2014MNRAS.439..788H

We present new Strömgren and Washington data sets for the Boötes I dwarf galaxy, and combine them with the available Sloan Digital Sky Survey photometry. The goal of this project is to refine a ground-based, practical, accurate method to determine age and metallicity for individual stars in Boötes I that can be selected in an unbiased imaging survey, without having to take spectra. With few bright upper red giant branch stars and distances of about 35-250kpc, the ultra-faint dwarf galaxies (UDFs) present observational challenges in characterizing their stellar population. Other recent studies have produced spectra and proper motions, making Boötes I an ideal test case for our photometric methods. We produce photometric metallicities from Strömgren and Washington photometry, for stellar systems with a range of -1.0 > [Fe/H] > -3.5. Needing to avoid the collapse of the metallicity sensitivity of the Strömgren m1-index on the lower red giant branch, we replace the Strömgren v filter with the broader Washington C filter to minimize observing time. We construct two indices: m* = (C - T1)0 - (T1 - T2)0 and m** = (C - b)0 - (b - y)0. We find that CT1by is the most successful filter combination, for individual stars with [Fe/H] < -2.0, to maintain ∼ 0.2 dex [Fe/H]-resolution over the whole red giant branch. The m**-index would be the best choice for space-based observations because the (C - y) colour is not sufficient to fix metallicity alone in an understudied system. Our photometric metallicites of stars in the central regions of Boötes I confirm that there is a metallicity spread of at least -1.9 > [Fe/H] > -3.7. The best-fitting Dartmouth isochrones give a mean age, for all the Boötes I stars in our data set, of 11.5±0.4Gyr. From ground-based telescopes, we show that the optimal filter combination is CT1by, avoiding the v filter entirely. We demonstrate that we can break the isochrones' age-metallicity degeneracy with the CT1by filters, using stars with logg = 2.5 - 3.0, which have less than a 2percent change in their (C - T1) colour due to age, over a range of 10^–14Gyr.