Atomic lines in IR spectra for ultracool dwarfs (Lyubchik+, 2004)

Details Atomic lines in IR spectra for ultracool dwarfs (Lyubchik+, 2004) Atomic lines in IR spectra for ultracool dwarfs (Lyubchik+, 2004)

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ycat..34160655l&link_type=abstract

VizieR On-line Data Catalog: J/A+A/416/655. Originally published in: 2004A&A...416..655L

Physics

Atomic Physics

Stars: Dwarfs, Spectra: Infrared, Atomic Physics

Scientific paper

Table 1 contains all identified lines with central intensities deeper than 0.8 of residual flux using "ultracool dwarf model" identifications.
Table 2 investigates the sensitivity of priority 1 lines identified in Table 1 to temperature, gravity and metallicity.
We compute some synthetic spectra for ultracool objects varying parameters of Teff, log g and metallicity to show the sensitivity of the central intensities of identified lines to these parameters. For our computations we chose the minimal step in model atmospheres grid: {Delta}Teff=100K, {Delta}logg=0.5, {Delta}[M/H]=-0.5. STeff shows the dependence of residual fluxes on effective temperature. For comparison a 2100/5.0/0.0 synthetic spectrum was used. One can see that only a few lines show strong temperature dependence for {Delta}=100K.
The NextGen 2000/4.5/0.0 model was used with 2000/5.0/0.0 to test gravity sensitivity. The dependence for {Delta}(log g)=0.5 is also relatively weak for most lines.
The NextGen model atmospheres 2000/5.0/-0.5 and 2000/5.0/0.0 to test metallicity sensitivity. The metallicity dependence is relatively high for all lines.
(2 data files).

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