GRB220930A

This page lists all entries on GRB220930A in GRBweb

Summary IPN Swift GCN 32603 GCN 32604 GCN 32605 GCN 32606 GCN 32607 GCN 32608 GCN 32609 GCN 32610 GCN 32611 GCN 32612 GCN 32613 GCN 32614 GCN 32617 GCN 32625

Summary table
Variable Value Source
T0 11:11:52 UTC GCN_circulars,Swift Det
ra 64.7172° Swift
decl 13.3490° Swift
pos_error 2.85e-04° Swift
GBM_located False
mjd 59852.466574074075 GCN_circulars,Swift Det
IPN table
GRB_name GRB220930A
ra 64.7375°
decl 13.3500°
pos_error 5.00e-02°
Swift table
GRB_name GRB220930A
t_trigger 11:11:52 UTC
ra 64.7172°
decl 13.3490°
pos_error 2.85e-04°
GCN 32603 table
GRB_name GRB220930A
GCN_number 32603
Detection_method Swift Det
t_trigger 11:11:52 UTC
ra 64.7370°
decl 13.3520°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32603 SUBJECT: GRB 220930A: Swift detection of a burst DATE: 22/09/30 11:36:03 GMT FROM: Kim Page at U.of Leicester S. B. Cenko (GSFC), A. P. Beardmore (U Leicester), C. Gronwall (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester) and T. M. Parsotan (GSFC/UMBC/CRESSTII) report on behalf of the Neil Gehrels Swift Observatory Team: At 11:11:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 220930A (trigger=1125809). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 64.737, +13.352 which is RA(J2000) = 04h 18m 57s Dec(J2000) = +13d 21' 06" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 20 sec and a secondary peak at about 70 seconds after the trigger time. The peak count rate was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 11:14:42.1 UT, 170.0 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 64.7149, 13.3500 which is equivalent to: RA(J2000) = 04h 18m 51.58s Dec(J2000) = +13d 21' 00.0" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 77 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 2.5 s image was 3.09e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 179 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.639. Burst Advocate for this burst is S. B. Cenko (brad.cenko AT nasa.gov). 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 32604 table
GRB_name GRB220930A
GCN_number 32604
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 32604 SUBJECT: GRB 220930A: COATLI Upper Limits DATE: 22/09/30 12:09:45 GMT FROM: Alan M Watson at UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Simone Dichiara (PSU), Tzveti Dimitrova (ASU), Océlotl López (UNAM), Diego González (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita Pereyra (UNAM), Eleonora Troja (UTV/ASU) and report: We observed the field of the Swift/BAT GRB 220930A (Cenko, GCN Circ. 32603) with the COATLI 50-cm telescope and HUITZI f/8 imager at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir (http://coatli.astroscu.unam.mx) from 2022-09-30 11:22 UTC to 11:59 UTC (10.5 to 48 minutes after the trigger), obtaining a total of 1920 seconds of exposure in the r filter. We do not detect any uncataloged sources in the XRT error region (Cenko, GCN Circ. 32603) to a 3-sigma limit of r = 22.5. Our photometry is calibrated against the Pan-STARRS1 catalog, are on an approximate AB system, and are not corrected for Galactic extinction in the direction of the GRB. We thank the COATLI/HUITZI technical team and the staff of the Observatorio Astronómico Nacional.
GCN 32605 table
GRB_name GRB220930A
GCN_number 32605
Detection_method Swift-XRT Other
ra 64.7172°
decl 13.3492°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32605 SUBJECT: GRB 220930A: Prompt enhanced Swift-XRT position DATE: 22/09/30 12:16:14 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 220930A, we find an enhanced XRT position of the afterglow: RA, Dec: 64.71723, 13.34924 which is equivalent to: RA (J2000) = 04 18 52.14 Dec (J2000) = +13 20 57.3 with an uncertainty of 1.9 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/1125809. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team.
