GRB250330A

This page lists all entries on GRB250330A in GRBweb

Summary Fermi GBM Swift GCN 39938 GCN 39941 GCN 39944 GCN 39947 GCN 39948 GCN 39949 GCN 39950 GCN 39957 GCN 39964 GCN 39970 GCN 40055

Summary table
Variable Value Source
GRB_name_Fermi GRB250330255
T0 6:07:38 UTC GCN_circulars,Swift Det
ra 252.9448° Swift
decl -86.8805° Swift
pos_error 2.98e-04° Swift
T90 4.8 s Fermi_GBM
T90_error 0.326 s Fermi_GBM
T90_start 6:07:38.165 UTC Fermi_GBM
fluence 1.48e-06 erg/cm² Fermi_GBM
fluence_error 1.40e-08 erg/cm² Fermi_GBM
T100 4.965 s
GBM_located False
mjd 60764.25530092593 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB250330255
trigger_name bn250330255
ra 252.9521°
decl -86.8797°
datum 2025-03-30
t_trigger 6:07:38.421 UTC
T90 4.8 s
T90_error 0.326 s
T90_start 6:07:38.165 UTC
fluence 1.48e-06 erg/cm²
fluence_error 1.40e-08 erg/cm²
flux_1024 6.50e+00 erg/cm²/s
flux_1024_error 2.91e-01 erg/cm²/s
flux_1024_time 2.56e-01 erg/cm²/s
flux_64 8.19e+00 erg/cm²/s
flux_64_error 1.21e+00 erg/cm²/s
Swift table
GRB_name GRB250330A
t_trigger 6:07:38 UTC
ra 252.9448°
decl -86.8805°
pos_error 2.98e-04°
GCN 39938 table
GRB_name GRB250330A
GCN_number 39938
Detection_method Swift Det
t_trigger 6:07:38 UTC
ra 252.7900°
decl -86.8700°
Circular_text TITLE: GCN CIRCULAR NUMBER: 39938 SUBJECT: GRB 250330A: Swift detection of a burst DATE: 25/03/30 06:28:16 GMT FROM: K.L. Page at U Leicester S. B. Cenko (GSFC), K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 06:07:38 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 250330A (trigger=1299776). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 252.790, -86.870 which is RA(J2000) = 16h 51m 10s Dec(J2000) = -86d 52' 11" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak structure with a duration of about 10 sec. The peak count rate was ~5800 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 06:08:51.3 UT, 73.2 seconds after the BAT trigger. Due to the proximity of Swift to the SAA, XRT centroided on a cosmic ray. Given the short visibility window, no other data are available at this time. UVOT data are not available at this time. Although this trigger occurred while Swift was close to the SAA, the BAT light-curve shows a definite peak, and Fermi-GBM also triggered at the same time. 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 39941 table
GRB_name GRB250330A
GCN_number 39941
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 39941 SUBJECT: GRB 250330A: VLT/FORS2 Optical Observations DATE: 25/03/30 10:22:23 GMT FROM: Rosa L. Becerra at Tor Vergata, Roma Rosa Becerra (U Rome), Eleonora Troja (U Rome), Muskan Yadav (U Rome), Roberto Ricci (U Rome) report on behalf of the ERC BHianca team: We observed the field of GRB 250330A (Cenko et al., GCN 39938) with the FORS2 imager on the ESO VLT UT1 (Antu). Observations began at T+1.25 hours after the trigger and were carried out in the R filter at an average seeing of 0.7" and airmass about 2.2. Image subtraction against the SkyMapper Southern Survey (SMSS) Fourth Data Release (DR4) catalog (Onken et al., 2024) shows no new uncataloged source down to r~21.5 AB. Several fainter objects are visible within the XRT position (Page et al., GCN 39940), however, additional observations are required to assess their variability We thank the staff at the VLT for the rapid execution of these observations.
