- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Fri 07 Jan 22 22:00:31 UT
NOTICE_TYPE: Fermi-GBM Final Position
RECORD_NUM: 0
TRIGGER_NUM: 663274898
GRB_RA: 218.880d {+14h 35m 31s} (J2000),
219.134d {+14h 36m 32s} (current),
218.303d {+14h 33m 13s} (1950)
GRB_DEC: +20.100d {+20d 06' 00"} (J2000),
+20.005d {+20d 00' 17"} (current),
+20.318d {+20d 19' 03"} (1950)
GRB_ERROR: 1.00 [deg radius, statistical only]
GRB_DATE: 19586 TJD; 7 DOY; 22/01/07
GRB_TIME: 68493.52 SOD {19:01:33.52} UT
GRB_PHI: 93.15 [deg]
GRB_THETA: 54.63 [deg]
E_RANGE: 50.000 - 300.000 [keV]
LOC_ALGORITHM: 415 (Gnd S/W Version number)
SUN_POSTN: 289.06d {+19h 16m 14s} -22.28d {-22d 16' 46"}
SUN_DIST: 80.28 [deg] Sun_angle= 4.7 [hr] (West of Sun)
MOON_POSTN: 358.20d {+23h 52m 47s} -5.90d {-05d 54' 00"}
MOON_DIST: 137.84 [deg]
MOON_ILLUM: 32 [%]
GAL_COORDS: 22.08, 65.20 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 208.93, 33.35 [deg] ecliptic lon,lat of the burst (or transient)
LC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220107793/quicklook/glg_lc_medres34_bn220107793.gif
LOC_URL: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220107793/quicklook/glg_locplot_all_bn220107793.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 has human-in-the-loop processing.
COMMENTS:
COMMENTS: NOTE: This GBM event is temporally(1.0<100sec) coincident with the KONUS event (trignum=1958668494).
- GCN Circular #31405
V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov,
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, D.Kuvshinov, D. Cheryasov
(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. Gres, N.M. Budnev
(Irkutsk State University, API),
B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov
(Blagoveschensk Educational State University)
MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB220107.79 (trigger No 663274898,14h 35m 31.20s , +20d 06m 00.0s, R=1) errorbox 9102 sec after notice time and 19844 sec after trigger time at 2022-01-08 00:32:17 UT, with upper limit up to 19.0 mag. The observations began at zenith distance = 60 deg. The sun altitude is -50.1 deg.
The galactic latitude b = 65 deg., longitude l = 22 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1842261
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
19874 | 2022-01-08 00:32:17 | MASTER-Tavrida | (14h 28m 27.11s , +20d 25m 06.2s) | C | 60 | 16.3 |
19954 | 2022-01-08 00:33:37 | MASTER-Tavrida | (14h 37m 07.04s , +20d 24m 54.8s) | C | 60 | 17.4 |
20034 | 2022-01-08 00:34:57 | MASTER-Tavrida | (14h 34m 30.14s , +18d 32m 50.0s) | C | 60 | 17.6 |
20113 | 2022-01-08 00:36:16 | MASTER-Tavrida | (14h 42m 56.29s , +18d 30m 52.6s) | C | 60 | 17.4 |
20272 | 2022-01-08 00:38:55 | MASTER-Tavrida | (14h 31m 55.04s , +22d 20m 05.5s) | C | 60 | 18.5 |
20651 | 2022-01-08 00:45:14 | MASTER-Tavrida | (14h 26m 54.19s , +18d 31m 46.9s) | C | 60 | 18.3 |
20730 | 2022-01-08 00:46:33 | MASTER-Tavrida | (14h 44m 39.82s , +20d 24m 56.5s) | C | 60 | 18.4 |
21090 | 2022-01-08 00:52:33 | MASTER-Tavrida | (14h 28m 26.85s , +20d 27m 21.8s) | C | 60 | 18.7 |
21169 | 2022-01-08 00:53:52 | MASTER-Tavrida | (14h 37m 05.75s , +20d 26m 06.4s) | C | 60 | 19.0 |
