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arXiv · 1501.06908

Carbon in Red Giants in Globular Clusters and Dwarf Spheroidal Galaxies

Evan N. Kirby·Michelle Guo·Andrew J. Zhang·Michelle Deng·Judith G. Cohen·Puragra Guhathakurta·Matthew D. Shetrone·Young Sun Lee·Luca Rizzi
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Abstract

We present carbon abundances of red giants in Milky Way globular clusters and dwarf spheroidal galaxies (dSphs). Our sample includes measurements of carbon abundances for 154 giants in the clusters NGC 2419, M68, and M15 and 398 giants in the dSphs Sculptor, Fornax, Ursa Minor, and Draco. This sample doubles the number of dSph stars with measurements of [C/Fe]. The [C/Fe] ratio in the clusters decreases with increasing luminosity above log(L/L_sun) ~= 1.6, which can be explained by deep mixing in evolved giants. The same decrease is observed in dSphs, but the initial [C/Fe] of the dSph giants is not uniform. Stars in dSphs at lower metallicities have larger [C/Fe] ratios. We hypothesize that [C/Fe] (corrected to the initial carbon abundance) declines with increasing [Fe/H] due to the metallicity dependence of the carbon yield of asymptotic giant branch stars and due to the increasing importance of Type Ia supernovae at higher metallicities. We also identified 11 very carbon-rich giants (8 previously known) in three dSphs. However, our selection biases preclude a detailed comparison to the carbon-enhanced fraction of the Milky Way stellar halo. Nonetheless, the stars with [C/Fe] < +1 in dSphs follow a different [C/Fe] track with [Fe/H] than the halo stars. Specifically, [C/Fe] in dSphs begins to decline at lower [Fe/H] than in the halo. The difference in the metallicity of the [C/Fe] "knee" adds to the evidence from [alpha/Fe] distributions that the progenitors of the halo had a shorter timescale for chemical enrichment than the surviving dSphs.

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Evan N. Kirby, Michelle Guo, Andrew J. Zhang, Michelle Deng, Judith G. Cohen, Puragra Guhathakurta, Matthew D. Shetrone, Young Sun Lee, Luca Rizzi. 2015-02-25. Carbon in Red Giants in Globular Clusters and Dwarf Spheroidal Galaxies. https://doi.org/10.1088/0004-637x%2F801%2F2%2F125

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