GRB 220310A
GCN Circular 31725
Subject
GRB 220310A: MAXI/GSC detection
Date
2022-03-10T01:24:33Z (3 years ago)
From
Motoko Serino at Aoyama Gakuin U. <serino@phys.aoyama.ac.jp>
H. Negoro, M. Nakajima (Nihon U.), M. Serino (AGU), Y. Kawakubo (LSU),
K. Kobayashi, K. Asakura, K. Seino (Nihon U.),
T. Mihara, T. Tamagawa, J. Li, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.),
M. Shidatsu, M. Iwasaki (Ehime U.),
N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA),
Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.),
H. Tsunemi (Osaka U.),
M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ),
K. Yamaoka (Nagoya U.),
M. Sugizaki (NAOC)
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered on a bright uncatalogued X-ray
transient source at 2022-03-10T00:27:57 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (168.612 deg, 23.451 deg) = (11 14 26, +23 27 03) (J2000)
with a 90% C.L. statistical error of 0.16 deg and an additional systematic
uncertainty of 0.1 deg (90% containment radius).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(168.038, 23.325) deg = (11 12 09, +23 19 29) (J2000)
(168.176, 23.093) deg = (11 12 42, +23 05 34) (J2000)
(169.335, 23.670) deg = (11 17 20, +23 40 12) (J2000)
(169.197, 23.903) deg = (11 16 47, +23 54 10) (J2000)
The X-ray flux averaged over the scan was 348 +- 37 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 3/9 22:55 UT
with an upper limit of 20 mCrab.
GCN Circular 31730
Subject
GRB 220310A: CALET Gamma-Ray Burst Monitor detection
Date
2022-03-10T08:13:34Z (3 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (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 220310A detected by MAXI/GSC (Negoro et al., GCN Circ. 31725)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 00:27:58.325 UTC
on 10 March 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1330907255/index.html).
The burst signal was seen by all CGBM detectors.
The burst light curve shows a multi-peaked structure which starts
at T+0.5 sec, peaks at T+33.6 sec,and ends at T+47.0 sec.
The T90 and T50 durations measured by the SGM data are 33.1 +- 8.3 sec
and 12.9 +- 1.2 sec (40-1000 keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1330907255/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 31731
Subject
GRB 220310A: Swift ToO observations
Date
2022-03-10T08:37:40Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the MAXI GRB 220310A.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021482
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 MAXI 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 31732
Subject
GRB 220310A: MASTER optical counterpart detection
Date
2022-03-10T10:09:01Z (3 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov (Lomonosov MSU), D.A.H.Buckley (SAAO),
V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, G.Antipov,
V.Senik, D.Kuvshinov, Ya.Kechin, Yu.Tselik (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),
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),
A. Gabovich, V.Yurkov (Blagoveschensk Educational State University)
MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
started MAXI GRB 220310A (Negoro et al. GCN 31725) observations in
MASTER-OAFA , MASTEr-SAAO, MASTER-Kislovodsk, MASTER-OAGH (Lipunov et al. 31724)
see cover map and OT at https://master.sai.msu.ru/site/master2/observ.php?id=1905736
MASTER OT J111302.33+231508.0 discovery
MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )
discovered GRB optical counterpart at (RA, Dec) = 11h 13m 02.33s +23d 15m 08.0s at 2022-03-10.05882 UT.
The OT unfiltered magnitude at first image is 15.6m (mlim=19.5).
There is no minor planet at this place.
We have reference image on 2018-05-15.77649 UT with unfiltered mlim=19.5m.
Spectral observations are required.
GCN Circular 31738
Subject
GRB 220310A: GIT confirmation of optical afterglow.
