| Issue |
A&A
Volume 557, September 2013
|
|
|---|---|---|
| Article Number | A10 | |
| Number of page(s) | 19 | |
| Section | Galactic structure, stellar clusters and populations | |
| DOI | https://doi.org/10.1051/0004-6361/201321829 | |
| Published online | 13 August 2013 | |
Online material
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Fig. 7
Best fits of the differential grids by Pöhnl & Paunzen (2010) to data from the programme open clusters, in order to determine the fundamental parameters including metallicity. For clarity, TN are effective temperatures normalised to the ZAMS. An equal scale is used for a better comparison of different ages and metallicities. Owing to interpolation in the available grids, the most luminous stars are sometimes not covered by the isochrone; however, for older clusters we also included evolved stars to illustrate the continuation of the cluster sequences. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
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Fig. 7
continued. |
| Open with DEXTER | |
© ESO, 2013
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