Automated Stellar Spectral Classification and Parameterization for the Masses

TL;DR

The paper discusses the development of automated methods for classifying and parameterizing stellar spectra, emphasizing their effectiveness across various parameters and the creation of a web-based tool for broader accessibility.

Contribution

It introduces a comprehensive automated system for stellar spectral classification and parameterization, including a web interface for wider use beyond existing surveys.

Findings

Automated classification is effective in spectral type and temperature domains.

Parameterization of metallicity and luminosity has been successfully automated.

A web-based tool for stellar classification and parameterization is proposed.

Abstract

Stellar spectroscopic classification has been successfully automated by a number of groups. Automated classification and parameterization work best when applied to a homogeneous data set, and thus these techniques primarily have been developed for and applied to large surveys. While most ongoing large spectroscopic surveys target extragalactic objects, many stellar spectra have been and will be obtained. We briefly summarize past work on automated classification and parameterization, with emphasis on the work done in our group. Accurate automated classification in the spectral type domain and parameterization in the temperature domain have been relatively easy. Automated parameterization in the metallicity domain, formally outside the MK system, has also been effective. Due to the subtle effects on the spectrum, automated classification in the luminosity domain has been somewhat more difficult, but still successful. In order to extend the use of automated techniques beyond a few surveys, we present our current efforts at building a web-based automated stellar spectroscopic classification and parameterization machine. Our proposed machinery would provide users with MK classifications as well as the astrophysical parameters of effective temperature, surface gravity, mean abundance, abundance anomalies, and microturbulence.