GRB190324A

This page lists all entries on GRB190324A in GRBweb

Summary Fermi GBM IPN Swift GCN 23993 GCN 23996 GCN 23997 GCN 23999 GCN 24001 GCN 24002 GCN 24003 GCN 24004 GCN 24006 GCN 24007 GCN 24011 GCN 24014 GCN 24015

Summary table
Variable Value Source
GRB_name_Fermi GRB190324947
T0 22:44:01 UTC GCN_circulars,Swift Det
ra 49.6156° Swift
decl -47.2146° Swift
pos_error 5.57e-05° Swift
T90 26.881 s Fermi_GBM
T90_error 9.941 s Fermi_GBM
T90_start 22:44:18.764 UTC Fermi_GBM
fluence 1.64e-05 erg/cm² Fermi_GBM
fluence_error 2.03e-07 erg/cm² Fermi_GBM
redshift 1.1715 GCN_circulars,Optical
T100 44.645 s
GBM_located False
mjd 58566.947233796294 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB190324947
trigger_name bn190324947
ra 49.5758°
decl -47.2389°
pos_error 2.51e+00°
datum 2019-03-24
t_trigger 22:44:02.636 UTC
T90 26.881 s
T90_error 9.941 s
T90_start 22:44:18.764 UTC
fluence 1.64e-05 erg/cm²
fluence_error 2.03e-07 erg/cm²
flux_1024 1.84e+01 erg/cm²/s
flux_1024_error 3.34e-01 erg/cm²/s
flux_1024_time 2.28e+01 erg/cm²/s
flux_64 2.12e+01 erg/cm²/s
flux_64_error 1.43e+00 erg/cm²/s
IPN table
GRB_name GRB190324A
ra 49.5750°
decl -47.2333°
pos_error 5.00e-02°
Swift table
GRB_name GRB190324A
t_trigger 22:44:01 UTC
ra 49.6156°
decl -47.2146°
pos_error 5.57e-05°
T90 28.4 s
fluence 7.20e-06 erg/cm²
redshift 1.1715
GCN 23993 table
GRB_name GRB190324A
GCN_number 23993
Detection_method Swift Det
t_trigger 22:44:01 UTC
ra 49.5760°
decl -47.2390°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23993 SUBJECT: GRB 190324A: Swift detection of a burst DATE: 19/03/24 23:01:38 GMT FROM: Boris Sbarufatti at PSU S. J. LaPorte (PSU), S. D. Barthelmy (GSFC), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), M. J. Moss (George Washington University), B. Sbarufatti (PSU) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 22:44:01 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190324A (trigger=894718). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 49.576, -47.239 which is RA(J2000) = 03h 18m 18s Dec(J2000) = -47d 14' 21" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a precursor at ~T0 and a bright multi-peaked structure starting at ~T+19 s. The total duration is about 40 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~21 sec after the trigger. Due to an observing constraint, Swift will not slew until T0+52.4 minutes. There will be no XRT or UVOT data until this time. Burst Advocate for this burst is S. J. LaPorte (extragsam AT gmail.com). 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 23996 table
GRB_name GRB190324A
GCN_number 23996
Detection_method Swift-UVOT Other
ra 49.6155°
decl -47.2147°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23996 SUBJECT: GRB 190324A: Swift/UVOT afterglow candidate DATE: 19/03/25 00:40:48 GMT FROM: Frank Marshall at Swift/UVOT F. E. Marshall (NASA/GSFC) reports on behalf of the Neil Gehrels Swift Observatory team: UVOT took a finding chart exposure of 150 seconds with the White filter starting 3302 seconds after the BAT trigger (LaPorte et al.GCN Circ. 23993). There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 03:18:27.72 = 49.61551 DEC(J2000) = -47:12:52.9 = -47.21469 with a 90%-confidence error radius of about 0.75 arc sec. The estimated magnitude is 17.10 with a 1-sigma error of about 0.14. With a single observation, we have no indication whether the source is variable. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02.
GCN 23997 table
GRB_name GRB190324A
GCN_number 23997
Detection_method Swift-XRT Other
ra 49.6205°
decl -47.2124°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23997 SUBJECT: GRB 190324A: Swift-XRT observations DATE: 19/03/25 00:51:49 GMT FROM: Phil Evans at U of Leicester M. Perri (ASDC), G. Tagliaferri (INAF-OAB), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), D.N. Burrows (PSU) and J.A. Kennea (PSU) report on behalf of the Swift-XRT team: The XRT began observing the field of GRB 190324A at 23:38:59.4 UT, 3297.9 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 49.62054, -47.21240 which is equivalent to: RA(J2000) = 03h 18m 28.93s Dec(J2000) = -47d 12' 44.6" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 145 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 http://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 (1.75 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 7 (+3.19/-2.76) x 10^21 cm^-2 (90% confidence).
