect the UVOT optical transient at r-mag 17 +/- 0.1 mag, 1.95 min post T0. We continuously detected the source for the first 30 min.
All the data have been reduced by a single data processing pipeline, STDPipe (Karpov et al., 2022). Images obtained in Johnson Cousin filters were calibrated using the Gaia DR3 and PS1 catalog.
We use the SkyPortal application (skyportal.io) to monitor our observational campaign (Coughlin et al. 2023).
GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).
View this GCN Circular online at https://gcn.nasa.gov/circulars/39417.
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TITLE: GCN CIRCULAR
NUMBER: 39416
SUBJECT: Fermi trigger No 761805304: Global MASTER-Net observations report
DATE: 25/02/22 02:32:22 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko,
A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin,
V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU),
O.Gress, N.Budnev (ISU),
C.Francile, …
[View More]F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
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) started inspect of the Fermi GRB250221.19 (trigger No 761805304,21h 13m 43.92s , -33d 13m 58.8s, R=10.22) errorbox 78509 sec after notice time and 78547 sec after trigger time at 2025-02-22 02:24:07 UT, with upper limit up to 17.8 mag. The observations began at zenith distance = 78 deg. The sun altitude is -24.1 deg.
The galactic latitude b = -44 deg., longitude l = 12 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2784950
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
78578 | 2025-02-22 02:24:07 | MASTER-SAAO | (20h 37m 17.51s , -38d 45m 28.5s) | C | 60 | 17.8 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39416.
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TITLE: GCN CIRCULAR
NUMBER: 39415
SUBJECT: Fermi Gamma-ray Burst Monitor trigger 761867337/250221909 is not a GRB
DATE: 25/02/22 01:10:05 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 761867337/250221909 at 21:48:52.46 UT
on 21 February 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/39415.
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