TITLE: GCN CIRCULAR
NUMBER: 35276
SUBJECT: LIGO/Virgo/KAGRA S231205c: One counterpart neutrino candidate event from an IceCube neutrino search
DATE: 23/12/06 01:14:20 GMT
FROM: acz2122(a)columbia.edu
IceCube Collaboration (http://icecube.wisc.edu/) reports:
We have performed a search for track-like muon neutrino events detected by IceCube consistent with the sky localization of the low-significance gravitational-wave candidate event S231205c in a time range of 1000 seconds centered on the alert event time (2023-12-05T00:49:30 UTC to 2023-12-05T01:06:10 UTC) [1,2].
During this time period IceCube was collecting good quality data. A single hypothesis test
was conducted, using a Bayesian approach to quantify the joint GW + neutrino event significance, which assumes a binary merger scenario and accounts for known astrophysical priors, such as GW source distance, in the statistical significance estimation [3].
One track-like event is found in spatial and temporal coincidence with the gravitational-wave
Candidate S231205c calculated from the map circulated in the S231205c-2-Preliminary notice. This represents an overall p-value of 0.0083 for the Bayesian search. The p-value
measures the consistency of the observed track-like events with the known atmospheric backgrounds for this single map (not accounting for statistical trials from multiple GW events).
Further details are available at https://gcn.nasa.gov/missions/icecube and at https://roc.icecube.wisc.edu/public/LvkNuTrackSearch.
Properties of the coincident events are shown below:
dt(s) RA(deg) Dec(deg) Angular uncertainty(deg) p-value(Bayesian)
-----------------------------------------------------------------------------------------------------
-198.05 220.38 +26.40 0.86 0.0083
where:
dt = Time of track event minus time of GW trigger (sec)
Angular uncertainty = Angular uncertainty of track event: the radius of a circle
representing 90% CL containment by area.
p-value = the p-value for this specific track event from this search.
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] M. G. Aartsen et al 2020 ApJL 898 L10
[2] Abbasi et al. Astrophys.J. 944 (2023) 1, 80
[3] I. Bartos et al. 2019 Phys. Rev. D 100, 083017
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TITLE: GCN CIRCULAR
NUMBER: 35275
SUBJECT: GRB 231205B: Enhanced Swift-XRT position
DATE: 23/12/06 00:40:47 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1474 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 231205B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 54.14875, +27.14134 which is equivalent
to:
RA (J2000): 03h 36m 35.70s
Dec (J2000): +27d 08' 28.8"
with an uncertainty of 2.0 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35275.
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TITLE: GCN CIRCULAR
NUMBER: 35274
SUBJECT: GRB 231204A: Glowbug gamma-ray detection
DATE: 23/12/05 20:09:43 GMT
FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil>
C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (MSFC), and M.S. Briggs (UAH) report:
The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 231204A, which was also detected by Fermi/GBM, AstroSat/CZTI, and CALET (GCN 35258, 35267, 35272).
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-12-04 20:00:02.808 with a duration of 11.3 s and a total significance of about 27.2 sigma. The light curve comprises a dominant triple-peaked structure from T0 to ~T0+6s and a fainter pulse at ~T0+9s.
Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=0.6 and a cutoff energy ("Epeak") of 619 keV. The modeled 10-10000 keV fluence is 1.3e-05 erg/cm^2.
The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006
Distribution Statement A: Approved for public release. Distribution is unlimited.
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TITLE: GCN CIRCULAR
NUMBER: 35273
SUBJECT: Swift GRB231205.70: Global MASTER-Net observations report
DATE: 23/12/05 19:28:39 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, 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 Swift GRB231205.70 (trigger No 1200812,03h 36m 36.96s , +27d 08m 45.6s, R=0.05) errorbox 8923 sec after notice time and 9002 sec after trigger time at 2023-12-05 19:14:01 UT, with upper limit up to 17.6 mag. The observations began at zenith distance = 66 deg. The sun altitude is -18.4 deg.
The galactic latitude b = -22 deg., longitude l = 163 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2325501
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
9092 | MASTER-SAAO | C | 180 | 17.6 |
9092 | MASTER-SAAO | C | 180 | 16.9 |
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/35273.
