GRB 220118A
GCN Circular 31519
Subject
GRB 220118A: TARGET optical upper limit
Date
2022-01-23T08:08:05Z (4 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
Y. Koyanagi, K. Hasuda, T. Sakamoto (AGU)
We observed the field of GRB 220118A detected by Swift
(Klingler et al., GCN Circ. 31490) with The AGU Robotic
Gravitational-wave Electromagnetic Telescope (TARGET)
equipped with the Veloce RH200 (20 cm OTA) and the large
format CCD camera (ATK11000) located at the Machida field
of Aoyama Gakuin University. 20 images of 60 sec exposures
were taken in the R filter starting from January 18
18:25:04 (UT) about 4.4 minutes after the trigger and
stopped on January 18 18:57:56 (UT). We do not detect the
optical afterglow both in the individual images and the
stacked image at the enhanced XRT position (Goad, et al.
GCN Circ. 31495). The estimated five sigma upper limit of
the combined image (total exposure of 1200 sec)
is ~16.1 mag using the USNO-B1 catalog.
GCN Circular 31507
Subject
GRB 220118A: 2.2m CAHA/CAFOS detections
Date
2022-01-20T17:33:32Z (4 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
D. A. Kann (HETH/IAA-CSIC), D. B. Malesani (Radboud Univ. and DAWN/NBI),
A. de Ugarte Postigo (Obs. Cote d'Azur), C. C. Thoene (HETH/ASU CAS
Ondrejov), M. Blazek (HETH), J. F. Agui Fernandez (HETH/IAA-CSIC), A.
Guijarro, and A. Fernandez (both CAHA) report:
We observed the afterglow of GRB 220118A (Swift detection: Klingler et
al., GCN #31490; Fermi/GBM Detection: Fletcher et al., GCN #31506;
afterglow detections: Hosokawa et al., GCN #31493; Kumar et al., GCN
#31496; Belles & Klingler, GCN #31498) with CAFOS, mounted on the 2.2 m
telescope, at the Calar Alto Observatory (Almeria, Spain). The
observation started at 01:09:11 UT on 19 January 2022 (6.81 hr after the
GRB) and consisted of 10 x 150 s integrations in the r' band and 9 x 150
s in the i' band. Observations were hampered by the Wolf Moon, but
otherwise conditions were very good (1".1 seeing, very good
transparency).
The afterglow is faintly detected in the stacked images in each filter.
Against several Pan-STARRS stars, we measure:
r' = 22.40 +/- 0.18 mag at 0.29916 d after trigger, and
i' = 22.07 +/- 0.17 mag at 0.32064 d after trigger.
No further observations are planned.
GCN Circular 31506
Subject
GRB 220118A: Fermi GBM detection
Date
2022-01-20T16:39:29Z (4 years ago)
From
Boyan A. Hristov at UAH <bah0046@uah.edu>
Cori Fletcher (USRA) and C. Meegan (UAH) and Boyan A. Hristov
(UAH) report on behalf of the Fermi GBM Team:
"At 18:20:35.84 UT on 18 January 2022, the Fermi Gamma-Ray
Burst Monitor (GBM) triggered and located GRB 220118A
(trigger 664222840 / 220118764), which was also detected by
the Swift BAT/XRT (N. J. Klingler et al. 2022, GCN 31490) and
observed by SWIFT UVOT (A. Belles et al. 2022, GCN 31498).
The Fermi GBM Final Real-time Localization (GCN 31489) is
consistent with the Swift position.
The GBM light curve shows a single peak with a duration (T90)
of about 19 s (50-300 keV). The time-averaged spectrum from
T0+0.003 s to T0+18.176 s is best fit by a power law function
with an exponential high-energy cutoff. The power law index is
-1.08 +/- 0.09 and the cutoff energy, parameterized as Epeak,
is 148.30 +/- 17.50 keV.
The event fluence (10-1000 keV) in this time interval is
(3.017 +/- 0.182)E-06. The 1-sec peak photon flux measured
starting from T0+3.39204 s in the 10-1000 keV band is
4.0 +/- 0.28 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 31505
Subject
GRB 220118A: COATLI Optical Observations
Date
2022-01-20T14:10:36Z (4 years ago)
From
Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada <mpereyra@astro.unam.mx>
Margarita Pereyra (UNAM), Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L.
