论文标题
通过模型的光谱调查方法来表征超球星大气的表征
Characterization of exoplanetary atmospheres through a model-unbiased spectral survey methodology
论文作者
论文摘要
语境。收集各种超球星大气测量对于提高我们对系外行星的理解至关重要。在这种情况下，该领域很可能会受益于广泛的物种调查，尤其是使用过境光谱，这是迄今为止迄今为止超级行星大气表征的最成功的技术。 目的：我们的目标是使用传输光谱法开发一种模型的稳态技术，以分析系外行驶传输数据中的每条合格的原子光谱线，并搜索相对吸收，即行星传输时线磁通量的减少。 方法：我们分析了来自Subaru的HDS的档案数据，凯克的雇用，VLT的Uves和Lasilla的竖琴来测试我们的光谱调查方法。它首先通过相对噪声水平过滤单个线路。它还纠正了光谱偏移和矫正污染。我们的方法沿时间和波长进行了分析。后者采用了自举佐证。 结果：我们强调了HD 209459B在Subaru获取的MN I和V II的可能检测（5916.4 $ \ angstrom $，$5.9σ$，$5.1σ$，in 6021.8 $ \ angstrom $）。在同一星球中对CA I的先前检测被我们的算法归类为尚无定论，但我们支持先前对SC II的检测（$3.5σ$ in 6604.6 $ \ angstrom $）。我们还强调了在HD 189733中可能检测到Ca I，SC II和Ti II的可能检测，Uves在VLT上获取的数据（$4.4σ$ $ 6572.8 \ Angstrom $，$6.8σ$，$ 6604.6 \ Angstrom $ $ 6604.6 \ Angstrom $，以及$ 5910.1 \ and and auft and and auft and auft auff aftection frouction frouction frouction。在VLT（$5.6σ$ at $ 6696.0 \ Angstrom $）。
Context. Collecting a large variety of exoplanetary atmosphere measurements is crucial to improve our understanding of exoplanets. In this context, it is likely that the field would benefit from broad species surveys, particularly using transit spectroscopy, which is the most successful technique of exoplanetary atmosphere characterization so far. Aims: Our goal is to develop a model-unbiased technique using transit spectroscopy to analyze every qualified atomic spectral line in exoplanetary transit data, and search for relative absorption, that is, a decrease in the flux of the line when the planet is transiting. Methods: We analyzed archive data from HDS at Subaru, HIRES at Keck, UVES at VLT, and HARPS at LaSilla to test our spectral survey methodology. It first filtered individual lines by relative noise levels. It also corrected for spectral offsets and telluric contamination. Our methodology performed an analysis along time and wavelength. The latter employed a bootstrap corroboration. Results: We highlight the possible detections of Mn I and V II in HD 209459b data taken by HDS at Subaru ($5.9σ$ at 5916.4 $\angstrom$, $5.1σ$ at 6021.8 $\angstrom$). The previous detection of Ca I in the same planet is classified as inconclusive by our algorithm, but we support the previous detection of Sc II ($3.5σ$ at 6604.6 $\angstrom$). We also highlight the possible detection of Ca I, Sc II, and Ti II in HD 189733 data taken by UVES at VLT ($4.4σ$ at $6572.8 \angstrom$, $6.8σ$ at $6604.6 \angstrom$, and $3.5σ$ at $5910.1 \angstrom$), in addition to the possible detection of Al I in WASP-74b data taken by UVES at VLT ($5.6 σ$ at $6696.0 \angstrom$).
