//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24794 SUBJECT: GRB 190611B: Fermi GBM detection DATE: 19/06/12 18:39:54 GMT FROM: Christian Malacaria at NASA-MSFC/USRA C. Malacaria (NASA-MSFC/USRA) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 22:47:49.34 UT on the 11th of June 2019, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 190611B (trigger 581986074 / 190611950). The on-ground calculated location, using the GBM trigger data, is RA = 88.9, DEC = 53.1 (J2000 degrees, equivalent to 05 h 56 m, 53 d 07 '), with a statistical uncertainty of 1.0 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error [Connaughton et al. 2015, ApJS, 216, 32] ). The angle from the Fermi LAT boresight at the GBM trigger time is 117.0 degrees. The GBM light curve consists of two broad pulses with a duration (T90) of about 100.6 s (50-300 keV). The time-averaged spectrum from T0-0.0 s to T0+18.2 s is best fit by a Band function with Epeak = 210.3 +/- 18.9 keV, alpha = -1.00 +/- 0.04, and beta = -1.98 +/- 0.05 The event fluence (10-1000 keV) in this time interval is (2.43 +/- 0.40)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+71.8 s in the 10-1000 keV band is 32.4 +/- 0.6 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 OPS NOTE(16jun19), Per author's request, the "190611A" in the first sentence was corrected to "190611B".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24811 SUBJECT: IPN Triangulation of GRB 190611B DATE: 19/06/13 14:03:15 GMT FROM: Dmitry Svinkin at Ioffe Institute K. Hurley, on behalf of the IPN, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova, and T. Cline on behalf of the Konus-Wind team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, A. Goldstein, M. S. Briggs, and C. Wilson-Hodge on behalf of the Fermi GBM team, S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the GRS-Odyssey GRB team, report: The long-duration GRB 190611B (Malacaria and Meegan, GCN Circ. 24794) was detected by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT) at about 82069 s UT (22:47:49). The burst was outside the coded field of view of the BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 84.968 (05h 39m 52s) +52.773 (+52d 46' 24") Corners: 81.481 (05h 25m 55s) +50.833 (+50d 49' 57") 88.130 (05h 52m 31s) +54.352 (+54d 21' 06") 89.119 (05h 56m 29s) +54.477 (+54d 28' 38") 82.284 (05h 29m 08s) +51.059 (+51d 03' 34") --------------------------------------------- The error box area is about 1.15 sq. deg, and its maximum dimension is 5.9 deg (the minimum one is 6.42 arcmin). The Sun distance was about 30 deg. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB190611_T82065/IPN/ The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24813 SUBJECT: GRB 190611B: BALROG localization (Fermi Trigger 581986074 / GRB 190611950) DATE: 19/06/13 14:34:27 GMT FROM: Jochen Greiner at MPE,Garching F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 581986074 at 22:47:49 on 11 June 2019 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 (1 sigma statistical errors) is: RA(2000.0) = 85.2+/-1.1 deg Decl.(2000.0) = 52.0+/-1.0 deg We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB190611950/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB190611950/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB190611950/json //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24827 SUBJECT: Konus-Wind observation of GRB 190611B DATE: 19/06/14 12:22:39 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, S. Golenetskii, R.Aptekar, A. Kozlova, A.Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 190611B (Fermi GBM detection: Malacaria & Meegan, GCN 24794; IPN triangulation: Hurley et al., GCN 24811) triggered Konus-Wind (KW) at T0=82065.599 s UT (22:47:45.599). The light curve of the burst shows two broad, multi-peaked pulses. The total duration of the burst is ~130 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/GRB190611_T82065/ As observed by Konus-Wind, the burst had a fluence of (9.2 ± 1.0)x10^-5 erg/cm2 and a 64-ms peak energy flux, measured from T0+17.344, of (1.33 ± 0.11)x10^-5 erg/cm2 (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+117.760 s) is best fit in the 20 keV - 20 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -1.01 (-0.08,+0.08), the high energy photon index beta = -2.74 (-0.88,+0.29), the peak energy Ep = 250 (-21,+24) keV, chi2 = 68/97 dof. The spectrum near the peak count rate (measured from T0+67.840 s to T0+77.568 s) is best fit in the 20 keV - 20 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.78 (-0.08,+0.09), the high energy photon index beta = -2.20 (-0.13,+0.10), the peak energy Ep = 307 (-29,+33) keV, chi2 = 83/97 dof. All the quoted errors are estimated at the 90% confidence level. All the presented results are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24830 SUBJECT: GRB 190611B: CALET Gamma-Ray Burst Monitor detection DATE: 19/06/14 14:25:24 GMT FROM: Valentin Pal'shin at AGU N. Cannady (GSFC/UMBC), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long, bright GRB 190611B (Fermi GBM detection: Malacaria and Meegan, GCN Circ. 24794; IPN Triangulation: Hurley et al., GCN Circ. 24811; BALROG localization: Kunzweiler et al., GCN Circ. 24813) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 22:47:46.257 UTC on 11 June 2019. The burst signal was seen by all CGBM detectors. The burst light curve shows two multi-peaked pulses: the first starts at T+2.8 sec, peaks at T+4.9 sec and ends at T+16.9 sec, the second starts at T+67.4 sec, peaks at T+75.4 sec and ends at T+118.8 sec. The T90 and T50 durations measured by the SGM data are 100.9 +- 3.9 sec and 13.9 +- 1.1 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1244328454/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24845 SUBJECT: GRB 190611B: AstroSat CZTI detection DATE: 19/06/18 04:27:34 GMT FROM: Prachee Ghumatkar at IUCAA/AstroSat P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed the detection of a long GRB 190611B, which was also detected by Fermi GBM (Malacaria C. et al., GCN #24794), Global MASTER-Net (Lipunov V. et al., GCN #24795), IPN Triangulation (Hurley K. et al., GCN #24811), BALROG (Kunzweiler F. et al., GCN #24813), Konus-Wind (Frederiks D. et al., GCN #24827) and CALET (Cannady N. et al., GCN #24830). The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 22:47:51.5 UT. Fermi/GBM lightcurve consists of two broad pulses. AstroSat could detect only first pulse of the burst, as during the second pulse the detector was in South Atlantic Anomaly (SAA). The measured peak count rate associated with the burst is 387 cts/s above the background in the combined data of four quadrants, with a total of 1251 cts. The local mean background count rate was 578 cts/s. Using cumulative rates, we measure a T90 of 7.35 s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.