  High spatial resolution CO observations of mid-inclination (30-75{\deg})
protoplanetary disks offer an opportunity to study the vertical distribution of
CO emission and temperature. The asymmetry of line emission relative to the
disk major axis allows for a direct mapping of the emission height above the
midplane, and for optically-thick, spatially-resolved emission in LTE, the
intensity is a measure of the local gas temperature. Our analysis of ALMA
archival data yields CO emission surfaces, dynamically-constrained stellar host
masses, and disk atmosphere gas temperatures for the disks around: HD 142666,
MY Lup, V4046 Sgr, HD 100546, GW Lup, WaOph 6, DoAr 25, Sz 91, CI Tau, and DM
Tau. These sources span a wide range in stellar masses (0.50-2.10 M$_{\odot}$),
ages (${\sim}$0.3-23 Myr), and CO gas radial emission extents
(${\approx}$200-1000 au). This sample nearly triples the number of disks with
mapped emission surfaces and confirms the wide diversity in line emitting
heights ($z/r\approx0.1$ to ${\gtrsim}0.5$) hinted at in previous studies. We
compute radial and vertical CO gas temperature distributions for each disk. A
few disks show local temperature dips or enhancements, some of which correspond
to dust substructures or the proposed locations of embedded planets. Several
emission surfaces also show vertical substructures, which all align with rings
and gaps in the millimeter dust. Combining our sample with literature sources,
we find that CO line emitting heights weakly decline with stellar mass and gas
temperature, which, despite large scatter, is consistent with simple scaling
relations. We also observe a correlation between CO emission height and disk
size, which is due to the flared structure of disks. Overall, CO emission
surfaces trace ${\approx}2$-$5\times$ gas pressure scale heights (H$_{\rm{g}}$)
and could potentially be calibrated as empirical tracers of H$_{\rm{g}}$.