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TITLE: GCN CIRCULAR
NUMBER: 35272
SUBJECT: GRB 231204A: CALET Gamma-Ray Burst Monitor detection
DATE: 23/12/05 19:10:01 GMT
FROM: Yuta Kawakubo at Louisiana State University <kawakubo1(a)lsu.edu>
T. Tamura (Kanagawa U), A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA),
Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The long GRB 231204A (Fermi GBM Final Real-time Localization:
Fermi GBM team, GCN Circ. 35258; AstroSat CZTI detection:
Waratkar et al., GCN Circ. 35267) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 20:00:00.75 UTC on 4 December 2023
(http://cgbm.calet.jp/cgbm_trigger/flight/1385755095/).
The burst signal was seen by only the SGM detector.
The burst light curve shows a weak pulse that starts
at T+3.1 sec, peaks at T+4.1 sec, and ends at T+7.9 sec.
The T90 and T50 durations measured by the SGM data are 4.5 +/- 0.5 sec
and 2.5 +/- 0.1 sec (40-1000 keV), respectively.
The ground-processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1385755095/index.html
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at Waseda University.
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TITLE: GCN CIRCULAR
NUMBER: 35271
SUBJECT: Fermi-LAT daily aperture light curve of T CrB now available
DATE: 23/12/05 18:52:43 GMT
FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil>
C. C. Cheung (NRL), T. J. Johnson (GMU, resident at NRL), P. Jean (IRAP, Toulouse), G. Marti-Devesa (Univ. of Innsbruck), on behalf of the Fermi Large Area Telescope Collaboration:
T Coronae Borealis (T CrB) is a known recurrent nova with the next, long-anticipated explosion expected in early 2024. The 2024 nova eruption prediction is based on the approximately 80-year recurrence between prior outbursts and the recent detection of the start of a pre-eruption dip (in March/April 2023; ATel #16107), which may indicate a change in the accretion state (e.g., Luna et al. 2020, ApJL, 902, L14). This dip was also observed prior to its last outburst in 1946. Because of its proximity (distance ~0.9 kpc; Schaefer 2022, MNRAS, 517, 6150), T CrB is expected to be detected brightly as a gamma-ray transient with a peak (E >100 MeV) flux of ~(1-2) x 10^-5 photons cm^-2 s^-1 if it is similar to other known recurrent symbiotic novae detected by Fermi-LAT (e.g., V407 Cyg; Ackermann et al. 2014, Sci, 345, 554; RS Oph 2021; Cheung et al. 2022, ApJ, 935, 44).
In consideration of its expected bright outburst in gamma rays, a preliminary Fermi-LAT aperture light curve (daily and weekly bins) is updated daily and publicly available at: https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/T_CrB . For this source the Fermi LAT contact is C.C. Cheung (Teddy.Cheung(a)nrl.navy.mil).
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.
Note: the text of this notice was also posted as: https://www.astronomerstelegram.org/?read=16336
View this GCN Circular online at https://gcn.nasa.gov/circulars/35271.
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TITLE: GCN CIRCULAR
NUMBER: 35270
SUBJECT: GRB 231205B: AKO Optical Upper Limit
DATE: 23/12/05 18:46:35 GMT
FROM: Mohammad Odeh at Al Khatim Observatory M44 <mshodeh(a)gmail.com>
Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE), and Dalya Akl (American University
of Sharjah, UAE), report:
We observed the field of GRB 231205B, which was detected by Swift/BAT (GCN
35269) with our 0.36m f/7.7 robotic telescope on December 05 starting at
17:37:44 UT (corresponding to 0.9 hours from the GRB trigger time) using an
(Ic) filter.
We obtained 17x180s images. We do not detect a credible source within the
Swift-XRT error region (Evans et al., GCN 35269). The following 5-sigma
upper limit is calculated using the ATLAS catalog as a reference: Ic =
20.0.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35270.
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TITLE: GCN CIRCULAR
NUMBER: 35269
SUBJECT: GRB 231205B: Swift detection of a burst
DATE: 23/12/05 17:11:16 GMT
FROM: K.L. Page at U Leicester <klp5(a)leicester.ac.uk>
P. A. Evans (U Leicester), S. Dichiara (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. M. Parsotan (GSFC/UMBC/CRESSTII) and
M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 16:43:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 231205B (trigger=1200812). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 54.154, +27.146 which is
RA(J2000) = 03h 36m 37s
Dec(J2000) = +27d 08' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single peak
structure with a duration of about 40 sec. However there
may be activity before the start of the immediately-available
data, as the burst occurred during a pre-planned slew. The peak count
rate was ~6000 counts/sec (15-350 keV), at T-3, before the
nominal trigger time.