GCN 23999 table
GRB_name GRB190324A
GCN_number 23999
Detection_method Optical
redshift 1.1715
Circular_text TITLE: GCN CIRCULAR NUMBER: 23999 SUBJECT: GRB 190324A: VLT/X-shooter redshift DATE: 19/03/25 02:59:34 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. A. Perley (LJMU), L. Izzo (HETH/IAA-CSIC), D. A. Kann (HETH/IAA-CSIC), D. B. Malesani (DAWN/NBI and DARK/NBI) report on behalf of the Stargate collabaration: We observed the optical afterglow (Marshall, GCN 23996) of GRB 190324A (LaPorte et al., GCN 23993) using the ESO VLT UT2 (Kueyen) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 2 exposures by 600 seconds each. The observation mid time was 2019 Mar 25.0441 UT (2.324 hr after the GRB). We detect continuum at high-S/N over the entire covered wavelength range. A multitude of absorption features are detected, including Ca II, Mg II, Mg I, Fe II, Al II, Cr II, all at a common redshift z = 1.1715. In particular, fine structure lines from Fe II* are visible, which confirm the association of the absorption system with the GRB. We acknowledge excellent support from the ESO observing staff in Paranal, in particular Romain Thomas, Anita Zanella, and Juan Carlos Olivares.
GCN 24001 table
GRB_name GRB190324A
GCN_number 24001
Detection_method Swift-XRT Det
ra 49.6159°
decl -47.2149°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24001 SUBJECT: GRB 190324A: Enhanced Swift-XRT position DATE: 19/03/25 04:14:49 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 1829 s of XRT Photon Counting mode data and 5 UVOT images for GRB 190324A, 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 = 49.61588, -47.21487 which is equivalent to: RA (J2000): 03h 18m 27.81s Dec (J2000): -47d 12' 53.5" with an uncertainty of 1.5 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 24002 table
GRB_name GRB190324A
GCN_number 24002
Detection_method Fermi GBM Det
t_trigger 22:44:02.640 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 24002 SUBJECT: GRB 190324A: Fermi GBM observation DATE: 19/03/25 04:21:58 GMT FROM: C. Michelle Hui at MSFC/Fermi-GBM C. M. Hui (MSFC) reports on behalf of the Fermi GBM Team: At 22:44:02.64 UT on 24 March 2019, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 190324A (trigger 575160247/190324947), which was also detected by Swift (LaPorte e al. 2019, GCN 23993). The GBM on-ground location is consistent with the Swift position. The GBM light curve shows an initial weak pulse followed by a stronger signal containing two peaks. The duration (T90) is about 26.9 s (50-300 keV). The time-averaged spectrum from T0+15.4 s to T0+32.8 s is adequately fit by a Band function with Epeak = 144.3 +/- 8.4 keV, alpha = -0.84 +/- 0.04, and beta = -2.06 +/- 0.05. The event fluence (10-1000 keV) in this time interval is (1.78 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+22.8 s in the 10-1000 keV band is 18.4 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog.
GCN 24003 table
GRB_name GRB190324A
GCN_number 24003
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 24003 SUBJECT: GRB190324A: MASTER OT observations DATE: 19/03/25 07:01:13 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, A. Chasovnikov, V.Topolev, D.Kuvshinov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova, S.Yazev (Applied Physics Institute, Irkutsk State University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), 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 JuanNational University) was pointed to the GRB190324A (LaPorte et al. GCN 23993, Kunzweiler et al. GCN 23994, Perri et al. GCN 23997, Beardmore et al. GCN 24001, Hui et al. GCN 24002) 17 sec after notice time and 252 sec after trigger time at 2019-03-24 22:48:14 UT (Lipunov et al., GCN23995). The SunAltitude was -1.09, so the GRB optical counterpart (MASTER OT J031827.61-471252.6 +-0.7arcsec) light curve started at 2019-03-24 23:26:22UT (2541 sec after trigger time) with m_OT=17.6 +-0.2(preliminary automatic light curve). The OT became brighter (17.0) and then shows classical decay. This OT was also detected by Swift (Marshall et al. GCN 23996), and the spectra was observed by Perley et al. GCN23999). MASTER-SAAO was pointed 12s after notice time, but the alert altitude was -0.6deg. Reduction will be continued. The message may be cited.
