We use the ~370deg^2^ 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{deg},+52{deg}] and |b|<5.1. We find that the molecular disk consists of two components with a layer thickness (FWHM) of ~85pc and ~280pc, respectively. In the inner Galaxy, the molecular mass in the thin disk is dominant, while the molecular mass traced by the discrete MCs with weak CO emission in the thick disk is probably ~100pc from the Galactic plane. However, only a few samples (i.e., 32 MCs or 3%) are located in the |z|>~360pc region. Typically, the discrete MCs of the thick-disk population have a median peak temperature of 2.1K, a median velocity dispersion of 0.8km/s, and a median effective radius of 2.5pc. Assuming a constant value of X_CO_=2x10^20^cm^-2^(K.km/s)^-1^, the median surface density of these MCs is 6.8M_{sun}/pc^2^, indicating very faint CO emission for the high-z gas. The cloud-cloud velocity dispersion is 4.9+/-1.3km/s and a linear variation with a slope of ~-0.4km/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 {rho}0(R)=1.28M_{sun}_/pc^3^e^-(R/3.2kpc)^ can be used to describe the distribution of the total mass density in the Galactic midplane.

Cone search capability for table J/ApJ/910/131/table1 (Parameters of 1055 molecular clouds far from the Galactic Plane based on the Milky Way Imaging Scroll Painting (MWISP) ^12^CO(J=1-0) emission)