Kinematics and chemical properties of the Galactic stellar populations.
  The HARPS FGK dwarfs sample
  (Abridged) We analyze chemical and kinematical properties of about 850 FGK
solar neighborhood long-lived dwarfs observed with the HARPS high-resolution
spectrograph. The stars in the sample have logg > 4 dex, 5000 < Teff < 6500 K,
and -1.39 < [Fe/H] < 0.55 dex. We apply a purely chemical analysis approach
based on the [alpha/Fe] vs. [Fe/H] plot to separate Galactic stellar
populations into the thin disk, thick disk and high-alpha metal-rich (hamr).
Our analysis shows a negative gradient of the rotational velocity of the thin
disk stars with [Fe/H] (-17 km s^-1 dex^-1), and a steep positive gradient for
both the thick disk and hamr stars with the same magnitude of about +42 km s^-1
dex^-1. For the thin disk stars we observed no correlation between orbital
eccentricities and metallicity, but observed a steep negative gradient for the
thick disk and hamr stars with practically the same magnitude (about -0.18
dex^-1). Our results suggest that radial migration played an important role in
the formation and evolution of the thin disk. For the thick disk stars it is
not possible to reach a firm conclusion about their origin. Based on the
eccentricity distribution of the thick disk stars only their accretion origin
can be ruled out, and the heating and migration scenario could explain the
positive steep gradient of V_phi with [Fe/H]. Analyzing the hamr stellar
population we found that they share properties of both the thin and thick disk
population. A comparison of the properties of the hamr stars with that of the
subsample of stars from the N-body/SPH simulation using radial migration
suggest that they may have originated from the inner Galaxy. Further detailed
investigations would help to clarify their exact nature and origin.