GCN 24004 table
GRB_name GRB190324A
GCN_number 24004
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24004 SUBJECT: GRB 190324A: Swift-XRT refined Analysis DATE: 19/03/25 08:51:40 GMT FROM: Phil Evans at U of Leicester A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and S.J. LaPorte report on behalf of the Swift-XRT team: We have analysed 6.6 ks of XRT data for GRB 190324A (LaPorte et al. GCN Circ. 23993), from 3.3 ks to 28.6 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN Circ. 24001). The light curve can be modelled with a power-law decay with a decay index of alpha=1.33 (+/-0.05). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.00 (+0.10, -0.09). The best-fitting absorption column is 8.6 (+2.4, -2.2) x 10^20 cm^-2, in excess of the Galactic value of 1.7 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.3 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8.6 (+2.4, -2.2) x 10^20 cm^-2 Galactic foreground: 1.7 x 10^20 cm^-2 Excess significance: 5.0 sigma Photon index: 2.00 (+0.10, -0.09) If the light curve continues to decay with a power-law decay index of 1.33, the count rate at T+24 hours will be 0.032 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-12 (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/00894718. This circular is an official product of the Swift-XRT team.
GCN 24006 table
GRB_name GRB190324A
GCN_number 24006
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 24006 SUBJECT: GRB 190324A: CALET Gamma-Ray Burst Monitor detection DATE: 19/03/25 14:03:29 GMT FROM: Valentin Pal'shin at AGU Y. Sone, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, T. Ito, H. Morita (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), A. V. Penacchioni, P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 190324A (Swift-BAT trigger #894718: LaPorte et al., GCN Circ. 23993; Fermi GBM detection: Hui, GCN Circ. 24002) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 22:44:16.902 UTC on 24 March 2019. The burst signal was seen by all CGBM detectors. The burst light curve shows a single multi-peaked pulse which starts at T=2.7 sec, peaks at 5.1 sec and ends at T+20.5 sec. The precursor is not seen in the CGBM data. The T90 and T50 durations measured by the SGM data are 12.6 +- 2.3 sec and 4.5 +- 0.5 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1237502436/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 24007 table
GRB_name GRB190324A
GCN_number 24007
Detection_method Swift-BAT Det
ra 49.6030°
decl -47.2120°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24007 SUBJECT: GRB 190324A: Swift-BAT refined analysis DATE: 19/03/25 22:05:14 GMT FROM: Amy Lien at GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (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 190324A (trigger #894718) (LaPorte et al., GCN Circ. 23993). The BAT ground-calculated position is RA, Dec = 49.603, -47.212 deg which is RA(J2000) = 03h 18m 24.8s Dec(J2000) = -47d 12' 42.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 56%. The mask-weighted light curve shows a precursor from ~T0 to ~T+5 s, and a bright multi-peaked structure that starts at ~T+18 s and ends at ~T+40 s. In addition, there are some weak emission lasting till ~T+80 s. T90 (15-350 keV) is 28.4 +- 11.6 sec (estimated error including systematics). The time-averaged spectrum from T+0.09 to T+83.30 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.46 +- 0.06. The fluence in the 15-150 keV band is 7.2 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+23.74 sec in the 15-150 keV band is 11.9 +- 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/894718/BA/
GCN 24011 table
GRB_name GRB190324A
GCN_number 24011
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 24011 SUBJECT: GRB 190324A: Insight-HXMT/HE detection DATE: 19/03/26 13:35:55 GMT FROM: Qi Luo at IHEP Q. Luo, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu, A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: At 2019-03-24T22:44:20.500 (T0), the Insight-HXMT/HE detected GRB 190324A(trigger ID: HEB190324947) in a routine search of the data, which was also triggered by Swift/BAT(S. J. LaPorte et al. ,GCN 23993), Fermi/GBM(F. Kunzweiler et al. ,GCN 23994) and CALET/CGBM(Y. Sone et al. ,GCN 24006). The Insight-HXMT/HE light curve mainly consists of two pulses with a duration (T90) of 6.41 s measured from T0+0.14 s. The 1-ms peak rate, measured from T0+1.283 s, is 1111 cnts/sec. The total counts from this burst is 3551 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB190324947_lc.jpg All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (record energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. Insight-HXMT is the first Chinese space X-ray telescope, which was fundedjointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org.
