TITLE: GCN CIRCULAR
NUMBER: 35840
SUBJECT: Swift BAT Triggers 1218081 and 1218082 are not astrophysical
DATE: 24/02/29 20:32:53 GMT
FROM: Jamie Kennea at Penn State <jak51(a)psu.edu>
J. A. Kennea (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:
Swift BAT Triggers 1218081 and 1218082 are due to an outage of
the star trackers, and are therefore not astrophysical.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35840.
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TITLE: GCN CIRCULAR
NUMBER: 35839
SUBJECT: GRB 240225B: further SAO RAS optical observations
DATE: 24/02/29 18:48:28 GMT
FROM: Moskvitin Alexander at SAO RAS <mosk(a)sao.ru>
A. S. Moskvitin, O. I. Spiridonova (SAO RAS)
report on behalf of the GRB follow-up team.
We observed the field of GRB 240225B (Nakajima et al., GCN 35796;
Evans, GCN 35797; Joshi et al., GCN 35798; D'Ai et al., GCN 35810;
Kawakubo et al., GCN 35811; Frederiks et al., GCN 35835)
with the SAO RAS 1m telescope Zeiss-1000 equipped with CCD-photometer.
We obtained 8 x 300 sec frames in the Rc band on Feb. 29,
17:11:52--18:03:46 UT (t_mid - T0 = 3.8903 days).
The OT (Gompertz et al., GCN 35805; Liu et al., GCN 35812;
Malesani et al., GCN 35819; Wise et al., GCN 35820;
Gompertz & Malesani, GCN 35824; Pankov et al., GCN 35826;
Ror et al., GCN 35830; Sasada et al., GCN 35831; Schneider et al.,
GCN 35832) is clearly detected in our stacked frame
with the brightness of R = 21.11 +/- 0.04.
The photometry is based on nearby SDSS stars (magnitudes converted
with Lupton 2005 equations).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35839.
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TITLE: GCN CIRCULAR
NUMBER: 35836
SUBJECT: GRB 240225B: Swift ToO observations
DATE: 24/02/29 15:26:30 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 ToO observation of the MAXI GRB 240225B.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021682
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the MAXI event. 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/35836.
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TITLE: GCN CIRCULAR
NUMBER: 35835
SUBJECT: Konus-Wind detection of GRB 240225B (long)
DATE: 24/02/29 14:46:36 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:
GRB 240225B (MAXI/GCS detection: Nakajima et al., GCN 35796;
AstroSat CZTI detection: Joshi al., GCN 35798)
triggered Konus-Wind (KW) at T0=72727.251 s UT (20:12:07.251),
i.e., ~3.5 min before the MAXI trigger.
The burst light curve shows a multi-peaked emission
pulse, which starts at ~T0 - 2 s, peaks around ~T0 + 6 s,
and has a total duration of ~35 s.
The emission is seen up to ~3 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240225_T72727/
As observed by Konus-Wind, the burst had
a fluence of (2.16 ± 0.35)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 6.144 s,
of (2.87 ± 0.41)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).
A time-averaged spectrum (measured from T0 to T0+41.216 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.37 (-0.14,+0.15),
the high energy photon index beta = -2.74 (-7.26,+0.43),
the peak energy Ep = 270 (-43,+64) keV,
chi2 = 107/97 dof.
A spectrum near the peak count rate (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.85 (-0.110,+0.10),
the high energy photon index beta = -2.43 (-0.55,+0.24),
the peak energy Ep = 287 (-47,+59) keV,
chi2 = 75/79 dof.
Assuming the redshift z=0.946 (Schneider et al., GCN 35832)
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 (5.38 ± 0.95)x10^52 erg,
the isotropic peak luminosity L_iso to (1.87 ± 0.27)x10^52 erg/s,
the rest-frame peak energy of the time-integrated spectrum Ep,i,z to ~525 keV,
and the rest-frame peak energy at the peak of the emission Ep,p,z to ~558 keV.
With the obtained estimates, GRB 240225B is inside 68% prediction bands for
both 'Amati' and '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/GRB240225_T72727/GRB240225B_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/35835.
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TITLE: GCN CIRCULAR
NUMBER: 35834
SUBJECT: GRB 240229A: BALROG localization (Fermi Trigger 730908432 / GRB 240229588)
DATE: 24/02/29 14:44:04 GMT
FROM: Jochen Greiner at MPE <jcgrog(a)mpe.mpg.de>
B. Biltzinger, T. Preis, J. Burgess & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
730908432 at 14:07:07 on 29 Feb. 2024 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).
