GRB200303A

This page lists all entries on GRB200303A in GRBweb

Summary Fermi GBM IPN Swift GCN 27294 GCN 27297 GCN 27300 GCN 27301 GCN 27303 GCN 27304 GCN 27307 GCN 27308 GCN 27309 GCN 27311 GCN 27312 GCN 27314 GCN 27316

Summary table
Variable Value Source
GRB_name_Fermi GRB200303107
T0 2:34:23 UTC GCN_circulars,Fermi GBM final loc
ra 212.7190° Swift
decl 51.3593° Swift
pos_error 1.81e-04° Swift
T90 82.177 s Fermi_GBM
T90_error 3.874 s Fermi_GBM
T90_start 2:34:26.151 UTC Fermi_GBM
fluence 2.37e-05 erg/cm² Fermi_GBM
fluence_error 1.22e-07 erg/cm² Fermi_GBM
T100 128.2 s
GBM_located False
mjd 58911.10721064815 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB200303107
trigger_name bn200303107
ra 212.7192°
decl 51.3592°
pos_error 3.66e+00°
datum 2020-03-03
t_trigger 2:34:23.847 UTC
T90 82.177 s
T90_error 3.874 s
T90_start 2:34:26.151 UTC
fluence 2.37e-05 erg/cm²
fluence_error 1.22e-07 erg/cm²
flux_1024 9.24e+00 erg/cm²/s
flux_1024_error 4.20e-01 erg/cm²/s
flux_1024_time 3.51e+01 erg/cm²/s
flux_64 1.23e+01 erg/cm²/s
flux_64_error 1.80e+00 erg/cm²/s
IPN table
GRB_name GRB200303A
ra 212.6958°
decl 51.3667°
pos_error 5.00e-02°
Swift table
GRB_name GRB200303A
t_trigger 2:34:57 UTC
ra 212.7190°
decl 51.3593°
pos_error 1.81e-04°
T90 94.2 s
fluence 1.30e-05 erg/cm²
GCN 27294 table
GRB_name GRB200303A
GCN_number 27294
Detection_method Fermi GBM final loc
t_trigger 2:34:23 UTC
ra 207.4000°
decl 50.8000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27294 SUBJECT: GRB 200303A: Fermi GBM Final Real-time Localization DATE: 20/03/03 02:44:36 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 02:34:23 UT on 3 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200303A (trigger 604895668.847358 / 200303107). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 207.4, Dec = 50.8 (J2000 degrees, equivalent to J2000 13h 49m, 50d 47'), with a statistical uncertainty of 3.8 degrees. The angle from the Fermi LAT boresight is 108.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200303107/quicklook/glg_skymap_all_bn200303107.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200303107/quicklook/glg_healpix_all_bn200303107.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200303107/quicklook/glg_lc_medres34_bn200303107.gif
GCN 27297 table
GRB_name GRB200303A
GCN_number 27297
Detection_method Swift Det
t_trigger 2:34:57 UTC
ra 212.6980°
decl 51.3600°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27297 SUBJECT: GRB 200303A: Swift detection of a burst DATE: 20/03/03 02:49:25 GMT FROM: Scott Barthelmy at NASA/GSFC S. B. Cenko (GSFC), S. D. Barthelmy (GSFC), C. Gronwall (PSU), J.D. Gropp (PSU), N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), M. J. Moss (GWU), K. L. Page (U Leicester), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 02:34:57 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200303A (trigger=959431). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 212.698, +51.360, which is RA(J2000) = 14h 10m 47s Dec(J2000) = +51d 21' 35" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a multi-peak structure with a duration of about 60 sec. The peak count rate was ~3500 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 02:36:25.1 UT, 87.7 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 212.7173, 51.3583 which is equivalent to: RA(J2000) = 14h 10m 52.15s Dec(J2000) = +51d 21' 29.9" with an uncertainty of 4.7 arcseconds (radius, 90% containment). This location is 43 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 8.77e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 96 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 0.02. This source lies within the current (Sector 22) field-of-view of TESS camera 3. 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 27300 table
GRB_name GRB200303A
GCN_number 27300
Detection_method Swift-XRT Det
ra 212.7190°
decl 51.3593°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27300 SUBJECT: GRB 200303A: Enhanced Swift-XRT position DATE: 20/03/03 07:27:17 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 822 s of XRT Photon Counting mode data and 1 UVOT images for GRB 200303A, 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 = 212.71895, +51.35930 which is equivalent to: RA (J2000): 14h 10m 52.55s Dec (J2000): +51d 21' 33.5" with an uncertainty of 1.7 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 27301 table
