Shown is the correlation in the published data of Amati et al. (2002), Ghirlanda et al. (2004), Nava et al. (2006), Campana et al. (2007), and Ghisellini et al. (2007) between the peak energy ﹩E_{p}﹩ and the true energy ﹩E_{\gamma }﹩ in γ‐rays of long‐duration GRBs with known redshifts and inferred opening angles, assuming a stellar‐wind‐type environment to the gamma‐ray burst progenitor and using redshift‐corrected durations ﹩T_{90}﹩. A linear fit gives a slope and Pearson coefficient ﹩( s,\,c) =( 1.01,\,0.85) ﹩ to ﹩Y=\mathrm{log}\,( E_{p}T^{1/ 2}_{90}) ﹩ (circles) and ﹩( s,\,c) =( 0.71,\,0.76) ﹩ in the Ghirlanda correlation to ﹩Y=\mathrm{log}\,( E_{p}) ﹩ (triangles).