GCN 39944 table
GRB_name GRB250330A
GCN_number 39944
Detection_method Fermi GBM Other
ra 254.9600°
decl -66.0200°
Circular_text TITLE: GCN CIRCULAR NUMBER: 39944 SUBJECT: GRB 250330A: Fermi GBM Final Localization DATE: 25/03/30 12:59:41 GMT FROM: Utkarsh Pathak at IIT Bombay The Fermi GBM team reports the detection of a likely LONG GRB "At 06:07:38.42 UT on 30 March 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250330A (trigger 765007663/250330255). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 254.96, Dec = -66.02 (J2000 degrees, equivalent to J2000 16h 51m, -86d 52'), with a statistical uncertainty of 6.9 degrees. This localization is consistent with Swift-BAT location (Cenko et al. 2025, GCN 39938) and Swift-XRT (Page et al. 2025, 39940). The angle from the Fermi LAT boresight is 46 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250330255/quicklook/glg_skymap_all_bn250330255.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250330255/quicklook/glg_healpix_all_bn250330255.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250330255/quicklook/glg_lc_medres34_bn250330255.gif"
GCN 39947 table
GRB_name GRB250330A
GCN_number 39947
Detection_method Swift-XRT Other
ra 252.9448°
decl -86.8805°
Circular_text TITLE: GCN CIRCULAR NUMBER: 39947 SUBJECT: GRB 250330A: Swift-XRT afterglow detection DATE: 25/03/30 16:52:55 GMT FROM: Phil Evans at U of Leicester J.P. Osborne (U. Leicester), R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAR), D.N. Burrows (PSU), M. A. Williams (PSU), S. Dichiara (PSU), K.L. Page (U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Swift-BAT-detected burst GRB 250330A. We searched for X-ray sources in 1.4 ks of Photon Counting (PC) mode data. The total exposure at the position of the afterglow (see below) is 5.1 ks, obtained between T0+3.9 ks and T0+28.0 ks. Two uncatalogued X-ray sources are detected within the estimated 3-sigma Swift-BAT error region (296 arcsec), of which one ("Source 1") is above the LSXPS 3-sigma upper limit at this position and fading with >3-sigma significance, and is therefore likely the GRB afterglow. Using 1474 s of PC mode data and 4 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 252.94482, -86.88053 which is equivalent to: RA (J2000): 16h 51m 46.76s Dec(J2000): -86d 52' 49.9" with an uncertainty of 2.3 arcsec (radius, 90% confidence). This position is 48 arcsec from the Swift-BAT position. The light curve can be modelled with a power-law decay with a decay index of alpha=1.01 (+0.15, -0.14). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.3 (+0.4, -0.3). The best-fitting absorption column is 4.9 (+1.9, -1.5) x 10^21 cm^-2, in excess of the Galactic value of 1.2 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (7.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 4.9 (+1.9, -1.5) x 10^21 cm^-2 Galactic foreground: 1.2 x 10^21 cm^-2 Excess significance: 3.9 sigma Photon index: 2.3 (+0.4, -0.3) If the light curve continues to decay with a power-law decay index of 1.01, the count rate at T+24 hours will be 7.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.8 x 10^-13 (5.4 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01299776. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/01299776. This circular is an official product of the Swift-XRT team.
GCN 39948 table
GRB_name GRB250330A
GCN_number 39948
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 39948 SUBJECT: GRB 250330A: Swift/UVOT Upper Limits DATE: 25/03/30 17:15:45 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (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 250330A 3944 s after the BAT trigger (Cenko et al., GCN Circ. 39938). No optical afterglow consistent with the XRT position (Osborne et al., GCN Circ. 39947) 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 3944 4094 147 >21.2 white 3944 4094 147 >21.2 v 4101 4300 197 >20.0 b 4921 5109 185 >20.9 u 4716 4915 197 >20.0 w1 4511 4711 197 >21.3 m2 4306 4505 197 >19.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.147 in the direction of the burst (Schlegel et al. 1998).
