Spatial distribution of stellar populations in the Magellanic Clouds: implementation to Gaia
M. K. Belcheva1, E. Livanou1, M. Kontizas1, G. B. Nikolov1,2 and E. Kontizas3
Department of Astrophysics Astronomy & MechanicsFaculty of
Physics, University of Athens,
2 Department of Astronomy, Sofia University St. Kliment Ohridski, 1164 Sofia, Bulgaria
3 IAA, National Observatory of Athens, PO Box 20048, 11810 Athens, Greece
Received: 29 September 2010
Accepted: 12 November 2010
Aims. The main goal of our project is to investigate the spatial distribution of different stellar populations in the Magellanic Clouds. The results from modelling the Magellanic Clouds can also be useful for simulations during the Gaia mission preparation.
Methods. Isodensity contour maps have been used in order to trace the morphology of the different stellar populations and estimate the size of these structures. Moreover, star density maps are constructed through star counts and projected radial density profiles obtained. Fitting exponential disk and King law curves to the spatial distribution allows us to derive the structural parameters that describe these profiles.
Results. The morphological structure and spatial distributions of various stellar components in the Magellanic Clouds (young and intermediate age stars, carbon stars), along with the overall spatial distribution in both Clouds, are provided.
Key words: Magellanic Clouds / Local Group / galaxies: structures / galaxies: stellar content
© ESO, 2011