晚型星K波段光谱合成的Vsini-s
Vsini-s for late-type stars from spectral synthesis in K-band region
摘要：
我们分析了中等分辨率的光谱（R \sim 18000）的19晚型矮星，以确定vsini-s使用合成，而不是观测的模板光谱。为此目的，观测数据约2.2 $μ$米的恒星光谱类从G8 V到M9.5 V的模拟。我们发现，钠I（2.2062和2.2090 $μ$ m）和$^{12}$ CO 2-0带功能建模足够好，用于vsini测定，而不需要一个合适的观测模板光谱。在我们的光谱的分辨率的限制内，我们使用合成光谱模板来导出与使用观察到的模板在光学制度中导出的那些一致的VSINI值。我们量化的错误，在我们的vsini确定由于模型参数\Teff，日志$g$，$v_{\rm micro}$，[Fe/H]或FWHM的选择不正确，并表明它们通常小于10%。我们注意到，我们的数据的光谱分辨率（\sim 16公里/秒）限制了这项研究相对较快的转子和分辨率为60000将需要访问最晚型矮星。
英文摘要：
We analyse medium-resolution spectra (R\sim 18000) of 19 late type dwarfs in order to determine vsini-s using synthetic rather than observational template spectra. For this purpose observational data around 2.2 $μ$m of stars with spectral classes from G8V to M9.5V were modelled. We find that the Na I (2.2062 and 2.2090 $μ$m) and $^{12}$CO 2-0 band features are modelled well enough to use for vsini determination without the need for a suitable observational template spectra. Within the limit of the resolution of our spectra, we use synthetic spectra templates to derive vsini values consistent with those derived in the optical regime using observed templates. We quantify the errors in our vsini determination due to incorrect choice of model parameters \Teff, log $g$, $v_{\rm micro}$, [Fe/H] or FWHM and show that they are typically less than 10 per cent. We note that the spectral resolution of our data(\sim 16 km/s) limited this study to relatively fast rotators and that resolutions of 60000 will required to access most late-type dwarfs.
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