多路精密RV：在疏散星团中寻找气体巨星的关闭
Multiplexing Precision RVs: Searching for Close in Gas Giants in Open Clusters
摘要：
我们提出了一个多路复用，高分辨率（R~50,000中位数）光谱调查，旨在检测两个南部星团（NGC 2516和NGC 2422）的系外行星候选人使用密歇根/麦哲伦光纤系统（M2 FS）的麦哲伦/粘土望远镜在Las Campanas天文台。在我们的观测模式中有128个可用的光纤，我们能够瞄准每个星团核心半度内的每一颗恒星，这些恒星可能是太阳模拟成员。我们基于模板的光谱拟合提供了基本恒星属性的精确测量- $T_{eff}$（$\pm$ 30 K）、[Fe/H]和[ $α$ /Fe]（$\pm$ 0.02 dex），和$v_r\sin(i)$（$\pm$ 0.3 km/s）和径向速度（RV），使用7160至7290 $Å$的大地吸收特征作为251中F至中F的波长参考。K星（NGC 2516中有126颗，NGC 2422中有125颗）组成了我们的调查。在每个集群中，我们已经获得了我们目标的~10-12个时期。使用RV标准星的重复观测，我们表明我们的方法可以在我们1.1年的观测基线上在宽的S/N范围内获得25 m/s至60 m/s的单历元速度精度。我们的技术适用于非快速旋转的恒星，温度低于中F。在本文中，我们描述了我们的观测样本，分析方法，并提出了一个详细的研究，我们的方法可达到的精度和测量能力。随后的论文将提供在目标星团中观察到的恒星的结果，分析我们的RV时间序列数据集的恒星抖动和恒星和亚恒星同伴，并考虑我们的发现对星团本身的影响。
英文摘要：
We present a multiplexed, high-resolution (R~50,000 median) spectroscopic survey designed to detect exoplanet candidates in two southern star clusters (NGC 2516 and NGC 2422) using the Michigan/Magellan Fiber System (M2FS) on the Magellan/Clay telescope at Las Campanas Observatory. With 128 available fibers in our observing mode, we are able to target every star in the core half-degree of each cluster that could plausibly be a solar-analog member. Our template-based spectral fits provide precise measurements of fundamental stellar properties - $T_{eff}$ ($\pm$30 K), [Fe/H] and [$α$/Fe] ($\pm$0.02 dex), and $v_r\sin(i)$ ($\pm$0.3 km/s) - and radial velocities (RVs) by using telluric absorption features from 7160 to 7290 $Å$ as a wavelength reference for 251 mid-F to mid-K stars (126 in NGC 2516 and 125 in NGC 2422) that comprise our survey. In each cluster we have obtained ~10-12 epochs of our targets. Using repeat observations of an RV standard star we show our approach can attain a single-epoch velocity precision of 25 m/s to 60 m/s over a broad range of S/N throughout our observational baseline of 1.1 years. Our technique is suitable for non-rapidly rotating stars cooler than mid-F. In this paper we describe our observational sample, analysis methodology, and present a detailed study of the attainable precision and measurement capabilities of our approach. Subsequent papers will provide results for stars observed in the target clusters, analyze our dataset of RV time-series for stellar jitter and stellar and sub-stellar companions, and consider the implications of our findings on the clusters themselves.
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