{
  "createdOn": 1730919199266,
  "circularId": 38103,
  "subject": "Konus-Wind detection of GRB 241105A (short with extended emission)",
  "submittedHow": "email",
  "eventId": "GRB 241105A",
  "body": "D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin,\nA. Tsvetkova,  M. Ulanov, and T. Cline,\non behalf of the Konus-Wind team, report:\n\nThe likely short GRB 241105A (Fermi GBM team, GCN 38085)\ntriggered Konus-Wind (KW) at T0=57966.516 s UT (16:06:06.516).\n\nThe burst light curve shows a short initial pulse,\nwhich starts at ~T0-0.5 s, peaks at ~T0, and has a total duration\nof ~1.5 s, which was followed by a weaker extended emission,\nvisible in KW up to ~T0+60 s.\nThe emission is seen up to ~4 MeV.\n\nThe Konus-Wind light curve of this GRB is available at\nhttp://www.ioffe.ru/LEA/GRBs/GRB241105_T57966/\n\nAs observed by Konus-Wind, the burst had\na fluence of (2.01 ± 0.47)x10^-5 erg/cm^2 and\na 64-ms peak energy flux, measured from T0 - 0.064 s,\nof (2.37 ± 0.30)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).\n\nThe time-integrated spectrum (measured from T0 to T0+57.640 s)\nis best fit in the 20 keV - 15 MeV range\nby a GRB (Band) function with the following model parameters:\nthe low-energy photon index alpha = -0.69 (-0.37,+0.67),\nthe high energy photon index beta = -1.76 (-0.55,+0.21),\nthe peak energy Ep = 374 (-165,+437) keV,\nchi2 = 98/97 dof.\n\nThe spectrum of the initial pulse alone (measured from T0-0.512 s to T0+0.960 s)\ncan be described by a power law with exponential cutoff (CPL) model:\ndN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)\nwith  alpha = -0.90(-0.15,+0.15) and Ep = 417(-82,+111) keV.\n\nAssuming the redshift z=2.702 (Izzo et al., GCN 38097)\nand a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,\nand Omega_Lambda = 0.685 (Planck Collaboration, 2014),\nwe estimate the burst isotropic energy release E_iso to (3.42 ± 0.80)x10^53 erg,\nthe isotropic peak luminosity L_iso to (1.49 ± 0.18)x10^53 erg/s,\nthe rest-frame peak energy of the time-integrated spectrum Ep,i,z to ~1380 keV,\nand the rest-frame peak energy at the peak of the emission Ep,p,z to ~1540 keV.\nWith the obtained estimates, GRB 241105A fits 68% prediction bands for\nboth 'Amati' and 'Yonetoku' relations derived for the sample of >300 long\nKW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),\nsee http://www.ioffe.ru/LEA/GRBs/GRB241105_T57966/GRB241105A_rest_frame.pdf\n\nAll the quoted errors are estimated at the 68% confidence level.\nAll the presented results are preliminary.\n",
  "submitter": "Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>",
  "bibcode": "2024GCN.38103....1F"
}