0 Assigned ID: 1140 ----- Attempting Submission 1 (Sat Apr 12 00:00:21 GMT 2014) ----- HST Phase I Proposal 1140 (phase1-AR.apt) successfully submitted. ----- Attempting Submission 2 (Sat Apr 12 00:05:05 GMT 2014) ----- HST Phase I Proposal 1140 (phase1-AR.apt) successfully submitted. ----- Attempting Submission 3 (Sat Apr 12 00:06:02 GMT 2014) ----- Resolved stellar populations in Local Group galaxies are the best place to study the earliest epochs of star formation. Isolated Local Group Dwarfs are also ideal places to test the physics of star formation and the role of stellar/supernova feedback in moderating star formation. For the first time, high resolution, fully cosmological simulations of isolated dwarf galaxies have not only overcome long-standing modeling problems like the "cusp/core" problem and the "exponential disk" dilemma, but also successfully match observational trends such as metallicities and effective yields, colors, cold gas fractions, and cumulative SFHs. Therefore, for the first time, we are in a position to interpret observations of resolved stellar populations in Local Group dwarfs, and make predictions to test the models. In fact, exploratory work shows that the same physics that overcomes the problems with dwarf galaxy formation in CDM may also explain why observations seem to suggest outside-in growth, instead of the inside-out growth predicted by theory. The redistribution of stars in dwarfs has dramatic implications for interpreting observations of resolved stellar populations. We will produce results that are directly comparable to observations by creating artificial CMDs at varying radii, quantifying the observed age and metallicity gradients of dwarfs as well as quantifying the role that dark matter core creation and new radial migration schemes play. RESOLVED STELLAR POPULATIONS Default Medium false false false false true SUPPORTED