Individual alpha elements, C, N, and Ba in early-type galaxies
- Department of Physics and Astronomy, Washington State University, 1245 Webster Hall, Pullman, WA 99164-2814 (United States)
- Bellevue College, 3000 Landerholm Circle SE, Bellevue, WA 98007-6484 (United States)
Spectral data on early-type galaxies are analyzed for chemical abundance with an emphasis on obtaining detailed abundances for the elements O and Si in addition to C, N, Na, Mg, Ca, Fe, and Ba. The abundance trends with velocity dispersion fit preconceptions based upon previous Mg conclusions, namely, that larger galaxies have a higher alpha element to iron peak ratio indicative of a higher ratio of Type II to Type Ia supernova products. The heaviest alpha elements, Ca and Ti, do not participate in this trend, although this fact does not necessarily alter the basic picture given the uncertainties in nucleosynthetic yields. Elements that likely have significant contributions from intermediate-mass stars, namely, C, N, and Ba, also gain ground relative to Fe in massive galaxies at a modest level, with the Ba conclusion uncertain from our data alone. After the velocity dispersion trend is subtracted, [M/H], [N/Fe], [Na/Fe], [Mg/Fe], and [Ca/Fe] probably have cosmic scatter, and no quantity can be shown to not have cosmic scatter.
- OSTI ID:
- 22351383
- Journal Information:
- Astrophysical Journal, Vol. 783, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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