Metal Pipe: A Broadly Applicable Stellar Abundance Pipeline Using Isochronal Parameters

Le résumé fourni par la source

Abstract Characterizing exoplanet host stars at the population level requires a method of homogeneously characterizing stellar properties across all spectral types. To this end, we have developed Metal Pipe, a new code for determining stellar parameters and abundances, which is designed for use across a wider range of spectral types than many commonly used codes. It combines the widely used package MOOG with photometric stellar parameters, a user-supplied high-resolution spectrum, and a newly curated list of spectral lines. Metal Pipe outputs values for T eff , log ( g ) , M * , R * , and L * from isochrones, and the abundances of C, O, Na, Mg, Al, Si, S, Ca, Ti, and Fe from MOOG . In this paper, we describe the Metal Pipe algorithm and tests of Metal Pipe against previous abundance measurements on archival HIRES spectra of 503 F-, G-, and K-type stars. We find rms scatter of ∼100 K in T eff , ∼0.10 dex in log ( g ) , and ∼0.10 dex for all measured abundances. These values are comparable to the estimated measurement uncertainties, verifying Metal Pipe for continued use in building a detailed abundance catalog. Future papers in this series will test Metal Pipe’s applicability to late-K and M dwarf stars, and provide other improvements.

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