Volume 451, Number 1, May III 2006
|Page(s)||125 - 139|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||25 April 2006|
Kinematics and stellar content of the Milky Way populations toward the North Galactic Pole
INAF, Padova Astronomical Observatory, vicolo Osservatorio 5, 35122, Padova,Italy e-mail: [pasetto;vallenari;bertelli]@pd.astro.it
2 Department of Astronomy, Padova University, vicolo dell'Osservatorio 2, 35122, Padova, Italy e-mail: email@example.com
3 INAF, Torino Astronomical Observatory, via Osservatorio 20, 10025 Pino Torinese, Italy e-mail: firstname.lastname@example.org
Accepted: 17 January 2006
Aims.The formation and evolution of galaxies is one of the forefront problems of Astrophysics. Detailed studies of our own Galaxy are the first step to understand these complex processes. In this paper we discuss the stellar populations and kinematics toward the North Galactic Pole (NGP) using data taken from the Guide Star Catalog II.
Methods.The Padova Galaxy model has been upgraded including the possibility of simulating in a consistent way color magnitude diagrams, luminosity functions and proper motions. Particular care is paid to simulate the kinematics of the thin disk, using a velocity dispersion tensor with off-diagonal term accounting for the vertical tilt.
Results.To reproduce the observational color distribution of the studied fields, one of the most critical parameters is the IMF slope. The canonical Kroupa IMF gives a poor fit of the data. The most convincing solutions are obtained assuming that about of the stars are in binaries and that the initial mass function changes slope at 0.8 instead than at the canonical value of 0.5 . We derive a Thin Disk IMF slope of in the mass range 0.2-0.8 . We derive the velocity ellipsoids of the Thin disk populations. The Thick disk and the Thin disk are well separated concerning their kinematic properties. The Thick disk is found to have a mean rotational velocity of implying a moderate rotational lag with respect to the solar motion. The data are not consistent with a significant vertical velocity gradient. This points in favor of a formation of the Thick disk by a quick heating of the precursor disk. Finally, no significant rotation velocity is found in the Halo.
© ESO, 2006
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