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Towards a photometric metallicity scale for open clusters
Solar and Stellar Astrophysics · Submitted 8 Jul 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The method provides an accurate way of obtaining properly scaled metallicity values for open clusters.
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The abstract, sentence by sentence
Open clusters are a useful tool when investigating several topics connected with stellar evolution; for example the age or distance can be more accurately determined than for field stars. However, one important parameter, the metallicity, is only known for a marginal percentage of open clusters. We aim at a consistent set of parameters for the open clusters investigated in our photometric Delta-a survey of chemically peculiar stars. Special attention is paid to expanding our knowledge of cluster metallicities and verifying their scale. Making use of a previously developed method based on normalised evolutionary grids and photometric data, the distance, age, reddening, and metallicity of open clusters were derived. To transform photometric measurements into effective temperatures to use as input for our method, a set of temperature calibrations for the most commonly used colour indices and photometric systems was compiled. We analysed 58 open clusters in total. Our derived metallicity values were in excellent agreement with about 30 spectroscopically studied targets. The mean value of the absolute deviations was found to be 0.03 dex, with no noticeable offset or gradient. The method was also applied using recent evolutionary models based on the currently accepted lower solar abundance value Z=0.014. No significant differences were found compared to grids using the former adopted solar value Z=0.02. Furthermore, some divergent photometric datasets were identified and discussed. The method provides an accurate way of obtaining properly scaled metallicity values for open clusters. In light of present and future homogeneous photometric sky surveys, the sample of stellar clusters can be extended to the outskirts of the Milky Way, where spectroscopic studies are almost impossible. This will help for determining galactic metallicity gradients in more detail.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Open clusters are a useful tool when investigating several topics connected with stellar evolution; for example the age or distance can be more accurately determined than for field stars. | background 1.00 | 0.05 | 0.02 | asserted 0.87 |
| s1 | However, one important parameter, the metallicity, is only known for a marginal percentage of open clusters. | gap 0.99 | 0.05 | 0.02 | asserted 1.00 |
| s2 | We aim at a consistent set of parameters for the open clusters investigated in our photometric Delta-a survey of chemically peculiar stars. | contribution 0.95 | 0.46 | 0.03 | asserted 0.83 |
| s3 | Special attention is paid to expanding our knowledge of cluster metallicities and verifying their scale. | contribution 0.81 | 0.39 | 0.04 | asserted 0.65 |
| s4 | Making use of a previously developed method based on normalised evolutionary grids and photometric data, the distance, age, reddening, and metallicity of open clusters were derived. | method 0.99 | 0.93 | 0.07 | asserted 1.00 |
| s5 | To transform photometric measurements into effective temperatures to use as input for our method, a set of temperature calibrations for the most commonly used colour indices and photometric systems was compiled. | method 1.00 | 0.88 | 0.02 | asserted 1.00 |
| s6 | We analysed 58 open clusters in total. | contribution 0.81 | 0.94 | 0.02 | asserted 1.00 |
| s7 | Our derived metallicity values were in excellent agreement with about 30 spectroscopically studied targets. | result 1.00 | 0.94 | 0.21 | asserted 0.99 |
| s8 | The mean value of the absolute deviations was found to be 0.03 dex, with no noticeable offset or gradient. | result 1.00 | 0.97 | 0.16 | asserted 1.00 |
| s9 | The method was also applied using recent evolutionary models based on the currently accepted lower solar abundance value Z=0.014. | method 0.84 | 0.88 | 0.03 | asserted 0.97 |
| s10 | No significant differences were found compared to grids using the former adopted solar value Z=0.02. | result 0.97 | 0.91 | 0.06 | asserted 1.00 |
| s11 | Furthermore, some divergent photometric datasets were identified and discussed. | result 0.72 | 0.88 | 0.03 | asserted 0.99 |
| s12 | The method provides an accurate way of obtaining properly scaled metallicity values for open clusters. | interpretation 0.57 | 0.75 | 0.82 | asserted 1.00 |
| s13 | In light of present and future homogeneous photometric sky surveys, the sample of stellar clusters can be extended to the outskirts of the Milky Way, where spectroscopic studies are almost impossible. | future work 0.94 | 0.09 | 0.06 | hedged possibility 0.81 |
| s14 | This will help for determining galactic metallicity gradients in more detail. | future work 0.77 | 0.08 | 0.07 | hedged possibility 0.67 |
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Original abstract
Open clusters are a useful tool when investigating several topics connected with stellar evolution; for example the age or distance can be more accurately determined than for field stars. However, one important parameter, the metallicity, is only known for a marginal percentage of open clusters. We aim at a consistent set of parameters for the open clusters investigated in our photometric Delta-a survey of chemically peculiar stars. Special attention is paid to expanding our knowledge of cluster metallicities and verifying their scale. Making use of a previously developed method based on normalised evolutionary grids and photometric data, the distance, age, reddening, and metallicity of open clusters were derived. To transform photometric measurements into effective temperatures to use as input for our method, a set of temperature calibrations for the most commonly used colour indices and photometric systems was compiled. We analysed 58 open clusters in total. Our derived metallicity values were in excellent agreement with about 30 spectroscopically studied targets. The mean value of the absolute deviations was found to be 0.03 dex, with no noticeable offset or gradient. The method was also applied using recent evolutionary models based on the currently accepted lower solar abundance value Z=0.014. No significant differences were found compared to grids using the former adopted solar value Z=0.02. Furthermore, some divergent photometric datasets were identified and discussed. The method provides an accurate way of obtaining properly scaled metallicity values for open clusters. In light of present and future homogeneous photometric sky surveys, the sample of stellar clusters can be extended to the outskirts of the Milky Way, where spectroscopic studies are almost impossible. This will help for determining galactic metallicity gradients in more detail.
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