Infrared Mn I laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

Details Infrared Mn I laboratory oscillator strengths for the study of late type stars and ultracool dwarfs Infrared Mn I laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011a%26a...525a..44b&link_type=abstract

Astronomy and Astrophysics, Volume 525, id.A44

Astronomy and Astrophysics

Astrophysics

2

Atomic Data, Line: Identification, Methods: Laboratory, Stars: Late-Type

Scientific paper

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 Å, 15 of which are in the infrared. The transitions at 12 899 Å and 12 975 Å are observed as strong features in the spectra of late-type stars and ultracool dwarfs. We have fitted our calculated spectra to the observed Mn I lines in spectra of late-type stars. Using the new experimentally measured Mn I log(gf) values together with existing data for Mn I hyperfine structure splitting factors we determined the manganese abundance to be log N(Mn) = -6.65 ± 0.05 in the atmosphere of the Sun, log N(Mn) = 6.95 ± 0.20 in the atmosphere of Arcturus, and log N(Mn) = -6.70 ± 0.20 in the atmosphere of M 9.5 dwarf 2MASSW 0140026+270150.

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