GCN 32606 table
GRB_name GRB220930A
GCN_number 32606
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 32606 SUBJECT: GRB 220930A: BOOTES-5/JGT early optical upper limit DATE: 22/09/30 13:19:08 GMT FROM: Youdong HU at IAA-CSIC Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, I. Perez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar and I. Carrasco (UMA), I. H. Park (SKKU) on behalf of a larger collaboration, report: Following the detection of GRB 220930A by Swift (Cenko et al. GCNC 32603), the BOOTES-5/JGT 0.6m robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) observed the GRB location starting on Sep. 30, 11:13:05 UT (~ 73 s after trigger). In the early co-added image (18 x 10 s exposures in the clear filter), no optical afterglow is detected within the enhanced Swift/XRT error region (Evans et al. GCNC 32605) down to 21.0 mag, which is consistent with the limits reported by UVOT (Cenko et al. GCNC 32603) and COATLI (Watson et al. GCNC 32604). We thank the staff at Observatorio Astronomico Nacional in San Pedro Martir for their excellent support.
GCN 32607 table
GRB_name GRB220930A
GCN_number 32607
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 32607 SUBJECT: Swift GRB 220930A: Global MASTER-Net observations report DATE: 22/09/30 15:08:15 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs 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-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 220930A ( S. B. Cenko et al., GCN 32603) errorbox 11539 sec after notice time and 11568 sec after trigger time at 2022-09-30 14:24:40 UT, with upper limit up to 19.3 mag. The observations began at zenith distance = 69 deg. The sun altitude is -41.3 deg. The galactic latitude b = -25 deg., longitude l = 181 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2105765 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 11659 | MASTER-Amur | C | 180 | 19.3 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 32608 table
GRB_name GRB220930A
GCN_number 32608
Detection_method Swift-XRT Det
ra 64.7172°
decl 13.3490°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32608 SUBJECT: GRB 220930A: Enhanced Swift-XRT position DATE: 22/09/30 15:35:59 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 892 s of XRT Photon Counting mode data and 1 UVOT images for GRB 220930A, 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 = 64.71717, +13.34902 which is equivalent to: RA (J2000): 04h 18m 52.12s Dec (J2000): +13d 20' 56.5" 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 32609 table
GRB_name GRB220930A
GCN_number 32609
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 32609 SUBJECT: GRB 220930A: Swift/UVOT Upper Limits DATE: 22/09/30 20:39:10 GMT FROM: Alexander Belles at PSU/Swift A. Belles (PSU) and S. B. Cenko (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 220930A 180 s after the BAT trigger (Cenko et al., GCN Circ. 32603). No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 32608) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag wh_FC 180 330 147 >20.71 u_FC 338 588 245 >19.95 wh 618 1368 225 >20.93 v 669 1418 97 >18.73 b 594 1343 77 >19.59 u 744 1318 58 >18.99 w1 719 1467 77 >18.83 m2 693 1442 77 >18.59 w2 644 1393 97 >19.10 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.639 in the direction of the burst (Schlegel et al. 1998).
GCN 32610 table
GRB_name GRB220930A
GCN_number 32610
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 32610 SUBJECT: GRB 220930A: LCOGT Optical Upper Limits DATE: 22/10/01 04:03:35 GMT FROM: Robert Strausbaugh at University of Minnesota R. Strausbaugh (University of Minnesota), A. Cucchiara (College of Marin) report on behalf of a larger collaboration: We observed the Swift GRB 220930A (Cenko et al., GCN 32603) field with the LCOGT 1-meter Sinistro instrument at the South African Astronomical Observatory site, on October 1, from 00:42 to 01:24 (corresponding to 13.52 to 14.22 hours from the GRB trigger time) with the SDSS i and r filters. We performed a series of 3x300s exposures in i and r bands. We do not detect any uncatalogued sources in the XRT enhanced error region (Evans et al., GCN 32608), in either band, consistent with other optical upper limits (Watson et al., GCN 32604; Hu et al., GCN 32606; Belles et al., GCN 32609). The following upper limits are calculated using the Pan-STARRS catalog as reference: r > 22.08 i > 21.73 These magnitudes are not corrected for galactic extinction.
