{
  "bibcode": "2019GCN.23637....1T",
  "body": "A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,\nM. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline\non behalf of the Konus-Wind team, report:\n\nThe�� GRB 190106A (Swift detection: Sonbas et al., GCN 23615;\nPalmer et al., GCN 23625)\ntriggered Konus-Wind at T0=48887.602 s UT (13:34:47.602).\n\nThe burst light curve shows a multi-peaked structure\nwhich starts at ~T0-5 s and has a total duration of ~79 s.\nThe emission is seen up to ~2 MeV.\n\nAs observed by Konus-Wind, the burst\nhad a fluence of 1.12(-0.17,+0.25)x10^-5 erg/cm2,\nand a 64-ms peak energy flux, measured from T0-0.044 s,\nof 1.81(-0.89,+1.19)x10^-6 erg/cm2/s\n(both in the 20 keV - 10 MeV energy range).\n\nThe time-integrated spectrum of the burst\n(measured from T0 to T0+82.176 s)\nis best fit in the 20 keV - 16 MeV range\nby a power law with exponential cutoff model:\ndN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)\nwith�� alpha = -1.00(-0.50,+0.63),\nand Ep = 171(-42,+90) keV (chi2 = 81/98 dof).\nFitting by the GRB (Band) model yields the same alpha and Ep,\nand an upper limit on the high energy photon index:\nbeta < -2.31 (chi2 = 81/97 dof).\n\nThe spectrum near the peak count rate\n(measured from T0 to T0+8.448 s)\nis best fit in the 20 keV - 1.2 MeV range\nby the power law with exponential cutoff model:\nwith�� alpha = -1.15(-0.50,+0.66),\nand Ep = 216(-66,+308) keV (chi2 = 55/60 dof).\nFitting by the GRB (Band) model yields the same alpha and Ep,\nand an upper limit on the high energy photon index:\nbeta < -1.85 (chi2 = 55/59 dof).\n\nAssuming the redshift z=1.859 (Xu et al., GCN 23629;\nMao et al., GCN 23630; Schady et al., GCN 23632)\nand a standard cosmology model with H_0 = 67.3 km/s/Mpc,\nOmega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),\nwe estimate the following rest-frame parameters:\nthe isotropic energy release E_iso is 9.96(-1.55,+2.25)x10^52 erg,\nthe peak luminosity L_iso is 4.62(-2.28,+3.03)x10^52 erg/s,\nand the rest-frame peak energy of the time-integrated spectrum,\nEp,i, is 489(-120,+257) keV, and the rest-frame peak energy of\nthe 'peak' spectrum, Ep,p,z, is 618(-189, 881) keV.\nWith these energetics, the burst lies within the 68% prediction bands\nfor both 'Amati' and 'Yonetoku' relations built for the sample\nof 138 long KW GRBs with known redshifts\n(Tsvetkova et al., ApJ 850 161, 2017).\n\nThe Konus-Wind light curve of this GRB is available at\nhttp://www.ioffe.ru/LEA/GRBs/GRB190106_T48887/\n\nAll the quoted errors are at the 90% confidence level.\nAll the quoted values are preliminary.",
  "circularId": 23637,
  "createdOn": 1546892523000,
  "email": "tsvetkova@mail.ioffe.ru",
  "subject": "Konus-Wind observation of GRB 190106A",
  "submitter": "Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>",
  "eventId": "GRB 190106A"
}