TITLE: GCN CIRCULAR
NUMBER: 35595
SUBJECT: GRB 240122A: Tiled Swift observations
DATE: 24/01/22 16:50:08 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 240122A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00119
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/35595.
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TITLE: GCN CIRCULAR
NUMBER: 35594
SUBJECT: Konus-Wind detection of GRB 240119A (short/hard)
DATE: 24/01/22 15:40:27 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 short GRB 240119A (Fermi-GBM detection: The Fermi GBM team, GCN 35583;
AstroSat-CZTI detection: Joshi et al.: GCN 35589;
GECAM-B detection: Zhang et al.: GCN 355921;
IPN triangulation: Svinkin et al., GCN 35592)
triggered Konus-Wind (KW) at T0=62945.465 s UT (17:29:05.465).
The burst light curve shows a single emission pulse
which starts at ~T0-0.032 s and has a duration of ~0.13 s.
The emission is seen up to ~2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240119_T62945/
As observed by Konus-Wind, the burst had
a total fluence of (8.1 ± 1.7)x10^-7 erg/cm^2 and
a 16-ms peak energy flux, measured from T0-0.016 s,
of (1.9 ± 0.4)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).
The spectrum of the burst (measured from T0-0.048 s to T0+0.080 s)
can be described, in the 20 keV - 1.5 MeV range, by a power law with
exponential cutoff (CPL) model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.23(-0.32,+0.40) and Ep = 678(-141,+254) keV.
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/35594.
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TITLE: GCN CIRCULAR
NUMBER: 35593
SUBJECT: GRB 240122A: MAXI/GSC detection
DATE: 24/01/22 14:53:25 GMT
FROM: Hitoshi Negoro at Nihon University/MAXI team <negoro.hitoshi(a)nihon-u.ac.jp>
H. Negoro (Nihon U.), W. Iwakiri (Chiba U.), M. Serino (AGU),
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, Y. Niida (Ehime U.),
I. Takahashi, M. Niwano, S. Sato, N. Higuchi, Y. Yatsu (Tokyo Tech),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, S. Ogawa, T. 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), and M. Sugizaki (NAOC)
The MAXI/GSC nova alert system triggered on a faint uncatalogued X-ray transient source
at 10:28:03 UT on January 22, 2024.
Because our localization program did not run, we can not provide a precise error region.
The source position determined with the nova alert system (Negoro et al. 2016) is
(R.A., Dec) = (92.827 deg, -19.031 deg) = (06 11 18, -19 01 51) (J2000)
with an uncertainty of more than 30 arc-min. The burst duration is about 10 sec, and
the 2-10 keV X-ray flux around the peak was about 150 mCrab.
There was no significant excess flux in the previous transit at 08:55 UT
and in the next transit at 12:00 UT with an upper limit of 20 mCrab for each.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35593.
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TITLE: GCN CIRCULAR
NUMBER: 35592
SUBJECT: IPN triangulation of GRB 240119A (short)
DATE: 24/01/22 14:47:24 GMT
FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru>
D. Svinkin, D. Frederiks, A. Ridnaia, A. Lysenko,
and T. Cline on behalf of the Konus-Wind team,
A. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,
E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
and
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team, report:
The bright, short-duration GRB 240119A
(Fermi-GBM detection: The Fermi GBM team, GCN 35583;
AstroSat-CZTI detection: Joshi et al.: GCN 35589;
GECAM-B detection: Zhang et al.: GCN 35591)
was detected by Fermi (GBM trigger 727378152), INTEGRAL (SPI-ACS),
Swift (BAT), Konus-Wind, AstroSat (CZTI), and GECAM-B
at about 62948 s UT (17:29:08).
The burst was outside the coded field of view of the BAT.
We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
359.940 (23h 59m 46s) -75.259 (-75d 15' 33")
Corners:
342.700 (22h 50m 48s) -82.193 (-82d 11' 33")
343.891 (22h 55m 34s) -82.325 (-82d 19' 29")
4.927 (00h 19m 42s) -67.683 (-67d 41' 00")
4.404 (00h 17m 37s) -67.603 (-67d 36' 12")
---------------------------------------------
The error box area is 3.2 sq. deg, and its maximum
dimension is 15.4 deg (the minimum one is 12.5 arcmin).
