- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Mon 04 Nov 24 18:30:35 UT
NOTICE_TYPE: Fermi-GBM Flight Position
RECORD_NUM: 50
TRIGGER_NUM: 752437820
GRB_RA: 27.267d {+01h 49m 04s} (J2000),
27.643d {+01h 50m 34s} (current),
26.513d {+01h 46m 03s} (1950)
GRB_DEC: +42.000d {+42d 00' 00"} (J2000),
+42.123d {+42d 07' 22"} (current),
+41.752d {+41d 45' 06"} (1950)
GRB_ERROR: 9.18 [deg radius, statistical plus systematic]
GRB_INTEN: 334 [cnts/sec]
DATA_SIGNIF: 17.20 [sigma]
INTEG_TIME: 1.024 [sec]
GRB_DATE: 20618 TJD; 309 DOY; 24/11/04
GRB_TIME: 66615.42 SOD {18:30:15.42} UT
GRB_PHI: 155.00 [deg]
GRB_THETA: 55.00 [deg]
DATA_TIME_SCALE: 1.0240 [sec]
HARD_RATIO: 0.95
LOC_ALGORITHM: 3 (version number of)
MOST_LIKELY: 96% GRB
2nd_MOST_LIKELY: 2% GRO_J0422_32
DETECTORS: 0,0,0, 0,0,0, 0,0,0, 0,1,1, 0,0,
SUN_POSTN: 220.39d {+14h 41m 32s} -15.69d {-15d 41' 17"}
SUN_DIST: 151.38 [deg] Sun_angle= -11.2 [hr] (East of Sun)
MOON_POSTN: 257.90d {+17h 11m 36s} -27.95d {-27d 57' 09"}
MOON_DIST: 137.16 [deg]
MOON_ILLUM: 10 [%]
GAL_COORDS: 134.25,-19.60 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 41.21, 28.59 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
COMMENTS: Fermi-GBM Flight-calculated Coordinates.
COMMENTS: This trigger occurred at longitude,latitude = 130.35,20.07 [deg].
COMMENTS: The LC_URL file will not be created until ~15 min after the trigger.
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Mon 04 Nov 24 18:30:52 UT
NOTICE_TYPE: Fermi-GBM Ground Position
RECORD_NUM: 60
TRIGGER_NUM: 752437820
GRB_RA: 30.830d {+02h 03m 19s} (J2000),
31.188d {+02h 04m 45s} (current),
30.111d {+02h 00m 27s} (1950)
GRB_DEC: +29.180d {+29d 10' 48"} (J2000),
+29.299d {+29d 17' 55"} (current),
+28.940d {+28d 56' 24"} (1950)
GRB_ERROR: 3.70 [deg radius, statistical only]
DATA_SIGNIF: 20.00 [sigma]
DATA_INTERVAL: 2.048 [sec]
GRB_DATE: 20618 TJD; 309 DOY; 24/11/04
GRB_TIME: 66615.42 SOD {18:30:15.42} UT
GRB_PHI: 165.00 [deg]
GRB_THETA: 65.00 [deg]
E_RANGE: 44.032 - 279.965 [keV]
LOC_ALGORITHM: 4173 (Gnd S/W Version number)
SUN_POSTN: 220.39d {+14h 41m 33s} -15.69d {-15d 41' 17"}
SUN_DIST: 163.97 [deg] Sun_angle= -11.4 [hr] (East of Sun)
MOON_POSTN: 257.90d {+17h 11m 37s} -27.95d {-27d 57' 10"}
MOON_DIST: 139.25 [deg]
MOON_ILLUM: 10 [%]
GAL_COORDS: 141.27,-31.12 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 38.88, 15.62 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
POS_MAP_URL: http://gcn.gsfc.nasa.gov/notices_f/gbm_gnd_loc_map_752437820.fits
COMMENTS: Fermi-GBM Ground-calculated Coordinates.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: The LC_URL file will not be created/available until ~15 min after the trigger.
