GRB240718A

This page lists all entries on GRB240718A in GRBweb

Summary Fermi GBM IPN GCN 36898 GCN 36899 GCN 36901 GCN 36903 GCN 36905 GCN 36907 GCN 36954

Summary table
Variable Value Source
GRB_name_Fermi GRB240718270
T0 6:29:00 UTC GCN_circulars,Fermi GBM final loc
ra 252.7792° IPN
decl -25.1000° IPN
pos_error 3.00e-01° IPN
T90 58.625 s Fermi_GBM
T90_error 0.81 s Fermi_GBM
T90_start 6:29:00.754 UTC Fermi_GBM
fluence 5.58e-05 erg/cm² Fermi_GBM
fluence_error 2.57e-08 erg/cm² Fermi_GBM
T100 59.379 s
GBM_located False
mjd 60509.27013888889 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB240718270
trigger_name bn240718270
ra 257.7800°
decl -25.1100°
pos_error 2.61e+00°
datum 2024-07-18
t_trigger 6:29:00.434 UTC
T90 58.625 s
T90_error 0.81 s
T90_start 6:29:00.754 UTC
fluence 5.58e-05 erg/cm²
fluence_error 2.57e-08 erg/cm²
flux_1024 2.99e+01 erg/cm²/s
flux_1024_error 4.90e-01 erg/cm²/s
flux_1024_time 2.56e-01 erg/cm²/s
flux_64 4.17e+01 erg/cm²/s
flux_64_error 2.82e+00 erg/cm²/s
IPN table
GRB_name GRB240718A
ra 252.7792°
decl -25.1000°
pos_error 3.00e-01°
GCN 36898 table
GRB_name GRB240718A
GCN_number 36898
Detection_method Fermi GBM final loc
t_trigger 6:29:00 UTC
ra 252.9000°
decl -27.3000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36898 SUBJECT: GRB 240718A: Fermi GBM Final Real-time Localization DATE: 24/07/18 06:39:25 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 06:29:00 UT on 18 Jul 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240718A (trigger 742976945.434234 / 240718270). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 252.9, Dec = -27.3 (J2000 degrees, equivalent to J2000 16h 51m, -27d 18'), with a statistical uncertainty of 1.3 degrees. The angle from the Fermi LAT boresight is 50.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240718270/quicklook/glg_skymap_all_bn240718270.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240718270/quicklook/glg_healpix_all_bn240718270.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240718270/quicklook/glg_lc_medres34_bn240718270.gif
GCN 36899 table
GRB_name GRB240718A
GCN_number 36899
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36899 SUBJECT: GRB 240718A: BALROG localization (Fermi Trigger 742976945 / GRB 240718270) DATE: 24/07/18 07:15:28 GMT FROM: Jochen Greiner at MPE T. Preis, B. Biltzinger, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 742976945 at 06:29:00 on 18 July 2024 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position is: RA(2000.0) = 250.8 deg Decl.(2000.0) = -26.9 deg The 1 sigma statistical error radius is 1.9 deg. We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB240718270/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB240718270/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB240718270/json
GCN 36901 table
GRB_name GRB240718A
GCN_number 36901
Detection_method Fermi LAT Det
t_trigger 6:29:00 UTC
ra 252.7800°
decl -25.1100°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36901 SUBJECT: GRB 240718A: Fermi-LAT Detection DATE: 24/07/18 15:51:08 GMT FROM: Davide Depalo at Politecnico and INFN Bari D. Depalo (Politecnico & INFN Bari), E. Bissaldi (Politecnico & INFN Bari), R. Gupta (NASA/GSFC), and A. Holzmann (DF, University of Buenos Aires, Argentina) report on behalf of the Fermi-LAT Collaboration: At 06:29:00 UT on July, 18, 2024 Fermi-LAT detected high-energy emission from GRB 240718A which was also detected by Fermi-GBM (trigger 742976945 / 240718270, GCN 