TITLE: GCN CIRCULAR
NUMBER: 35296
SUBJECT: GRB231115A: TURBO Pre-Burst Optical Upper Limits
DATE: 23/12/06 21:42:43 GMT
FROM: Robert Strausbaugh at Eastern Illinois University <rstrausbaugh(a)eiu.edu>
R. Strausbaugh (Eastern Illinois University), Daniel Warshofsky (UMN), Pat Kelly (UMN), Mandeep S. S. Gill (UMN), Alexandre Toscano (UMN), Yilin Lu(UMN), Sydney Leggio (UMN), Aksinya Kamenshikova (UMN) report on behalf of a larger collaboration:
We observed M82, including the localization region for the Fermi GRB 231115A (Fermi GBM team, GCN 35035), with the Total-Coverage Ultrafast Response to Binary-Mergers Observatory (TURBO) prototype telescope in St. Paul, Minnesota, USA, as part of a high-cadence ongoing survey for transients in nearby galaxies. We visited the field 55 times on November 15 UT, with the last visit occurring at 9:06 UT in SDSS r and g bands respectively (corresponding to 6.5 hours before the GRB trigger time).
Each exposure is 30 seconds. We do not detect a source at the same location as the GROWTH-India counterpart (Kumar et al., GCN 35041) in either band.
The 3-sigma upper limits in the table below are calculated using the Pan-STARRS catalog as reference, and are not corrected for Galactic extinction.
The TURBO prototype in St. Paul consists of two co-mounted 11-inch telescopes each with a 6.6 square degree field of view.
TURBO, which is under construction, will consist of two arrays of 8 pairs of co-mounted 11-inch telescopes at two dark-sky sites: Magdalena Ridge Observatory, New Mexico, USA and Skinakas Observatory, Crete, Greece.
mjd
g upper limit (AB)
r upper limit (AB)
60262.97035880
-
16.0
60262.97244213
16.9
-
60263.00063657408
-
15.9
60263.00407407407
-
15.7
60263.007106481484
-
16.1
60263.012094907404
-
15.6
60263.015555555554
-
15.9
60263.01940972222
-
16.0
60263.02327546296
-
15.9
60263.02715277778
-
16.3
60263.03057870371
-
16.1
60263.034212962964
-
16.1
60263.03765046296
-
16.4
60263.04111111111
-
15.7
60263.04293981481
-
15.8
60263.04591435185
16.5
15.7
60263.04896990741
-
16.4
60263.05202546297
16.5
15.8
60263.055
16.5
15.6
60263.058020833334
-
15.8
60263.061006944445
-
16.0
60263.06407407407
-
15.9
60263.070497685185
-
16.3
60263.07403935185
-
16.2
60263.07748842592
-
15.8
60263.080462962964
-
16.3
60263.08472222222
-
16.1
60263.087592592594
16.5
16.4
60263.09365740741
16.4
16.3
60263.09645833333
15.9
16.5
60263.099375
-
16.4
60263.1171412037
-
16.7
60263.120150462964
16.3
16.3
60263.12315972222
-
15.4
60263.14434027778
16.6
15.6
60263.14716435185
16.0
15.7
60263.15039351852
15.7
16.1
60263.15372685185
16.5
16.0
60263.156539351854
15.8
16.0
60263.159421296295
16.0
16.3
60263.162314814814
16.6
15.8
60263.165138888886
15.8
16.8
60263.16957175926
16.3
16.2
60263.172997685186
16.4
-
60263.176516203705
16.5
16.5
60263.19818287037
16.8
15.8
60263.21885416667
16.9
16.8
60263.22230324074
17.4
17.0
60263.24633101852
17.3
16.4
60263.268900462965
17.3
16.6
60263.27537037037
16.9
16.9
60263.27885416667
17.3
17.0
60263.283229166664
17.0
16.9
60263.28666666667
16.9
17.0
60263.29603009259
17.4
16.8
View this GCN Circular online at https://gcn.nasa.gov/circulars/35296.
