Chlorine Abundances in Cool Stars

TL;DR

This study measures chlorine abundances in 16 nearby evolved stars using infrared spectroscopy, revealing discrepancies with chemical evolution models and providing insights into galactic chemical processes.

Contribution

First measurement of Cl abundances in evolved giants and an M dwarf using infrared spectroscopy, highlighting model underestimations at high metallicity.

Findings

Cl abundances are slightly below model predictions.

The Cl/O ratio aligns with planetary nebula and H II region data.

The isotope ratio $^{35}$Cl/$^{37}$Cl is consistent with Galactic ISM values.

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.