光学和近红外颜色作为恒星星族年龄和金属丰度的判别
Optical and near infra-red colours as a discriminant of the age and metallicity of stellar populations
摘要：
我们提出了一个全面的分析能力，目前的恒星星族模型再现的光学（ugriz）和近红外（JHK）颜色的一个小样本的研究附近的椭圆和S 0星系。我们发现广泛的年龄和金属丰度之间的协议，使用不同的人口模型，虽然不同的模型显示不同的系统偏差测量的宽带通量。虽然可以将简单的恒星星族模型限制在年龄-金属丰度空间中的一个明确定义的区域，但即使使用如此全范围的精确颜色，这些参数之间也存在明显的简并性。仅使用具有实际误差的宽波段光度法，年龄和金属丰度可以独立确定的精度为Delta{[Fe/H]} ~ 0.18和Delta{log（Age）} ~ 0.25。为了进一步限制星族和恒星形成的历史，有必要将宽带光学红外测光与谱线指数结合起来，或者在这个范围之外的波长处进行测光。
英文摘要：
We present a comprehensive analysis of the ability of current stellar population models to reproduce the optical (ugriz) and near infra-red (JHK) colours of a small sample of well-studied nearby elliptical and S0 galaxies. We find broad agreement between the ages and metallicities derived using different population models, although different models show different systematic deviations from the measured broad-band fluxes. Although it is possible to constrain Simple Stellar Population models to a well defined area in age-metallicity space, there is a clear degeneracy between these parameters even with such a full range of precise colours. The precision to which age and metallicity can be determined independently, using only broad band photometry with realistic errors, is Delta{[Fe/H]} ~ 0.18 and Delta{log(Age)} ~ 0.25. To constrain the populations and therefore the star formation history further it will be necessary to combine broad-band optical-IR photometry with either spectral line indices, or else photometry at wavelengths outside of this range.
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