dc.contributor.author |
Kennedy, C. R |
|
dc.contributor.author |
Sivarani, T |
|
dc.contributor.author |
Beers, T. C |
|
dc.contributor.author |
Lee, Y. S |
|
dc.contributor.author |
Placco, V. M |
|
dc.contributor.author |
Rossi, S |
|
dc.contributor.author |
Christlieb, N |
|
dc.contributor.author |
Herwig, F |
|
dc.contributor.author |
Plez, B |
|
dc.date.accessioned |
2011-03-01T11:31:07Z |
|
dc.date.available |
2011-03-01T11:31:07Z |
|
dc.date.issued |
2011-03 |
|
dc.identifier.citation |
The Astronomical Journal, Vol. 141, No. 3, 102 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/5399 |
|
dc.description |
Open Access |
en |
dc.description.abstract |
We report on oxygen abundances determined from medium-resolution near-infrared spectroscopy for a sample of 57 carbon-enhanced metal-poor (CEMP) stars selected from the Hamburg/ESO Survey. The majority of our program stars exhibit oxygen-to-iron ratios in the range +0.5< [O/Fe]<+2.0. The [O/Fe] values for this sample are statistically compared to available high-resolution estimates for known CEMP stars as well as to high-resolution estimates for a set of carbon-normal metal-poor stars. Carbon, nitrogen, and oxygen abundance patterns for a sub-sample of these stars are compared to yield predictions for very metal-poor asymptotic giant branch (AGB) abundances in the recent literature. We find that the majority of our sample exhibit patterns that are consistent with previously studied CEMP stars having s-process-element enhancements and thus have very likely been polluted by carbon- and oxygen-enhanced material transferred from a metal-poor AGB companion. |
en |
dc.language.iso |
en |
en |
dc.publisher |
IOP Publishing |
en |
dc.relation.uri |
http://dx.doi.org/10.1088/0004-6256/141/3/102 |
en |
dc.rights |
© IOP Publishing |
en |
dc.subject |
Galaxy: halo |
en |
dc.subject |
Stars: abundances |
en |
dc.subject |
Stars: agb and post-agb |
en |
dc.subject |
Stars: population II |
en |
dc.subject |
Techniques: spectroscopic |
en |
dc.title |
[O/Fe] Estimates for Carbon-enhanced Metal-poor Stars from Near-infrared Spectroscopy |
en |
dc.type |
Article |
en |