GCN 32611 table
GRB_name GRB220930A
GCN_number 32611
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 32611 SUBJECT: GRB 220930A: Swift-XRT refined Analysis DATE: 22/10/01 04:58:30 GMT FROM: Phil Evans at U of Leicester V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti (INAF-OAB), D.N. Burrows (PSU), J. D. Gropp (PSU), S. Dichiara (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. D'Ai (INAF-IASFPA) and S.B. Cenko report on behalf of the Swift-XRT team: We have analysed 6.9 ks of XRT data for GRB 220930A (Cenko et al. GCN Circ. 32603), from 160 s to 35.9 ks after the BAT trigger. The data comprise 390 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 32605). The late-time light curve (from T0+5.1 ks) can be modelled with a power-law decay with a decay index of alpha=1.28 (+/-0.11). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.59 (+/-0.08). The best-fitting absorption column is 4.9 (+0.6, -0.5) x 10^21 cm^-2, in excess of the Galactic value of 2.8 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.82 (+0.16, -0.15) and a best-fitting absorption column of 6.4 (+1.2, -1.1) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.7 x 10^-11 (7.3 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.4 (+1.2, -1.1) x 10^21 cm^-2 Galactic foreground: 2.8 x 10^21 cm^-2 Excess significance: 5.4 sigma Photon index: 1.82 (+0.16, -0.15) If the light curve continues to decay with a power-law decay index of 1.28, the count rate at T+24 hours will be 0.017 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.3 x 10^-13 (1.3 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01125809. This circular is an official product of the Swift-XRT team.
GCN 32612 table
GRB_name GRB220930A
GCN_number 32612
Detection_method Swift-BAT Det
ra 64.7250°
decl 13.3530°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32612 SUBJECT: GRB 220930A: Swift-BAT refined analysis DATE: 22/10/02 03:35:10 GMT FROM: Sibasish Laha at GSFC S. D. Barthelmy (GSFC), 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), T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 220930A (trigger #1125809) (Cenko et al., GCN Circ. 32603). The BAT ground-calculated position is RA, Dec = 64.725, 13.353 deg which is RA(J2000) = 04h 18m 54.0s Dec(J2000) = +13d 21' 12.0" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 11%. The BAT light curve showed a complex structure with a duration of about 200 sec. T90 (15-350 keV) is 180.47 +- 104.20 sec (estimated error including systematics). The time-averaged spectrum from T-0.42 to T+235.67 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.59 +- 0.13. The fluence in the 15-150 keV band is 5.5 +- 0.4 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T-0.31 sec in the 15-150 keV band is 6.2 +- 1.0 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/1125809/BA/
GCN 32613 table
GRB_name GRB220930A
GCN_number 32613
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 32613 SUBJECT: GRB 220930A: AstroSat CZTI detection DATE: 22/10/02 05:27:01 GMT FROM: Gaurav Waratkar at IIT,Bombay R. Gopalakrishnan (IUCAA), V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/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 the detection of a long GRB 220930A which was also detected by Swift-BAT (Cenko et at., GCN 32603), Swift-XRT (Evans et al., GCN 32608), and Swift/UVOT (Belles et al., GCN 32609). The source was clearly detected in the 20-200 keV energy range. The light curve peaks at 2022-09-30 11:11:52.50 UTC. The measured peak count rate associated with the burst is 435 (+49, -54) counts/s above the background in the combined data of all quadrants, with a total of 1508 (+301, -353) counts. The local mean background count rate was 501 (+3, -3) counts/s. Using cumulative rates, we measure a T90 of 9 (+8, -5) s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2022-09-30 11:11:51.80 UTC. The measured peak count rate is 911 (+80, -88) counts/s above the background in the combined Veto data of all quadrants, with a total of 3694 (+515, -521) counts. The local mean background count rate was 1597 (+6, -7) counts/s. We measure a T90 of 13 (+5, -5) 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. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.
