Fitting isochrones to open cluster photometric data - II. Nonparametric open cluster membership likelihood estimation and its application in optical and 2MASS near-IR data

W. S. Dias; H. Monteiro; T. C. Caetano; A. F. Oliveira

doi:10.1051/0004-6361/201118206

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Volume 539 (March 2012)

A&A, 539 (2012) A125

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Issue		A&A Volume 539, March 2012


Article Number		A125
Number of page(s)		21
Section		Galactic structure, stellar clusters and populations
DOI		https://doi.org/10.1051/0004-6361/201118206
Published online		06 March 2012

Online material

	Fig. 3 Graphs for the filtering of open cluster NGC 2477. Upper graphs give all UBV data and lower ones the filtered and weighted data and the fitted isochrone and ZAMS (solid lines). The symbol size is proportional to likelihood value.
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	Fig. 4 Graphs for the filtering of open cluster NGC 2477. Upper graphs give all 2MASS data and lower ones the filtered and weighted data and the fitted isochrone and ZAMS (solid lines). The symbol size is proportional to likelihood value.
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	Fig. 5 Same as Fig. 1 for NGC 7044.
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	Fig. 6 Same as Fig. 2 for NGC 7044.
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	Fig. 7 Same as Fig. 1 for NGC 2266.
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	Fig. 8 Same as Fig. 2 for NGC 2266.
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	Fig. 9 Same as Fig. 1 for Berkeley 32.
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	Fig. 10 Same as Fig. 2 for Berkeley 32.
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	Fig. 11 Same as Fig. 1 for NGC 2682 (Ref. 31).
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	Fig. 12 Same as Fig. 1 for NGC 2682 (Ref. 54).
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	Fig. 13 Same as Fig. 1 for NGC 2682 (Ref. 335).
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	Fig. 14 Same as Fig. 2 for NGC 2682.
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	Fig. 15 Same as Fig. 1 for NGC 2506 (Ref. 284).
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	Fig. 16 Same as Fig. 1 for NGC 2506 (Ref. 163).
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	Fig. 17 Same as Fig. 2 for NGC 2506.
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	Fig. 18 Same as Fig. 1 for NGC 2355 (Ref. 44).
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	Fig. 19 Same as Fig. 1 for NGC 2355 (Ref. 217).
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	Fig. 20 Same as Fig. 2 for NGC 2355.
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	Fig. 21 Same as Fig. 1 for Melotte 105 (Ref. 289).
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	Fig. 22 Same as Fig. 1 for Melotte 105 (Ref. 32).
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	Fig. 23 Same as Fig. 2 for Melotte 105.
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	Fig. 24 Same as Fig. 1 for Trumpler 1 (Ref. 86).
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	Fig. 25 Same as Fig. 1 for Trumpler 1 (Ref. 320).
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	Fig. 26 Same as Fig. 2 for Trumpler 1.
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	Fig. 27 Same as Fig. 1 for Dias 6 observed by our group.
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	Fig. 28 Same as Fig. 2 for Dias 6.
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	Fig. 29 Comparison of our fit with that of Bica et al. (2004) for Dias 6. See the text for details.
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	Fig. 30 Comparison of our fit with that of Tadross (2008) for Dias 6. See the text for details.
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© ESO, 2012

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