  Coronal Holes (CHs) have subdued intensity and net blueshifts when compared
to Quiet Sun (QS) at coronal temperatures. At transition region temperatures,
such differences are obtained for regions with identical photospheric absolute
magnetic flux density ($\vert$B$\vert$). In this work, we use spectroscopic
measurements of the \car 1334~{\AA} line from Interface Region Imaging
Spectrograph (IRIS), formed at chromospheric temperatures, to investigate the
intensity, Doppler shift, line width, skew, and excess kurtosis variations with
$\vert$B$\vert$. We find the intensity, Doppler shift, and line widths to
increase with $\vert$B$\vert$ for CHs and QS. The CHs show deficit in intensity
and excess total widths over QS for regions with identical $\vert$B$\vert$. For
pixels with only upflows, CHs show excess upflows over QS, while for pixels
with 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 more
skewed and flatter than a Gaussian, with no difference between CH and QS. These
results are important in understanding the heating of the atmosphere in CH and
QS, including solar wind formation, and provide further constraints on the
modeling of the solar atmosphere.