GRB_name GRB200303A
GCN_number 27301
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 27301 SUBJECT: GRB 200303A: CALET Gamma-Ray Burst Monitor detection DATE: 20/03/03 09:23:42 GMT FROM: Valentin Pal'shin at AGU Y. Asaoka (Waseda U), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), S. Torii (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 200303A (Fermi GBM Final Real-time Localization: Fermi GBM Team, GCN Circ. 27294; Swift detection: Cenko et al., GCN Circ. 27297; https://gcn.gsfc.nasa.gov/other/200303A.gcn3) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 02:34:20.728 UTC on 3 March 2020. The burst signal was seen by all CGBM detectors. The burst light curve shows a multi-peaked structure which starts at T+2.3 sec, peaks at T+39.4 sec, and ends at T+88.8 sec. The T90 and T50 durations measured by the SGM data are 68.9 +- 12.8 sec and 28.9 +- 3.3 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1267237773/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 27303 table
GRB_name GRB200303A
GCN_number 27303
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27303 SUBJECT: GRB 200303A: Optical limit from CAHA DATE: 20/03/03 11:24:50 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann, C. Thoene, J. F. Agui Fernandez, M. Blazek (all HETH/IAA-CSIC), R. Pedro Hedrosa (CAHA) report: We observed the field of GRB 200303A (Cenko et al. GCN 27297) with CAFOS, on the 2.2 m telescope, at Calar Alto observatory (Almeria, Spain). Observations consisted of 5x360s in R-band with mean epoch 03:48:02 UT (1.249 hr after the burst). Our initial analysis does not reveal any object within the refined error box (Goad et al. GCN 27300) down to a 3-sigma limit of R(AB) > 24.0 mag, with photometry performed against SDSS field stars.
GCN 27304 table
GRB_name GRB200303A
GCN_number 27304
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 27304 SUBJECT: GRB 200303A: GOTO observations upper limit DATE: 20/03/03 12:21:44 GMT FROM: Ben Gompertz at U of Warwick Y.-L. Mong (1); K. Ackley (1); D. K. Galloway (1); D. Steeghs (2); V. Dhillon (3); P. O'Brien (4); G. Ramsay (5); D. Pollacco (2); E. Thrane (1); S. Poshyachinda (6); R. Kotak (7); L. Nuttall (8); E. Pall\'e (9); K. Ulaczyk (2); J. Lyman (2); R. Cutter (2); A. Levan (2); T. Marsh (2); R. West (2); E. Stanway (2); B. Gompertz (2); K. Wiersema (2); T. Killestein (2); A. Casey (1); M. Brown (1); B. Muller (1); M. Dyer (3); J. Mullaney (3); E. Daw (3); S. Littlefair (3); J. Maund (3); L. Makrygianni (3); U. Burhanudin (3); R. Starling (4); R. Eyles (4); S. Tooke (4); S. Aukkaravittayapun (6); U. Sawangwit (6); S. Awiphan (6); D. Mkrtichian (6); P. Irawati (6); S. Mattila (7); T. Heikkil\"a (7); E. Rol (1) ((1) Monash University, (2) Warwick University, (3) University of Sheffield, (4) University of Leicester, (5) Armagh Observatory & Planetarium, (6) National Astronomical Research Institute of Thailand, (7) University of Turku, (8) University of Portsmouth, (9) Instituto de Astrofisica de Canarias) report on behalf of the GOTO collaboration: We carried out observations with the Gravitational-wave Optical Transient Observer (GOTO), in response to GRB 2000303A (Cenko et al. 2020; GCN #27297; Fermi GBM; GCN #27294). We made a series of 3 x 60 s exposures using our wide L-band filter (400-700 nm) covering the Swift XRT position (Cenko et al. 2020; GCN #27297), starting at 6.4 minutes after the Swift BAT trigger with midtime 02:52:17 UT on 03 March 2020. Using a difference imaging analysis with recent survey observations of the same pointings as reference, we identify no viable afterglow candidate. Our mean 5-sigma detection limit was g=19.6 mag based on PS1 catalogue calibrators. GOTO is operated at the La Palma observing facilities of the University of Warwick on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT) and the Instituto de Astrofisica de Canarias (IAC) (https://goto-observatory.org)
GCN 27307 table
GRB_name GRB200303A
GCN_number 27307
