TITLE: GCN CIRCULAR
NUMBER: 37311
SUBJECT: GRB 240819A: Swift afterglow confirmation
DATE: 24/08/27 16:41:54 GMT
FROM: Antonino D'Ai' at IASF-PA <antonino.dai(a)inaf.it>
Antonino D’Ai, Elena Ambrosi (INAF/IASF-PA) report on behalf of the Swift-XRT team:
Swift performed a second epoch follow-up observation for Source2 (D’Avanzo et al., GCN 37218), the likely counterpart for the SVOM/Eclairs-detected X-ray transient GRB 240819A (Coleiro et al., GCN 37208). We collected 3.4 ks of …
[View More]Photon Counting (PC) mode data between T0+6.01 days and T0+7.67 days.
At the position of Source2 (previously detected at rate 11(+3.5, -2.9) x 10^-3 ct/sec), no source is detected with a 3-sigma upper limit of 3.5 x 10^-3 ct/sec.
The upper limit is evidence for the lightcurve fading of this source, confirming the afterglow association with GRB 240819A.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37311.
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TITLE: GCN CIRCULAR
NUMBER: 37310
SUBJECT: GRB 240825A: TNG optical photometry and spectroscopy
DATE: 24/08/27 10:19:29 GMT
FROM: Andrea Melandri at INAF-OAR <andrea.melandri(a)inaf.it>
A. Melandri (INAF-OAR), P. D'Avanzo, M. Ferro (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), D. B. Malesani (DAWN/NBI and Radboud Univ.), A. Rossi (INAF-OAS), A. Harutyunyan , and D. Carosati (INAF-TNG) report on behalf of the CIBO collaboration:
We observed the optical afterglow of long …
[View More]bright GRB 240825A (Gupta et al., GCN 37274; Fermi GBM team, GCN 37273; Di Lalla et al., GCN 37288; Frederiks et al., GCN 37302) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with the DOLoRes camera in spectroscopic mode. Observations were carried out with the LR-B grism, covering the range 3500-8000 AA. The observations consisted of one spectrum carried out at a mean time of Aug 25.9562 UT (~7.4 hours after the burst).
In the acquisition image we clearly detect the optical afterglow (Gupta et al., GCN 37274; Jiang et al. GCN 37275; Dutton et al. GCN 37276; Odeh et al. GCN 37277; Zhang et al. GCN 37278; Li et al. GCN 37280; Izzo & Malesani, GCN 37287; Lipunov et al. GCN 37289; Leonini et al. GCN 37291; Wu et al. GCN 37292; Brivio et al. GCN 32795; Odeh, GCN 37299) with a magnitude r~20, calibrated against the Pan-STARRS catalogue.
The spectrum has a low SNR. From a preliminary reduction, we identify a single absorption feature consistent with Mg II at a redshift of z~0.66, in agreement with the results reported by Martin-Carrillo et al. (GCN 37293).
View this GCN Circular online at https://gcn.nasa.gov/circulars/37310.
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TITLE: GCN CIRCULAR
NUMBER: 37309
SUBJECT: LIGO/Virgo/KAGRA S240825ar: Updated Sky localization
DATE: 24/08/27 07:48:46 GMT
FROM: Nihar.Gupte(a)aei.mpg.de
We have conducted further analysis of the LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S240825ar (GCN Circular 37268). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, …
[View More]distributed via GCN Notice, is available for retrieval from the GraceDB event page:
https://gracedb.ligo.org/superevents/S240825ar
For the Bilby.multiorder.fits,0 sky map, the 90% credible region is 351 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1311 +/- 309 Mpc (a posteriori mean +/- standard deviation).
For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/.
[1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. (2023) arXiv:2307.13380
View this GCN Circular online at https://gcn.nasa.gov/circulars/37309.
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TITLE: GCN CIRCULAR
NUMBER: 37308
SUBJECT: LIGO/Virgo/KAGRA S240825ar: Updated Sky localization
DATE: 24/08/27 07:48:43 GMT
FROM: Nihar.Gupte(a)aei.mpg.de
We have conducted further analysis of the LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S240825ar (GCN Circular 37268). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, …
[View More]distributed via GCN Notice, is available for retrieval from the GraceDB event page:
https://gracedb.ligo.org/superevents/S240825ar
For the Bilby.multiorder.fits,0 sky map, the 90% credible region is 351 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1311 +/- 309 Mpc (a posteriori mean +/- standard deviation).
For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/.
[1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. (2023) arXiv:2307.13380
View this GCN Circular online at https://gcn.nasa.gov/circulars/37308.