The Sun distance was 62 deg.
This localization may be improved.
The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM localizations.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB240119_T62945/IPN/
The Konus-Wind time history and spectrum will be given
in a forthcoming GCN Circular.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35592.
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TITLE: GCN CIRCULAR
NUMBER: 35591
SUBJECT: GRB 240119A: GECAM detection of a short burst
DATE: 24/01/21 07:42:30 GMT
FROM: wenlongzhang2018(a)163.com
Wen-Long Zhang, Shao-Lin Xiong, Chen-Wei Wang, Yue Wang, Yan-Qiu Zhang report on behalf of the GECAM team:
GECAM-B was triggered in-flight by a short burst, GRB 240119A, at 2024-01-19T17:29:07.700 UTC (T0), which was also detected by Fermi/GBM (GCN #35583) and AstroSat CZTI (GCN #35589). At the same time, GECAM-C was also triggered on-ground by this burst.
According to the light curves, this burst shows a total duration of ~0.1 sec (20-1000 keV).
According to the in-flight software, GECAM-B localized this burst to the following position (J2000):
Ra: 355.51 deg
Dec: -81.39 deg
Err: 5.76 deg (1-sigma, statistical only)
This GECAM-B localization is consistent with that of Fermi/GBM within the error.
We note that these results are very preliminary. Refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor(GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35591.
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TITLE: GCN CIRCULAR
NUMBER: 35590
SUBJECT: GRB 240118C: GECAM-B detection of a long burst
DATE: 24/01/21 07:39:21 GMT
FROM: wenlongzhang2018(a)163.com
Wen-Long Zhang, Shao-Lin Xiong, Yan-Qiu Zhang report on behalf of the GECAM team:
GECAM-B was triggered on-ground by a long burst, GRB 240118C, at 2024-01-18T17:23:24.000 UTC (T0), which was also observed by Fermi/GBM (GCN #35576 and GCN #35586) and Swift/BAT-GUANO(GCN #35581).
According to the GECAM-B light curve, this burst consists of roughly three pulses with a total duration of ~40 sec.
The GECAM-B ground calculated location (J2000) is:
Ra: 308.64 deg
Dec: -1.56 deg
Err: 4.65 deg (1-sigma, statistical only)
This GECAM-B localization is consistent with that of Fermi/GBM within the error.
We note that these results are very preliminary. Refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor(GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35590.
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TITLE: GCN CIRCULAR
NUMBER: 35589
SUBJECT: GRB 240119A: AstroSat CZTI detection of a short burst
DATE: 24/01/21 06:57:24 GMT
FROM: Gaurav Waratkar at IIT Bombay <gauravwaratkar(a)iitb.ac.in>
J. Joshi (IUCAA), G. Waratkar (IITB), 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 a short-duration GRB 240119A which was also detected by Fermi-GBM (Fermi GBM team, GCN Circ. 35583).
The source was detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2024-01-19 17:29:07.67 UTC. The measured peak count rate associated with the burst is 1304 (+583, -314) counts/s above the background in the combined data of three quadrants (out of four), with a total of 53 (+17, -18) counts. The local mean background count rate was 250 (+25, -36) counts/s. Using cumulative rates, we measure a T90 of 0.06 (+0.02, -0.03) s.
The source was also faintly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range but we cannot make quantitative inferences due to the intrinsic 1 s binning of Veto data.
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/35589.
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TITLE: GCN CIRCULAR
NUMBER: 35588
SUBJECT: GRB 240118A: Mondy optical observations
DATE: 24/01/20 23:54:29 GMT
FROM: Alexei Pozanenko at IKI, Moscow <apozanen(a)iki.rssi.ru>
N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of IKI GRB FuN:
We observed the field of Fermi LAT localization of GRB 240118A (Bissaldi, GCN 35560), which was also detected by Fermi GBM (Fermi GBM team, GCN 35558; Hamburg, GCN 35563), NuSTAR (Grefenstette, GCN 35564), Konus-Wind (Frederiks, GCN 35567), Swift BAT (DeLaunay, GCN 35568), and GRBAlpha (Dafcikova et al., GCN 35580), and the localization area observed by MASTER-Tunka observatory (Lipunov et al., GCN 35561) and Abastumani observatory (Pankov et al., GCN 35572).
