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We present the HR-pyPopStar model, which provides a complete set (in ages) ofhigh resolution (HR) Spectral Energy Distributions of Single StellarPopulations. The model uses the most recent high wavelength-resolutiontheoretical atmosphere libraries for main sequence, post-AGB/planetary nebulaeand Wolf-Rayet stars. The Spectral Energy Distributions are given for more thana hundred ages ranging from 0.1 Myr to 13.8 Gyr, at four different values ofthe metallicity (Z = 0.004, 0.008, 0.019 and 0.05), considering four differentIMFs. 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 fortheir age and wavelength ranges. The models include the ionising stellarpopulations 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 HRspectra recently observed with MEGARA at GTC. We highlight the importance ofwavelength-resolution in reproducing and interpreting the observational datafrom the last and forthcoming generations of astronomical instruments operatingat 8-10m class telescopes, with higher spectral resolution than theirpredecessors.

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