21307 | 2022-01-08 00:56:10 | MASTER-Tavrida | (14h 42m 58.44s , +18d 31m 12.9s) | C | 60 | 18.5 |
21465 | 2022-01-08 00:58:48 | MASTER-Tavrida | (14h 31m 58.11s , +22d 19m 26.0s) | C | 60 | 18.9 |
21545 | 2022-01-08 01:00:08 | MASTER-Tavrida | (14h 39m 48.34s , +22d 20m 53.2s) | C | 60 | 18.6 |
21784 | 2022-01-08 01:04:07 | MASTER-Tavrida | (14h 26m 56.97s , +18d 32m 32.5s) | C | 60 | 18.7 |
21864 | 2022-01-08 01:05:27 | MASTER-Tavrida | (14h 44m 40.00s , +20d 25m 00.2s) | C | 60 | 19.0 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Sat 08 Jan 22 03:05:53 UT
NOTICE_TYPE: Fermi-LAT Offline Position
TRIGGER_NUM: 220107793
GRB_RA: 216.500d {+14h 26m 00s} (J2000),
216.756d {+14h 27m 01s} (current),
215.920d {+14h 23m 41s} (1950)
GRB_DEC: +20.000d {+20d 00' 00"} (J2000),
+19.902d {+19d 54' 06"} (current),
+20.225d {+20d 13' 29"} (1950)
GRB_ERROR: 16.80 [arcmin radius, 90% containment, statistical only]
GRB_DATE: 19586 TJD; 7 DOY; 22/01/07
GRB_TIME: 68493.52 SOD {19:01:33.52} UT
TRIGGER_ID: 0x20000000
MISC: 0x40000000
SUN_POSTN: 289.29d {+19h 17m 10s} -22.25d {-22d 15' 04"}
SUN_DIST: 82.40 [deg] Sun_angle= 4.8 [hr] (West of Sun)
MOON_POSTN: 0.72d {+00h 02m 52s} -4.69d {-04d 41' 31"}
MOON_DIST: 141.78 [deg]
MOON_ILLUM: 34 [%]
GAL_COORDS: 19.77, 67.23 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 206.51, 32.42 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi LAT Offline position.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: It is the result of human-in-the-loop processing.
COMMENTS: This is a human generated position of a LAT ground detection.
COMMENTS: This source corresponds to GBM trigger.
- GCN Circular #31407
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
Fermi/LAT GRB 220107B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00103
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 Fermi/LAT 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.
- GCN Circular #31409
M. Arimoto (Kanazawa Univ.), N. Di Lalla (Stanford Univ.), M. Axelsson (KTH & Stockholm Univ.) and S. Cutini (INFN Perugia) report on behalf of the Fermi-LAT Collaboration:
On January 7th, 2022, Fermi-LAT detected high-energy emission from GRB 220107B, which was also detected by Fermi-GBM (trigger 663274898/220107793).
The best LAT on-ground location is found to be
RA, Dec = 216.5, 20.0 (degrees, J2000)
with an error radius of 0.22 deg (90% containment, statistical error only).
This was 54 deg from the LAT boresight at the time of the GBM trigger:
T0 = 19:01:33.52 UT.
The data from the Fermi-LAT show a significant increase in the event rate after the GBM trigger that is temproally and spatially correlated with the GBM emission (2.3 degrees from the GBM location) with high significance. The photon flux above 100 MeV in the time interval 0-500s after the GBM trigger is 1.4E-5 +/- 2.4E-6 ph/cm2/s.
The estimated photon index above 100 MeV is -2.14 +/- 0.17.
The highest-energy photon is a 2.4 GeV event which is observed ~8 seconds after the GBM trigger.
A Swift ToO has been approved for this burst.
The Fermi-LAT point of contact for this burst is Sara Cutini (sara.cutini@pg.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.
