2018A&A...618A..25A

Context. Models of stellar spectra are necessary for interpreting light from individual stars, planets, integrated stellar populations, nebulae, and the interstellar medium.
Aims. We provide a comprehensive and homogeneous collection of synthetic spectra for a wide range of atmospheric parameters and chemical compositions.
Methods. 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 ASSεT.
Results. The resulting collection of spectra is made publicly available at medium and high-resolution (R~λ/δλ=10000, 100000 and 300000) spectral grids, which include variations in effective temperature between 3500K and 30000K, surface gravity (0≤logg≤5), and metallicity (-5≤[Fe/H]≤+0.5), spanning the wavelength interval 120-6500nm. A second set of denser grids with additional dimensions, [α/Fe] and micro-turbulence, are also provided (covering 200-2500nm). We compare models with observations for a few representative cases.