TITLE: GCN CIRCULAR
NUMBER: 37331
SUBJECT: GRB 240828A: Fermi-LAT detection
DATE: 24/08/29 01:53:02 GMT
FROM: Rahul Gupta at NASA GSFC <rahulbhu.c157(a)gmail.com>
R. Gupta (NASA GSFC), and N. Di Lalla (Stanford University) report on
behalf of the Fermi-LAT Collaboration:
On Aug 28, 2024, Fermi-LAT detected high-energy emission from GRB 240828A,
which was also detected by Fermi-GBM (trigger 746549711 / 240828622, GCN
37317), and AstroSat CZTI (GCN 37328).
The best LAT on-ground …
[View More]location is found to be:
RA, Dec = 225.49, 36.64 (J2000)
with an error radius of 0.30 deg (90 % containment, statistical error only).
This was 93 deg from the LAT boresight at the time of the GBM trigger: T0 =
14:55:06 UT.
The data from the Fermi-LAT show a significant increase in the event rate
that is spatially and temporally correlated with the GBM emission with high
significance. The photon flux above 100 MeV in the time interval 3500-6100
s after the GBM trigger is (8.2 +/- 3.8) E-7 ph/cm2/s. The estimated photon
index above 100 MeV is -2.1 +/- 0.4.
The highest-energy photon is a 1.7 GeV event which is observed ~ 5400
seconds after the GBM trigger.
A Swift ToO has been approved for this burst.
The Fermi-LAT point of contact for this burst is Niccolo' Di Lalla (
niccolo.dilalla(a)stanford.edu).
The Fermi-LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an
international collaboration between NASA and DOE in the U.S. and many
scientific institutions across France, Italy, Japan and Sweden.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37331.
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TITLE: GCN CIRCULAR
NUMBER: 37330
SUBJECT: GRB 240828A: Tiled Swift observations
DATE: 24/08/29 00:55:15 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
Fermi/LAT GRB 240828A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00127
Any uncatalogued X-ray sources detected …
[View More]in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT 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/37330.
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TITLE: GCN CIRCULAR
NUMBER: 37329
SUBJECT: LAT GRB240828.62: Global MASTER-Net observations report
DATE: 24/08/28 23:55:48 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,
G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij
(Lomonosov Moscow State University, SAI, …
[View More]Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gress, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez
(INAOE, Guillermo Haro Astrophysics Observatory),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich
(Blagoveschensk Educational State University)
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) was pointed to the LAT GRB240828.62 (trigger No 1080646295,15h 01m 58.08s , +36d 38m 27.6s, R=0.300833) errorbox 8021 sec after trigger time at 2024-08-28 17:08:48 UT, with upper limit up to 18.1 mag. Observations started at twilight. The observations began at zenith distance = 75 deg. The sun altitude is -11.1 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the LAT GRB240828.62 errorbox 17444 sec after trigger time at 2024-08-28 19:45:51 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 62 deg. The sun altitude is -30.3 deg.