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TITLE: GCN CIRCULAR
NUMBER: 37307
SUBJECT: GRB 240825A: NUTTelA-TAO / BSTI Optical Limits
DATE: 24/08/27 04:22:06 GMT
FROM: Zhanat Maksut at Nazarbayev University <zhanat.maksut(a)nu.edu.kz>
Z. Maksut (NU), B. Grossan (UCB, NU), T. Komesh (NU), Z. Abdullayev (NU), M. Krugov (FAI) and E. Abdikamalov (NU) report on behalf of the Energetic Cosmos Laboratory:
The Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) observed the field of …
[View More]GRB 240825A, 3.7 h after receipt an automated GCN / BAT position alert, observing in Sloan g' and r' bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14).
We started observations of GRB 240825A (Gupta et al., GCN 37274; Jiang et al. GCN 37275; Dutton et al. GCN 37276; Odeh et al. GCN 37277; Zhang et al. GCN 37278; Li et al. GCN 37280; Izzo & Malesani, GCN 37287; Lipunov et al. GCN 37289; Leonini et al. GCN 37291; Wu et al. GCN 37292; Martin-Carrillo et al. GCN 37293) at UT 19:34:01 on 2024-08-25, 3.7 h after the BAT trigger. Observations were made in partly cloudy conditions. We report the following upper limit results:
start time t-t0(h) end time UL g' UL r' exposure_time (s)
-----------------------------------------------------------------------
19:34:01 3.7 19:43:01 19.31 19.38 10x60
start time is in UT. t-t0(h) gives the time since the trigger, in hours. UL gives the 5 sigma upper limit sensitivity in magnitudes, for images co-added to the given exposure time. Calibration was done with 4 Pan-STARRS catalog stars on our images.
----------------------------------
NU = Nazarbayev University, Nur-Sultan, 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. AP14870504). The NUTTelA-TAO Team acknowledges the support of the staff of the Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazakhstan.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37307.
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TITLE: GCN CIRCULAR
NUMBER: 37306
SUBJECT: GRB 240825A: GMG Continued Optical Observation on the Second Night
DATE: 24/08/27 02:34:35 GMT
FROM: wangbaiting(a)ynao.ac.cn
B.-T. Wang, F.-F. Song, R.-Z. Li, J. Mao, Y.-X. Xin, and J.-M. Bai (YNAO, CAS) report:
We observed the field of GRB 240825A (Gupta et al., GCN 37274, T0 at 2024-08-25T15:52:59) for the second time using the GMG-2.4m telescope at the Lijiang Observatory. The observation began at 2024-08-26T15:14:04, about 23.4 hours …
[View More]after the trigger. A optical counterpart was still observable.
The preliminary analysis results are shown as follows:
+----------------+------------+----------+--------------+----------------+
| Tmid-T0 [hr] | Exp. [s] | Filter | Mag | 5-sigma U.L. |
+================+============+==========+==============+================+
| 23.4 | 1800 | sdssr |21.34 +/-0.09 | 22.3 |
+----------------+------------+----------+--------------+----------------+
We acknowledge the staff at the Lijiang Observatory for their efforts in conducting the observation.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37306.
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TITLE: GCN CIRCULAR
NUMBER: 37305
SUBJECT: GRB 240824B: Ondrejov D50 optical limit
DATE: 24/08/26 21:44:19 GMT
FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek(a)asu.cas.cz>
Martin Jelinek, Jan Strobl, Alzbeta Malenakova, Rene Hudec and Cyril
Polasek (ASU CAS Ondrejov, CZ), report:
We observed the Swift-XRT localization (Kennea et al. GCN 37270) of the
Fermi/GBM (Fermi GBM Team GCN 37260, Sharma et al. GCN 37284), MAXI/GSC
(Nakajima et al. GCN 37261) and Swift/…
[View More]BAT (DeLaunay et al. GCN 37267)
detected GRB 240824A with the 50 cm robotic telescope (D50) of Ondrejov
observatory in Czech republic.
We obtained a set of 120 s Sloan-i' band exposures starting at 00:10 UT,
i.e. 10.985 h after the initial trigger. Consistently with Malesani et al.
(GCN 37281) and Zheng et al (GCN 37286), we do not detect any emission in
or near the Swift-XRT error box. The magnitude limit of our 2.15 h summed
integration with a mean time T-T0 12.067 h post burst is i' > 21.3 (AB).
View this GCN Circular online at https://gcn.nasa.gov/circulars/37305.
