TITLE: GCN CIRCULAR
NUMBER: 35221
SUBJECT: GRB 231129C: Fermi GBM detection of a very bright burst
DATE: 23/11/29 21:13:24 GMT
FROM: Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma(a)nasa.gov>
V. Sharma (NASA-GSFC/UMBC) and O. Roberts (NASA-MSFC/USRA) reports on behalf of the Fermi GBM Team:
"At 19:10:18.11 UT on 29 November 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231129C (trigger 722977823/231129799).
The GBM light curve consists of a very bright pulse, with a duration of about 15 seconds. This event, a likely, long GRB, is very bright and follow-up across all wavelengths is encouraged.
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 2.04, Dec = -81.53 (J2000 degrees, equivalent to J2000 00h 08m, -81d 32'), with a statistical uncertainty of 1.00 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216, 32]).
The angle from the Fermi LAT boresight is 50 degrees.
A full science circular is forthcoming.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231129799/…
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231129799/…
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231129799/…."
View this GCN Circular online at https://gcn.nasa.gov/circulars/35221.
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TITLE: GCN CIRCULAR
NUMBER: 35220
SUBJECT: GRB 231129A: Enhanced Swift-XRT position
DATE: 23/11/29 20:56:33 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2261 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 231129A, 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 = 317.54381, +41.52204 which is equivalent
to:
RA (J2000): 21h 10m 10.51s
Dec (J2000): +41d 31' 19.4"
with an uncertainty of 2.2 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/35220.
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TITLE: GCN CIRCULAR
NUMBER: 35219
SUBJECT: LIGO/Virgo/KAGRA S231129ac: Updated Sky localization
DATE: 23/11/29 20:43:19 GMT
FROM: Michael Puerrer at University of Rhode Island <mpuerrer(a)uri.edu>
The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:
We have conducted further analysis of the LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) data around the time of the compact binary merger (CBC) candidate S231129ac (GCN Circular 35211). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page:
https://gracedb.ligo.org/superevents/S231129ac
For the Bilby.multiorder.fits,0 sky map, the 90% credible region is 3089 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3964 +/- 1513 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/userguide/.
After parameter estimation by RapidPE-RIFT [2], the updated classification of the GW signal, in order of descending probability is BBH (99%), Terrestrial (1%), NSBH (<1%), or BNS (<1%).
[1] Ashton et al. ApJS 241, 27 (2019) and Morisaki et al. arXiv:2307.13380 (2023)
[2] Rose et al. arXiv:2201.05263 (2022) and Pankow et al. PRD 92, 023002 (2015)
View this GCN Circular online at https://gcn.nasa.gov/circulars/35219.
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TITLE: GCN CIRCULAR
NUMBER: 35218
SUBJECT: GRB 231129A: Swift-XRT refined Analysis
DATE: 23/11/29 20:35:31 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
D.N. Burrows (PSU), J. D. Gropp (PSU), S. Dichiara (PSU), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E.
Ambrosi (INAF-IASFPA) and P.A. Evans report on behalf of the
Swift-XRT team:
We have analysed 7.0 ks of XRT data for GRB 231129A, from 115 s to 43.8
ks after the BAT trigger. The data comprise 174 s in Windowed Timing
(WT) mode with the remainder in Photon Counting (PC) mode. The refined
XRT position is RA, Dec = 317.5437, +41.5206 which is equivalent to:
RA (J2000): 21 10 10.49
Dec(J2000): +41 31 14.2
with an uncertainty of 3.5 arcsec (radius, 90% confidence).
The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=4.86 (+/-0.21). At T+165 s the decay
steepens to an alpha of 6.44 (+0.28, -0.24) before breaking again at
T+308 s to a final decay with index alpha=0.83 (+0.05, -0.06).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.83 (+/-0.07). The
best-fitting absorption column is 1.09 (+/-0.08) x 10^22 cm^-2, in
excess of the Galactic value of 5.9 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.18 (+0.31, -0.29)
and a best-fitting absorption column of 1.6 (+/-0.4) x 10^22 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 5.0 x 10^-11 (1.2 x 10^-10) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.6 (+/-0.4) x 10^22 cm^-2
Galactic foreground: 5.9 x 10^21 cm^-2
Excess significance: 4.5 sigma
Photon index: 2.18 (+0.31, -0.29)
If the light curve continues to decay with a power-law decay index of
0.83, the count rate at T+24 hours will be 0.014 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.2 x
10^-13 (1.8 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/01199764.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35218.
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TITLE: GCN CIRCULAR
NUMBER: 35215
SUBJECT: GRB 231129B: Tiled Swift observations
DATE: 23/11/29 17:28:07 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
MAXI GRB 231129B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00116
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI 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/35215.