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TITLE: GCN CIRCULAR
NUMBER: 35295
SUBJECT: GRB 231205B: AGILE detection
DATE: 23/12/06 21:37:52 GMT
FROM: Claudio Casentini at INAF-IAPS <claudio.casentini(a)inaf.it>
C. Casentini (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, Y. Evangelista, L. Foffano, G. Piano (INAF/IAPS), L. Baroncelli, A. Bulgarelli, A. Ciabattoni,
A. Di Piano, V. Fioretti (INAF/OAS-Bologna), G. Panebianco (Univ. Bologna - INAF/OAS Bologna), N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli (SSDC, and INAF/OAR), P.W. Cattaneo (INFN Pavia), F. Longo (Univ. Trieste, and INFN Trieste), M. Marisaldi (INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois (INAF/OA-Cagliari), A. Ursi (ASI and INAF/IAPS), I. Donnarumma, E. Menegoni (ASI),
A. Giuliani (INAF/IASF-Mi), F. Cutrona (Univ. Milano Bicocca) and P. Tempesta (TeleSpazio) report on behalf of the AGILE Team:
The AGILE satellite detected the GRB 231205B at T0 = 2023-12-05 16:43:59 s (UTC), reported by Swift (GCNs #35269, #35275, #35291) and GECAM-B (GCN #35279).
The burst is clearly visible in the AGILE scientific ratemeters of the MiniCALorimeter (MCAL; 0.4-100 MeV), and AntiCoincidence (AC; 50-200 keV) detectors. The event lasted about 18 s and it released a total number of 11057 counts in the MCAL detector (above a background rate of 539 Hz) and 54466 counts in the AC-Top detector (above a background rate of 2889 Hz).
In the scientific ratemeters of the AC-Top detector is visible a GRB precursor, centered around -25 s to the Swift T0 and lasting 10 seconds.
The AGILE ratemeters light curves can be found at: http://www.agilescienceapp.it/notices/GRB231205B_AGILE_RM_ND.png
Additional analysis of AGILE data is in progress. Automatic MCAL GRB alert Notices can be found at: https://gcn.gsfc.nasa.gov/agile_mcal.html.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35295.
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TITLE: GCN CIRCULAR
NUMBER: 35292
SUBJECT: GRB 231205B: Ondrejov D50 optical upper limit
DATE: 23/12/06 18:45:19 GMT
FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek(a)asu.cas.cz>
Alzbeta Malenakova, Martin Jelinek, Jan Strobl, Rene Hudec,
Cyril Polasek (ASU CAS Ondrejov, CZ),
and Sergey Karpov (Institute of Physics, Prague, CZ)
report:
The 50 cm robotic telescope D50 located at Ondrejov
observatory (Czech Republic) reacted robotically to the
Swift-BAT alert of GRB 231205B (Evans et al., GCNC 35269),
reported also by GECAM-B (Liu et al., GCNC 35279), obtaining a
series of 20 s unfiltered images starting at 16:45:46 UT, i.e.
107 s post trigger.
We do not detect any new optical source in the XRT error box
(neither any new or strongly variable source in the BAT
errorbox) in single images (detection limit r' > 18.7) nor in
a combined 30 x 20 s frame (mean exp time 290 s post trigger,
with a limit r' > 21.0) similarly to Odeh et al. (GCNC 35270),
Jiang et al. (GCNC 35280), Jiang et al. (GCNC 35281) and
Komesh et al. (GCNC 35287). All magnitudes are calibrated
with Atlas Refcat 2.0 (Tonry et al., ApJ 867, 105, 2018).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35292.
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TITLE: GCN CIRCULAR
NUMBER: 35291
SUBJECT: GRB 231205B: Swift-XRT refined Analysis
DATE: 23/12/06 15:26:36 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
S. Dichiara (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U.
Leicester), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M.
Perri (SSDC & INAF-OAR), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto)
and P.A. Evans report on behalf of the Swift-XRT team:
We have analysed 6.5 ks of XRT data for GRB 231205B, from 224 s to 68.4
ks after the BAT trigger. The data comprise 3 s in Windowed Timing
(WT) mode (taken while Swift was slewing), with the remainder in Photon
Counting (PC) mode.
