GRB240527B

This page lists all entries on GRB240527B in GRBweb

Summary Fermi GBM IPN GCN 36546 GCN 36547 GCN 36550 GCN 36553 GCN 36558

Summary table
Variable Value Source
GRB_name_Fermi GRB240527586
T0 14:03:51.500 UTC GCN_circulars,Fermi GBM Det
ra 128.1000° IPN
decl -14.4833° IPN
pos_error 1.83e-01° IPN
T90 24.832 s Fermi_GBM
T90_error 0.81 s Fermi_GBM
T90_start 14:03:52.016 UTC Fermi_GBM
fluence 1.18e-05 erg/cm² Fermi_GBM
fluence_error 2.25e-08 erg/cm² Fermi_GBM
T100 25.348 s
GBM_located False
mjd 60457.58601273148 GCN_circulars,Fermi GBM Det
Fermi GBM table
GRB_name_Fermi GRB240527586
trigger_name bn240527586
ra 128.5100°
decl -12.6800°
pos_error 2.67e+00°
datum 2024-05-27
t_trigger 14:03:51.504 UTC
T90 24.832 s
T90_error 0.81 s
T90_start 14:03:52.016 UTC
fluence 1.18e-05 erg/cm²
fluence_error 2.25e-08 erg/cm²
flux_1024 1.09e+01 erg/cm²/s
flux_1024_error 3.16e-01 erg/cm²/s
flux_1024_time 1.38e+01 erg/cm²/s
flux_64 1.39e+01 erg/cm²/s
flux_64_error 1.32e+00 erg/cm²/s
IPN table
GRB_name GRB240527B
ra 128.1000°
decl -14.4833°
pos_error 1.83e-01°
GCN 36546 table
GRB_name GRB240527B
GCN_number 36546
Detection_method Fermi GBM Other
ra 128.5100°
decl -12.6800°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36546 SUBJECT: GRB 240527B: Fermi GBM Final Localization DATE: 24/05/27 15:08:45 GMT FROM: Cori Fletcher at USRA The Fermi GBM team reports the detection of a likely LONG GRB "At 14:03:51.50 UT on 27 May 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240527B (trigger 738511436/240527586). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 128.51, Dec = -12.68 (J2000 degrees, equivalent to J2000 8h 34m, -12d 40'), with a statistical uncertainty of 1.70 degrees. The angle from the Fermi LAT boresight is 78 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240527586/quicklook/glg_skymap_all_bn240527586.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/bn240527586/quicklook/glg_healpix_all_bn240527586.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240527586/quicklook/glg_lc_medres34_bn240527586.gif"
GCN 36547 table
GRB_name GRB240527B
GCN_number 36547
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36547 SUBJECT: Fermi GRB 240527B: Global MASTER-Net observations report DATE: 24/05/27 17:15:55 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 240527B ( Fermi GBM team, GCN 36546) errorbox 9266 sec after notice time and 9291 sec after trigger time at 2024-05-27 16:38:42 UT, with upper limit up to 19.4 mag. Observations started at twilight. The observations began at zenith distance = 33 deg. The sun altitude is -11.7 deg. The galactic latitude b = 16 deg., longitude l = 237 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2472451 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 9321 | 2024-05-27 16:38:42 | MASTER-SAAO | (08h 28m 27.08s , -12d 11m 25.9s) | C | 60 | 18.5 | 9401 | 2024-05-27 16:40:02 | MASTER-SAAO | (08h 36m 37.47s , -12d 10m 23.3s) | C | 60 | 18.6 | 10243 | 2024-05-27 16:54:04 | MASTER-SAAO | (08h 28m 28.80s , -12d 10m 06.2s) | C | 60 | 19.1 | 10323 | 2024-05-27 16:55:24 | MASTER-SAAO | (08h 36m 36.04s , -12d 10m 49.2s) | C | 60 | 19.3 | 10403 | 2024-05-27 16:56:44 | MASTER-SAAO | (08h 32m 25.70s , -14d 04m 43.2s) | C | 60 | 19.2 | 10483 | 2024-05-27 16:58:04 | MASTER-SAAO | (08h 40m 34.75s , -14d 05m 43.1s) | C | 60 | 19.2 | 10563 | 2024-05-27 16:59:24 | MASTER-SAAO | (08h 25m 05.25s , -10d 15m 57.2s) | C | 60 | 19.2 | 10642 | 2024-05-27 17:00:43 | MASTER-SAAO | (08h 33m 14.26s , -10d 17m 11.8s) | C | 60 | 19.3 | 10803 | 2024-05-27 17:03:24 | MASTER-SAAO | (08h 24m 52.36s , -14d 03m 20.3s) | C | 60 | 19.2 | 10883 | 2024-05-27 17:04:44 | MASTER-SAAO | (08h 43m 57.14s , -12d 11m 27.0s) | C | 60 | 19.3 | 11042 | 2024-05-27 17:07:23 | MASTER-SAAO | (08h 40m 33.16s , -10d 16m 51.0s) | C | 60 | 19.4 | 11202 | 2024-05-27 17:10:03 | MASTER-SAAO | (08h 28m 19.16s , -12d 10m 06.0s) | C | 60 | 19.3 | 11282 | 2024-05-27 17:11:23 | MASTER-SAAO | (08h 36m 32.47s , -12d 09m 07.5s) | C | 60 | 19.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 36550 table
GRB_name GRB240527B
GCN_number 36550
Detection_method Fermi LAT Det
t_trigger 14:03:51.500 UTC
ra 128.1000°