The XRT began observing the field at 16:47:54.0 UT, 234.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 54.14912, 27.14099 which is equivalent
to:
RA(J2000) = 03h 36m 35.79s
Dec(J2000) = +27d 08' 27.6"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 23 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.
UVOT took a finding chart exposure starting 237 seconds after the
BAT trigger. No credible afterglow candidate has been found in
the initial data products.
Burst Advocate for this burst is P. A. Evans (pae9 AT leicester.ac.uk).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
View this GCN Circular online at https://gcn.nasa.gov/circulars/35269.
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TITLE: GCN CIRCULAR
NUMBER: 35268
SUBJECT: GRB 231205A: joint location of multiple instruments by ETJASMIN
DATE: 23/12/05 16:33:30 GMT
FROM: yqzhang_cl(a)163.com
Yanting Zhang, Shaolin Xiong, Yue Huang, Shuo Xiao, Xiaoyun Zhao, Ping Wang,
report on behalf of the GECAM team:
The short burst, GRB 231205A, has been detected by GECAM-B (Tan et al., GCN 35266), Fermi/GBM (Fermi/GBM team, GCN 35263) and INTEGRAL/SPI-ACS. With the ETJASMIN pipeline (Energetic Transients joint analysis system for Multi-INstrument, Xiao et al., MNRAS, 514, 2397, 2022) and the realtime data of GECAM-B, INTEGRAL/SPI-ACS and Fermi/GBM, we did a low-latency joint location for this burst.
Firstly, we applied the Li-CCF method (Xiao et al., ApJ, 920, 43, 2021) to the realtime high temporal resolution (~1 ms) light curve of GECAM-B and the low-latency public 50 ms light curve of INTEGRAL/SPI-ACS, and derived the triangulation location as the following annuli:
--------------------------------------------------------------------------------------------------
Annulus Ra (deg) Dec (deg) Radius (deg) Radius-Error (deg, 3sigma)
GECAM-B + SPI-ACS 209.519 59.889 40.961 1.272
--------------------------------------------------------------------------------------------------
Then, we combined this annulus location, the stand-alone locations provided by GECAM-B (Tan et al., GCN 35266) and Fermi/GBM (Fermi/GBM team, GCN 35263), as well as the Earth occultation of these instruments, and derived a refined location, which is much smaller than stand-alone ones.
This refined location (~3 sigma region) could be approximately described by a polygon region,
whose center and corners are:
--------------------------------------
Ra (deg) Dec (deg)
Center 205.313 19.155
Corner1 215.859 19.155
Corner2 209.883 18.724
Corner3 202.148 18.871
Corner4 194.766 20.427
Corner5 205.313 19.524
--------------------------------------
For this refined location, the sky map and probability data could be found at:
Sky map: http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB231205A-jointLoc-skymap-v01.png
Data file: http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB231205A-jointLoc-healpix-v01.f…
ETJASMIN is developed for joint observation of high energy transients by the GECAM team.
We acknowledge the public data of Fermi/GBM and INTEGRAL/SPI-ACS.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35268.
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TITLE: GCN CIRCULAR
NUMBER: 35267
SUBJECT: GRB 231204A: AstroSat CZTI detection
DATE: 23/12/05 14:16:15 GMT
FROM: Gaurav Waratkar at IIT Bombay <gauravwaratkar(a)iitb.ac.in>
G. Waratkar (IITB), P. K. Navaneeth (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 et al., 2021, JApA, 42, 73) showed the detection of the long-duration GRB 231204A which was also detected by Fermi-GBM (Fermi GBM Team, GCN Circ. 35258).
The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-12-04 20:00:04.5 UTC. The measured peak count rate associated with the burst is 230.7 (+39.0, -34.4) counts/s above the background in the combined data of all quadrants, with a total of 1319 (+234, -237) counts. The local mean background count rate was 347.5 (+2.1, -2.9) counts/s. Using cumulative rates, we measure a T90 of 13 (+7, -5) s.
It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2023-12-04 20:00:06.6 UTC. The measured peak count rate is 873.2 (+83.1, -58.1) counts/s above the background in the combined Veto data of all quadrants, with a total of 6070 (+508, -547) counts. The local mean background count rate was 1532.5 (+4.8, -5.7) counts/s. We measure a T90 of 12 (+8, -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/35267.
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