Becerra (UNAM), Oc��lotl L��pez (UNAM), Diego Gonz��lez (UNAM), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Eleonora Troja (GSFC) and Tzveti
Dimitrova (ASU) report:
We observed the field of GRB 220118A (Klingler et al., GCN Circ. 31490 ;
Fermi GBM Team, GCN Circ. 31489) with the COATLI 50-cm telescope and
interim imager at the Observatorio Astron��mico Nacional on the Sierra de
San Pedro M��rtir (http://coatli.astroscu.unam.mx) from 2022-01-19 07:32 UTC
to 13:26 UTC (13.24 to 19.1 hours after the trigger), obtaining a total of
16215 seconds of exposure in the r filter.
We do not detect any uncataloged sources in the enhanced XRT error region
(Goad et al., GCN Circ. 31495) to a 3-sigma limit of r = 22.9, which
confirms the afterglow fading reported by the GTI and Swift/UVOT teams
(Kumar et al., GCN Circ. 31496; Belles et al., GCN Circ. 31498)
Our r magnitudes are calibrated against the Pan-STARRS1 catalog, are on an
approximate AB system (Becerra et al., 2019, ApJ, 872, 118), and are not
corrected for Galactic extinction in the direction of the GRB.
We thank the COATLI technical team and the staff of the Observatorio
Astron��mico Nacional.
GCN Circular 31502
Subject
GRB 220118A: NUTTelA-TAO / BSTI Early Optical Limits (Preliminary)
Date
2022-01-20T08:11:17Z (4 years ago)
From
Toktarkhan Komesh at Nazarbayev University <toktarkhan.komesh@nu.edu.kz>
T. Komesh (NU), B. Grossan (UCB, NU), Z. Maksut (NU), M. Krugov (FAI),��
E. Linder (UCB, NU), E. Abdikamalov (NU), K. Baigarin (NU), G. F. Smoot
(HKUST, UCB, NU), report on behalf of the Energetic Cosmos Laboratory:
The Nazarbayev University Transient Telescope at Assy-Turgen
Astrophysical Observatory (NUTTelA-TAO) observed the field of GRB
220118A 11 s after receipt an automated GCN / BAT position alert,
observing in Sloan i' band, with the Burst Simultaneous Three-Channel
Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14).
We started observations at 18:21:08 UT on 2022-01-18, 30 s after the BAT
trigger. Observations were made in cloudy conditions starting at about
25 deg. target altitude. No source consistent with the XRT (M.R. Goad et
al., GCN Circ. 31495) was detected.�� We report the following results:
start time������ t-t0(s)�� end time�������������� ULi'������������ exposure_time (s)
------------������ --------�� ------------������������������ ------ --------------------
18:21:08 ������ 30 �� �� 18:22:08 ���������������� 15.3 ������������������ 60
18:22:32 ������ 114 �� 18:25:02 ���������������� 16.0 �������������� 150
18:25:02�������� 264 �� 18:27:32������������������ 16.4���������������� 150
18:27:32�������� 414 �� 18:30:02������������������ 17.2���������������� 150
18:30:02�������� 564 �� 18:32:32�������������� �� 17.4 �� �� �� �� 150
start time is in UT. t-t0(s) gives the time since trigger, in seconds.
UL i', gives the 5 sigma upper limit sensitivity in magnitudes, for
images co-added to the given exposure time. The first row in the table
corresponds to co-adds of an initial short exposure image sequence of
7.5 s. The following rows correspond to co-adds from a continuing series
of 15 s exposures.�� Calibration was done with the 4 bright Pan-STARRS
catalog stars on our images.
We caution the reader that these are preliminary results, without color
or other corrections. Please also note that times are approximate.
----------------------------------
NU = Nazarbayev University, Nur-Sultan, Kazakhstan
UCB = University of California, Berkeley, USA
HKUST = Hong Kong University of Science and Technology
FAI = Fesenkov Astrophysical Institute, Kazakhstan
The NUTTelA-TAO Team acknowledges the support of the staff of the
Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the
Fesenkov Astrophysical Institute, Almaty, Kazkhstan.
GCN Circular 31499
Subject
GRB 220118A: Swift-BAT refined analysis
Date
2022-01-19T21:02:06Z (4 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
N. J. Klingler (GSFC/UMBC/CRESSTII), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC/UMBC), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220118A (trigger #1093742)
(Klingler et al., GCN Circ. 31490). The BAT ground-calculated position is
RA, Dec = 192.277, 22.911 deg which is
RA(J2000) = 12h 49m 06.4s
Dec(J2000) = +22d 54' 37.8"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.
The mask-weighted light curve shows a single-peaked structure that
starts at ~T-4 s, peaks at ~T+1 s, and ends at ~T+10 s.
