A collection of model stellar spectra for spectral types B to early-M

TL;DR

This paper provides a comprehensive, publicly available collection of synthetic stellar spectra across a wide range of parameters, useful for interpreting various astrophysical observations.

Contribution

It introduces a large, homogeneous set of synthetic spectra based on the latest models and atomic data, covering extensive parameter space and multiple resolutions.

Findings

Spectra cover 120-6500 nm with resolutions up to 300,000.

Models validated against observational data for select cases.

Provides dense grids including [$eta$/Fe] and micro-turbulence parameters.

Abstract

Models of stellar spectra are necessary for interpreting light from individual stars, planets, integrated stellar populations, nebulae, and the interstellar medium. We provide a comprehensive and homogeneous collection of synthetic spectra for a wide range of atmospheric parameters and chemical compositions. We compile atomic and molecular data from the literature. We adopt the largest and most recent set of ATLAS9 model atmospheres, and use the radiative code ASS$\epsilon$T.The resulting collection of spectra is made publicly available at medium and high-resolution ($R\equiv\lambda/\delta\lambda$ = 10,000, 100,000 and 300,000 spectral grids, which include variations in effective temperature between 3500 K and 30,000 K, surface gravity ($0\le \log g \le 5$), and metallicity ($-5 \le$[Fe/H]$\le +0. 5$), spanning the wavelength interval 120-6500 nm. A second set of denser grids with additional dimensions, [$\alpha$/Fe] and micro-turbulence, are also provided (covering 200-2500 nm). We compare models with observations for a few representative cases.