COMMENTS: The POS_MAP_URL file will not be created/available until ~1.5 min after the notice.
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Mon 04 Nov 24 18:31:37 UT
NOTICE_TYPE: Fermi-GBM Ground Position
RECORD_NUM: 1
TRIGGER_NUM: 752437820
GRB_RA: 30.780d {+02h 03m 07s} (J2000),
31.138d {+02h 04m 33s} (current),
30.061d {+02h 00m 15s} (1950)
GRB_DEC: +29.090d {+29d 05' 24"} (J2000),
+29.209d {+29d 12' 31"} (current),
+28.850d {+28d 50' 60"} (1950)
GRB_ERROR: 2.99 [deg radius, statistical only]
DATA_SIGNIF: 23.30 [sigma]
DATA_INTERVAL: 8.192 [sec]
GRB_DATE: 20618 TJD; 309 DOY; 24/11/04
GRB_TIME: 66615.42 SOD {18:30:15.42} UT
GRB_PHI: 165.00 [deg]
GRB_THETA: 65.00 [deg]
E_RANGE: 44.032 - 279.965 [keV]
LOC_ALGORITHM: 41731 (Gnd S/W Version number)
SUN_POSTN: 220.39d {+14h 41m 33s} -15.69d {-15d 41' 17"}
SUN_DIST: 164.02 [deg] Sun_angle= -11.4 [hr] (East of Sun)
MOON_POSTN: 257.91d {+17h 11m 39s} -27.95d {-27d 57' 12"}
MOON_DIST: 139.18 [deg]
MOON_ILLUM: 10 [%]
GAL_COORDS: 141.26,-31.22 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 38.80, 15.56 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
POS_MAP_URL: http://gcn.gsfc.nasa.gov/notices_f/gbm_gnd_loc_map_752437820.fits
COMMENTS: Fermi-GBM Ground-calculated Coordinates.
COMMENTS: This is likely a Long GRB.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: The LC_URL file will not be created/available until ~15 min after the trigger.
COMMENTS: The POS_MAP_URL file will not be created/available until ~1.5 min after the notice.
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Mon 04 Nov 24 18:32:06 UT
NOTICE_TYPE: Fermi-GBM Ground Position
RECORD_NUM: 2
TRIGGER_NUM: 752437820
GRB_RA: 30.950d {+02h 03m 48s} (J2000),
31.312d {+02h 05m 15s} (current),
30.224d {+02h 00m 54s} (1950)
GRB_DEC: +31.340d {+31d 20' 24"} (J2000),
+31.458d {+31d 27' 30"} (current),
+31.100d {+31d 06' 01"} (1950)
GRB_ERROR: 2.39 [deg radius, statistical only]
DATA_SIGNIF: 25.40 [sigma]
DATA_INTERVAL: 11.264 [sec]
GRB_DATE: 20618 TJD; 309 DOY; 24/11/04
GRB_TIME: 66615.42 SOD {18:30:15.42} UT
GRB_PHI: 164.00 [deg]
GRB_THETA: 63.00 [deg]
E_RANGE: 44.032 - 279.965 [keV]
LOC_ALGORITHM: 41731 (Gnd S/W Version number)
SUN_POSTN: 220.39d {+14h 41m 33s} -15.69d {-15d 41' 18"}
SUN_DIST: 162.19 [deg] Sun_angle= -11.4 [hr] (East of Sun)
MOON_POSTN: 257.92d {+17h 11m 40s} -27.95d {-27d 57' 14"}
MOON_DIST: 139.67 [deg]
MOON_ILLUM: 10 [%]
GAL_COORDS: 140.59,-29.04 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 39.78, 17.61 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
POS_MAP_URL: http://gcn.gsfc.nasa.gov/notices_f/gbm_gnd_loc_map_752437820.fits
COMMENTS: Fermi-GBM Ground-calculated Coordinates.
