低质量恒星有效温度的高分辨H波段光谱研究
Effective Temperatures of Low-Mass Stars from High-Resolution H-band Spectroscopy
摘要：
高分辨率的近红外光谱将成为寻找和表征低质量恒星周围类地行星的主要工具。然而，如果没有对宿主恒星的准确和精确的测量，就无法精确地确定系外行星的性质。浸没光栅红外光谱仪（IGRINS）获得的光谱同时提供了大多数恒星参数的诊断，但任何分析的第一步是确定有效温度。本文报道了利用Fe I、OH和Al I的吸收线深度对高分辨率H带光谱进行校准，以精确确定4000-3000 K（$\sim$ K8-M5）恒星的有效温度。这里使用的场星样本包含254颗K和M星，其温度是使用BT-Settl合成光谱得出的。我们使用文献中106颗具有精确温度的恒星来校准我们的方法，典型误差约为140 K，系统不确定度小于$\sim$ 120 K。为了最广泛的适用性，我们提出了T $_{\rm eff}$ -线深度比的关系，我们测试了12个成员的TW长蛇座协会和光谱分辨率之间的$\sim$ 10，000 - 120，000。这些比率提供了一个简单但准确的测量冷恒星的有效温度的方法，它与距离和红化无关。
英文摘要：
High-resolution, near-infrared spectra will be the primary tool for finding and characterizing Earth-like planets around low-mass stars. Yet, the properties of exoplanets can not be precisely determined without accurate and precise measurements of the host star. Spectra obtained with the Immersion GRating INfrared Spectrometer (IGRINS) simultaneously provide diagnostics for most stellar parameters, but the first step in any analysis is the determination of the effective temperature. Here we report the calibration of high-resolution H-band spectra to accurately determine effective temperature for stars between 4000-3000 K ($\sim$K8--M5) using absorption line depths of Fe I, OH, and Al I. The field star sample used here contains 254 K and M stars with temperatures derived using BT-Settl synthetic spectra. We use 106 stars with precise temperatures in the literature to calibrate our method with typical errors of about 140 K, and systematic uncertainties less than $\sim$120 K. For the broadest applicability, we present T$_{\rm eff}$--line-depth-ratio relationships, which we test on 12 members of the TW Hydrae Association and at spectral resolving powers between $\sim$10,000--120,000. These ratios offer a simple but accurate measure of effective temperature in cool stars that is distance and reddening independent.
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