AN EMPIRICAL UBV RI JHK COLOR–TEMPERATURE CALIBRATION FOR STARS
AN EMPIRICAL UBV RI JHK COLOR–TEMPERATURE CALIBRATION FOR STARS
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DOI：
10.1088/0067-0049/193/1/1
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发表时间：
2006-04
期刊：
影响因子：
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通讯作者：
G. Worthey;Hyun-Chul Lee
中科院分区：
文献类型：
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作者：
G. Worthey;Hyun-Chul Lee
收集的约翰逊/雷金斯测光已知[Fe/H]的恒星被用来产生颜色的颜色关系，包括丰度的依赖。文献温度和热辐射校正（BC）的依赖性连接到颜色关系。JHK颜色被转换到Bessell & Brett均质化系统。这项工作的主要结果是七种颜色和V波段BC作为Teff，log g和[Fe/H]的函数（−1.06 <V-K < 10.2）的表格以及附带的插值程序。对目前校准的改进将涉及填补测光差距，获得更准确和系统上的测光，了解更好的log g和[Fe/H]值，改善数据贫乏的恒星群（如贫金属K矮星）的统计，在处理管道中应用小的调整，并获得更好的经验温度和BC关系，特别是对于超巨星和M星。指出了一种从M矮星的颜色估计尘埃消光的方法。
A collection of Johnson/Cousins photometry for stars with known [Fe/H] is used to generate color–color relations that include the abundance dependence. Literature temperature and bolometric correction (BC) dependences are attached to the color relations. The JHK colors are transformed to the Bessell & Brett homogenized system. The main result of this work is the tabulation of seven colors and the V-band BC as a function of Teff, log g, and [Fe/H] for −1.06 < V − K < 10.2 and an accompanying interpolation program. Improvements to the present calibration would involve filling photometry gaps, obtaining more accurate and on-system photometry, knowing better log g and [Fe/H] values, improving the statistics for data-impoverished groups of stars such as metal-poor K dwarfs, applying small tweaks in the processing pipeline, and obtaining better empirical temperature and BC relations, especially for supergiants and M stars. A way to estimate dust extinction from M dwarf colors is pointed out.