Date
2022-03-11T10:23:08Z (3 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 220310A detected by MAXI/GSC H. Negoro et al., (GCN #31725)
and optical afterglow discovered by V. Lipunov (GCN #31732), with 0.7m
GROWTH-India Telescope (GIT). We obtained multiple 300-sec exposures in the
g',r' and i' filters. We clearly detected the afterglow in our stacked
image. The photometric results follow as:
-------------------------------------------------------------------
JD (mid) | T_mid-T0(days) | Filter | Magnitude (AB) |
-------------------------------------------------------------------
2459649.085963 | 0.566 | g' | 19.86 +/- 0.03
2459649.093405 | 0.574 | r' | 19.45 +/- 0.04
2459649.100833 | 0.581 | i' | 19.11 +/- 0.04
2459649.327412 | 0.810 | g' | 20.66 +/- 0.08
2459649.334752 | 0.815 | r' | 20.21 +/- 0.07
2459649.342128 | 0.823 | i' | 19.70 +/- 0.09
-------------------------------------------------------------------
On the basis of fading seen in our observations, we confirm the MASTER OT
J111302.33+231508.0 (GCN #31732) as an afterglow of GRB 220310A. Further,
using our r'-band data, we estimated the index of power-law decay index =
1.99 +/- 0.17. 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 31748
Subject
Konus-Wind detection of GRB 220310A
Date
2022-03-12T08:25:44Z (3 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova,
A. Lysenko, A. Ridnaia, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 220310A
(MAXI/GSC detection: Negoro et al., GCN Circ. 31725;
CALET-CGBM detection: Negoro et al., GCN Circ. 31730)
triggered Konus-Wind at T0=1702.557 s UT (00:28:22.557).
The burst light curve shows an initial weak episode
which starts at ~T0-24 s and ends at ~T0-12 s,
followed by a brighter multipeaked structure
seen up to ~T0+37 s. The total burst duration is ~61 s.
The emission is seen up to ~7 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220310_T01702/
As observed by Konus-Wind, the burst
had a fluence of 3.15(-0.46,+0.54)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+14.144 s,
of 2.32(-0.62,+0.62)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+41.216 s)
is best fit in the 20 keV - 8 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.49(-0.37,+0.61),
the high energy photon index beta = -2.47(-0.67,+0.25),
the peak energy Ep = 138(-27,+32) keV
(chi2 = 75/85 dof).
The spectrum near the maximum count rate
(measured from T0+8.448 s to T0+16.640 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model:
with alpha = -0.70(-0.24,+0.28)
and Ep = 168(-18,+23) keV (chi2 = 67/75 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.5
(chi2 = 67/74 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 31750
Subject
GRB 220310A: [KAO-Egypt] SDSS r, i observation
Date
2022-03-13T08:17:39Z (3 years ago)
From
Ahmed Fouad at NRIAG <ahmed.fouad@nriag.sci.eg>
Ahmed M. Fouad, Ali Takey, Mona Molham, Saad Ata, Ola Ali (NRIAG)
report:
We observed the optical counterpart of GRB 220310A
(H. Negoro et al., GCN 31725)
using a 1.88-m telescope at the Kottamia Astronomical Observatory (KAO),
NRIAG, Egypt.
The source was visible at the position discovered by
(V. Lipunov et al., GCN 31732)
where the SDSS galaxy (ObjID: 1237667910586532614) is located.
KAO observations started from 22:05:22 to 23:06:00 UT on 10-03-2022,
~ 21.5 hrs after the MAXI/GSC trigger.
The combined images of 10 x 150sec were created for SDSS r,i images.
We report the preliminary photometry as:
--------------------------------------------------------
Object / r-mag / r-err / i-mag / i-err
-------------------------------/------------/-----------/------------/---------
GRB220310A by KAO / 19.723 / 0.141 / 19.727 / 0.090
Published SDSS-gal. / 21.94 / 0.19 / 21.62 / 0.22
-------------------------------------------------------------------------------
Aperture photometry was done based on 9 stars around the GRB in
a FoV = 8' x 8', selected from the SDSS-DR16.
The magnitude is not corrected for Galactic extinction
in the direction of the GRB.
GCN Circular 31751
Subject
GRB 220310A: K-800 of Terskol observatory optical upper limit
Date
2022-03-13T10:30:02Z (3 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI, HSE), V. Agletdinov (KIAM), A. Pozanenko (IKI), I.
