HR-pyPopStar: high wavelength-resolution stellar populations evolutionary synthesis model

TL;DR

The HR-pyPopStar model offers high wavelength-resolution spectral energy distributions for stellar populations across a wide age and metallicity range, aiding interpretation of advanced astronomical observations.

Contribution

It introduces the first high-resolution spectral library covering a broad age, metallicity, and wavelength range for stellar population synthesis.

Findings

Spectra cover 91 to 24,000 Å with R~50,000 at 5000 Å.

Includes ionising populations for young and old stars.

Validated with recent GTC observations.

Abstract

We present the HR-pyPopStar model, which provides a complete set (in ages) of high resolution (HR) Spectral Energy Distributions of Single Stellar Populations. The model uses the most recent high wavelength-resolution theoretical atmosphere libraries for main sequence, post-AGB/planetary nebulae and Wolf-Rayet stars. The Spectral Energy Distributions are given for more than a hundred ages ranging from 0.1 Myr to 13.8 Gyr, at four different values of the metallicity (Z = 0.004, 0.008, 0.019 and 0.05), considering four different IMFs. The wavelength range goes from 91 to 24 000 {\AA} in linear steps {\delta}{\lambda} = 0.1 {\AA}, giving a theoretical resolving power R_{th,5000} ~ 50 000 at 5000 {\AA}. This is the main novelty of these spectra, unique for their age and wavelength ranges. The models include the ionising stellar populations that are relevant both at young (massive hot stars) as well as old (planetary nebulae) ages. We have tested the results with some examples of HR spectra recently observed with MEGARA at GTC. We highlight the importance of wavelength-resolution in reproducing and interpreting the observational data from the last and forthcoming generations of astronomical instruments operating at 8-10m class telescopes, with higher spectral resolution than their predecessors.