FeH、CrH 和 NiH 实验室谱线表与 ESPaDOnS 和 SPIRou 采集的 M 型星光谱之间的相关性
Correlations between laboratory line lists for FeH, CrH, and NiH and M-star spectra collected with ESPaDOnS and SPIRou
AI总结：
本文报告了从近红外和可见光实验室数据中筛选的 FeH、CrH 和 NiH 等金属单氢化物谱线表，通过交叉相关分析证明其特定跃迁可用于识别 M 型星光谱并测定视向速度，同时揭示了磁场对 CrH 和 FeH 特征的影响。
摘要：
金属氧化物和氢化物的分子谱带主导着 M 型矮星的可见光和近红外光谱。这些谱带的高分辨率光谱在测定恒星多项性质方面具有巨大潜力，例如有效温度、表面重力、元素丰度、视向速度或表面磁场。相关技术正在开发中，但仍受限于当前分子数据和谱线表的可用性与准确性。本文报告了从近红外和可见光实验室数据中筛选出的金属单氢化物谱线表，以展示几个电子跃迁中的特定谱带可用于在 M 型星中识别 CrH、NiH 和 FeH，并利用多普勒频移测定视向速度。此外，还研究了 FeH 和 CrH 测量磁场的可能性。我们采用系统交叉相关分析，对选定 M 型星的非偏振光谱与特定能态的实验室谱线表进行了比对。这些谱线表由现有数据与在多普勒受限分辨率下记录的新实验室激光激发光谱相结合生成，条件为零磁场或高达 0.6 特斯拉的磁场。结果：我们表明，FeH 和 NiH 在可见光波长的跃迁（通常在 M 型星光谱分析中被忽略）实际上对光谱有贡献，并展示了磁敏感性对 CrH 和 FeH 选定跃迁的影响。尽管新谱线表侧重于在显著低于恒星物体温度下记录的跃迁，但它们依然具有相关性，因为覆盖了高光谱密度的某些带头区域。FeH 谱带可作为原子谱线的有效补充，用于分析 M 型矮星的高分辨率可见光和近红外光谱。我们展示了磁场对 862 nm 附近 CrH 特征的影响。
英文摘要：
Molecular bands of metal oxides and hydrides dominate the optical and near-infrared spectra of M dwarfs. High-resolution spectra of these bands have immense potential for determining many properties of these stars, such as effective temperature, surface gravity, elemental abundances, radial velocity, or surface magnetic fields. Techniques are being developed to do this but remain limited by the current availability and accuracy of molecular data and spectral line lists. This paper reports metal monohydride line lists selected from near-infrared and visible laboratory data to show that specific bands in several electronic transitions can be used to identify CrH, NiH, and FeH in M stars and to determine radial velocities from Doppler shifts. The possibility of measuring magnetic fields is also investigated for FeH and CrH. We used systematic cross-correlation analysis between unpolarised spectra from a selection of M stars and state-specific laboratory line lists. These lists were generated from a combination of existing data and new laboratory laser-excitation spectra recorded at Doppler-limited resolution, in zero-field conditions or in magnetic fields up to 0.6 tesla. Results. We show that transitions at visible wavelengths in FeH and NiH, usually neglected in the analysis of the spectra of M-type stars, do in fact contribute to the spectra, and we demonstrate the influence of magnetic sensitivity on selected transitions in CrH and FeH. Although the new line lists focus on transitions recorded at temperatures significantly lower than those of stellar objects, they remain pertinent because they cover some band-head regions of high spectral density. FeH bands can provide a useful supplement to atomic lines for the analysis of high-resolution optical and near-infrared spectra of M dwarfs. We demonstrate the influence of a magnetic field on CrH signatures around 862 nm.
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