IR O I triplet, [O I] lines in F-K dwarfs/giants (Takeda, 2003)

Details IR O I triplet, [O I] lines in F-K dwarfs/giants (Takeda, 2003) IR O I triplet, [O I] lines in F-K dwarfs/giants (Takeda, 2003)

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003ycat..34020343t&link_type=abstract

VizieR On-line Data Catalog: J/A+A/402/343. Originally published in: 2003A&A...402..343T

Computer Science

Stars: Metal-Deficient, Abundances: Peculiar, Models: Atmosphere

Scientific paper

Table2 contains the results of non-LTE abundance corrections for each of the O I triplet lines (at 7771.94, 7774.17, and 7775.39 Å) computed on a large grid of models [Teff= 4500, 5000, 5500, 6000, 6500K, logg (cm/s2) = 1.0, 2.0, 3.0, 4.0, 5.0, and [Fe/H] = 0, -1, -2, -3] for the microturbulence values of 1, 2, and 3km/s. See Table 1 below for the adopted atomic data.
Table 3 gives the numerical coefficients (a, b) used with the analytic formula, Δ=a*10b*Wλ, where Δ is the non-LTE abundance correction and Wλ the equivalent width), for evaluating the non-LTE correction, corresponding to each of the atmospheric models (combination of each Teff and logg). These data were computed for three values of the microturbulent velocity (ξ=1, 2, and 3km/s) for each of the three lines of the O I triplet (O I 7771.94, 7774.17, and 7775.39). The minimum and the maximum value of the equivalent-widths (in mÅ), used to established the coefficients, are also given. (These indicate the range of the Wλ values to which the formula with these coefficients can be applied.)
Table7 contains the results of non-LTE abundance corrections for the O I 6158.2 line (blend of three components at 6158.149, 6158.172, 6158.187Å) computed on a large grid of models [Teff= 4500, 5000, 5500, 6000, 6500K, logg (cm/s2) = 1.0, 2.0, 3.0, 4.0, 5.0, and [Fe/H] = 0, -1] for the microturbulence values of 1, 2, and 3km/s. The blending of three components was correctly treated by synthesizing the spectrum in evaluating the equivalent width of the O I 6158 line as well as in deriving the abundance there from. See Table 1 below for the adopted atomic data.
Table5: The data contained in each file are: 1. Published values in the corresponding literature which was adopted here Equivalent widths (for the O I 7771/7774/7775 lines and/or [O I] 6300/6363 lines) Atmospheric parameters (Teff, log g, xi, and [Fe/H]) 2. Results of the reanalysis: LTE abundance, non-LTE correction, final NLTE abundance (for each line) averaged [O/Fe]77 and [O/Fe]63 over available lines (for O I and [O I]) averaged non-LTE correction 77 for the O I triplet lines.
These data further form the basis of Fig. 8: Fig. 8a --> [Fe/H], [O/Fe]77, and [O/Fe]63; Fig. 8b --> [Fe/H] and 77.
(5 data files).

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