Aims. The aim of our new laboratory measurements is to measure accurate absolute oscillator strengths for neutral manganese transitions in the infrared needed for the study of late-type stars and ultracool dwarfs. Methods. Branching fractions have been measured by high resolution Fourier transform spectroscopy and combined with radiative level lifetimes in the literature to yield oscillator strengths. Results. We present experimental oscillator strengths for 20 Mn I transitions in the wavelength range 3216 to 13 997 angstrom, 15 of which are in the infrared. The transitions at 12 899 angstrom and 12 975 angstrom are observed as strong features in the spectra of late-type stars and ultracool dwarfs. We have fitted our calculated spectra to t...
Context. The stellar abundance ratio of Mg/Fe is an important tool in diagnostics of galaxy evolutio...
International audienceContext. Being the most numerous and oldest stars in the galaxy, M dwarfs are ...
The three Mn i lines at 17325, 17339, and 17349Å are among the 25 strongest lines (log(gf ) > 0.5) i...
Original article can be found at: http://www.aanda.org/ Copyright The European Southern ObservatoryA...
We report laboratory measurements of oscillator strengths for 44 transitions in the Mn T spectrum co...
The goal of the present work is to produce transition probabilities with very low uncertainties for ...
International audienceAn extensive analysis of the Mn spectrum was carried out using high-resolution...
This thesis reports on the term analysis of singly-ionised manganese carried out in order to improve...
Context. Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
We estimate the Mn abundances in the atmospheres of 247 F-G-K-type dwarf stars belonging to the thin...
Context.Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
M dwarfs are the prominent targets of planet search projects, while the complexity of their spectra ...
We use exact curve-of-growth analysis and spectral synthesis to deduce the abundance of Mn from high...
Context. Reliable metallicity values for late K and M dwarfs are important for studies of the chemic...
The manganese abundances was determined in the atmospheres of clump giants stars whose election was ...
Context. The stellar abundance ratio of Mg/Fe is an important tool in diagnostics of galaxy evolutio...
International audienceContext. Being the most numerous and oldest stars in the galaxy, M dwarfs are ...
The three Mn i lines at 17325, 17339, and 17349Å are among the 25 strongest lines (log(gf ) > 0.5) i...
Original article can be found at: http://www.aanda.org/ Copyright The European Southern ObservatoryA...
We report laboratory measurements of oscillator strengths for 44 transitions in the Mn T spectrum co...
The goal of the present work is to produce transition probabilities with very low uncertainties for ...
International audienceAn extensive analysis of the Mn spectrum was carried out using high-resolution...
This thesis reports on the term analysis of singly-ionised manganese carried out in order to improve...
Context. Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
We estimate the Mn abundances in the atmospheres of 247 F-G-K-type dwarf stars belonging to the thin...
Context.Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
M dwarfs are the prominent targets of planet search projects, while the complexity of their spectra ...
We use exact curve-of-growth analysis and spectral synthesis to deduce the abundance of Mn from high...
Context. Reliable metallicity values for late K and M dwarfs are important for studies of the chemic...
The manganese abundances was determined in the atmospheres of clump giants stars whose election was ...
Context. The stellar abundance ratio of Mg/Fe is an important tool in diagnostics of galaxy evolutio...
International audienceContext. Being the most numerous and oldest stars in the galaxy, M dwarfs are ...
The three Mn i lines at 17325, 17339, and 17349Å are among the 25 strongest lines (log(gf ) > 0.5) i...