The spiral structure of the Galaxy as seen from near infrared star counts

Details The spiral structure of the Galaxy as seen from near infrared star counts The spiral structure of the Galaxy as seen from near infrared star counts

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf..589a&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

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Scientific paper

Star counts models constitute an important useful tool to study galactic structure and evolution. In particular, the Besançon Model provides a description of the Galaxy in the evolutive point of view joining both the kinematics and dynamical properties. In the present work, we study the spiral structure of the Galaxy doing comparisons between the predicted and observed (2 MASS data in J, H and K bands) color-color and color-magnitude diagrams in the tangential directions of spiral arms. The main objectives are: study how the stellar population changes when a spiral arm is crossed, elaborate a spiral model in which reproduce adequately the star counts in the arms and interarms regions.
Our main procedure consists in adjust the parameters of spiral arms (initial radius, inclination angle, phase, amplitude) in order to reproduce the observed color-color and color-magnitude diagrams. The spiral model is also made consistent with others tracers of spiral galactic structure, such as the longitudinal profile in the K band obtained by DIRBE/COBE experiment. In order to do this we use a genetic algorithm, which is a robust optimization technique to fit several parameters. We present here the method used to adjust the parameters of the spiral arms, a comparison with other spiral models and also the analysis of color-color and color-magnitude diagrams of tangential directions of spiral arms.

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