We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the
- Award ID(s):
- 1927130
- NSF-PAR ID:
- 10464299
- Date Published:
- Journal Name:
- Astronomy & Astrophysics
- Volume:
- 672
- ISSN:
- 0004-6361
- Page Range / eLocation ID:
- A143
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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Abstract α -elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2M ⊙. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies. -
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Accepted Manuscript1.0
- Journal Article:
- https://doi.org/10.1051/0004-6361/202244189
