tokens: than 25 (i.e., approximately 5 σ for a χ 2 with 2 degrees of freedom). We use the same criterion to compare the Band+BB and Band+BB+PL models, or the Band+CPL and Band+CPL+PL models. The spectral parameters obtained from the best models along with the C-stat values are presented in Table 1 . Often the brighter GRBs require more complex models such as SBPL + BB, Band + BB, Band + CPL + PL; etc., for fitting their spectra. Figure 2 shows the νF ν energy spectrum using the best model of spectral fit for each GRB in Table 1 . The top left panel shows the spectra fitted with Band or Band + BB and the top right panel shows the spectra fitted with SBPL or SBPL + BB. The bottom left panel shows GRB 160625B spectrum fitted with Band + BB + PL and GRB 160509A spectrum fitted with Band + CPL + PL. The bottom right panel shows the spectra of GRB 130427A, GRB 090926A, GRB 090902B and GRB 090510, all fitted with Band + PL. The shaded regions correspond to the 1 σ confidence intervals of the models. Figure 2. νF ν spectra of Fermi -LAT/GBM GRBs with known redshift resulting from the time-integrated spectral analysis over the T 90 duration. The top left panel shows the Band or Band+BB model fits, while the top right panel shows SBPL or SBPL+BB model fits. The bottom panels show more complex models along with their components. The 1 σ confidence regions of the models are shown with shades of the same color as the model lines. 3.2. Isotropic Energy Calculation We computed the isotropic radiated energy E iso in the source rest frame at a luminosity distance d L aswhereis the bolometric fluence integrated over the minimum photon energy E min = 1 keV, and the maximum photon energy E max = 10 4 or 10 5 keV. Here, N i ( E ) represents the best-fit spectral model discussed previously. The luminosity distance strongly depends on the cosmological model. Assuming a flat ΛCDM cosmology with , the d L can be expressed as We have used Monte Carlo simulations to estimate the errors on S bolo and E iso . In particular, we assume the parameters of the spectral models follow a multivariate Gaussian function. Using the covariance matrix obtained from a spectral fit, we generate 10 4 sets of random values for the parameters to calculate S bolo in Equation ( 2 ). We select 68.27% confidence intervals from the resulting distribution of S bolo values to evaluate its error. The results of S bolo and E iso are reported in Table 2 . The values of (F10) and (F10) correspond to the energy interval 1–10 4 keV, while the values of (F100) and (F100) correspond to the energy interval 1–10 5 keV. The intrinsic peak energies of the νF ν spectra are reported as in Table 2 . In all cases, . Figure 3 shows the distributions of bolometric fluence, isotropic radiated energy and peak energy of the νF ν spectra of Fermi GRBs and those in the W2016 sample. There are small differences between the bolometric fluence (F10) and (F100) for the Fermi sample (the green and red histograms, respectively,
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