COMMENTS: This is likely a Long GRB.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: The LC_URL file will not be created/available until ~15 min after the trigger.
COMMENTS: The POS_MAP_URL file will not be created/available until ~1.5 min after the notice.
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Mon 04 Nov 24 18:39:38 UT
NOTICE_TYPE: Fermi-GBM Final Position
RECORD_NUM: 0
TRIGGER_NUM: 752437820
GRB_RA: 32.390d {+02h 09m 34s} (J2000),
32.755d {+02h 11m 01s} (current),
31.658d {+02h 06m 38s} (1950)
GRB_DEC: +31.770d {+31d 46' 12"} (J2000),
+31.887d {+31d 53' 12"} (current),
+31.534d {+31d 32' 02"} (1950)
GRB_ERROR: 2.84 [deg radius, statistical only]
GRB_DATE: 20618 TJD; 309 DOY; 24/11/04
GRB_TIME: 66615.42 SOD {18:30:15.42} UT
GRB_PHI: 165.00 [deg]
GRB_THETA: 62.00 [deg]
E_RANGE: 44.032 - 279.965 [keV]
LOC_ALGORITHM: 41731 (Gnd S/W Version number)
SUN_POSTN: 220.39d {+14h 41m 34s} -15.69d {-15d 41' 23"}
SUN_DIST: 162.38 [deg] Sun_angle= -11.5 [hr] (East of Sun)
MOON_POSTN: 257.99d {+17h 11m 58s} -27.96d {-27d 57' 40"}
MOON_DIST: 140.88 [deg]
MOON_ILLUM: 10 [%]
GAL_COORDS: 141.75,-28.23 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 41.15, 17.57 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
LOC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_locplot_all_bn241104771.png
COMMENTS: Fermi-GBM Final Position.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: The LC_URL file should be available by the time this FINAL notice is produced.
COMMENTS: This notice was generated completely by automated pipeline processing.
COMMENTS: This is likely a Long GRB.
- GCN Circular #38075
The Fermi GBM team reports the detection of a likely LONG GRB
At 18:30:15 UT on 4 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241104A (trigger 752437820.424838 / 241104771).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 32.4, Dec = 31.8 (J2000 degrees, equivalent to J2000 02h 09m, 31d 48'), with a statistical uncertainty of 2.8 degrees.
The angle from the Fermi LAT boresight is 62.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_skymap_all_bn241104771.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_healpix_all_bn241104771.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
- GCN Circular #38076
V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko,
A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin,
V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU),
O.Gress, N.Budnev (ISU),
C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory)
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) started inspect of the Fermi GRB 241104A ( Fermi GBM team, GCN 38075) errorbox 35 sec after notice time and 57 sec after trigger time at 2024-11-04 18:31:12 UT, with upper limit up to 20.1 mag. The observations began at zenith distance = 34 deg. The sun altitude is -49.2 deg.