Observations started on 2024-01-18 (UT) 14:13:46 with AZT-33IK telescope of Sayan observatory (Mondy) in the R-filter. The observations have been carried out in moderate weather conditions with FWHM of 2.5". We report observations of XRT candidates detected in the Swift TOO program (Evans et al., GCN 35573).
XRT #1 - out of FOV
XRT #2 - matches bright USNO-B1.0 star with R2=9.98 mag
XRT #3 - within the XRT #3 error circle we detect a faint source, which matches SDSS J011408.49+294753.1 source with SDSS DR12 r'= 22.117 and redshift of z_phot = 0.68
XRT #4 - out of FOV
XRT #5 - matches bright Gaia DR3 star with G=6.48 mag
XRT #6 - out of FOV
XRT #7 - out of FOV
Preliminary photometry of the faint source XRT #3 suggested as an X-ray afterglow (Beardmore et al., GCN 35587) is following
Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
(mid, days) (s)
2024-01-18 14:13:46 0.537932 R 29*120 22.1 0.3 22.1
The photometry is based on nearby USNO-B1.0 stars.
At this time we cannot say anything about the variability of the source. The source at coordinates 01:14:08.48 +29:47:53.2, spatially coinciding with the galaxy SDSS J011408.49+294753.1 with a redshift of 0.68 could be a host galaxy of GRB 240118A.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35588.
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TITLE: GCN CIRCULAR
NUMBER: 35587
SUBJECT: GRB 240118A: Swift-XRT afterglow detection
DATE: 24/01/20 22:41:31 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
A.P. Beardmore (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi
(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), A. Tohuvavohu (U. Toronto),
D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester) and
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 240118A, collecting 4.7 ks of Photon
Counting (PC) mode data between T0+96.2 ks and T0+109.0 ks.
Two uncatalogued X-ray sources are detected consistent with being
within 296 arcsec of the Fermi/LAT position, of which one ("Source 3")
is believed to be the afterglow. Using 4697 s of PC mode data and 3
UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 18.53587, +29.79798 which is equivalent to:
RA (J2000): 01h 14m 08.61s
Dec(J2000): +29d 47' 52.7"
with an uncertainty of 2.7 arcsec (radius, 90% confidence). This
position is 2.1 arcmin from the Fermi/LAT position. The light curve is
consistent with a constant source of mean count rate 3.6e-02 ct/sec. A
power-law fit gives an index of 1.9 (+1.0, -2.8).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+/-0.6). The
best-fitting absorption column is 1.1 (+0.8, -0.6) x 10^22 cm^-2, in
excess of the Galactic value of 7.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.5 x 10^-11 (9.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.1 (+0.8, -0.6) x 10^22 cm^-2
Galactic foreground: 7.1 x 10^20 cm^-2
Excess significance: 3.1 sigma
Photon index: 2.2 (+/-0.6)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021644.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021644.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35587.
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TITLE: GCN CIRCULAR
NUMBER: 35586
SUBJECT: GRB 240118C: Fermi GBM Observation
DATE: 24/01/20 01:01:56 GMT
FROM: Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma(a)nasa.gov>
V. Sharma (NASA-GSFC/UMBC) and C. Meegan (UAH) report on behalf of the
Fermi Gamma-ray Burst Monitor Team:
"At 17:23:23.93 UT on 18 January 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 240118C (trigger 727291408/240118725), which was also
detected by Swift/BAT-GUANO (DeLaunay et al. 2024, GCN 35581).
The Fermi Final Real-time Localization is reported in GCN 35576.
The angle from the Fermi LAT boresight is 90 degrees.
The GBM light curve consists of multiple pulses with a duration (T90)
of about 31 s (50-300 keV). The time-averaged spectrum from
T0-0.6 to T0+32.5 s is best fit by a power law function with
an exponential high-energy cutoff.
The power law index is -1.39 +/- 0.03 and the cutoff energy,
parameterized as Epeak, is 144 +/- 10 keV.
The event fluence (10-1000 keV) in this time interval is (1.23 +/- 0.04)E-05 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+29.7 s in the 10-1000 keV band
is 13.6 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/."
View this GCN Circular online at https://gcn.nasa.gov/circulars/35586.
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