The galactic latitude b = 61 deg., longitude l = 60 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2579813
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
8051 | 2024-08-28 17:08:48 | MASTER-SAAO | (14h 53m 16.72s , +37d 14m 30.3s) | C | 60 | 13.4 |
8552 | 2024-08-28 17:17:08 | MASTER-SAAO | (15h 03m 20.23s , +37d 15m 11.4s) | C | 60 | 17.4 |
9476 | 2024-08-28 17:32:33 | MASTER-SAAO | (14h 53m 14.86s , +37d 15m 50.5s) | C | 60 | 18.0 |
9555 | 2024-08-28 17:33:52 | MASTER-SAAO | (15h 03m 19.09s , +37d 16m 15.9s) | C | 60 | 18.1 |
10458 | 2024-08-28 17:48:54 | MASTER-SAAO | (15h 03m 19.97s , +37d 16m 48.7s) | C | 60 | 18.1 |
11211 | 2024-08-28 18:01:28 | MASTER-SAAO | (15h 00m 13.36s , +35d 22m 55.7s) | C | 60 | 14.0 |
17475 | 2024-08-28 19:45:51 | MASTER-Tavrida | (14h 53m 21.53s , +36d 03m 58.8s) | C | 60 | 18.0 |
18524 | 2024-08-28 20:03:20 | MASTER-Tavrida | (14h 53m 24.35s , +36d 04m 05.1s) | C | 60 | 17.7 |
19572 | 2024-08-28 20:20:48 | MASTER-Tavrida | (14h 53m 27.59s , +36d 03m 37.4s) | C | 60 | 17.8 |
22677 | 2024-08-28 21:12:34 | MASTER-Tavrida | (14h 55m 41.91s , +37d 23m 27.8s) | C | 60 | 17.6 |
23600 | 2024-08-28 21:27:56 | MASTER-Tavrida | (14h 55m 41.63s , +37d 22m 39.0s) | C | 60 | 17.6 |
24533 | 2024-08-28 21:43:29 | MASTER-Tavrida | (14h 55m 46.76s , +37d 23m 38.0s) | C | 60 | 13.5 |
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/37329.
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TITLE: GCN CIRCULAR
NUMBER: 37328
SUBJECT: GRB 240828A: AstroSat CZTI detection of a long burst
DATE: 24/08/28 21:17:13 GMT
FROM: Varun Bhalerao at IIT Bombay <varunb(a)iitb.ac.in>
S. Srijan (IITB), G. Waratkar (IITB), J. Joshi (IUCAA), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data with the CIFT framework (Sharma …
[View More]et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 240828A which was also detected by Fermi/GBM (Fermi GBM team, GCN Circ. 37317) and INTEGRAL/SPI-ACS (Trigger 10876).
The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2024-08-28 14:55:46 UTC. The measured peak count rate associated with the burst is 368 (+43, -46) counts/s above the background in the combined data of all quadrants, with a total of 4077 (+335, -387) counts. We caution that there is a 0.3 s readout dead time in CZT data during the burst which affects the calculated total counts. The local mean background count rate was 329 (+2, -3) counts/s. Using cumulative rates, we measure a T90 of 39.6 (+1.5, -1.0) s.
It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-08-28 14:55:45 UTC. The measured peak count rate is 1695 (+94, -66) counts/s above the background in the combined Veto data of all quadrants, with a total of 24765 (+699, -823) counts. The local mean background count rate was 1491 (+5, -6) counts/s. We measure a T90 of 39.6 (+0.5, -0.3) s from the cumulative Veto light curve.
CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.
CZTI GRB detections are reported regularly on the payload site at:
http://astrosat.iucaa.in/czti/?q=grb
View this GCN Circular online at https://gcn.nasa.gov/circulars/37328.
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TITLE: GCN CIRCULAR
NUMBER: 37327
SUBJECT: Fermi GRB 240828A: Bassano Bresciano Observatory upper limit
DATE: 24/08/28 20:57:33 GMT
FROM: Ulisse Quadri at Bassano Bresciano Observatory <osservatoriobassano(a)gmail.com>
U.Quadri, L.Strabla and P.Madurini (Bassano Bresciano Astronomical Observatory),
Members of:
GRB/UAI - Gamma ray Burst section of Unione Astrofili Italiani.
AAVSO - American Association of Variable Star Observers.
GAC - Gruppo Astrofili Cremonesi.
In a large …
[View More]collaboration with:
M.G. Dainotti (National Astronomical Observatory of Japan),
Y. Niino (Tokyo University, Institute of Astronomy),
K. Kalinowski (Aarhus University, Department of Physics and Astronomy),
B. De Simone (Universita' degli Studi Di Salerno)
report:
We performed optical follow-up observations of the GRB 240828A discovered by the Fermi satellite.
We used the Baker-Schmidt telescope (Diam 250mm F/3) of the (IAU station 565) Bassano Bresciano Astronomical Observatory (Italy).