The galactic latitude b = -28 deg., longitude l = 142 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2659245
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
62 | 2024-11-04 18:31:12 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.6s) | C | 10 | 17.8 |
77 | 2024-11-04 18:31:12 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.6s) | C | 40 | 18.8 | Coadd
75 | 2024-11-04 18:31:25 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.8s) | C | 10 | 17.9 |
94 | 2024-11-04 18:31:39 | MASTER-Tunka | (02h 03m 04.47s , +29d 10m 35.9s) | C | 20 | 18.5 |
117 | 2024-11-04 18:32:02 | MASTER-Tunka | (02h 03m 04.45s , +29d 10m 36.7s) | C | 20 | 18.5 |
153 | 2024-11-04 18:32:33 | MASTER-Tunka | (02h 03m 36.52s , +31d 21m 04.2s) | C | 30 | 18.7 |
188 | 2024-11-04 18:32:33 | MASTER-Tunka | (02h 03m 36.52s , +31d 21m 04.2s) | C | 100 | 19.7 | Coadd
187 | 2024-11-04 18:33:07 | MASTER-Tunka | (02h 03m 36.49s , +31d 21m 05.1s) | C | 30 | 18.8 |
225 | 2024-11-04 18:33:40 | MASTER-Tunka | (02h 03m 36.47s , +31d 21m 06.0s) | C | 40 | 18.8 |
274 | 2024-11-04 18:34:23 | MASTER-Tunka | (02h 03m 36.41s , +31d 21m 07.0s) | C | 50 | 19.1 |
332 | 2024-11-04 18:35:17 | MASTER-Tunka | (02h 03m 36.35s , +31d 21m 08.4s) | C | 60 | 19.2 |
644 | 2024-11-04 18:39:59 | MASTER-Tunka | (02h 09m 20.45s , +31d 47m 01.4s) | C | 120 | 19.4 |
799 | 2024-11-04 18:39:59 | MASTER-Tunka | (02h 09m 20.45s , +31d 47m 01.4s) | C | 430 | 20.1 | Coadd
777 | 2024-11-04 18:42:02 | MASTER-Tunka | (02h 09m 20.33s , +31d 47m 04.1s) | C | 140 | 19.5 |
935 | 2024-11-04 18:44:25 | MASTER-Tunka | (02h 09m 20.15s , +31d 47m 07.5s) | C | 170 | 19.4 |
1114 | 2024-11-04 18:47:19 | MASTER-Tunka | (02h 09m 19.95s , +31d 47m 11.2s) | C | 180 | 19.4 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
- GCN Circular #38081
H. Zhou (PMO, CAS), R.-Z. Li (YNAO, CAS), Q. C. Liu (TSU), H. Q. Cheng, Z.
X. Ling (NAO,CAS) report on behalf of the Einstein Probe team:
We report on the detection of an X-ray transient, designated EP241104a, by
the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) missi=
on. The WXT position of EP241030a is R.A.= 32.574 deg, DEC = 31.555 deg
(J2000) with an uncertainty of 2.7 arcmin (radius, 90% C.L. statistical and
systematic).
The lightcurve of the transient observed by the WXT lasts around 400 seconds
and has a peak flux of ~5.0 x 10^-10 erg/s/cm^2 in the 0.5-4 keV band. The
average 0.5-4 keV spectrum can be fitted with an absorbed power law with
a photon index of 1.3(-0.7, +0.8) and a fixed absorbing column density value
of 7.8 x 10^20 cm^-2. The derived average unabsorbed 0.5-4 keV flux is
2.0(-1.1, +1.0) x 10^-10 erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters.
EP241104a is spatially and temporally consistent with GRB 241104A (Fermi GB=
M Team, GCN 38075; Vladimir et al., GCN 38076; St=C3=A9phane et al., GCN 38=
078). The EP-WXT detection is about 4 minutes after the Fermi-GBM trigger (=
2024-11-04T18:30:15). Before the detection, the WXT observation was interru=
pted by the Earth obscuration for about 1.5 ks which covered the Fermi GBM =
trigger time. EP-FXT follow-up observation has been arranged.=20
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the
soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook
of X-ray and Gamma-ray Astrophysics).
- GCN Circular #38082
SVOM/GRM team: Jin-Peng Zhang, Chen-Wei Wang, Shi-Jie Zheng, Yong-Wei Dong,
Jiang-Tao Liu, Jian-Chao Sun, Yue Huang, Jiang He, Min Gao, Hao-Xuan Guo,
Lu Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li
Tuo, Wen-Long Zhang, Wen-Jun Tan, Yue Wang, Hao-Xi Wang, Jin Wang, Jin-Zhou=
Wang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-Bing Wu, Shao-Lin Xiong, Jia=
n-Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang,
Shuang-Nan Zhang, Yan-Qiu Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao, Chao=
Zheng (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IR=
AP), David Corre (CEA), Tais Maiolino (LUPM), Fr=C3=A9d=C3=A9ric Piron (LUP=
M), St=C3=A9phane Schanne (CEA), Jingwei Wang (IAP), JeanLuc Att=C3=A9ia (I=
RAP)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Fr=
=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP),
Andrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lac=
haud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Par=
is), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong
(IHEP), Bing Zhang (UNLV)
Report on behalf of the SVOM team:
During the commissioning phase, the SVOM/GRM was triggered in-flight by GRB
241104A at 2024-11-04T18:30:14 UT (T0), which was also observed by Fermi/GBM
(Fermi GBM Team, GCN 38075) and SVOM/ECLAIRs (GCN 38078).
