The Galactic Chemical Evolution of Chlorine

We measured \(^{35}\)Cl abundances in 52 M giants with metallicities between -0.5 \(<\) [Fe/H] \(<\) 0.12. Abundances and atmospheric parameters were derived using infrared spectra from CSHELL on the IRTF and from optical echelle spectra. We measured Cl abundances by fitting a H\(^{35}\)Cl mol...

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Bibliographic Details
Published inarXiv.org
Main Authors Maas, Z G, Pilachowski, C A
Format Paper Journal Article
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 26.01.2021
Subjects
Abundance
Astrochemistry
Atmospheric models
Calcium
Chemical evolution
Chlorine
Galactic evolution
Infrared spectra
Metallicity
Nuclear fusion
Physics - Astrophysics of Galaxies
Physics - Solar and Stellar Astrophysics
Stellar evolution
Supernovae
Titanium
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Summary:We measured \(^{35}\)Cl abundances in 52 M giants with metallicities between -0.5 \(<\) [Fe/H] \(<\) 0.12. Abundances and atmospheric parameters were derived using infrared spectra from CSHELL on the IRTF and from optical echelle spectra. We measured Cl abundances by fitting a H\(^{35}\)Cl molecular feature at 3.6985 \(\mu\)m with synthetic spectra. We also measured the abundances of O, Ca, Ti, and Fe using atomic absorption lines. We find that the [Cl/Fe] ratio for our stars agrees with chemical evolution models of Cl and the [Cl/Ca] ratio is broadly consistent with the solar ratio over our metallicity range. Both indicate that Cl is primarily made in core-collapse supernovae with some contributions from Type Ia SN. We suggest other potential nucleosynthesis processes, such as the \(\nu\)-process, are not significant producers of Cl. Finally, we also find our Cl abundances are consistent with H II and planetary nebular abundances at a given oxygen abundance, although there is scatter in the data.
ISSN:2331-8422
DOI:10.48550/arxiv.2101.11068