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Coronal Holes (CHs) have subdued intensity and net blueshifts when comparedto Quiet Sun (QS) at coronal temperatures. At transition region temperatures,such differences are obtained for regions with identical photospheric absolutemagnetic flux density ($\vert$B$\vert$). In this work, we use spectroscopicmeasurements of the \car 1334~{\AA} line from Interface Region ImagingSpectrograph (IRIS), formed at chromospheric temperatures, to investigate theintensity, Doppler shift, line width, skew, and excess kurtosis variations with$\vert$B$\vert$. We find the intensity, Doppler shift, and line widths toincrease with $\vert$B$\vert$ for CHs and QS. The CHs show deficit in intensityand excess total widths over QS for regions with identical $\vert$B$\vert$. Forpixels with only upflows, CHs show excess upflows over QS, while for pixelswith only downflows, CHs show excess downflows over QS that cease to exist at$\vert$B$\vert$ $\le$ 40. Finally, the spectral profiles are found to be moreskewed and flatter than a Gaussian, with no difference between CH and QS. Theseresults are important in understanding the heating of the atmosphere in CH andQS, including solar wind formation, and provide further constraints on themodeling of the solar atmosphere.

Properties of the C II 1334 {\AA} line in Coronal Hole and Quiet Sun as observed by IRIS