The real-time alert data and light curves of SVOM/GRM were downlinked to th=
e ground through the VHF system with low latency. With the event-by-event d=
ata downloaded through the X-band ground station, the GRM light curve shows=
that this burst consists of multiple pulses, with a T90 of 11.9 +0.3/-0.3 =
s.
The GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb241104A.png
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA, China), National Cen=
ter for Space Studies (CNES, France) and the Chinese Academy of Sciences (C=
AS, China), which is dedicated to observing gamma-ray bursts and other tran=
sient phenomena in the energetic universe. GRM is developed by the Institut=
e of High Energy Physics (IHEP) of CAS.
The SVOM point of contact for this burst is: Jin-Peng Zhang (IHEP)(zhangjinpeng@ihep.ac.cn)
- GCN Circular #38078
SVOM/ECLAIRs Commissioning Team: St=C3=A9phane Schanne, Nicolas Dagoneau, H=
erv=C3=A9 Le Provost, Fr=C3=A9d=C3=A9ric Chateau (CEA), Jean-Luc Atteia, La=
urent Bouchet, Sebastien Guillot, Juliette Alaux, Hui Yang (IRAP), Tais Mai=
olino (LUPM), Wenjin Xie, Donghua Zhao (NAOC), Alexis Coleiro (APC), Karine=
Mercier, Marie-Claire Charmeau, Stefano Crepaldi (CNES)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Olivier Godet (IRAP), Arnaud Claret (CEA), =
Zi-Gao Dai (USTC), Fr=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), A=
ndrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lacha=
ud (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:
During the commissioning phase, the SVOM/ECLAIRs telescope detected and loc=
alized the bright long duration GRB 241104A at 2024-11-04T18:30:15 UTC (Tb)=
, previously detected by Fermi (Fermi GBM team, GCN circular 38075), and by=
SVOM/GRM (SVOM reference: sb24110402).
The onboard trigger was not in operations, the following information was ob=
tained by reprocessing the data on ground in the flight trigger algorithms.=
The burst was detected by the Count-Rate Trigger (CRT) and Image Trigger (=
IMT) which produced 21 Alert messages. The best Alert was obtained by CRT i=
n the 8-120 keV energy band with a signal-to-noise ratio of 55.5 in a time =
window of 10.24 s starting at Tb.
The event location is RA, Dec =3D 32.552, 31.554 (J2000).
The statistical uncertainty on this position is 1.6 arcminutes to which we =
recommend adding 2 arcminutes of systematic uncertainty in quadrature.
SVOM did not slew to the burst since automated slewing was not enabled.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA), French Space Agency=
(CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to o=
bserving gamma-ray bursts and other transient phenomena in the energetic un=
iverse. ECLAIRs was developed jointly by APC, CEA, CNES, and IRAP.
The SVOM point of contact for this burst is: s.schanne AT cea.fr.