36898) and SVOM/GRM (GCN 36900). The best LAT on-ground location is found to be RA, Dec = 252.78, -25.11 (J2000) with an error radius of 0.23 deg (90 % containment, statistical error only). This was 52 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The photon flux above 100 MeV in the time interval 0-400 s after the GBM trigger is (1.25 +/- 0.43) E-5 ph/cm2/s. The estimated photon index above 100 MeV is - 2.2 +/- 0.3. The highest-energy photon is a 2.7 GeV event which is observed about 17 seconds after the GBM trigger. A Swift ToO has been requested. The Fermi-LAT point of contact for this burst is Davide Depalo (d.depalo2@phd.poliba.it). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 36903 table
GRB_name GRB240718A
GCN_number 36903
Detection_method Fermi GBM Det
t_trigger 6:29:00.430 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36903 SUBJECT: GRB 240718A: Fermi GBM Observation DATE: 24/07/18 17:41:09 GMT FROM: Cuán de Barra at UCD C. de Barra (UCD) and C. Meegan (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 06:29:00.43 UT on 18 July 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240718A (trigger 742976945/240718270), which was also detected by Fermi-LAT (Depalo et al. 2024, GCN 36901), SPI-ACS, and SVOM/GRM (SVOM/GRM Team 2024, GCN 36900). The Final Real-time Localization was reported previously (Fermi GBM Team 2024, GCN 36898).The Fermi GBM on-ground location is consistent with the Fermi-LAT position. The angle from the Fermi LAT boresight is 52 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 59 s (50-300 keV). The time-averaged spectrum from T0-2.7 to T0+59.8 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.00 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 1626 +/- 106 keV. The event fluence (10-1000 keV) in this time interval is (5.81 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.26 s in the 10-1000 keV band is 29.9 +/- 0.5 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 36905 table
GRB_name GRB240718A
GCN_number 36905
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36905 SUBJECT: Fermi GRB 240718A: Global MASTER-Net observations report DATE: 24/07/18 19:33:13 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko, G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij (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. Gress, N.M. Budnev, O.Ershova (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), V. Yurkov, A. Gabovich (Blagoveschensk Educational State University) 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 240718A ( Fermi GBM team, GCN 36898) errorbox 42681 sec after notice time and 42709 sec after trigger time at 2024-07-18 18:20:49 UT, with upper limit up to 15.5 mag. The observations began at zenith distance = 19 deg. The sun altitude is -30.7 deg. The galactic latitude b = 10 deg., longitude l = 355 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2534080 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 42724 | 2024-07-18 18:20:49 | MASTER-SAAO | (16h 49m 33.00s , -25d 18m 29.3s) | C | 30 | 15.2 | 42774 | 2024-07-18 18:21:38 | MASTER-SAAO | (16h 49m 26.14s , -25d 19m 28.7s) | C | 30 | 15.5 | 42823 | 2024-07-18 18:22:28 | MASTER-SAAO | (16h 49m 33.34s , -25d 19m 11.5s) | C | 30 | 15.4 | 42877 | 2024-07-18 18:23:22 | MASTER-SAAO | (16h 49m 29.78s , -25d 17m 44.9s) | C | 30 | 15.2 | 42927 | 2024-07-18 18:24:12 | MASTER-SAAO | (16h 49m 29.74s , -25d 19m 18.0s) | C | 30 | 15.3 | 43172 | 2024-07-18 