The single Field of the telescope is 41.2' x 30.7'
To cover the uncertainty zone of the satellite position, we performed a mosaic of 9 images in order to cover a rectangle with sides of 2.1 x 1.5 degrees centered on the coordinates J2000 14h 36m, 35d 47'
We performed a total of 9 pointings to cover an area of 3.9 square degrees. For each pointing, 10 images were taken with duration of 20 seconds each.
The limiting magnitude is CR 17 (CR= Unfiltered with R zero point).
The sequence of pointing and the taking of images were automated by means of a telescope control software developed at our observatory.
The image analysis was performed using the subtraction method, with the template from POSS2/UKTSU Red images.
The observations started 4 hour after the GRB trigger.
For each field, we co-added 10 exposures of 20 sec each.
Start T0+ End T0+ CR lim
4.03 hour 4.81 hour 17
We did not found any credible optical counterpart in the error box of the
Fermi Satellite.
Magnitudes were estimated with the pan-STARRS cat
and are derived using Lupton (2005) equations.
Not corrected for galactic dust extinction.
Reference:
http://www.osservatoriobassano.org
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37327.
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TITLE: GCN CIRCULAR
NUMBER: 37326
SUBJECT: GRB 240825A: Upper limits from a neutrino search with IceCube
DATE: 24/08/28 20:37:55 GMT
FROM: Jessie Thwaites at IceCube/U Wisc-Madison <thwaites(a)wisc.edu>
The IceCube Collaboration (http://icecube.wisc.edu/) reports:
IceCube has performed a search for track-like muon neutrino events arriving from the direction of GRB 240825A (GCN Circular 37274 (Swift); 37301 (Fermi-GBM)). The search was performed at the position of the candidate …
[View More]optical counterpart reported by Swift-UVOT in a time range of -1 hour/+2 hours from the initial trigger reported by Swift-BAT (T0=2024-08-25 15:52:59 UTC) during which IceCube was collecting good quality data.
Zero track-like events are found to be coincident with the position of the GRB. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/ dE = 2.8 x 10^-2 GeV cm^-2 at 90% CL, under the assumption of an E^-2 power law. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum have energies in the approximate energy range between 1 TeV and 5 PeV.
A subsequent search was performed including 2 days of data centered on the Swift-BAT trigger (2024-08-24 15:52:59 UTC to 2024-08-26 15:52:59 UTC). In this case, we report a p-value of 1.0, consistent with background expectation. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/ dE = 3.0 x 10^-2 GeV cm^-2 at 90% CL, under the assumption of an E^-2 power law.
The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc(a)icecube.wisc.edu.
[1] IceCube Collaboration, R. Abbasi et al., ApJ 910 4 (2021)
View this GCN Circular online at https://gcn.nasa.gov/circulars/37326.
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TITLE: GCN CIRCULAR
NUMBER: 37325
SUBJECT: GRB 240819A as a likely X-Ray Flash
DATE: 24/08/28 19:55:10 GMT
FROM: sebastien.guillot(a)irap.omp.eu
SVOM/ECLAIRs commissioning team: Sebastien Guillot, Olivier Godet, Laurent Bouchet, Juliette Alaux (IRAP), Tais Maiolino (LUPM), Floriane Cangemi (APC), Stéphane Schanne, Frédéric Chateau, Nicolas Dagoneau, Hervé Le Provost (CEA), Karine Mercier, Marie-Claire Charmeau, Stefano Crepaldi (CNES)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (…
[View More]CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Jean-Luc Atteia (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Bing Zhang (UNLV)
report on behalf of the SVOM team:
Following the trigger of the X-ray transient, named GRB 240819A, by SVOM/ECLAIRs (Coleiro, et al., GCN 37208) at 2024-08-19T02:35:21.2 UT (T0), further analyses of the X-band data from ECLAIRs indicate a rather soft event with most photons below 40 keV (signal-to-noise of ~10 for events between 4 to 40 keV; versus S/N < 4 for events above 40 keV).
