Metallicity Distribution Function for Leo I Based on HST WFC3 Photometry

Details Metallicity Distribution Function for Leo I Based on HST WFC3 Photometry Metallicity Distribution Function for Leo I Based on HST WFC3 Photometry

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21924421r&link_type=abstract

American Astronomical Society, AAS Meeting #219, #244.21

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a preliminary metallicity distribution function (MDF) for Leo I, derived from photometry with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope (HST). We obtained relatively high S/N photometry in V (F555W), I (F814W) and Ca H & K (F390M) for giants. Using the medium band filter that covers the Ca H & K lines - the strongest metal absorption lines in the visible spectrum - in conjunction with the V and I band photometry, we calculate the stellar metallicities of individual stars with an expected accuracy of approximately 0.2 dex. From the photometric metallicities we construct a MDF for Leo I containing almost 4000 stars, 5 times more stellar metallicities than have been obtained from the ground. While the metallicity accuracy in our study is lower than spectroscopic measurements, the larger number of data points provides some advantages in looking for rarer components of the population and possible substructure. While the Leo I MDF presented here is a preliminary result, our long term goals are to use the distribution of metallicities of Leo I to constrain the formation and evolution of the system, through and understanding of its chemical evolution.

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