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Title:
Numerical Color-Magnitude Diagram Analysis of Sloan Digital Sky Survey Data and Application to the New Milky way Satellites
Authors:
de Jong, J. T. A.; Rix, H.-W.; Martin, N. F.; Zucker, D. B.; Dolphin, A. E.; Bell, E. F.; Belokurov, V.; Evans, N. W.
Affiliation:
AA(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AB(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AC(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AD(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ), AE(Steward Observatory, University of Arizona, 933 N. Cherry Ave, Tucson, AZ, 85721, USA), AF(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AG(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ), AH(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK )
Publication:
The Astronomical Journal, Volume 135, Issue 4, pp. 1361-1383 (2008). (AJ Homepage)
Publication Date:
04/2008
Origin:
IOP
AJ Keywords:
galaxies: dwarf, galaxies: stellar content, methods: numerical, methods: statistical, surveys
DOI:
10.1088/0004-6256/135/4/1361
Bibliographic Code:
2008AJ....135.1361D

Abstract

We have tested the application to Sloan Digital Sky Survey (SDSS) data of the software package MATCH, which fits color-magnitude diagrams (CMDs) to estimate stellar population parameters and distances. These tests on a set of six globular clusters show that these techniques recover their known properties. New ways of using the CMD-fitting software enable us to deal with an extended distribution of stars along the line-of-sight, to constrain the overall properties of sparsely populated objects, and to detect the presence of stellar overdensities in wide-area surveys. We then also apply MATCH to CMDs for 12 recently discovered Milky Way satellites to derive in a uniform fashion their distances, ages, and metallicities. While the majority of them appear consistent with a single stellar population, CVn I, UMa II, and Leo T exhibit (from SDSS data alone) a more complex history with multiple epochs of star formation.
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