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Studying Milky Way structure using stellar populations

Published online by Cambridge University Press:  01 December 2006

J. T. A. de Jong ,
D. J. Butler ,
H-W. Rix ,
A. E. Dolphin  and
D. Martínez-Delgado
J. T. A. de Jong
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
D. J. Butler
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
H-W. Rix
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
A. E. Dolphin
Affiliation:
Steward Observatory, Univ. of Arizona, 933 N. Cherry Ave, Tucson, AZ, 85721, United States
D. Martínez-Delgado
Affiliation:
Instituto de Astrofísica de Canarias, C/Vía Láctea, E38200, La Laguna, Spain
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Abstract

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With the advent of large wide-field cameras and deep, CCD-based “all-sky” surveys, the study of the structure of the Milky Way (MW) through its stellar populations has become feasible. We are developing tools to apply CMD fitting techniques for this purpose. Here we present two applications. First we constrain the properties of the old and young stellar populations of the Canis Major overdensity. Secondly, we demonstrate how CMD fitting can be used to detect faint overdensities in the halo of the MW and determine their properties, using data from the Sloan Digital Sky Survey (SDSS).

Keywords

Galaxy: haloGalaxy: stellar contentGalaxy: structuregalaxies: dwarfgalaxies: individual (Canis Major)galaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 213 - 217
Copyright
Copyright © International Astronomical Union 2007

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