GCN 39949 table
GRB_name GRB250330A
GCN_number 39949
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 39949 SUBJECT: GRB 250330A: BOOTES-7 early optical upper limit DATE: 25/03/30 18:13:56 GMT FROM: I. Perez-Garcia at Institute of Astrophysics of Andalusia I. Perez-Garcia, A. J. Castro-Tirado, E. Fernandez-Garcia, S.-Y. Wu, M.D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy (IAA-CSIC), C. Perez del Pulgar (Univ. de Malaga), G. Garcia-Segura (Inst. de Astronomia, UNAM), M. Gritsevich (Univ. of Helsinki), D. R. Xiong (Yunnan Observatories of CAS), Y.-D. Hu (GuangXi Univ.), B.-B. Zhang (Nanjing Univ.) and A. Maury (Space, San Pedro de Atacama), on behalf of a larger collaboration, report: Following the detection of GRB 250330A by Swift/BAT (Cenko et al., GCNC [39938](https://gcn.nasa.gov/circulars/39938)) and Fermi (Fermi GRB Team, GCNC [39944](https://gcn.nasa.gov/circulars/39944)), the 0.6m BOOTES-7 robotic telescope at San Pedro de Atacama (Chile) responded to the alert on Nov. 9, 06:08:48 UT (i.e. 57s after trigger, and 70s after the event). Within the reported Swift/XRT error circle (Page et al., GCNC [39940](https://gcn.nasa.gov/circulars/39940)) , no optical transient is detected down to 17.6 mag (clear filter). On a coadd (620s) of images at 06:31:17 UT (mid exposure time; i.e. 23.8 min post burst), nothing is detected down to 19.3 mag, in agreement with the deeper VLT/FORS2 observations taken later on (Becerra et al., GCNC [39941](https://gcn.nasa.gov/circulars/39941)). We thank the staff at San Pedro de Atacama Celestial Observations for their excellent support.
GCN 39950 table
GRB_name GRB250330A
GCN_number 39950
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 39950 SUBJECT: Fermi GRB 250330A: Global MASTER-Net observations report DATE: 25/03/30 19:16:02 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity) D.Buckley (SAAO), R.Rebolo (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) MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 250330A ( Fermi GBM team, GCN 39944) errorbox 41642 sec after notice time and 41678 sec after trigger time at 2025-03-30 17:42:16 UT, with upper limit up to 18.5 mag. Observations started at twilight. The observations began at zenith distance = 69 deg. The sun altitude is -14.6 deg. The galactic latitude b = -16 deg., longitude l = 316 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2828018 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 41709 | 2025-03-30 17:42:16 | MASTER-SAAO | (16h 01m 09.95s , -72d 45m 24.7s) | C | 60 | 18.1 | 41788 | 2025-03-30 17:43:36 | MASTER-SAAO | (16h 28m 26.03s , -72d 45m 15.7s) | C | 60 | 18.2 | 41868 | 2025-03-30 17:44:56 | MASTER-SAAO | (16h 02m 18.38s , -74d 39m 19.9s) | C | 60 | 18.0 | 41947 | 2025-03-30 17:46:15 | MASTER-SAAO | (16h 32m 49.13s , -74d 37m 47.3s) | C | 60 | 18.3 | 42026 | 2025-03-30 17:47:34 | MASTER-SAAO | (15h 04m 24.83s , -74d 37m 