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TITLE: GCN CIRCULAR
NUMBER: 35214
SUBJECT: GRB 231129B: MAXI/GSC detection
DATE: 23/11/29 15:23:40 GMT
FROM: Motoko Serino at Aoyama Gakuin U. <serino(a)phys.aoyama.ac.jp>
M. Kurihara (JAXA), H. Negoro (Nihon U.), M. Serino (AGU), W. Iwakiri (Chiba U.),
M. Nakajima, K. Kobayashi, M. Tanaka, Y. Soejima, Y. Kudo (Nihon U.),
T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU),
Y. Tsuboi, S. Urabe, S. Nawa, N. Nemoto, E.Goto (Chuo U.),
M. Shidatsu (Ehime U.),
I. Takahashi, M. Niwano, S. Sato, N. Higuchi, Y. Yatsu (Tokyo Tech),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, S. Ogawa, M. Kurihara (JAXA),
Y. Ueda, K. Setoguchi, T. Yoshitake, Y. Nakatani, Y. Okada (Kyoto U.),
M. Yamauchi, Y. Hagiwara, Y. Umeki, Y. Otsuki (Miyazaki U.),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU),
M. Sugizaki (NAOC),
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 14:03:05 UT on 29 November 2023.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (285.662 deg, 40.278 deg) = (19 02 38, +40 16 40) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.39 deg and 0.26 deg, respectively.
The roll angle of long axis from the north direction is 75.0 deg counterclockwise.
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(283.889, 39.749) deg = (18 55 33, +39 44 56) (J2000)
(284.232, 39.302) deg = (18 56 55, +39 18 07) (J2000)
(286.730, 40.399) deg = (19 06 55, +40 23 56) (J2000)
(286.398, 40.853) deg = (19 05 35, +40 51 10) (J2000)
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 141 +- 32 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 12:30 UT
with an upper limit of 20 mCrab.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35214.
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TITLE: GCN CIRCULAR
NUMBER: 35213
SUBJECT: Fermi-LAT gamma-ray observations of IceCube-231125A
DATE: 23/11/29 13:33:08 GMT
FROM: Leonard Pfeiffer at University of Würzburg <pfeiffer.leo(a)gmail.com>
L. Pfeiffer (Univ. of Wuerzburg), S. Buson (Univ. of Wuerzburg), S. Garrappa (Weizmann Institute of Science), C. Bartolini (INFN Bari) and J. Sinapius (DESY) on behalf of the Fermi-LAT collaboration:
We report an analysis of observations of the vicinity of the IC231125A high-energy neutrino event (GCN 35194) 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 2023-11-25 at 22:34:56.64 UT (T0) with J2000 position RA = 177.53 (+3.99, -4.03) deg, Decl. = +53.62 (+1.57, -1.64) deg (90% PSF containment). There are two gamma-ray (>100 MeV; 4FGL-DR4, The Fermi-LAT collaboration 2023, arXiv:2307.12546) sources located within the 90% IC231125A localization region. These are:
4FGL J1215.0+5351, associated with the BL LAC GB6 J1215+5349;
4FGL J1208.9+5441, associated with the FSRQ TXS 1206+549
We searched for intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC231125A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC231125A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 1.77e-10 ph cm^-2 s^-1 for ~15-years (2008-08-04 to 2023-11-26 UTC), and < 8.10e-9 (<8.91e-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 these observations the Fermi-LAT contact person is L. Pfeiffer (leonard.pfeiffer at stud-mail.uni-wuerzburg.de).
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/35213.
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TITLE: GCN CIRCULAR
NUMBER: 35212
SUBJECT: Integral GRB231129.21: Global MASTER-Net observations report
DATE: 23/11/29 10:57:31 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-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Integral GRB231129.21 (trigger No 10436,21h 10m 18.76s , +41d 31m 39.2s, R=0.0528333) errorbox 17767 sec after notice time and 17792 sec after trigger time at 2023-11-29 10:02:31 UT, with upper limit up to 15.1 mag. Observations started at twilight. The observations began at zenith distance = 9 deg. The sun altitude is -8.7 deg.
The galactic latitude b = -5 deg., longitude l = 85 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2319548
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
17795 | MASTER-Tunka | C | 5 | 13.3 |
17820 | MASTER-Tunka | C | 5 | 13.4 |
17846 | MASTER-Tunka | C | 10 | 13.0 |
17878 | MASTER-Tunka | C | 15 | 13.5 |
17917 | MASTER-Tunka | C | 26 | 13.7 |
17967 | MASTER-Tunka | C | 36 | 13.6 |
18027 | MASTER-Tunka | C | 45 | 13.9 |
18099 | MASTER-Tunka | C | 60 | 13.9 |
18178 | MASTER-Tunka | C | 60 | 14.1 |
18273 | MASTER-Tunka | C | 90 | 14.1 |
18491 | MASTER-Tunka | C | 90 | 14.8 |
18600 | MASTER-Tunka | C | 90 | 14.6 |
18755 | MASTER-Tunka | C | 180 | 14.4 |
19151 | MASTER-Tunka | C | 180 | 14.9 |
20388 | MASTER-Tunka | C | 180 | 15.1 |
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/35212.
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