T90 (15-350 keV) is 10.61 +- 1.78 sec (estimated error including
systematics).
The time-averaged spectrum from T-3.90 to T+9.54 sec is best fit
by a simple power-law model. The power law index of the time-averaged
spectrum is 1.67 +- 0.12. The fluence in the 15-150 keV band
is 1.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from
T+0.68 sec in the 15-150 keV band is 3.3 +- 0.5 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1093742/BA/
GCN Circular 31498
Subject
GRB 220118A: Swift/UVOT Detection
Date
2022-01-19T17:27:54Z (4 years ago)
From
Alexander Belles at PSU/Swift <aub1461@psu.edu>
A. Belles (PSU) and N. J. Klingler (GSFC/UMBC/CRESSTII)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 220118A
99 s after the BAT trigger (Klingler et al., GCN Circ. 31490).
A fading source consistent with the XRT position
(Goad et al., GCN Circ. 31495) is detected in the initial
UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 12:49:04.52 = 192.26885 (deg.)
Dec (J2000) = +22:54:56.2 = 22.91562 (deg.)
with an estimated uncertainty of 0.44 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early
exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
wh 119 268 145 17.73+/-0.07
wh 11382 11797 404 >20.26
u 276 454 175 17.33+/-0.12
b 10470 11377 885 >20.56
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.025 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 31496
Subject
GRB 220118A: GIT optical observations
Date
2022-01-19T11:29:04Z (4 years ago)
From
Harsh Kumar at Indian Inst of Tech,Bombay <harshkosli13@gmail.com>
H. Kumar(IITB), J. Stanzin (IAO), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA) report on behalf of the GIT team:
We observed GRB 220118A detected by Fermi-GBM (GCN #31489) and Swift-BAT (N.
J. Klingler et al., GCN #31490) with 0.7m GROWTH-India Telescope (GIT). We
obtained multiple 300-sec exposures in the g', r', i' and z' filters. We
detect a faint (~ 3.5 sigma) afterglow in our stacked images. The obtained
upper magnitudes and upper limits follow as:
---------------------------------------------------------------------------------
JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Mag(AB)/Lim_mag
(5-sigma)
---------------------------------------------------------------------------------
2459598.2802666 | 0.38 | 300 | r' | > 17.23
2459598.2839984 | 0.47 | 300 | i' | > 17.78
2459598.2877512 | 0.56 | 300 | g' | > 17.38
2459598.2915685 | 0.65 | 300 | z' | > 16.99
2459598.3202152 | 1.34 | 3000(stacked) | r' | > 19.84
---------------------------------------------------------------------------------
2459598.3568823 | 2.22 | 3000(stacked) | i' | 20.35 +/- 0.05
2459598.5042212 | 5.75 | 3000(stacked) | r' | 21.53 +/- 0.09
---------------------------------------------------------------------------------
The detected magnitudes and upper limits are in agreement with R. Hosokawa
et al., (GCN #31493). The magnitudes are calibrated against PanSTARRS DR1
(Chambers et al., 2016) and not corrected for Galactic extinction.
The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics (IIA) and the
Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and
IUSSTF. It is located at the Indian Astronomical Observatory (Hanle),
operated by IIA. We acknowledge funding by the IITB alumni batch of 1994,
which partially supports operations of the telescope. Telescope technical
details are available at https://sites.google.com/view/growthindia/.
GCN Circular 31495
Subject
GRB 220118A: Enhanced Swift-XRT position
Date
2022-01-19T10:09:15Z (4 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.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 300 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220118A, 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 = 192.26849, +22.91528 which is equivalent
to:
RA (J2000): 12h 49m 4.44s
Dec (J2000): +22d 54' 55.0"
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.
GCN Circular 31493
Subject
GRB 220118A: MITSuME Akeno optical observation
Date
2022-01-18T23:03:56Z (4 years ago)
From
Ryohei Hosokawa at Tokyo Institute of Technology <hosokawa@hp.phys.titech.ac.jp>
R. Hosokawa, N. Ito, K. L. Murata, M. Niwano, Y. Imai, Y. Takamatsu,
R. Yamaguchi, R. Noto, S. Sato, M. Takaku, Y. Yatsu, and N. Kawai
(Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 220118A(The Fermi GBM team GCN Circular
#31489, N. J. Klingler et al. GCN Circular #31490) with the optical
three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope Akeno. The observation started at 2022-01-18 18:21:29 UT (51
sec after Swift BAT trigger). We stacked the images with good
conditions. We detected the optical afterglow candidate reported by
the Swift UVOT observation (N. J. Klingler et al. GCN Circular
#31490).
