http://arxiv.org/abs/1909.06227
We present and discuss the results of a search for extremely metal-poor stars based on photometry from data release DR1.1 of the SkyMapper imaging survey of the southern sky. In particular, we outline our photometric selection procedures and describe the low-resolution ($R$ $\approx$ 3000) spectroscopic follow-up observations that are used to provide estimates of effective temperature, surface gravity and metallicity ([Fe/H]) for the candidates. The selection process is very efficient: of the 2618 candidates with low-resolution spectra that have photometric metallicity estimates less than or equal to -2.0, 41% have [Fe/H] $\leq$ -2.75 and only $\sim$7% have [Fe/H] $>$ -2.0 dex. The most metal-poor candidate in the sample has [Fe/H] $<$ -4.75 and is notably carbon-rich. Except at the lowest metallicities ([Fe/H] $<$ -4), the stars observed spectroscopically are dominated by a `carbon-normal’ population with [C/Fe]${1D,LTE}$ $\leq$ +1 dex. Consideration of the A(C)${1D, LTE}$ versus [Fe/H]${1D, LTE}$ diagram suggests that the current selection process is strongly biased against stars with A(C)${1D, LTE}$ $>$ 7.3 (predominantly CEMP-$s$) while any bias against stars with A(C)${1D, LTE}$ $<$ 7.3 and [C/Fe]${LTE}$ $>$ +1 (predominantly CEMP-no) is not readily quantifiable given the uncertainty in the SkyMapper $v$-band DR1.1 photometry. We find that the metallicity distribution function of the observed sample has a power-law slope of $\Delta$(Log N)/$\Delta$[Fe/H] = 1.5 $\pm$ 0.1 dex per dex for -4.0 $\leq$ [Fe/H] $\leq$ -2.75, but appears to drop abruptly at [Fe/H] $\approx$ -4.2, in line with previous studies.
G. Costa, M. Bessell, A. Mackey, et. al.
Mon, 16 Sep 19
27/74
Comments: 21 pages, 19 figures, accepted for publication in MNRAS
You must be logged in to post a comment.