18:28:29 | MASTER-SAAO | (16h 49m 26.41s , -25d 19m 23.3s) | C | 5 | 14.7 | 43197 | 2024-07-18 18:28:54 | MASTER-SAAO | (16h 49m 33.59s , -25d 19m 06.3s) | C | 5 | 14.9 | 43225 | 2024-07-18 18:29:22 | MASTER-SAAO | (16h 49m 29.53s , -25d 17m 33.6s) | C | 5 | 15.1 | 43252 | 2024-07-18 18:29:49 | MASTER-SAAO | (16h 49m 29.54s , -25d 18m 57.2s) | C | 5 | 14.9 | 43283 | 2024-07-18 18:30:19 | MASTER-SAAO | (16h 49m 33.16s , -25d 17m 50.4s) | C | 5 | 14.8 | 43314 | 2024-07-18 18:30:51 | MASTER-SAAO | (16h 49m 26.33s , -25d 18m 21.2s) | C | 5 | 14.9 | 43343 | 2024-07-18 18:31:20 | MASTER-SAAO | (16h 49m 27.07s , -25d 17m 21.3s) | C | 5 | 14.8 | 43367 | 2024-07-18 18:31:44 | MASTER-SAAO | (16h 49m 31.97s , -25d 18m 20.6s) | C | 5 | 15.1 | 43393 | 2024-07-18 18:32:10 | MASTER-SAAO | (16h 49m 26.06s , -25d 19m 20.7s) | C | 5 | 14.6 | 43417 | 2024-07-18 18:32:34 | MASTER-SAAO | (16h 49m 32.43s , -25d 19m 07.1s) | C | 5 | 14.7 | 43442 | 2024-07-18 18:32:59 | MASTER-SAAO | (16h 49m 29.51s , -25d 17m 25.4s) | C | 5 | 14.8 | 43467 | 2024-07-18 18:33:24 | MASTER-SAAO | (16h 49m 29.48s , -25d 19m 11.9s) | C | 5 | 14.7 | 43494 | 2024-07-18 18:33:51 | MASTER-SAAO | (16h 49m 32.06s , -25d 17m 19.6s) | C | 5 | 14.9 | 43518 | 2024-07-18 18:34:15 | MASTER-SAAO | (16h 49m 26.51s , -25d 18m 18.5s) | C | 5 | 14.9 | 43549 | 2024-07-18 18:34:46 | MASTER-SAAO | (16h 49m 26.37s , -25d 17m 18.0s) | C | 5 | 14.8 | 43574 | 2024-07-18 18:35:11 | MASTER-SAAO | (16h 49m 32.19s , -25d 18m 18.2s) | C | 5 | 14.8 | 43598 | 2024-07-18 18:35:35 | MASTER-SAAO | (16h 49m 28.07s , -25d 19m 17.4s) | C | 5 | 15.1 | 43629 | 2024-07-18 18:36:06 | MASTER-SAAO | (16h 49m 33.98s , -25d 18m 54.5s) | C | 5 | 15.0 | 43653 | 2024-07-18 18:36:30 | MASTER-SAAO | (16h 49m 30.73s , -25d 17m 23.2s) | C | 5 | 14.6 | 43677 | 2024-07-18 18:36:54 | MASTER-SAAO | (16h 49m 31.09s , -25d 18m 59.1s) | C | 5 | 13.5 | 43933 | 2024-07-18 18:41:07 | MASTER-SAAO | (16h 49m 28.90s , -25d 18m 12.4s) | C | 10 | 14.0 | 43962 | 2024-07-18 18:41:37 | MASTER-SAAO | (16h 49m 30.19s , -25d 17m 12.1s) | C | 10 | 14.2 | 43991 | 2024-07-18 18:42:06 | MASTER-SAAO | (16h 49m 35.45s , -25d 18m 12.1s) | C | 10 | 14.1 | 44029 | 2024-07-18 18:42:44 | MASTER-SAAO | (16h 49m 30.96s , -25d 19m 11.0s) | C | 10 | 14.5 | 44058 | 2024-07-18 18:43:13 | MASTER-SAAO | (16h 49m 37.16s , -25d 19m 02.1s) | C | 10 | 14.6 | 44090 | 2024-07-18 18:43:45 | MASTER-SAAO | (16h 49m 34.06s , -25d 17m 38.5s) | C | 10 | 14.1 | 44122 | 2024-07-18 18:44:17 | MASTER-SAAO | (16h 49m 34.13s , -25d 18m 59.1s) | C | 10 | 14.4 | 44151 | 2024-07-18 18:44:46 | MASTER-SAAO | (16h 49m 36.55s , -25d 17m 37.3s) | C | 10 | 14.7 | 44181 | 2024-07-18 18:45:16 | MASTER-SAAO | (16h 49m 31.31s , -25d 18m 09.3s) | C | 10 | 14.9 | 44211 | 2024-07-18 18:45:46 | MASTER-SAAO | (16h 49m 31.18s , -25d 17m 08.7s) | C | 10 | 15.1 | 44240 | 2024-07-18 18:46:15 | MASTER-SAAO | (16h 49m 37.46s , -25d 18m 08.2s) | C | 10 | 14.9 | 44281 | 2024-07-18 18:46:56 | MASTER-SAAO | (16h 49m 31.70s , -25d 19m 08.0s) | C | 10 | 15.0 | 44319 | 2024-07-18 18:47:33 | MASTER-SAAO | (16h 49m 38.03s , -25d 18m 50.2s) | C | 10 | 15.0 | 44349 | 2024-07-18 18:48:04 | MASTER-SAAO | (16h 49m 35.84s , -25d 17m 18.5s) | C | 10 | 14.7 | 44380 | 2024-07-18 18:48:35 | MASTER-SAAO | (16h 49m 36.01s , -25d 18m 54.3s) | C | 10 | 14.8 | 44410 | 2024-07-18 18:49:05 | MASTER-SAAO | (16h 49m 39.77s , -25d 17m 12.7s) | C | 10 | 14.9 | 44439 | 2024-07-18 18:49:34 | MASTER-SAAO | (16h 49m 