Searching For Transiting Planets Around Halo Stars. I. Sample Selection and Validation

Searching For Transiting Planets Around Halo Stars. I. Sample Selection and Validation

Abstract By measuring the elemental abundances of a star, we can gain insight into the composition of its initial gas cloud—the formation site of the star and its planets. Planet formation requires metals, the availability of which is determined by the elemental abundance. In the case where metals a...

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Bibliographic Details
Published in:The Astronomical journal 2021-10, Vol.162 (4), p.125
Main Authors: Kolecki, Jared R., Wang, Ji, Johnson, Jennifer A., Zinn, Joel C., Ilyin, Ilya, Strassmeier, Klaus G.
Format: Article
Language:eng
Subjects:
Abundance
ASTRONOMY AND ASTROPHYSICS
Cloud formation
Exoplanets
Extrasolar planets
Halo stars
Kinematics
Metallicity
Metals
Planet formation
Planets
Spectroscopy
Stars
Stellar kinematics
Transit
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Summary:Abstract By measuring the elemental abundances of a star, we can gain insight into the composition of its initial gas cloud—the formation site of the star and its planets. Planet formation requires metals, the availability of which is determined by the elemental abundance. In the case where metals are extremely deficient, planet formation can be stifled. To investigate such a scenario requires a large sample of metal-poor stars and a search for planets therein. This paper focuses on the selection and validation of a halo star sample. We select ∼17,000 metal-poor halo stars based on their Galactic kinematics, and confirm their low metallicities ([Fe/H] < −0.5), using spectroscopy from the literature. Furthermore, we perform high-resolution spectroscopic observations using LBT/PEPSI and conduct detailed metallicity ([Fe/H]) analyses on a sample of 13 previously-known halo stars that also have hot kinematics. We can use the halo star sample presented here to measure the frequency of planets and to test planet formation in extremely metal-poor environments. The result of the planet search and its implications will be presented and discussed in a companion paper by Boley et al.
ISSN:0004-6256
1538-3881