Improved Vanadium Abundance Measurements for 255 Metal-poor stars
Abstract
We present vanadium abundances for 255 metal-poor stars. We have reanalyzed published high-resolution optical spectroscopy obtained using the Magellan Inamori Kyocera Echelle spectrograph on the Magellan Telescopes at Las Campanas Observatory, the Robert G. Tull Coude Spectrograph on the Harlan J. Smith Telescope at McDonald Observatory, and the High Resolution Spectrograph on the Hobby-Eberly Telescope at McDonald Observatory. We use updated V I and V II atomic transition data from the Wisconsin group and increase the number of V I lines (from 1 to 4 lines) and V II lines (from 2 to 7 lines) relative to previous analysis. As a result, we reduce the V abundance uncertainties and expand the number of stars with V detections from 204 to 255. We calculate a mean [VI/FeI] = -0.10 ± 0.16, mean [VII/FeII] = +0.13 ± 0.16, and mean [V II/V I] = +0.25 ± 0.15. We examine these revised vanadium abundances with abundances of other elements derived previously for these stars to study the correlation between vanadium and other iron-group elements including calcium, scandium, titanium, and chromium. We notice significant correlation with scandium and titanium. This work has been supported by NSF grants AST 1613536 and AST 1815403 to IUR, NSF grant AST-1616040 to CS, AST-1516182 to JEL, and NASA grant NNX16AE96G to JEL.
- Publication:
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American Astronomical Society Meeting Abstracts #235
- Pub Date:
- January 2020
- Bibcode:
- 2020AAS...23527308O