33.27s , -25d 18m 05.7s) | C | 10 | 14.9 | 44469 | 2024-07-18 18:50:04 | MASTER-SAAO | (16h 49m 32.75s , -25d 17m 05.6s) | C | 10 | 14.9 | 44498 | 2024-07-18 18:50:33 | MASTER-SAAO | (16h 49m 39.76s , -25d 18m 05.1s) | C | 10 | 15.0 | 44528 | 2024-07-18 18:51:03 | MASTER-SAAO | (16h 49m 34.55s , -25d 19m 04.1s) | C | 10 | 15.1 | 44557 | 2024-07-18 18:51:32 | MASTER-SAAO | (16h 49m 41.20s , -25d 18m 51.6s) | C | 10 | 14.9 | 44587 | 2024-07-18 18:52:02 | MASTER-SAAO | (16h 49m 37.54s , -25d 17m 22.1s) | C | 10 | 15.0 | 45632 | 2024-07-18 19:09:27 | MASTER-SAAO | (16h 49m 47.32s , -25d 18m 48.2s) | C | 10 | 13.3 | 45724 | 2024-07-18 19:10:59 | MASTER-SAAO | (16h 49m 48.12s , -25d 16m 59.8s) | C | 10 | 13.1 | 45753 | 2024-07-18 19:11:28 | MASTER-SAAO | (16h 49m 43.00s , -25d 17m 47.9s) | C | 10 | 12.3 | 45787 | 2024-07-18 19:12:02 | MASTER-SAAO | (16h 49m 44.34s , -25d 16m 47.7s) | C | 10 | 12.1 | 45817 | 2024-07-18 19:12:32 | MASTER-SAAO | (16h 49m 49.91s , -25d 17m 47.3s) | C | 10 | 13.1 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 36907 table
GRB_name GRB240718A
GCN_number 36907
Detection_method Konus-Wind Det
t_trigger 6:29:05.357 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36907 SUBJECT: Konus-Wind detection of GRB 240718A DATE: 24/07/19 15:45:08 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 240718A (Fermi-GBM detection: Fermi GBM team, GCN 36898; Preis et al., GCN 36899; de Barra & Meegan, GCN 36903; SVOM/GRM observation: Zhang et al., GCN 36900; Fermi-LAT detection: Depalo et al., GCN 36901) triggered Konus-Wind at T0=23345.357 s UT (06:29:05.357). The burst light curve shows a multipeaked structure which starts at ~T0-0.2 s and has a total duration of ~53 s. The emission is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240718_T23345/ As observed by Konus-Wind, the burst had a fluence of 1.22(-0.11,+0.11)x10^-4 erg/cm2, and a 64-ms peak flux, measured from T0+0.560 s, of 5.04(-0.58,+0.59)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+59.648 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.91(-0.08,+0.08) and Ep = 1355(-178,+213) keV (chi2 = 115/83 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.4 (chi2 = 115/82 dof). The spectrum near the maximum count rate (measured from T0+0.256 to T0+2.304 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model with alpha = -0.38(-0.08,+0.08) and Ep = 1126(-77,+82) keV (chi2 = 67/63 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.6 (chi2 = 67/62 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 36954 table
GRB_name GRB240718A
GCN_number 36954
Detection_method Fermi GBM Det
t_trigger 6:29:06.700 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36954 SUBJECT: GRB 240718A: GRBAlpha detection DATE: 24/07/27 19:57:33 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa, M. Kolar (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Duriskova, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. The long-duration GRB 240718A (Fermi/GBM detection: GCN 36898; SVOM/GRM detection: GCN 36900; Konus/Wind detection: GCN 36907; INTEGRAL/SPI-ACS detection: trigger no. 10795) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract). The detection was confirmed at the peak time 2024-07-18 06:29:06.7 UTC. The T90 duration measured by GRBAlpha is 13.5 s and the overall significance during T90 reaches 27 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240718A_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.