The light curve can be modelled with an initial power-law decay with an
index of alpha=0.27 (+0.04, -0.05), followed by a break at T+6137 s to
an alpha of 1.32 (+/-0.08).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.06 (+/-0.10). The
best-fitting absorption column is 4.5 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.8 x 10^-11 (6.2 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 9.6 sigma
Photon index: 2.06 (+/-0.10)
If the light curve continues to decay with a power-law decay index of
1.32, the count rate at T+24 hours will be 0.063 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-12 (3.9 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01200812.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35291.
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TITLE: GCN CIRCULAR
NUMBER: 35290
SUBJECT: Fermi-LAT gamma-ray observations of IceCube-231202A
DATE: 23/12/06 14:52:23 GMT
FROM: chiara.bartolini-1(a)unitn.it
C. Bartolini (Univ of Trento & INFN Bari), S. Garrappa (Weizmann Institute of Science), S. Buson (Univ of Wuerzburg), J. Sinapius (DESY) and Leonard Pfeiffer (Univ of Wuerzburg) on behalf of the Fermi-LAT collaboration:
We report an analysis of observations of the vicinity of the IC231202A high-energy neutrino event (GCN 35225) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2023-12-02 at 17:08:24.09 UT (T0) with J2000 position RA = 139.04 (+1.52, -1.96) deg, Decl. = +0.37 (+1.11, -1.40) deg (90% PSF containment). According to the fourth Fermi LAT source catalog (4FGL-DR4), there is one 4FGL-DR4 cataloged gamma-ray (>100 MeV; The Fermi-LAT collaboration 2022, ApJS, 260, 53) source, 4FGL J0909.1+0121 (PKS 0906+01), in the 90% IC231202A uncertainty localization region. Based on a preliminary analysis of the LAT data over one month and day timescale prior T0, this object is not significantly detected at gamma rays.
We searched for intermediate (days to years) timescale emission from a new gamma-ray source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC231202A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC231202A best-fit position, the >100 MeV flux upper limit (95% confidence) is <6.0e-10 ph cm^-2 s^-1 for ~15-years (2008-08-04 to 2023-12-02 UTC), and < 4.3e-9 (<6.1 e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0.
Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this region will continue. For this observation the Fermi-LAT contact person is C. Bartolini (chiara.bartolini at ba.infn.it).
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/35290.
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TITLE: GCN CIRCULAR
NUMBER: 35289
SUBJECT: GRB 231205B: REM optical/NIR upper limits
DATE: 23/12/06 14:26:13 GMT
FROM: Riccardo Brivio <riccardo.brivio(a)inaf.it>
R. Brivio, M. Ferro, P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) on behalf of the REM team, report:
We observed the field of GRB 231205B (Evans et al., GCN 35269) with the REM 60cm robotic telescope located at the ESO Observatory of La Silla (Chile). The observations were carried out in the g,r,i,z, J,H,K bands, starting on 2023 Dec 06 at 00:32:29 UT (i.e. about 7.81 hours after the Swift trigger) and lasted for about 1 hour.
From preliminary analysis, we do not find any source at the enhanced XRT position (Osborne et al., GCN 35275), down the the following 3 sigma upper limits:
r > 20.4 (AB; calibrated against the Pan-STARRS catalogue)
at a mid time of t-t0 ~ 8.54 h after the GRB trigger;
H > 17.8 (Vega; calibrated against the 2MASS catalogue)
at a mid time of t-t0 ~ 8.24 h after the GRB trigger.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35289.
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TITLE: GCN CIRCULAR
NUMBER: 35288
SUBJECT: GRB 231129C: ASIM MXGS observation and localization
DATE: 23/12/06 12:42:06 GMT
FROM: Martino Marisaldi at U of Bergen, Norway <martino.marisaldi(a)uib.no>
M. Marisaldi (University of Bergen), A. Mezentsev (University of Bergen), P.Connell, Javier Navarro-Gonzalez (University of Valencia),
N. Østgaard (University of Bergen), V. Reglero (University of Valencia)
and T. Neubert (DTU Space) report on behalf of the ASIM Team:
At 19:10:18 UT on 29 November 2023, the Atmosphere-Space Interactions Monitor (ASIM)
mission triggered on the long bright GRB 231129C.
