Abstract
We investigate the characteristics of the thick disk in the Canada - France - Hawaii - Telescope Legacy Survey (CFHTLS) fields, complemented at bright magnitudes with Sloan Digital Sky Survey (SDSS) data. The ((Fe/H), Z) distributions are derived in the W1 and W3 fields, and compared with simulated maps produced using the Besancon model. It is shown that the thick disk, represented in star-count models by a distinct component, is not an adequate description of the observed ((Fe/H), Z) distributions in these fields.
Highlights
Our knowledge of the characteristics of the thick disk remains limited in practically every aspects
We investigate the characteristics of the thick disk in the Canada – France – Hawaii – Telescope Legacy Survey (CFHTLS) fields, complemented at bright magnitudes with Sloan Digital Sky Survey (SDSS) data
The observed distribution is compatible with similar distribution presented in [2], which shows a halo dominating the counts above 3 kpc at mean metallicity near −1.5 dex, and a thick disk component dominating the distribution below this limit
Summary
Our knowledge of the characteristics of the thick disk remains limited in practically every aspects. Its structure on large scales (>kpc) is not well defined, and its connections with the collapsed part of the halo or the old thin disk are essentially not understood. The SDSS photometric survey has provided a wealth of new informations on the thick disk, see in particular [1], [2] and [3]. The data have barely been directly confronted to star-count models, and little insights have been given on how the thick disk in these models really represent the survey data. We initiate such comparisons by comparing the Besançon model with metallicity and distance informations in the W1 and W3 CFHTLS fields, and provide a brief discussion of our results
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