2014/11/18 by F. Paletou, T. Böhm, V. Watson +3
Physics and Astronomy · #Astronomical spectroscopy #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Gamma-ray bursts and supernovae #High resolution #Physics #Remote sensing #Spectral line #Stars #Stellar evolution #Stellar, planetary, and galactic studies #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201424741
published as A&A 573, A67 (2015) · 13 pages, 8 figures (accepted A&A). arXiv admin note: text overlap with arXiv:1401.1083
arxiv created 2014/11/18 · openalex publication_date 2014/11/26 · arxiv updated 2014/12/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The general context of this study is the inversion of stellar fundamental parameters from high-resolution Echelle spectra. We aim at developing a fast and reliable tool for the post-processing of spectra produced by ESPaDOnS and Narval spectropolarimeters. Our inversion tool relies on principal component analysis. It allows reducing dimensionality and defining a specific metric for the search of nearest neighbours between an observed spectrum and a set of observed spectra taken from the Elodie stellar library. Effective temperature, surface gravity, total metallicity, and projected rotational velocity are derived. Various tests presented in this study that were based solely on information coming from a spectral band centred on the Mg i b-triplet and had spectra from FGK stars are very promising.