Structure and kinematical properties of the Galaxy at intermediate galactic latitudes

We have carried out a sample survey in UBVR photometry and proper motions in different directions in the Galaxy, as part of an investigation of galactic structure and evolution. Three fields in the direction of galactic anticentre, centre and antirotation have been surveyed. Using our new data together with wide-area surveys in other fields available to date, we discuss the radial and vertical structure of the Galaxy. The density laws for stars with M$_{V}\ge$3.5 follow a sum of two exponentials with scale heights of 260$\pm$50 pc (thin disk) and 760$\pm$50 pc, respectively. This second exponential corresponds to a thick disk with a local density of 7.4$^{+2.5}_{-1.5}$ \% relative to the thin disk. The scale lengths for these two populations are respectively 2.3$\pm$0.6 kpc and 3$\pm$1 kpc. The thick disk appears as a kinematically distinct population from the thin disk and shows no vertical gradient. Of the many models that have been proposed for the origin of the thick disk, the evidence at present seems to favour a model in which thick disk formed through the rapid dynamical heating of an early disk by satellite accretion into the disk.