Chlorine Abundances in Cool Stars

Abstract

Chlorine abundances are reported in 15 evolved giants and one M dwarf in the solar neighborhood. The Cl abundance was measured using the vibration-rotation 1-0 P8 line of H${}^{35}$Cl at 3.69851 $\mu$m. The high resolution L-band spectra were observed using the Phoenix infrared spectrometer on the Kitt Peak Mayall 4m telescope. The average [${}^{35}$Cl/Fe] abundance in stars with --0.72$<$[Fe/H]$<$0.20 is [${}^{35}$Cl/Fe]=(--0.10$\pm$0.15) dex. The mean difference between the [${}^{35}$Cl/Fe] ratios measured in our stars and chemical evolution model values is (0.16$\pm$0.15) dex. The [${}^{35}$Cl/Ca] ratio has an offset of $\sim$0.35 dex above model predictions suggesting chemical evolution models are under producing Cl at the high metallicity range. Abundances of C, N, O, Si, and Ca were also measured in our spectral region and are consistent with F and G dwarfs. The Cl versus O abundances from our sample match Cl abundances measured in planetary nebula and \ion{H}{2} regions. In one star where both H${}^{35}$Cl and H${}^{37}$Cl could be measured, a ${}^{35}$Cl/${}^{37}$Cl isotope ratio of 2.2$\pm$0.4 was found, consistent with values found in the Galactic ISM and predicted chemical evolution models.

arXiv comment22 pages, 10 figures, Accepted for publication in The Astronomical Journal

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