Gamma-ray Burst 220310A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

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Results of Observations

GCN NOTICE

TITLE:           GCN/MAXI NOTICE
NOTICE_DATE:     Thu 10 Mar 22 01:01:46 UT
NOTICE_TYPE:     MAXI Unknown Source Position
EVENT_ID_NUM:      9648001812
EVENT_RA:        168.61d {+11h 14m 27s} (J2000),
                 168.91d {+11h 15m 38s} (current),
                 167.95d {+11h 11m 47s} (1950)
EVENT_DEC:       +23.45d {+23d 27' 04"} (J2000),
                 +23.33d {+23d 19' 47"} (current),
                 +23.72d {+23d 43' 25"} (1950)
EVENT_ERROR:     1.0 [deg radius, stat+sys, 90% containment]
EVENT_FLUX:      348.0 +- 0.0 [mCrab]
EVENT_DATE:      19648 TJD;    69 DOY;   22/03/10
EVENT_TIME:      1702.00 SOD {00:28:22.00} UT
EVENT_TSCALE:    1s
EVENT_EBAND:     Low, 2-4 keV
SUN_POSTN:       350.29d {+23h 21m 10s}   -4.18d {-04d 10' 49"}
SUN_DIST:        160.80 [deg]
MOON_POSTN:       73.54d {+04h 54m 09s}  +24.35d {+24d 21' 15"}
MOON_DIST:        85.12 [deg]
MOON_ILLUM:      46 [%]
GAL_COORDS:      217.07, 67.81 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS:      160.16, 17.04 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS:        MAXI Unknown Source Position. GRB or unknown X-ray Transient.

GCN Circular #31724
V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko,
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D.Cheryasov, Ya.Kechin (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),
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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the MAXI GRB220310.02 (trigger No 648001812,11h 14m 26.88s , +23d 27m 03.6s, R=1) errorbox 1874 sec after trigger time at 2022-03-10 00:59:36 UT, with upper limit up to 17.9 mag. The observations began at zenith distance = 76 deg. The sun altitude is -25.7 deg.
MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the MAXI GRB220310.02 errorbox 8 sec after notice time and 2024 sec after trigger time at 2022-03-10 01:02:06 UT, with upper limit up to 18.7 mag. The observations began at zenith distance = 65 deg. The sun altitude is -41.9 deg.
MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the MAXI GRB220310.02 errorbox 30 sec after notice time and 2046 sec after trigger time at 2022-03-10 01:02:28 UT, with upper limit up to 15.2 mag. The observations began at zenith distance = 50 deg. The sun altitude is -27.8 deg.
The galactic latitude b = 68 deg., longitude l = 218 deg.
Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1905736
We obtain a following upper limits.
```
Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________

    1964 | 2022-03-10 00:59:36 |         MASTER-OAFA | (11h 14m 46.59s , +24d 18m 03.1s) |   C |   180 | 17.0 |        
    2144 | 2022-03-10 00:59:36 |         MASTER-OAFA | (11h 14m 46.59s , +24d 18m 03.1s) |   C |   540 | 17.9 |  Coadd 
    2114 | 2022-03-10 01:02:06 |         MASTER-SAAO | (11h 14m 29.14s , +23d 34m 47.5s) | P\  |   180 | 17.8 |        
    2294 | 2022-03-10 01:02:06 |         MASTER-SAAO | (11h 14m 29.12s , +23d 34m 47.6s) | P\  |   540 | 18.7 |  Coadd 
    2136 | 2022-03-10 01:02:28 |   MASTER-Kislovodsk | (11h 14m 31.95s , +23d 26m 31.3s) |  P- |   180 | 14.8 |        
    2136 | 2022-03-10 01:02:28 |   MASTER-Kislovodsk | (11h 14m 14.53s , +23d 50m 31.6s) |   C |   180 | 13.3 |        
    2281 | 2022-03-10 01:04:53 |         MASTER-OAFA | (11h 14m 53.44s , +24d 17m 02.7s) |   C |   180 | 16.9 |        
    2301 | 2022-03-10 01:05:12 |         MASTER-OAFA | (11h 14m 52.60s , +24d 16m 15.7s) |   C |   180 | 17.4 |        
    2313 | 2022-03-10 01:05:25 |         MASTER-SAAO | (11h 14m 36.14s , +23d 33m 54.3s) | P\  |   180 | 17.9 |        
    2337 | 2022-03-10 01:05:48 |   MASTER-Kislovodsk | (11h 14m 37.19s , +23d 26m 35.9s) |  P- |   180 | 14.4 |        
    2513 | 2022-03-10 01:08:45 |         MASTER-SAAO | (11h 14m 29.52s , +23d 33m 01.4s) | P\  |   180 | 18.0 |        
    2537 | 2022-03-10 01:09:09 |   MASTER-Kislovodsk | (11h 14m 35.47s , +23d 28m 22.4s) |  P- |   180 | 15.2 |        
    2537 | 2022-03-10 01:09:09 |   MASTER-Kislovodsk | (11h 14m 13.90s , +23d 52m 18.3s) |   C |   180 | 13.1 |        
    2520 | 2022-03-10 01:09:51 |         MASTER-OAFA | (11h 08m 46.46s , +22d 56m 48.2s) |   C |    60 | 17.2 |        
```
Filter C is a clear (unfiltred) band.
The observation and reduction will continue. The message may be cited.
GCN Circular #31725
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
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
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
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
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
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
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
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
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
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).

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