The burst was also detected by Fermi-GBM (Sharma et al., GCN Circ. 35221, and Sharma et al., GCN Circ. 227),
MAXI/GSC (Kawakubo et al., GCN Circ. 35223), CALET (Shimizu et al., GCN Circ. 35228),
AstroSat CZTI (Waratkar et al., GCN Circ. 35230), GECAM-B (Zheng et al., GCN Circ. 35231),
Swift-XRT (Gropp et al., GCN Circ. 35234), Glowbug (Cheung et al., GCN Circ. 35235),
GRBAlpha (Dafcikova et al., GCN Circ. 35236), Fermi-LAT (Arimoto et al., GCN Circ. 35238,
AGILE (Panebianco et al., GCN Circ. 35244), and Konus-Wind (Lysenko et al., GCN Circ. 35256).
Photon by photon data with <1 microsecond time resolution have been
collected for a time interval of 19 seconds.
The emission is detected in the MXGS High Energy Detector (HED), sensitive in the range 0.3 to >30 MeV,
and in the MXGS Low Energy Detector (LED), sensitive in the range 0.05 to 0.4 MeV.
In January 2022 ASIM was relocated so that the MXGS coded mask imaging system is pointing towards the Earth’s limb, observing a large fraction of unocculted sky, therefore enabling localization of the GRB prompt emission.
This GRB was observed within the MXGS Field of View resulting in a very high significant localization (>100 sigma) at
R.A.,Dec(2000) = 00:51:12.56 -81:45:35.5
consistent within a 25 arcmin error (radius, 99% confidence level) with the Swift-XRT X-ray afterglow (Gropp et al., GCN Circ. 35251) and the MASTER OT detection (Antipov et al., GCN Circ.35240).
ASIM is an ESA mission onboard the International Space Station dedicated to the
observation of Terrestrial Gamma-ray Flashes (TGFs) and Transient Luminous Events (TLEs)
operative since June 2018 (Neubert et al., Space Sci Rev (2019) 215:26
https://doi.org/10.1007/s11214-019-0592-z ).
The payload includes the Modular X- and Gamma-Ray Sensor (MXGS)
(Østgaard et al., Space Sci Rev (2019) 215:23 https://doi.org/10.1007/s11214-018-0573-7 ),
and the the Modular Multispectral Imaging Array (MMIA)
(Chanrion et al., Space Sci Rev (2019) 215:28 https://doi.org/10.1007/s11214-019-0593-y ).
The ASIM Science Data Centre (ASDC) website is https://asdc.space.dtu.dk/
View this GCN Circular online at https://gcn.nasa.gov/circulars/35288.
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TITLE: GCN CIRCULAR
NUMBER: 35287
SUBJECT: GRB 231205B: NUTTelA-TAO / BSTI Early Optical Limits
DATE: 23/12/06 09:54:28 GMT
FROM: Toktarkhan Komesh at Nazarbayev University <toktarkhan.komesh(a)nu.edu.kz>
T. Komesh (NU), B. Grossan (UCB, NU), Zh. Maksut (NU), Zh. 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 GRB 231205B, 10 s after receipt an automated GCN / BAT position alert, observing in Sloan g', r' and i' bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14).
We started observations at 16:45:33 UT on 2023-12-05, 94 s after the BAT trigger. Observations were made in clear conditions. No source consistent with the XRT (J.P. Osborne et al., GCN Circ. 35275) was detected. We report the following results:
start time t-t0(s) end time UL g' UL r' ULi' exposure_time (s)
-----------------------------------------------------------------------
16:45:33 94 16:46:29 19.9 19.5 18.3 52.5
16:46:43 164 16:49:13 20.3 19.9 19.0 150
start time is in UT. t-t0(s) gives the time since trigger, in seconds. UL i', gives the 5 sigma upper limit sensitivity in magnitudes, for images co-added to the given exposure time. The first row in the table corresponds to co-adds of an initial short exposure image sequence of 0.5 s for g' and r' (these sub-second exposures are read-noise suppressed by our EMCCD cameras, with high gain electron multiplication active; other images are taken in conventional CCD operation mode), and 7.5 s for i'. The second row corresponds to co-adds from a continuing series of 3 s exposures for g' and r', and 15 s for i'. Calibration was done with the 3 bright 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, Kazkhstan.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35287.
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