14.9s) | C | 60 | 18.4 | 42106 | 2025-03-30 17:48:54 | MASTER-SAAO | (15h 34m 57.62s , -74d 38m 25.7s) | C | 60 | 18.4 | 42186 | 2025-03-30 17:50:14 | MASTER-SAAO | (15h 09m 38.19s , -72d 45m 00.7s) | C | 60 | 18.2 | 42265 | 2025-03-30 17:51:33 | MASTER-SAAO | (15h 36m 45.01s , -72d 44m 01.7s) | C | 60 | 18.3 | 42345 | 2025-03-30 17:52:52 | MASTER-SAAO | (16h 01m 11.29s , -72d 45m 24.8s) | C | 60 | 18.2 | 42424 | 2025-03-30 17:54:12 | MASTER-SAAO | (16h 28m 23.83s , -72d 44m 12.1s) | C | 60 | 18.2 | 42866 | 2025-03-30 18:01:34 | MASTER-SAAO | (16h 02m 13.55s , -74d 39m 54.2s) | C | 60 | 17.9 | 42945 | 2025-03-30 18:02:53 | MASTER-SAAO | (16h 32m 48.33s , -74d 40m 05.2s) | C | 60 | 18.3 | 43025 | 2025-03-30 18:04:13 | MASTER-SAAO | (15h 04m 23.51s , -74d 37m 45.9s) | C | 60 | 18.4 | 43104 | 2025-03-30 18:05:32 | MASTER-SAAO | (15h 34m 50.67s , -74d 39m 22.5s) | C | 60 | 18.5 | 43184 | 2025-03-30 18:06:52 | MASTER-SAAO | (15h 09m 34.64s , -72d 44m 00.2s) | C | 60 | 18.2 | 43263 | 2025-03-30 18:08:11 | MASTER-SAAO | (15h 36m 38.09s , -72d 44m 59.8s) | C | 60 | 18.3 | 43343 | 2025-03-30 18:09:31 | MASTER-SAAO | (16h 01m 06.13s , -72d 44m 09.8s) | C | 60 | 18.2 | 45719 | 2025-03-30 18:49:07 | MASTER-SAAO | (16h 28m 13.93s , -72d 47m 17.6s) | C | 60 | 18.2 | 45798 | 2025-03-30 18:50:26 | MASTER-SAAO | (16h 02m 10.31s , -74d 39m 28.3s) | C | 60 | 18.1 | 45878 | 2025-03-30 18:51:46 | MASTER-SAAO | (16h 32m 34.04s , -74d 40m 31.3s) | C | 60 | 18.3 | 46778 | 2025-03-30 19:06:46 | MASTER-SAAO | (15h 04m 04.80s , -74d 39m 00.1s) | C | 60 | 18.5 | 46858 | 2025-03-30 19:08:05 | MASTER-SAAO | (15h 34m 34.17s , -74d 41m 15.3s) | C | 60 | 18.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 39957 table
GRB_name GRB250330A
GCN_number 39957
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 39957 SUBJECT: GRB 250330A: SVOM/VT optical upper limit DATE: 25/03/31 04:35:08 GMT FROM: SVOM_group Z.M. Wang, A. Li (BNU), L.P. Xin, H.L. Li, Y. L. Qiu, C. Wu, Z.H. Yao, Y. Xu, P.P. Zhang, J. Wang, Y.N. Ma, X.H. Han, H.B. Cai, J.Y. Wei(NAOC) report on behalf of the SVOM/VT team: SVOM performed two Target of Opportunity observations of GRB 250330A (Cenko et al., GCN 39938; Pathak, GCN 39944; Osborne et al., GCN 39947) in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously， starting at 2025-03-30T09:17:44 UT, and 2025-03-30T12:40:58 UT, respectively. No sources were detected in the stacked images within the XRT source position (Page, GCN 39940). The 3 sigma limits in VT_R is 21.7 mag (AB) with the exposure time of 3 x 100s at the medium time of 3.2 hours after the Swift BAT trigger, and 23.0 mag with the exposure of 12*120s, at the medium time of 6.8 hours after the burst. This result is consistent with the reports (Becerra, GCN 39941; Siegel et al., GCN 39948; Perez-Garcia et al., GCN 39949; Lipunov et al., GCN 39950). The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC),CAS.
