# StePar: an automatic code to infer stellar atmospheric parameters

## TL;DR

StePar is an automated Python tool that accurately derives stellar atmospheric parameters for FGK stars using the EW method, validated against Gaia benchmark stars and publicly available for community use.

## Contribution

The paper introduces StePar, a new automated code for stellar parameter determination, and validates its performance with benchmark stars, highlighting its limitations and providing the code for public access.

## Key findings

- Small internal scatter in parameters: 9 K in Teff, 0.07 dex in log(g), 0.03 dex in [Fe/H]
- Validated against Gaia benchmark stars with consistent results
- Advised against use on certain spectra and stellar types due to limitations

## Abstract

Context: StePar is an automatic code written in Python 3.X designed to compute the stellar atmospheric parameters Teff, log(g), [Fe/H], and of FGK-type stars by means of the EW method. This code has already been extensively tested in different spectroscopic studies of FGK-type stars with several spectrographs and against myriads of Gaia-ESO Survey UVES U580 spectra of late-type, low-mass stars as one of its thirteen pipelines. Aims: We describe the code and test it against a library of well characterised Gaia benchmark stars. We also release the code to the community and provide the link for download. Methods: We carried out the required EW determination of Fe I and Fe II spectral lines using the automatic tool TAME. StePar implements a grid of MARCS model atmospheres and the MOOG radiative transfer code to compute stellar atmospheric parameters by means of a Downhill Simplex minimisation algorithm. Results: We show the results of the benchmark star test and also discuss the limitations of the EW method, and hence the code. In addition, we found a small internal scatter for the benchmark stars of 9 +- 32 K in Teff, 0.00 +- 0.07 dex in log(g), and 0.00 +- 0.03 dex in [Fe/H]. Finally, we advise against using StePar on double-lined spectroscopic binaries or spectra with R < 30,000, SNR < 20 or vsini >15 km/s as well as stars later than K4 or earlier than F6.