GCN 32614 table
GRB_name GRB220930A
GCN_number 32614
Detection_method Konus-Wind Det
t_trigger 11:11:52.503 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 32614 SUBJECT: Konus-Wind detection of GRB 220930A DATE: 22/10/02 17:09:27 GMT FROM: Anna Ridnaia at Ioffe Institute 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 220930A (Swift-BAT detection: Cenko et al., GCN 32603, Barthelmy et al., GCN 32612; AstroSat-CZTI detection: Gopalakrishnan et al., GCN 32613) triggered Konus-Wind at T0=40312.503 s UT (11:11:52.503). The burst light curve shows a multipeaked structure which starts at ~T0-1.5 s and has a total duration of ~76.0 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/GRB220930_T40312/ As observed by Konus-Wind, the burst had a fluence of 1.78(-0.64,+0.98)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+0.960 s, of 5.39(-2.28,+2.15)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+73.984 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.06(-1.06,+1.43), the high energy photon index beta = -2.41(-0.51,+0.46), the peak energy Ep = 198(-58,+181) keV (chi2 = 91/98 dof). The spectrum near the maximum count rate (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.38(-0.56,+0.66), the high energy photon index beta = -2.25(-1.42,+0.23), the peak energy Ep = 215(-52,+121) keV (chi2 = 97/96 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 32617 table
GRB_name GRB220930A
GCN_number 32617
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 32617 SUBJECT: GRB 220930A: AbAO Optical Upper Limit DATE: 22/10/02 22:48:28 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (IKI), R. Ya. Inasaridze (AbAO), A. Pozanenko (IKI), S. Belkin (IKI, HSE), V. R. Ayvazian (AbAO), D. Datashvili (AbAO), G. V. Kapanadze (AbAO) report on behalf of GRB IKI FuN: We observed the field of GRB 220930A (Cenko et. al, GCN 32603) with AS-32 telescope of Abastumani Observatory (AbAO). We do not detect any objects within enhanced Swift-XRT error region (Evans et. al, GCN 32608). The 3-sigma upper limit is following: Date, UT start, t-T0, Exp., Filter, OT, Err, UL(3 sigma) (mid, days) 2022-09-30 22:09:17 0.48085 70*60 R n/d n/d 22.3 The photometry is based on nearby USNO-B1.0 stars USNO_B10_id R2 1033-0057261 16.60 1033-0057239 17.39 The obtained result is consistent with non-detections reported earlier (Watson et. al, GCN 32604; Hu et al, GCN 32606; Lipunov et al, GCN 32607; Belles and Cenko, GCN 32609; Strausbaugh and Cucchiara, GCN 32610).
GCN 32625 table
GRB_name GRB220930A
GCN_number 32625
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 32625 SUBJECT: GRB 2209030A: MITSuME Akeno optical upper limits DATE: 22/10/05 08:46:19 GMT FROM: Tateda Mahiro at Tokyo Tech M. Tateda, I.Takahashi, K. L. Murata, Y. Imai, N. Ito, M. Niwano, S. Sato, N. Higuchi, Y. Takamatsu, R. Hosokawa, M. Sasada, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:We observed the field of GRB 220930A (S. B. Cenko et al. GCN Circular #32603, Alan M. Watson et al. GCN Circular #32604, The Swift-XRT team GCN Circular #32605,, Y.-D. Hu et al. GCN Circular #32606, V. Lipunov et al. GCN Circular #32607, P.A. Evans et al. GCN Circular #32608, A. Belles et al. GCN Circular #32609, R. Strausbaugh et al. GCN Circular #32610, V. D'Elia et al. GCN Circular #32611, S. D. Barthelmy et al. GCN Circular #32612, R. Gopalakrishnan et al. GCN Circular #32613, A.Ridnaia et al. GCN Circular #32614, N. Pankov et al. GCN Circular #32617) 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 2022-09-30 13:10:00 UT (118.1 minutes after the Swift/BAT trigger). We stacked the images with good conditions. We did not detect any uncatalogued sources within the enhanced Swift/XRT error region (Evans et al. GCN Circular #32608). We obtained the 5-sigma limits of the stacked images as follows.T0+[days] | MID-UT | T-EXP[sec] | 5-sigma limits ------------------------------------------------------------------------------------------------ 0.23 | 2022-09-30 16:39:02.52 | 14460 | g'>21.0, Rc>20.9, Ic>20.4 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure timeWe 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)..