Sokolov (INASAN, KIAM), N. Pankov (HSE) report on behalf of GRB IKI FuN:
We observed GRB 220310A (Negoro et al., GCN 31725; Yoshida et al., GCN
31730; Svinkin et al., GCN 31748) with K-800 telescope of Terskol
observatory starting on Mar. 12 (UTC) 21:34:44. We do not detect the
optical afterglow (Lipunov et al., GCN 31732; Kumar et al., GCN 31738;
Fouad et al., GCN 31750). Preliminary photometry of the field in
Clear filter is following
Date UT start t-T0 Filter Exp. OT Err UL(3sigma)
2022-03-12 21:34:44 2.89151 Clear 68*30 n/d n/d 20.8
The photometry is based on the nearby SDSS-DR12 stars R (Lupton
transformations)
R.A. Dec R
11:13:05.99760 +23:17:03.0084 16.852
11:12:35.64984 +23:13:33.4308 16.911
GCN Circular 31756
Subject
IPN triangulation of GRB 220310A
Date
2022-03-14T21:25:39Z (3 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the HEND/Mars-Odyssey team,
A. Ridnaia, D. Frederiks, D. Svinkin, A. Lysenko,
and T. Cline on behalf of the Konus-Wind team, and
W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr,
and A.S. Gardner on on behalf of the GRS-Odyssey GRB team,
report:
The long-duration GRB 220310A
(MAXI/GSC detection: Negoro et al., GCN Circ. 31725;
CALET-CGBM detection: Yoshida et al., GCN Circ. 31730;
Konus-Wind detection: Svinkin et al., GCN Circ. 31748)
was detected by MAXI(GSC), CALET (GBM), Konus-Wind,
and Mars-Odyssey (HEND) at about 1702 s UT (00:28:22).
We have triangulated it to a Konus-HEND annulus centered at
RA(2000)=124.878 deg (08h 19m 31s) Dec(2000)=+20.557 deg (+20d 33' 25"),
whose radius is 40.183 +/- 0.041 deg (3 sigma).
The MAXI/GSC localization is consistent with the annulus.
The position of the optical transient J111302.33+231508.0
(Lipunov et al., GCN Circ. 31732) is inside the annulus at 0.7 arcmin
from its center line.
The positional and temporal coincidence of this burst with the OT
supports the conclusion that the OT is the GRB counterpart.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB220310_T01702/IPN
GCN Circular 31765
Subject
GRB 220310A: MITSuME Akeno optical observation
Date
2022-03-18T00:15:23Z (3 years ago)
From
Ryohei Hosokawa at Tokyo Institute of Technology <hosokawa@hp.phys.titech.ac.jp>
R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, N. Ito, Y. Takamatsu,
R. Noto, S. Sato, M. Takaku, R. Yamaguchi, Y. Yatsu, and N. Kawai
(Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 220310A (H. Negoro et al. GCN Circular
#31725, A. Yoshida et al. GCN Circular #31730, P. A. Evans et al. GCN
Circular #31731, V. Lipunov et al. GCN Circular #31732, H. Kumar et
al. GCN Circular #31738, D. Svinkin et al. GCN Circular #31748, Ahmed
M. Fouad et al. GCN Circular #31750, S. Belkin et al. GCN Circular
#31751, A.S. Kozyrev et al. GCN Circular #31756) 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 2022-03-10 15:13:33 UT (14.7 hours after MAXI trigger). We
stacked the images with good conditions. We marginally detected the
optical counterpart candidate at the position reported previously (V.
Lipunov et al. GCN Circular #31732, H. Kumar et al. GCN Circular
#31738, Ahmed M. Fouad et al. GCN Circular #31750).
The magnitudes of the source are as follows.
T0+[hour] | Band | MID-UT | T-EXP[sec] | candidate magnitude
------------------------------------------------------------
16.1 | g' |2022-03-10 16:32:13 | 6720.0 | 19.62+/-0.18
16.1 | Rc |2022-03-10 16:32:13 | 6780.0 | 19.67+/-0.18
16.1 | Ic |2022-03-10 16:32:13 | 6780.0 | 19.05+/-0.23
------------------------------------------------------------
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).