decl -14.4800°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36550 SUBJECT: GRB 240527B: Fermi-LAT detection DATE: 24/05/27 23:09:39 GMT FROM: Rahul Gupta at NASA/GSFC R. Gupta (NASA/GSFC), F. Longo (University and INFN, Trieste), and A. Holzmann (DF, University of Buenos Aires, Argentina) report on behalf of the Fermi-LAT Collaboration: At 14:03:51.50 on May, 27, 2024 Fermi-LAT detected high-energy emission from GRB 240527B which was also detected by Fermi-GBM (trigger 738511436 / 240527586, GCN 36546). The best LAT on-ground location is found to be RA, Dec = 128.10, -14.48 (J2000) with an error radius of 0.19 deg (90 % containment, statistical error only). This was 77 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 0-3000 s after the GBM trigger is (6.2 +/- 3.0) E-7 ph/cm2/s. The estimated photon index above 100 MeV is - 1.6+/- 0.2. The highest-energy photon is a 4.0 GeV event which is observed about 1200 seconds after the GBM trigger. A Swift ToO has been approved. The Fermi-LAT point of contact for this burst is Rahul Gupta ( rahul.gupta@nasa.gov). 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 36553 table
GRB_name GRB240527B
GCN_number 36553
Detection_method Fermi GBM Det
t_trigger 14:03:51.500 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36553 SUBJECT: GRB 240527B: Fermi GBM Observation DATE: 24/05/28 03:01:00 GMT FROM: Cori Fletcher at USRA C. Fletcher (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 14:03:51.50 UT on 27 May 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240527B (trigger 738511436/240527586). which was also detected by Fermi LAT (R. Gupta et al. 2024, GCN 36550). The Fermi GBM on-ground location (GCN 36546) is consistent with the Fermi LAT position. The angle from the Fermi LAT boresight is 78 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 24.8 s (50-300 keV). The time-averaged spectrum from T0+0.003 to T0+29.440 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.07 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 280 +/- 20 keV. The event fluence (10-1000 keV) in this time interval is (1.46 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+14 s in the 10-1000 keV band is 10.9 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 201 +/- 20 keV, alpha = -0.95 +/- 0.05 and beta = -2.1 +/- 0.1. 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/"C. Fletcher (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 14:03:51.50 UT on 27 May 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240527B (trigger 738511436/240527586). which was also detected by Fermi LAT (R. Gupta et al. 2024, GCN 36550). The Fermi GBM on-ground location (GCN 36546) is consistent with the Fermi LAT position. The angle from the Fermi LAT boresight is 78 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 24.8 s (50-300 keV). The time-averaged spectrum from T0+0.003 to T0+29.440 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.07 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 280 +/- 20 keV. The event fluence (10-1000 keV) in this time interval is (1.46 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+14 s in the 10-1000 keV band is 10.9 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 201 +/- 20 keV, alpha = -0.95 +/- 0.05 and beta = -2.1 +/- 0.1. 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 36558 table
GRB_name GRB240527B
GCN_number 36558
Detection_method Swift-XRT Other
ra 128.1539°
decl -14.4374°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36558 SUBJECT: GRB 240527B: Swift-XRT afterglow detection DATE: 24/05/29 05:53:44 GMT FROM: Phil Evans at U of Leicester J. D. Gropp (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAR), T. Sbarrato (INAF-OAB) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 240527B, collecting 5.2 ks of Photon Counting (PC) mode data between T0+27.3 ks and T0+135.5 ks. Eight uncatalogued X-ray sources are detected, of which one ("Source 7") is above the RASS 3-sigma upper limit at this position and fading with >3-sigma significance, and is therefore likely the GRB afterglow. Using 1624 s of PC mode data and 3 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 = 128.15387, -14.43738 which is equivalent to: RA (J2000): 08h 32m 36.93s Dec(J2000): -14d 26' 14.6" with an uncertainty of 2.0 arcsec (radius, 90% confidence). This position is 4.0 arcmin from the Fermi/LAT position. The light curve can be modelled with a power-law decay with a decay index of alpha=1.23 (+0.16, -0.14). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.70 (+0.08, -0.06). The best-fitting absorption column is consistent with the Galactic value of 5.7 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 3.8 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.7 (+/-1.9) x 10^20 cm^-2 Galactic foreground: 5.7 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.70 (+0.08, -0.06) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00021694. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/00021694. This circular is an official product of the Swift-XRT team.