- GCN Circular #31411
J. D. Gropp (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester),
J.P. Osborne (U. Leicester), T. Sbarrato (INAF-OAB), P. D'Avanzo
(INAF-OAB), M.G. Bernardini (INAF-OAB), A. Tohuvavohu (U. Toronto) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 220107B (Arimoto et al. GCN Circ. 31409)
in a series of observations tiled on the sky. The total exposure time
is 1.3 ks, distributed over 2 tiles; the maximum exposure at a single
sky location was 1.0 ks. The data were collected between T0+35.7 ks and
T0+36.2 ks, and are entirely in Photon Counting (PC) mode.
An uncatalogued X-ray source is detected and is above the RASS 3-sigma
upper limit at this position, and is therefore likely the GRB
afterglow. Using 546 s of PC mode data and 1 UVOT image, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 216.40652, +20.17064
which is equivalent to:
RA (J2000): 14h 25m 37.56s
Dec(J2000): +20d 10' 14.3"
with an uncertainty of 3.4 arcsec (radius, 90% confidence). This
position is 11.5 arcmin from the Fermi/LAT position. The source has a
mean count rate of 1.3e-01 ct/sec; while we cannot determine at the
present time whether it is fading, the fact that the source is well
above RASS limit strongly suggests it is the X-ray afterglow of GRB
220107B. More data are currently being collected.
The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/xrt_products/TILED_GRB00103/Source1.php.
The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00103.
This circular is an official product of the Swift-XRT team.
- GCN Circular #31412
A. Suresh (IITB), V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute
(IUCAA), V. Bhalerao (IITB), D. Bhattacharya (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 detection of a long GRB 220107B, which was
also detected by Fermi-GBM (trigger 663274898/220107793), Fermi-LAT
(Axelsson et al., GCN 31409) and Swift-XRT (Gropp et al., GCN 31411).
The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2022-01-07 19:01:45.50 UT. Quadrant B was noisy, and we exclude it from
further analysis. The measured peak count rate associated with the burst
is 372 (+44 -42) cts/s above the background in the combined data of
three quadrants (out of four), with a total of 2558 (+225 -239) cts. The
local mean background count rate was 382 (+2 -2) cts/s. Using cumulative
rates, we measure a T90 of 19 (+3 -1) s.
It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve showed multiple peaks
of emission with the strongest peak at 2022-01-07 19:01:35.775 UT. The
measured peak count rate is 826 (+81 -85) cts/s above the background in
the combined Veto data of four quadrants, with a total of 5424 (+496
-555) cts. The local mean background count rate was 1721 (+4 -5) cts/s.
We measure a T90 of 22 (+2 -3) s from the cumulative Veto light curve.
CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=grb [1]. CZTI is built by a TIFR-led
consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC,
and PRL. The Indian Space Research Organisation funded, managed, and
facilitated the project.
Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb
- GCN Circular #31414
P. Veres and C. Meegan (both UAH)
report on behalf of the Fermi GBM Team:
"At 19:01:33.52 UT on 7 January 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220107B (trigger 663274898 / 220107793),
which was also detected by the Fermi LAT (Arimoto et al., GCN 31409).
The GBM on-ground location is consistent with the LAT position.
The GBM light curve consists of multiple separated pulses
with a duration (T90) of about 25 s (50-300 keV).
The time-averaged spectrum from T0-1.7 s to T0+27 s is
best fit by a Band function with Epeak = 391 +/- 21 keV,
alpha = -0.86 +/- 0.03, and beta = -2.40 +/- 0.16.
The event fluence (10-1000 keV) in this time interval is
(2.68 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+12.0 s in the 10-1000 keV band
is 14.4 +/- 0.3 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/"
- GCN Circular #31417
S.Q. Jiang, S.Y. Fu (NAOC), Z.P. Zhu (NAOC, HUST), X. Liu, D. Xu (NAOC),
X. Gao (Urumqi No.1 Senior High School), J.Z. Liu (XAO) report:
We observed the field of GRB 220107B detected by Fermi (Arimoto et al.,
GCN 31409; Veres & Meegan, GCN 31414) and AstroSat (Suresh et al., GCN
31412), using the NEXT-0.6m telescope located at Nanshan, Xinjiang,
China. We obtained 6x300 s frames in the Sloan r-band and 5x300 s frames
in Sloan z-band, starting at 21:30:31 UT on 2022-01-08.