The best-fit position is:
RA(2000.0) = 195.9 deg
Decl.(2000.0) = 16.3 deg
The 1 sigma statistical error radius is 1.7 deg.
We estimate an additional systematic error of 1 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB240229588/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB240229588/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB240229588/json
View this GCN Circular online at https://gcn.nasa.gov/circulars/35834.
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TITLE: GCN CIRCULAR
NUMBER: 35832
SUBJECT: GRB 240225B: VLT/X-shooter redshift
DATE: 24/02/29 10:36:12 GMT
FROM: Andrea Rossi at INAF <andrea.rossi(a)inaf.it>
B. Schneider (MIT), G. Pugliese (API), A. Rossi (INAF/OAS), J. Palmerio (GEPI/Obs. de Paris & IAP), D. B. Malesani (DAWN/NBI and Radboud Univ.), Z. Zhu (NAOC), D. Xu (NAOC), B. P. Gompertz (Birmingham), A. Saccardi (GEPI/Obs. de Paris) report on behalf of the Stargate collaboration:
We observed the field of the MAXI/GSC GRB 240225B (Nakajima et al., GCN 35796; see also Joshi et al. 2024, GCN 35798; Kawakubo et al., GCN 35811) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 4 exposures of 1200 s each. The observation mid-time is 02:29:56 UT on 2024 Feb 29 (~3.3 days after the MAXI trigger).
In grz images taken with the acquisition camera on Feb 29 01:37:53 UT, we clearly detect the optical afterglow (Gompertz et al., GCN 35805; Liu et al., GCN 35812; Malesani et al., GCN 35819; Wise et al., GCN 35820; Gompertz et al., GCN 35824; Pankov et al., GCN 35826; Moskvitin et al., GCN 35828; Mo et al., GCN 35829; Ror et al., GCN 35830; Sasada et al., GCN 35831), for which we measure a preliminary AB magnitude r ~ 21 (the absolute calibration is uncertain due to the low number of Pan-STARRS calibrators in our small FoV).
In a preliminary reduction of the spectra, we clearly detect a continuum over the entire wavelength range. From detection of multiple absorption features, which we interpret as being due to Fe II, Mg II, AlIII, Ca II, and Fe II*, we infer a common redshift of z = 0.946. We conclude this is the redshift of the burst. We also detect emission lines ([O II] and [O III] doublets, and H_alpha) at a consistent redshift, which we interpret as being due to the GRB host galaxy. As noted by Gompertz & Malesani (GCN 35824), the host galaxy is also detected in the Legacy Survey with r ~ 24.2 and a photometric redshift z ~ 0.9, which is consistent with the value we measured.
We acknowledge expert support from the ESO staff in Paranal, in particular Francesca Lucertini, Israel Blanchard and Thomas Rivinius.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35832.
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TITLE: GCN CIRCULAR
NUMBER: 35831
SUBJECT: GRB 240225B : MITSuME Akeno optical afterglow candidate detection
DATE: 24/02/29 10:30:01 GMT
FROM: Mahito Sasada at Tokyo Institute of Technology <sasada(a)hp.phys.titech.ac.jp>
M. Sasada, I. Takahashi, M. Niwano, S. Sato, N. Higuchi, S. Hayatsu, H. Takei, H. Seki, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 240225B (Nakajima et al. GCN 35796) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno.
The observation with a series of 60 sec exposures started at 2024-02-27 09:49:24 UT (1.565 days after the MAXI trigger). We stacked the images in good conditions. Here we report the g’- and Rc-band magnitudes of the optical candidate and upper limits by the aperture photometry.
T0+[days] | MID-UT | T-EXP[sec] | candidate magnitude and 5-sigma limits
----------------------------------------------------------------------------------------------------------------
1.638 | 2024-02-27 11:35:11 | 9480 | g’=19.78+/-0.13, Rc=19.53+/-0.10, Ic>19.7
----------------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the trigger
T-EXP: Total Exposure time
The position of the optical candidate is consistent with Gompertz et al., GCN 35805. The obtained magnitudes are broadly consistent with Gompertz et al., GCN 35805; Liu et al., GCN 35812; Malesani et al., GCN 35819; Wise et al., GCN 35820; Gompertz et al., GCN 35824; Pankov et al., GCN 35826; Moskvitin et al., GCN 35828; and Geoffrey et al., GCN 35829; and Ror et al., GCN 35830.
We used the PS1 catalog for flux calibration. The catalog magnitudes in PS1 g, r and i bands were converted to our g'-, Rc- and Ic-band magnitudes following Tonry et al. (2012), Table 6. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35831.
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