GCN 24014 table
GRB_name GRB190324A
GCN_number 24014
Detection_method Swift-UVOT Det
ra 49.6156°
decl -47.2146°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24014 SUBJECT: GRB 190324A: Swift/UVOT Observations DATE: 19/03/26 16:50:58 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and S. J. LaPorte (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190324A 3302 s after the BAT trigger (LaPorte et al., GCN Circ. 23993). A fading source consistent with the XRT position (Beardmore et al. GCN Circ. 24001) is detected in the initial UVOT exposures, consistent with the initial report of Marshall (GCN Circ. 23996). The preliminary UVOT position is: RA (J2000) = 03:18:27.74 = 49.61559 (deg.) Dec (J2000) = -47:12:52.6 = -47.21462 (deg.) with an estimated uncertainty of 0.43 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 white 3302 3452 147 17.23 +/- 0.04 white 33037 33944 885 19.65 +/- 0.07 white 101768 119129 386 >20.79 v 3459 3659 197 17.55 +/- 0.11 v 28515 39157 496 >19.48 b 4281 4481 197 17.98 +/- 0.07 b 10929 11267 329 18.74 +/- 0.08 b 32125 44180 1489 20.65 +/- 0.34 b 101621 118983 386 >20.13 u 4075 4275 197 16.75 +/- 0.05 u 10016 10923 885 17.78 +/- 0.05 u 22022 22836 792 18.86 +/- 0.08 u 101474 118836 386 >19.68 uvw1 3870 4070 197 16.76 +/- 0.07 uvw1 9110 10010 885 17.65 +/- 0.07 uvw1 20525 21097 563 18.68 +/- 0.16 uvm2 3664 3864 197 16.79 +/- 0.09 uvm2 14888 15397 501 18.37 +/- 0.13 uvw2 4692 4892 197 17.82 +/- 0.12 uvw2 26341 38706 2052 19.76 +/- 0.15 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 24015 table
GRB_name GRB190324A
GCN_number 24015
Detection_method Konus-Wind Det
t_trigger 22:44:18.644 UTC
redshift 1.1715
Circular_text TITLE: GCN CIRCULAR NUMBER: 24015 SUBJECT: Konus-Wind observation of GRB 190324A DATE: 19/03/26 16:52:58 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 190324A (Swift-BAT detection: LaPorte et al., GCN Circ. 23993; Fermi-GBM observation: Hui, GCN Circ. 24002; CALET-GBM detection: Sone et al., GCN Circ. 24006; and Insight-HXMT/HE detection: Luo et al., GCN Circ. 24011) triggered Konus-Wind at T0=81858.644 s UT (22:44:18.644). The burst light curve shows a multipeaked structure which starts at ~T0-3.7 s and has a total duration of ~17.3 s, followed by a tail of softer emission seen up to ~T0+70 s. The initial weak pulse is marginally seen at ~T0-20 s. The emission is seen up to ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB190324_T81858/ As observed by Konus-Wind, the burst had a fluence of 2.07(-0.28,+0.31)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+1.648 s, of 7.59(-1.80,+1.86)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+16.640 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 = -0.90(-0.18,+0.22), the high energy photon index beta = -2.27(-0.23,+0.15), the peak energy Ep = 146(-21,+25) keV (chi2 = 91/97 dof). The spectrum near the maximum count rate (measured from T0+0.256 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 = -0.90(-0.17,+0.21), the high energy photon index beta = -2.26(-0.22,+0.15), the peak energy Ep = 159(-23,+27) keV (chi2 = 77/97 dof). Assuming the redshift z=1.1715 (Perley et al., GCN Circ. 23999) and a standard cosmology model with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014), we estimate the following rest-frame parameters: the isotropic energy release E_iso is ~7.8x10^52 erg, the peak luminosity L_iso is ~6.2x10^52 erg/s, and the rest-frame peak energy of the time-integrated spectrum, Ep,i, is ~317 keV. With these energetics, the burst lies within the 68% prediction bands for both 'Amati' and 'Yonetoku' relations built for the sample of 138 long KW GRBs with known redshifts (Tsvetkova et al., ApJ 850 161, 2017), see http://www.ioffe.ru/LEA/GRBs/GRB190324_T81858/GRB190324A.pdf All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.