No optical source is detected in our stacked images at the Swift-XRT
position (Gropp et al., GCN 31411). Preliminary photometric results are
as follows:
Tmid-T0 (hr) Filter Upper Limit(5-sigma)
26.97 r >21.3
27.44 z >19.3
calibrated with the nearby PanSTARRS field.
In addition, from Legacy Survey there exists a faint source at the
border of the Swift-XRT error circle at coordinates R.A. (J2000) =
14:25:37.66 and Dec. (J2000) = +20:10:17.01, and magnitudes of g ~
24.62, r ~ 24.51, z ~ 23.32 as well as a photo_redshift = 1.13 +/- 0.23.
The source is not present in SDSS and PanSTARR, and might be the host of
the burst.
- GCN Circular #31418
M. Niwano, R. Hosokawa, Y. Imai, K. L. Murata, Y. Takamatsu, N. Ito, R.
Noto, S. Sato, M. Takaku, R. Yamaguchi, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 220107B (M. Arimoto et al. GCN Circular
#31409, P. A. Evans et al. #31407, J. D. Gropp et al. #31411, A. Suresh
et al. #31412, P. Veres and C. Meegan #31414, S.Q. Jiang et al. #31417)
with the optical three color (g', Rc, and Ic) CCD cameras attached to
the MITSuME 50 cm telescope Akeno. The observation with a series of 60
sec exposures started at 2022-01-08 17:04:13 UT (22 hours after Fermi
trigger). We stacked the images with good conditions. We did not detect
any uncatalogued sources within the XRT error region (J. D. Gropp et al.
GCN Circular #31411). We obtained the 5-sigma limits of the stacked
images as follows.
T0+[hours] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
22.0 2022-01-08 18:58:13 11820 g'>20.7, Rc>20.9, Ic>20.1
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used PS1 catalog for flux calibration.
The magnitudes are expressed in the AB system.
The images were processed in real-time through the MITSuME GPU reduction
pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24;
https://github.com/MNiwano/Eclaire).
- GCN Circular #31427
K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed a second follow-up observation of the
Fermi/LAT-detected GRB 220107B (Arimoto et al., GCN 31409), ~184 ks after
the trigger. The source suggested to be the X-ray counterpart in GCN 31411
(Gropp et al.) has clearly faded, with a power-law slope of alpha = 1.54
(+0.32, -0.24), and is therefore confirmed as the X-ray afterglow.
This circular is an official product of the Swift-XRT team.
- GCN Circular #31430
A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin,
A. Tsvetkova, M. Ulanov, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 220107B
(Fermi-LAT detection: Arimoto et al., GCN 31409;
AstroSat CZTI detection: Suresh et al., GCN 31412;
Fermi-GBM observation: Veres and Meegan et al., GCN 31414)
triggered Konus-Wind at T0=68494.81 s UT (19:01:34.810).
The burst light curve shows a multipeaked structure
started at ~T0-1.2 s with a total duration of ~26.4 s.
The emission is seen up to ~4 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220107_T68494/
As observed by Konus-Wind, the burst
had a fluence of 4.20(-0.78,+0.91)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.728 s,
of 8.07(-2.17,+2.27)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+32.768 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.73(-0.19,+0.27),
the high energy photon index beta = -2.18(-0.38,+0.22),
the peak energy Ep = 309(-65,+72) keV
(chi2 = 54/69 dof).
The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.192 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.58(-0.17,+0.20),
the high energy photon index beta = -2.21(-0.37,+0.21),
the peak energy Ep = 334(-56,+68) keV
(chi2 = 54/70 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
Previous IAU Circulars 