0 Assigned ID: 79 ----- Attempting Submission 1 (Mon Apr 04 14:28:57 GMT 2016) ----- HST Phase I Proposal 79 (Cycle24_pcmd.apt) successfully submitted. Receipt: # 79-1 ----- Attempting Submission 2 (Mon Apr 04 15:01:56 GMT 2016) ----- HST Phase I Proposal 79 (Cycle24_pcmd.apt) successfully submitted. Receipt: # 79-2 ----- Attempting Submission 3 (Thu Apr 07 20:31:36 GMT 2016) ----- HST Phase I Proposal 79 (Cycle24_pcmd.apt) successfully submitted. Receipt: # 79-3 ----- Attempting Submission 4 (Fri Apr 08 15:45:06 GMT 2016) ----- The main body of nearly every galaxy within 20 Mpc is in the `semi-resolved' regime, in which source confusion/crowding dominates, and yet the brightest stars (e.g., massive stars and evolved giants) are rare enough to induce stochastic fluctuations in the light distribution. In this regime we define the concept of pixel color magnitude diagrams (pixel CMDs), which allow one to reconstruct non-parametric star formation histories (SFHs) from semi-resolved imaging data. Here we propose to analyze pixel CMDs for 20 galaxies within 20 Mpc in order to measure spatially resolved SFHs for a representative sample (by mass) of galaxies within the local universe. These measurements will enable a first estimate of the total SFH within the local volume, which can then be compared to the cosmic SFH from lookback studies and to detailed galaxy formation models. The resulting SFHs will also be used to investigate variations across morphological types, radial variations within galaxies, and differences (or not) between ellipticals, classical, and pseudobulges. As part of this program we will deliver a suite of well-tested tools for analyzing pixel CMDs from HST data. Galaxies 0 Legacy false false false SUPPORTED