In addition, observations by Swift-XRT at T0+0.23 days and T0+0.31 days (D'Avanzo, et al., GCN 37218) and at T0+6.01 days (D’ai, et al. GCN 37311) revealed a fading X-ray source from 11(+3.5, -2.9) x 10^-3 ct/sec to a 3-sigma upper limit of 3.5 x 10^-3 ct/sec. Therefore, the X-ray afterglow of GRB 240819A is likely source 2 (from D’ai, et al. GCN 37311), localized at RA=310.9464 (20:43:47.14) and Dec.=+49.5140 (+49:30:50.3) with a 90% c.l. error circle of 5.8 arcseconds.
The identification of the fading afterglow and the spectral softness of the event described above, are indicative of a likely X-Ray Flash (XRF, i.e., a soft GRB with lower luminosity and located at a closer distance than typical GRBs), rather than a Galactic transient.
We encourage deep optical follow-up observations to attempt the detection of a possible supernova that could be associated with this event. We caution that, due to the low galactic latitude of the transient, a potential supernova will undergo strong visible extinction (Av ~ 5).
View this GCN Circular online at https://gcn.nasa.gov/circulars/37325.
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TITLE: GCN CIRCULAR
NUMBER: 37324
SUBJECT: GRB 240828B: Swift ToO observations
DATE: 24/08/28 18:48:57 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 SVOM/ECLAIRs GRB 240828B.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021706
Any uncatalogued X-ray sources detected in this analysis will be
reported …
[View More]on this website and via GCN COUNTERPART notices. These are
not necessarily related to the SVOM/ECLAIRs 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/37324.
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TITLE: GCN CIRCULAR
NUMBER: 37323
SUBJECT: GRB 240821A: PRIME near-infrared observations
DATE: 24/08/28 16:59:13 GMT
FROM: Joe Durbak at UMD <gcn.joedurbak(a)gmail.com>
J. Durbak (UMD), E. Troja (U Rome), S. Atri(U Rome), A. S. Kutyrev (NASA/GSFC), O. Guiffreda (UMD), K. De (MIT), S. B. Cenko (NASA/GSFC)
Following the SVOM localization (GCN 37220), we observed the field of GRB 240821A in H-band with PRIME ~30 hours after the trigger. The total exposure time was 1800s.
At the …
[View More]position of the candidate optical counterpart (GCN 37319), we detect a source with H~20 mag, calibrated versus nearby 2MASS stars and not corrected for Galactic extinction.
Further observations to assess variability 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/37323.
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TITLE: GCN CIRCULAR
NUMBER: 37322
SUBJECT: GRB 240825A: VLA detection
DATE: 24/08/28 16:53:27 GMT
FROM: corinna.pena(a)utah.edu
C. Peña (University of Utah), T. Laskar (University of Utah), G. Schroeder (Northwestern University), K. D. Alexander (University of Arizona), C. Christy (University of Arizona), E. Berger (Harvard University), R. Chornock (UC Berkeley), W. Fong (Northwestern University), R. Margutti (UC Berkeley), and P. Schady (University of Bath) report on behalf of a …
[View More]larger collaboration:
“We observed GRB 240825A (Gupta et al., GCN 37274) with the Very Large Array (VLA) at multiple frequencies beginning on 2024 August 27 at 07:10 UT (39.3 hours post burst).
In preliminary analysis, we detect the radio counterpart (Laskar et al., GCN 37314) at 8.6 GHz with a flux density of F ~ 0.3mJy at the position:
RA(J2000) = 22:58:17.27 +/- 0.01”
Dec(J2000) = +01:01:36.78 +/- 0.02”
This is consistent with the X-ray position (Evans et al., GCN 37290), optical position (Gupta et al., GCN 37274; Jiang et al., GCN 37275; Dutton et al., GCN 37276; Odeh et al., GCN 37277; Li et al., GCN 37280; Evans et al., GCN 37290; Leonini et al., GCN 37291; Kuin et al., GCN 37296), and radio position (Laskar et al., GCN 37314). Further observations are planned.
We thank the VLA staff for scheduling and executing these observations.”
View this GCN Circular online at https://gcn.nasa.gov/circulars/37322.
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