- GCN Circular #38083
Alan M. Watson (UNAM), Francis Fortin (IRAP), St=C3=A9phane Basa (UAR Pytheas),
William H. Lee (UNAM), S. Antier (OCA), D. Akl (AUS), Jean-Luc Atteia
(IRAP), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), J.-G. Ducoin
(CPPM), Simona Lombardo (LAM), Francesco Magnani (CPPM), and Margarita
Pereyra (UNAM)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang
(IHEP), St=C3=A9phane Basa (LAM), Jean-Luc Atteia (IRAP), Arnaud Claret (CE=
A),
Zi-Gao Dai (USTC), Fr=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), A=
ndrea
Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (AP=
C),
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:
We imaged the field of GRB 241104A detected by Fermi/GBM, SVOM/GRM,
SVOM/ECLAIRs, and EP/WXT (Fermi GBM Team, GCN Circ. 38075; Schanne et al.,
GCN Circ. 38078; SVOM/GRM Team, GCN Circ. 38082; Zhou et al., GCN Circ.
38081) during the commissioning of the COLIBR=C3=8D (SVOM/F-GFT) telescope =
at
the Observatorio Astron=C3=B3mico Nacional on the Sierra de San Pedro M=C3=
=A1rtir in
Mexico.
We observed with the engineering test camera in a red filter that
approximates SDSS r. The data were reduced using custom software and then
analysed and calibrated against the PS1 catalog using the STDWeb service
(Karpov et al. 2022).
In 960 seconds of exposure from 2024-11-05 12:12 to 12:32 UTC (17.70 to
18.03 hours after the trigger), at high airmass, we detect no sources in
the ECLAIRs localization region other than those previously identified in
the PS1 or GAIA DR3 catalogs to a 5-sigma limiting AB magnitude of:
r > 20.8
We warmly thank the COLIBR=C3=8D engineering team and the staff of the
Observatorio Astron=C3=B3mico Nacional on the Sierra de San Pedro M=C3=A1rtir.
- GCN Circular #38084
Z. N. Wang (HNAS), A. Aryan, T.-W. Chen, W.-J. Hou (all NCU), J. Gillanders (Oxford), A. K. H. Kong (NTHU), S. J. Smartt (Oxford/QUB), Y. J. Yang, A. Sankar. K, Y.-C. Pan, C.-C. Ngeow, M.-H. Lee, H.-C. Lin, C.-H. Lai, H.-Y. Hsiao, C.-S. Lin, J.-K. Guo (all NCU), S. Yang, L. L. Fan, G. H. Sun (all HNAS), H.-W. Lin (UMich), H. F. Stevance, S. Srivastav, L. Rhodes (all Oxford), M. Nicholl, M. Fulton, T. Moore, K. W. Smith, C. Angus, A. Aamer (all QUB), A. Schultz and M. Huber (both IfA, Hawaii) report:
We observed the field of the GRB/fast X-ray transient GRB 241104A/EP241104a (Fermi GBM Team, GCN 38075; Schanne et al., GCN 38078; Zhou et al., GCN 38081, SVOM/GRM Team, GCN 38082, Watson et al., GCN 38083) using the 1m LOT at Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen & Yang et al., 2024arXiv240609270C). The first LOT epoch of observations started at 13:15 UTC on the 5th of November 2024 (MJD = 60619.552), 18.75hr after the EP WXT trigger.
We utilized the astroalign (Beroiz et al. 2020, A&C, 32, 100384) and astropy (Astropy Collaboration et al., 2022, ApJ, 935, 167) packages to align and stack the individual frames. We do not find any evidence of a new and uncataloged source in the stacked images within the 2.7 arcminute error circle of EP-WXT localization.
Moreover, we utilized the Python-based package AutoPhOT (Brennan & Fraser, 2022, A&A, 667, A62) to perform the PSF photometry on our stacked frames. The details of the observations and measured 3-sigma upper limit (in the AB system) are as follows:
Telescope | Filter | MJD (start) | t-t0 (hr) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass
LOT | r | 60619.552 | 18.75 | 300 * 6 | >22.8 | 1".29 | 1.07
The presented magnitudes are calibrated using field stars from the Pan-STARRS1 catalog, and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E(B-V) = 0.07 AB mag in the direction of the burst (Schlafly & Finkbeiner 2011).