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 27307 SUBJECT: GRB 200303A: FRAM-ORM optical limit DATE: 20/03/03 14:04:46 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ), Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ) report: The 25cm robotic telescope FRAM-ORM at La Palma (Spain) reacted robotically to the GBM/Swift/CALET alert of GRB200303A (Cenko et al, GCNC 27297, Goad et al. GCNC 27300, Asaoka et al. GCNC 27301 and Fermi GBM team GCNC 27294), obtaining a series of 20s unfiltered images starting at 02:35:38.75UT, i.e. 41.3s post trigger. We do not detect any new source in comparison to USNO-B2.0 catalog neither in single images (3-sigma limit R>~17.9) nor in a combined 20x20s frame (mean exp time 289s post trigger, 3-sigma limit R>~19.5) similarly to de Ugarte et al. (GCNC 27303) and Mong et al. (GCNC 27304)
GCN 27308 table
GRB_name GRB200303A
GCN_number 27308
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27308 SUBJECT: GRB 200303A: Swift/UVOT Upper Limits DATE: 20/03/03 15:21:17 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL) and S. B. Cenko (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 200303A 96 s after the BAT trigger (Cenko et al., GCN Circ. 27297). No optical afterglow consistent with the XRT position (Goad et al. GCN Circ. 27300) 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 white_FC 96 246 147 >20.7 u_FC 308 558 246 >20.4 white 96 5034 550 >21.5 v 1219 1238 19 >18.4 b 1144 1163 19 >19.4 u 308 558 246 >20.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 27309 table
GRB_name GRB200303A
GCN_number 27309
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 27309 SUBJECT: GRB 200303A: NOT optical observations DATE: 20/03/03 15:25:21 GMT FROM: Luca Izzo at IAA-CSIC D. Xu (NAOC), L. Izzo (DARK/NBI), D. B. Malesani (DTU Space), A.A. Djupvik (NOT), T. Pursimo (NOT) report on behalf of a larger collaboration: We observed GRB 200303A (Fermi GBM team, GCN 27294, Cenko et al., GCN 27297, Asaoka et al., GCN 27301) with the Nordic Optical Telescope (NOT) equipped with StanCAM, covering 100% of the afterglow region as provided by the Swift-XRT (Cenko et al. 27297). We obtained 3x300 s exposures with the Bessel R filter starting at 03:36:18 UT on March 3 (median time 1.161 hr after the GRB trigger) and 5x200 s exposures with the z-SDSS filter starting at 03:53:59 UT (median time 1.483 hr). We do not detect any optical afterglow candidate down to a limit of R > 23.0 mag (AB) and z > 21.5 mag (AB), calibrated against PS1 catalog. With the above upper limits, the optical to X-ray spectral index is then beta_OX < -0.09 (Fnu propto nu^-beta) computed assuming the R-Bessel value and X-rays data from Swift-XRT. This suggests a ‘’dark'' nature for GRB 200303A
GCN 27311 table
GRB_name GRB200303A
GCN_number 27311
Detection_method Swift-BAT Det
ra 212.6950°
decl 51.3580°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27311 SUBJECT: GRB 200303A: Swift-BAT refined analysis DATE: 20/03/03 17:01:22 GMT FROM: Hans Krimm at NSF/NASA-GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+605 sec from the recent telemetry downlink, we report further analysis of BAT GRB 200303A (trigger #959431) (Cenko, et al., GCN Circ. 27297). The BAT ground-calculated position is RA, Dec = 212.695, 51.358 deg which is RA(J2000) = 14h 10m 46.9s Dec(J2000) = +51d 21' 29.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 59%. The burst entered the BAT field of view around T-100 sec during a spacecraft slew. The mask-weighted light curve shows a single episode with multiple pulses, starting at T-45 sec, peaking at the trigger time and returning to near background by T+70 sec. There is extended low-level emission out to nearly T+200 sec. T90 (15-350 keV) is 94.2 +- 6.4 sec (estimated error including systematics). The time-averaged spectrum from T-36.55 to T+193.26 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.39 +- 0.17, and Epeak of 131.4 +- 75.1 keV (chi squared 46.32 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 1.3 +- 0.0 x 10^-5 erg/cm2 and the 1-sec peak flux measured from T+0.34 sec in the 15-150 keV band is 5.0 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.65 +- 0.04 (chi squared 53.75 for 57 d.o.f.). 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/959431/BA/
GCN 27312 table
GRB_name GRB200303A