GCN 39964 table
GRB_name GRB250330A
GCN_number 39964
Detection_method Fermi GBM Det
t_trigger 6:07:38.420 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 39964 SUBJECT: GRB 250330A: Fermi GBM Observation DATE: 25/03/31 06:48:11 GMT FROM: Utkarsh Pathak at IIT Bombay U. Pathak (IITB), R. Sonawane (IISER, TVM) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 06:07:38.42 UT on 30 March 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250330A (trigger 765007663/250330255). which was also detected by Swift-BAT (Cenko et al. 2025, GCN 39938). The afterglow has been detected by Swift-XRT (Osborne et al. 2025, GCN 39947). The Fermi GBM Final Localization (GCN 39944) is consistent with the Swift-BAT and Swift-XRT positions (Page et al. 2025, GCN 39940). The angle from the Fermi LAT boresight is 46 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 4.8 s (50-300 keV). The time-averaged spectrum from T0-0.6 to T0+6.53 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.9 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 95 +/- 8 keV. The event fluence (10-1000 keV) in this time interval is (1.50 +/- 0.08)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.26 s in the 10-1000 keV band is 6.5 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 86 +/- 10 keV, alpha = -0.8 +/- 0.2 and beta = -2.7 +/- 0.4. 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 39970 table
GRB_name GRB250330A
GCN_number 39970
Detection_method Other
ra 252.9459°
decl -86.8811°
Circular_text TITLE: GCN CIRCULAR NUMBER: 39970 SUBJECT: GRB 250330A: VLT/FORS2 Afterglow Detection DATE: 25/03/31 12:35:19 GMT FROM: Rosa L. Becerra at Tor Vergata, Roma Rosa L. Becerra (U Rome), Yu-Han Yang (U Rome), Simone Dichiara (PSU), Muskan Yadav (U Rome), Eleonora Troja (U Rome), Lei Hu (CMU) and Roberto Ricci (U Rome) report on behalf of the ERC BHianca team: We reobserved the field of GRB 250330A (Cenko et al., GCN 39938) with the FORS2 imager on the ESO VLT UT1 (Antu). Observations began at T+19.8 hours after the trigger and were carried out in the R filter at an average seeing of 1.0" and airmass about 2.5. A comparison to our first epoch (Becerra et al., GCN 39941) reveals a fading source within the XRT enhanced position (Evans et al., GCN 39947), located at RA, Dec (J2000) = 16:51:47.01, -86:52:51.85. We estimate a preliminary magnitude of R~23.2 AB mag at 1.25 h post-trigger, calibrated using nearby stars from the SkyMapper Southern Survey (SMSS) Fourth Data Release (DR4) catalog (Onken et al., 2024) and not corrected for Galactic extinction. We thank the staff at the VLT for the rapid execution of these observations.
GCN 40055 table
GRB_name GRB250330A
GCN_number 40055
Detection_method Swift-BAT Det
ra 252.6850°
decl -86.8750°
Circular_text TITLE: GCN CIRCULAR NUMBER: 40055 SUBJECT: GRB 250330A Swift-BAT refined analysis DATE: 25/04/04 16:15:22 GMT FROM: Mike Moss at NASA GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC), R. Gupta (GSFC), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-137 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 250330A (trigger #1299776) (Cenko, et al., GCN Circ. 39938). The BAT ground-calculated position is RA, Dec = 252.685, -86.875 deg which is RA(J2000) = 16h 50m 44.5s Dec(J2000) = -86d 52' 29.6" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 98%. The mask-weighted light curve shows a single well defined fast-rise exponential- decay pulse shape. the T90 (15-350 keV) is 11.27 +- 2.53 sec (estimated error including systematics). The time-averaged spectrum from T-0.16 to T+14.33 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.72 +- 0.10. The fluence in the 15-150 keV band is 9.2 +- 0.6 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T+0.26 sec in the 15-150 keV band is 4.0 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1299776