论文标题
使用光学中分辨率光谱来探索小型系外行星的M矮人的表征
Characterization of M dwarfs Using Optical Mid-Resolution Spectra for Exploration of Small Exoplanets
论文作者
论文摘要
我们介绍了附近338个M矮人的光谱，并计算其光谱类型，有效的温度（$ t _ {\ Mathrm {eff}}} $）和Radii。我们的光谱是使用具有光谱分辨率的几个光谱仪获得的，范围从1200到10000。多达97％的观察到的M型矮人中有97％的M3-M6具有光谱类型的M3-M6，典型的误差为0.4个亚型，其中最常见的是光谱M4-M5。我们通过将光谱与Phoenix模型中的理论光谱拟合，从而推断出样品的$ t _ {\ mathrm {eff}} $。我们推断的$ t _ {\ mathrm {eff}} $用m矮人的光谱进行了校准，其$ t _ {\ mathrm {eff}} $通过以前的间歇度观测值支持的校准得到很好的确定。我们的拟合程序利用VO吸收带（7320-7570Å）和光学区域（5000-8000Å），得出的典型误差为128 K（VO频段）和85 K（光学区域）。我们还根据样品的光谱能量分布（SED）确定了我们的样品的半径。我们发现大多数样本星的半径为$ <$ 0.6 $ r_ \ odot $，平均错误为3％。我们的目录可以有效地选择附近M型矮人附近的系外行星调查。
We present the optical spectra of 338 nearby M dwarfs, and compute their spectral types, effective temperatures ($T_{\mathrm{eff}}$), and radii. Our spectra have been obtained using several optical spectrometers with spectral resolutions that range from 1200 to 10000. As many as 97% of the observed M-type dwarfs have a spectral type of M3-M6, with a typical error of 0.4 sub-type, among which the spectral types M4-M5 are the most common. We infer the $T_{\mathrm{eff}}$ of our sample by fitting our spectra with theoretical spectra from the PHOENIX model. Our inferred $T_{\mathrm{eff}}$ is calibrated with the optical spectra of M dwarfs whose $T_{\mathrm{eff}}$ have been well determined with the calibrations that are supported by previous interferometric observations. Our fitting procedures utilize the VO absorption band (7320-7570 Å) and the optical region (5000-8000 Å), yielding typical errors of 128 K (VO band) and 85 K (optical region). We also determine the radii of our sample from their spectral energy distributions (SEDs). We find most of our sample stars have radii of $<$ 0.6 $R_\odot$, with the average error being 3%. Our catalog enables efficient sample selection for exoplanet surveys around nearby M-type dwarfs.