GCN_number 27312
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27312 SUBJECT: GRB 200303A: Swift-XRT refined Analysis DATE: 20/03/03 19:12:12 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), D.N. Burrows (PSU) and S.B. Cenko report on behalf of the Swift-XRT team: We have analysed 6.6 ks of XRT data for GRB 200303A (Cenko et al. GCN Circ. 27297), from 77 s to 41.6 ks after the BAT trigger. The data comprise 582 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 Goad et al. (GCN Circ. 27300). The late-time light curve (from T0+4.8 ks) can be modelled with a power-law decay with a decay index of alpha=1.27 (+0.09, -0.10). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.41 (+/-0.05). The best-fitting absorption column is 1.10 (+0.05, -0.04) x 10^22 cm^-2, in excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.38 (+0.15, -0.14) and a best-fitting absorption column of 7.5 (+1.0, -0.9) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (8.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 7.5 (+1.0, -0.9) x 10^21 cm^-2 Galactic foreground: 1.6 x 10^20 cm^-2 Excess significance: 13.4 sigma Photon index: 2.38 (+0.15, -0.14) If the light curve continues to decay with a power-law decay index of 1.27, the count rate at T+24 hours will be 0.043 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x 10^-12 (3.8 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/00959431. This circular is an official product of the Swift-XRT team.
GCN 27314 table
GRB_name GRB200303A
GCN_number 27314
Detection_method Fermi GBM Det
t_trigger 2:34:23.850 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 27314 SUBJECT: GRB 200303A: Fermi GBM observation DATE: 20/03/04 10:26:57 GMT FROM: Elisabetta Bissaldi at INFN,Bari C. Malacaria (NASA-MSFC/USRA) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 02:34:23.85 UT on 03 March 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 200303A (trigger 604895668 / 200303107), which was also detected by the Swift/BAT and Swift/XRT (Cenko et al. 2020, GCN 27297, Goad et al. 2020, GCN 27300). The Fermi GBM Final Real-time Localization (GCN 27294) is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 106 degrees. The GBM light curve shows a complex structure with a duration (T90) of about 82 s (50-300 keV). The time-averaged spectrum from T0-2.8 s to T0+95.7 s is best fit by a Band function with Epeak = 151 +/- 18 keV, alpha = -1.26 +/- 0.05, and beta = -2.14 +/- 0.10. The event fluence (10-1000 keV) in this time interval is (3.23 +/- 0.08)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+35.1 s in the 10-1000 keV band is 9.2 +/- 0.4 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 27316 table
GRB_name GRB200303A
GCN_number 27316
Detection_method Konus-Wind Det
t_trigger 2:34:28.336 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 27316 SUBJECT: Konus-Wind observation of GRB200303A DATE: 20/03/04 18:11:22 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Lysenko, A. Ridnaia and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB200303A (Swift detection of a burst: Cenko et al., GCN 27297; Palmer et al., GCN 27311; CALET Gamma-Ray Burst Monitor detection: Asaoka et al., GCN 27301; Fermi GBM observation: Malacaria & Meegan, GCN 27314) triggered Konus-Wind at T0=9268.336 s UT (02:34:28.336). The burst light curve shows a multi-peaked structure which starts at ~T0-4.0 s and has a total duration of~67.1 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 3.88(-1.20,+0.80)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+32.800 s, of 2.38(-0.96,+1.15)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+65.792 s) is best fit in the 20 keV - 3 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -1.25(-0.21,+0.28), the high energy photon index beta = -2.17(-7.83,+0.18), the peak energy Ep = 154(-44,+82) keV, chi2 = 72/66 dof. The spectrum near the peak count rate (measured from T0+24.832 to T0+41.216 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 = -1.39(-0.14,+0.20), the high energy photon index beta = -2.54(-7.46,+0.45), the peak energy Ep = 183(-53,+54) keV, chi2 = 80/86 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB200303_T09268/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.