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TITLE: GCN CIRCULAR
NUMBER: 37304
SUBJECT: GRB 240825A: KAIT optical observations
DATE: 24/08/26 17:49:29 GMT
FROM: Weikang Zheng at UC Berkeley <weikang(a)berkeley.edu>
WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to GRB 240825A (Gupta et al., GCN 37274;
Fermi GBM team, GCN 37273) starting at 05:36 UT, Aug. 26th, about
13.73 hours …
[View More]after the bust. Observations were performed in the clear
(roughly R) filter, and the exposure time was 60s per image, with a
total of 31 images were obtained. We clearly detected the optical
afterglow (Gupta et al., GCN 37274; Jiang et al., GCN 37275; Dutton
et al., GCN 37276; Odeh et al., GCN 37277, Zhang et al., GCN 37278;
Li et al., GCN 37280, Izzo et al., GCN 37287; Lipunov et al., GCN
37289; Leonini et al., GCN 37291; Wu et al., GCN 37292; Martin-Carrillo
et al., GCN 37293; Brivio et al., GCN 37295; Kuin et al., GCN 37296;
Odeh et al., GCN 37299; Le Floc’h et al., GCN 37300; Guiffreda et al.,
GCN 37303) in our coadd image, which we measured its brightness of
20.8 +/- 0.2 mag at a mid time of ~14.04 hours after the burst,
calibrated to the Pan-STARRS1 catalog.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37304.
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TITLE: GCN CIRCULAR
NUMBER: 37303
SUBJECT: GRB 250825A: PRIME near-infrared detection
DATE: 24/08/26 17:12:41 GMT
FROM: Joe Durbak at UMD <gcn.joedurbak(a)gmail.com>
O. Guiffreda (UMD), J. Durbak (UMD), S. Atri (U Rome), A. S. Kutyrev (NASA/GSFC), E. Troja (U Rome), K. De (MIT), S. B. Cenko (NASA/GSFC)
Following the Swift BAT detection (GCN 37274), and Fermi GBM detection (GCN 37273), we observed the transient field in J and H filters with PRIME ~8 hours after FERMI & Swift …
[View More]detection.
At the position of the optical counterpart reported by Swift UVOT (GCN 37274), we detect an uncatalogued source in J and H bands. Using nearby VISTA Hemispherical Survey (VHS) stars for preliminary calibration we derive the following magnitudes, not corrected for Galactic extinction:
Filter | Mag(AB) | SNR | Seeing | Exp. time (s)
-------|--------------|------|--------|---------------
J | 18.9 +/- 0.2 | 17.5 | 2.1” | 600
H | 18.5 +/- 0.2 | 34.0 | 2.3” | 600
The J-band results are consistent with the REM detection of 17.7 +/- 0.3 Mag(Vega) (GCN 32795) taken an hour later.
Further observations are planned.
PRIME is a 1.8m telescope with 1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South Africa at the South African Astronomical Observatory (SAAO) (Kutyrev et al. 2023, Yama et al. 2023).
We thank the Osaka University observers at PRIME and the staff at SAAO for their support with these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37303.
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TITLE: GCN CIRCULAR
NUMBER: 37302
SUBJECT: Konus-Wind detection of GRB 240825A (bright/long)
DATE: 24/08/26 17:10:30 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 bright, long GRB 240825A (Fermi GBM detection:
Fermi GBM team, GCN 37273; Sharma & Meegan, GCN 37303;
Swift detection: Gupta et al., GCN 37274;
Fermi LAT …
[View More]detection: Di Lalla et al., GCN 37288;
AstroSat CZTI detection: Joshi al., GCN 37298)
triggered Konus-Wind (KW) at T0=57185.048 s UT (15:53:05.048).
The burst light curve shows a bright multi-peaked emission pulse,
which starts at ~T0 - 0.1 s, peaks around ~T0 + 0.256 s,
and has a total duration of ~2 s.
This pulse is followed by a weaker emission, which lasts
until ~T0 + 25 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240825_T57185/
As observed by Konus-Wind, the burst had
a fluence of (1.66 ± 0.08)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 0.256 s,
of (1.52 ± 0.07)x10^-4 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).
A time-averaged spectrum (measured from T0 to T0+28.16 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 = -0.79 (-0.04,+0.05),
the high energy photon index beta = -2.10 (-0.8,+0.06),
the peak energy Ep = 403 (-37,+40) keV,
chi2 = 99/97 dof.
A spectrum near the peak count rate (measured from T0 to T0+0.512 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 = -0.30 (-0.11,+0.12),
the high energy photon index beta = -2.30 (-0.09,+0.08),
the peak energy Ep = 405 (-36,+41) keV,
chi2 = 68/63 dof.
Assuming the redshift z=0.659 (Martin-Carrillo et al., GCN 37253)
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 (2.00 ± 0.96)x10^53 erg,
the isotropic peak luminosity L_iso to (3.04 ± 0.14)x10^53 erg/s,
the rest-frame peak energy Ep,i,z to (670 ± 60) keV.
With the obtained estimates, GRB 240825A 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/GRB240825_T57185/GRB240825A_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/37302.
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