- GCN Circular #38086
SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, L. P. Xin, C. Wu, X. H. Ha=
n, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. De=
ng, L. Lan, X. M. Lu, R. S. Zhang, (NAOC), J. Zhang, L. J. Dan, G. Y. Zou,=
C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO).
=C2=A0
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Fr=
=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP),A=
ndrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lacha=
ud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris=
), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (I=
HEP), Bing Zhang (UNLV)
report on behalf of the SVOM team:
VT started to observe the field of GRB 241104A (Fermi GBM Team, GCN #38075;=
Schanne et al., GCN #38078; Zhou et al., GCN #38081; Zhang et al., GCN #38=
082) in ToO mode from 2024-11-05T13:51:35 UT, about 19.4 hours after the bu=
rst. The VT conducted observations in VT_B band (400-650nm) and VT_R band (=
650-1000nm) simutaneously.
An uncatalogued source was found in VT_R band stacked image with a total ex=
posure time of 900s ranging from 13:51:35 to 14:08:15 UT, after compared to=
the DESI DR10 catalog.
The coordinates are R.A.=3D 02:10:13.392, DEC.=3D +31:35:06.60, Error =3D 0=
.5 arcseconds, J2000.
The magnitude was VT_R=3D21.6+/-0.1 mag and VT_B>23.0 mag (3 sigma).
We proposed that it is likely the optical afterglow of the burst.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA, China), National Cen=
ter for Space Studies (CNES, France) and the Chinese Academy of Sciences (C=
AS, China), which is dedicated to observing gamma-ray bursts and other tran=
sient phenomena in the energetic universe. VT was jointly developed by Xi'a=
n Institute of Optics and Precision Mechanics (XIOPM), CAS and National ast=
ronomical observatories (NAOC),CAS.
- GCN Circular #38089
D. B. Malesani (DAWN/NBI and Radboud Univ.), A. Martin-Carrillo (UCD), D. Xu (NAOC), M. Turkki (NOT) report on behalf of a larger collaboration:
We observed the candidate optical counterpart (Qiu et al., GCN 38086) of GRB 241104A (Fermi GBM team, GCN 38075; Schanne et al., GCN 38078; Zhang et al., GCN 38082), using the Nordic Optical Telescope (NOT) equipped with the ALFOSC imager. Observations were carried out in the SDSS r, i, and z filters.
No object is detected at the location of the candidate counterpart, down to the following 3-sigma limiting magnitudes:
r > 24.0 AB 2024 Nov 5.859 UT (1.088 days after the trigger)
i > 23.7 AB 2024 Nov 5.871 UT (1.100 days after the trigger)
z > 22.2 AB 2024 Nov 5.847 UT (1.077 days after the trigger)
Calibration was performed against nearby Pan-STARRS sources.
- GCN Circular #38090
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the Fermi/GBM GRB 241104A.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021727
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Fermi/GBM 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.
- GCN Circular #38093
NUMBER: 38093
SUBJECT: GRB 241104A: The SVOM/VT candidate in GCN circular 38086 is not an astrophysical source
DATE: 24/11/06 05:57:04 GMT
FROM: Liping Xin at NAOC, SVOM
SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, L. P. Xin, C. Wu, X. H. Ha=
n, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. De=
ng, L. Lan, X. M. Lu, R. S. Zhang, (NAOC), J. Zhang, L. J. Dan, G. Y. Zou,=
C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO).
=20
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Fr=
=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP),A=
ndrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lacha=
ud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris=
), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (I=
HEP), Bing Zhang (UNLV)
report on behalf of the SVOM team:
After further analysis of all data acquired via the X-band downlink, the ca=
ndidate was reported by VT commission team in the previous report(Qiu et al=
., GCN #38086), is a defect on the detector in VT_R band image,that is dete=
ctable in other fields, as well as in the new dark master images.