The magnitudes and the 5-sigma limits of the stacked images are as follows.
T0+[sec] MID-UT T-EXP[sec] magnitude(or 5-sigma limits) 5-sigma limits
-----------------------------------------------------------------------------------------------------------------
56 | 2022-01-18 18:21:34 | 10 |g'>15.9, Rc>16.8,
Ic>16.8 | g'>15.9, Rc>16.8, Ic>16.8 |
84 | 2022-01-18 18:22:02 | 40 |g'=18.36+/-0.70, Rc=18.57+/-0.78,
Ic>17.5 | g'>17.3, Rc>17.9, Ic>17.5 |
171 | 2022-01-18 18:23:29 | 50 |g'=17.45+/-0.20, Rc=16.90+/-0.15,
Ic=17.12+/-0.41| g'>17.5, Rc>18.1, Ic>17.5 |
256 | 2022-01-18 18:24:54 | 60 |g'=17.31+/-0.18, Rc=16.87+/-0.09,
Ic=16.64+/-0.11| g'>17.7, Rc>18.5, Ic>18.1 |
325 | 2022-01-18 18:26:03 | 60 |g'=17.31+/-0.22, Rc=17.31+/-0.13,
Ic=17.08+/-0.15| g'>17.7, Rc>18.4, Ic>18.1 |
535 | 2022-01-18 18:29:33 | 300 |g'=18.21+/-0.17, Rc=17.80+/-0.10,
Ic=17.47+/-0.10| g'>18.7, Rc>19.5, Ic>19.1 |
1471 | 2022-01-18 18:45:09 | 1020 |g'=19.82+/-0.33, Rc=19.26+/-0.14,
Ic=18.81+/-0.15| g'>19.5, Rc>20.3, Ic>19.9 |
-----------------------------------------------------------------------------------------------------------------
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 31491
Subject
Swift GRB 220118A: Global MASTER-Net observations report
Date
2022-01-18T19:56:19Z (4 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
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-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) was pointed to the Swift GRB 220118A ( N. J. Klingler et al., GCN 31490) errorbox 4483 sec after notice time and 4505 sec after trigger time at 2022-01-18 19:35:43 UT, with upper limit up to 15.9 mag. The observations began at zenith distance = 29 deg. The sun altitude is -35.6 deg.
The galactic latitude b = 86 deg., longitude l = 303 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1853598
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
4595 | MASTER-Amur | C | 180 | 14.5 |
5133 | MASTER-Amur | C | 60 | 15.0 |
5353 | MASTER-Amur | C | 180 | 15.9 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 31490
Subject
GRB 220118A: Swift detection of a burst with an optical counterpart
Date
2022-01-18T18:33:38Z (4 years ago)
From
Kim Page at U.of Leicester <kimlpage1978@gmail.com>
N. J. Klingler (GSFC/UMBC/CRESSTII), E. Ambrosi (INAF-IASFPA),
A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC & INAF-OAR), S. Dichiara (PSU),
J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), B. Sbarufatti (PSU) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 18:20:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220118A (trigger=1093742). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 192.274, +22.909 which is
RA(J2000) = 12h 49m 06s
Dec(J2000) = +22d 54' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of about 20 sec. The peak count rate
was ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 18:22:08.3 UT, 90.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 192.26936,
22.91600 which is equivalent to:
RA(J2000) = 12h 49m 04.65s
Dec(J2000) = +22d 54' 57.6"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 29 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.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.25 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.4
(+2.60/-2.24) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 4.57e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 99 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 12:49:04.53 = 192.26888
DEC(J2000) = +22:54:56.2 = 22.91562
with a 90%-confidence error radius of about 0.75 arc sec. This position is 1.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.83 with a 1-sigma error of about 0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.025.
Burst Advocate for this burst is N. J. Klingler (noelklin AT umbc.edu).
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/)
GCN Circular 31489
Subject
GRB 220118A: Fermi GBM Final Real-time Localization
Date
2022-01-18T18:30:59Z (4 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 18:20:35 UT on 18 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220118A (trigger 664222840.838306 / 220118764).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 191.4, Dec = 23.6 (J2000 degrees, equivalent to J2000 12h 45m, 23d 36'), with a statistical uncertainty of 5.0 degrees.
The angle from the Fermi LAT boresight is 52.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_skymap_all_bn220118764.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_healpix_all_bn220118764.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_lc_medres34_bn220118764.gif