J/MNRAS/418/2202 Analysis of γ-ray bursts (Dainotti+, 2011)
Towards a standard gamma-ray burst: tight correlations between the prompt and the afterglow plateau phase emission. Dainotti M.G., Ostrowski M., Willingale R. <Mon. Not. R. Astron. Soc., 418, 2202-2206 (2011)> =2011MNRAS.418.2202D
ADC_Keywords: Gamma rays ; X-ray sources Keywords: radiation mechanisms: non-thermal - gamma-ray burst: general Abstract: To find out the astrophysical processes responsible for gamma-ray burst (GRB), it is crucial to discover and understand the relations between their observational properties. This work was performed in the GRB rest frames using a sample of 62 long Swift GRBs with known redshifts. Following the earlier analysis of the correlation between afterglow luminosity (L*a) and break time (T*a), we extend it to correlations between the afterglow and the prompt emission GRB physical parameters. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 140 69 *A data list for GRBs with known redshifts analysed in the paper
Note on table1.dat: For further discussion of the data one should refer to Willingale et al., 2007ApJ...662.1093W, Dainotti et al. (2010ApJ...722L.215D, 2011ApJ...730..135D) and the present paper.
See also: J/A+AS/129/1 : GRANAT/WATCH catalogue of gamma-ray bursts (Sazonov+ 1998) J/ApJS/169/62 : GRB database of spectral lags (Hakkila+, 2007) J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011) J/A+A/528/A122 : SwiftFT catalog (Puccetti+, 2011) J/ApJ/701/824 : Afterglows of short and long-duration GRBs (Nysewander+, 2009) J/ApJ/704/1405 : Testing the Epeak-Eiso relation for GRBs (Krimm+, 2009) J/ApJ/711/495 : Durations of Swift/BAT GRBs (Butler+, 2010) J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- n_GRB [long IC] class of GRB (1) 6- 12 A7 --- GRB GRB identification (1) 14- 18 F5.3 --- z Redshift 20- 23 F4.2 --- beta X-ray spectral index β_a_ of the emission at afterglow time T*a (2) 25- 28 F4.2 --- e_beta rms uncertainty on beta 30- 37 E8.3 mW/m2 FX X-ray observed flux not corrected for absorption, FX=Fa*exp(-Tp/Ta) (2) 39- 46 E8.3 mW/m2 e_FX rms uncertainty on FX 48- 53 F6.3 [s] logT*90 Time interval during which the background-subtracted cumulative counts increase from 5% to 95% 55- 59 F5.3 [s] e_logT*90 rms uncertainty on logT*90 61- 66 F6.3 [s] logT*45 Time spanned by the brightest 45% of the total counts above the background 68- 72 F5.3 [s] e_logT*45 rms uncertainty on logT*45 74- 79 F6.3 [s] logT*p Fitted transition time in which the exponential decay in the prompt phase changes to a power-law decay (2) 81- 85 F5.3 [s] e_logT*p rms uncertainty on logT*p 87- 90 F4.2 [s] logT*a Break (afterglow) time (2) 92- 97 F6.2 [s] e_logT*a rms uncertainty on logT*a 99-103 F5.2 [10-7W] logL*a X-ray luminosity (2) 105-110 F6.2 [10-7W] e_logL*a rms uncertainty on logL*a 112-116 F5.2 [10-7J] logE*i Isotropic energy 118-121 F4.2 [10-7J] e_logE*i rms uncertainty on logE*i 123-126 F4.2 [keV] logE*p Peak energy in the νFν spectrum 128-131 F4.2 [keV] e_logE*p rms uncertainty on logE*p 133-139 F7.3 --- u Value of the error parameter u defined by u2 = e_logT*a2 + e_logL*a2 140 A1 --- n_u [U] U for the U0.095 subsample ("upper envelope" with fit u≤0.095)
Note (1): One RGB name was corrected at CDS (GRB 061115 does not exist, this name was correctde into GRB 060115). The classes are: long = long GRBs with u<4 IC = intermediate GRB class (between long and short GRBs) Note (2): See Eq.(1) of the paper: L*a=4πD2(z)FX(T*a)/(1+z)(1-β) where D(z) is the source luminosity distance.
History: * 31-Jul-2012: From electronic version of the paper * 22-Oct-2012: Corrected GRB 061115 into 060115
(End) Patricia Vannier [CDS] 31-Jul-2012
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