[en] Spatially averaged ($><!--\; >\; -->{50}^{\mathrm{\prime <!--\; ???\; -->}\mathrm{\prime <!--\; ???\; -->}}$) EUV spectral lines in the transition region of solar quiet regions are known to be redshifted. Because the mechanism underlying this phenomenon is unclear, we require additional physical information on the lower corona in order to limit the theoretical models. To acquire this information, we measured the Doppler shifts over a wide coronal temperature range ($\mathrm{l}\mathrm{o}\mathrm{g}T[\mathrm{K}]=5.7$–6.3) using the spectroscopic data taken by the Hinode EUV Imaging Spectrometer. By analyzing the data over the center-to-limb variations covering the meridian from the south to the north pole, we successfully measured the velocity to an accuracy of 3 $\mathrm{k}\mathrm{m}{\mathrm{s}}^{-<!--\; ???\; -->1}$. Below $\mathrm{l}\mathrm{o}\mathrm{g}T[\mathrm{K}]=6.0,$ the Doppler shifts of the emission lines were almost zero with an error of 1–3 $\mathrm{k}\mathrm{m}{\mathrm{s}}^{-<!--\; ???\; -->1}$; above this temperature, they were blueshifted with a gradually increasing magnitude, reaching $-<!--\; ???\; -->6.3\pm <!--\; ??\; -->2.1\mathrm{k}\mathrm{m}{\mathrm{s}}^{-<!--\; ???\; -->1}$ at $\mathrm{l}\mathrm{o}\mathrm{g}T[\mathrm{K}]=\mathrm{6.25.}$