A more detailed analysis is still in progress.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA, China), National Cen=
ter for Space Studies (CNES, France) and the Chinese Academy of Sciences (C=
AS, China), which is dedicated to observing gamma-ray bursts and other tran=
sient phenomena in the energetic universe. VT was jointly developed by Xi'a=
n Institute of Optics and Precision Mechanics (XIOPM), CAS and National ast=
ronomical observatories (NAOC),CAS.
- GCN Circular #38094
S. Rushikesh (IISER, TVM), U. Pathak (IITB), O. Mukherjee (USRA), S. Bala (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team:
"At 18:30:15.42 UT on 04 November 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB241104A (trigger 752437820/241104771)
which was also detected by EP/WXT (Zhou et al. 2024, GCN 38081),
SVOM/VT (Qiu et al. 2024, GCN 38086) and SVOM/ECLAIRs (Schanne et al. 2024, GCN 38078).
The Fermi GBM on-ground location is consistent with the EP/WXT position.
The angle from the Fermi LAT boresight is 62 degrees.
The GBM light curve consist of single pulse with multiple peaks with a duration (T90)
of about 10.5 s (50-300 keV). The time-averaged spectrum
from T0-7.6 to T0+11.8 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.69 +/- 0.08 and the cutoff energy,
parameterized as Epeak, is 74 +/- 2 keV.
The event fluence (10-1000 keV) in this time interval is
(3.4 +/- 0.8)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.6 s in the 10-1000 keV band is 6.9 +/- 0.3 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 68 +/- 3 keV, alpha = -0.6 +/- 0.1 and beta = -3.0 +/- 0.3.
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/"
- GCN Circular #38096
S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), M. Capalbi (INAF-IASFPA), M.
Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR) and P.A. Evans (U.
Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
Fermi/GBM-detected burst GRB 241104A, using the localisation by
SVOM/ECLAIRs (Schanne et al., GCN 38078), collecting 2.9 ks of Photon
Counting (PC) mode data between T0+98.0 ks and T0+105.0 ks.
No X-ray sources have been detected consistent with being within 256
arcsec of the SVOM/ECLAIRs position. The 3-sigma upper limit in the
field is 0.005 ct s^-1, corresponding to a 0.3-10 keV observed flux of
2.1e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum).
Three uncatalogued sources were detected too far from the GRB position
to be likely afterglow candidates. These sources are also inconsistent
with the X-ray localisation by EP/WXT (Zhou et al., GCN 38081).
The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021727.
This circular is an official product of the Swift-XRT team.
- GCN Circular #38129
T. Tamura (Kanagawa U), A. Yoshida, T. Sakamoto, S. Sugita,
Y. Kawakubo (AGU), 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 241104A (Fermi GBM Final Real-time Localization:
Fermi GBM team, GCN Circ. 38075; Detection and localization by
SVOM/ECLAIRs: Schanne et al., GCN Circ. 38078; EP detection of GRB 241104A
X-ray emission: Zhou et al., GCN Circ. 38081; SVOM/GRM observation: Zhang
et al., GCN Circ. 38082) triggered the CALET Gamma-ray Burst Monitor (CGBM)
at 18:30:15.957 UTC on 04 November 2024
(https://cgbm.calet.jp/cgbm_trigger/flight/1414780091/index.html).
The burst signal was seen by only the SGM detector. Because of a problem
with the ground alert processing script, the GCN notice was not distributed
automatically for this event.
The burst light curve shows a multi-peaked structure that starts
at T-0.6 sec, peaks at T+2.6 sec, and ends at T+5.1 sec.
The T90 and T50 durations measured by the SGM data are 5.0 +/- 0.4 sec
and 3.3 +/- 0.5 sec (40-1000 keV), respectively.
The ground-processed light curve is available at
https://cgbm.calet.jp/cgbm_trigger/ground/1414780091/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at Waseda University.
Previous IAU Circulars 
