Molecular gas distribution perpendicular to the Galactic plane.

We use the ~370 square degrees data from the MWISP CO survey to study the vertical distribution of the molecular clouds (MCs) toward the tangent points in the region of l=[16,52]deg and |b| 100pc from the Galactic plane. However, only a few samples (i.e., 32 MCs) are located in the |z|>360pc region. Typically, the discrete MCs of the thick disk population have a median peak temperature of 2.1 K, a median velocity dispersion of 0.8km/s, and a median effective radius of 2.5pc. The median surface density of these MCs is 6.8 Msun/pc^2, indicating very faint CO emission for these high-z MCs. The cloud-cloud velocity dispersion is 4.9+-1.3 km/s and a linear variation with a slope of -0.4 km/s/kpc is obtained in the region of R_GC=2.2-6.4kpc. Assuming that these clouds are supported by their turbulent motions against the gravitational pull of the disk, a model of rho0(R) = 1.28exp(-R/3.2kpc) Msun/pc^3 can be used to describe the distribution of the total mass density in the Galactic midplane.