0 Assigned ID: 795 ----- Attempting Submission 1 (Fri Apr 07 19:35:17 GMT 2017) ----- HST Phase I Proposal 795 (proposal_cover.apt) successfully submitted. Receipt: # 795-1 ----- Attempting Submission 2 (Fri Apr 07 21:57:15 GMT 2017) ----- Understanding gas in galaxies and its movement as galactic winds in particular is critical in galaxy formation and evolution studies. While enormous progress has been made in the last decade, the detailed properties (spatial distribution, ionization state, phase and kinematic structure) of gas in and around galaxies are still poorly constrained. HST observations have been instrumental in advancing the study of the complex multi-phase galactic winds. However, they have been interpreted using useful but simple wind models. With the advent of advanced high resolution hydrodynamic cosmological galaxy simulations, which claim to realistically model gas and metal distributions in galaxies and self-consistently generate winds, it is time to develop more sophisticated wind models to interpret the observations and also make simulation outputs into observable spectra. To that end, we propose to use the existing 3D radiative transfer (RT) wind model of Prochaska et al. 2011 to post-process the outputs from state-of-art hydrodynamic simulations. In addition to developing interpretive tools to study galactic winds, we will produce a large suite of synthetic mock HST UV spectra (including noise and instrument effects) for robust and unprecedented comparison between wind observations and theory. We will share our analysis tools and thousands of mock wind profiles and emission-line maps of varying galaxy properties, viewing angles, signal-to-noise and redshift with the community. Effort will be made to use machine-learning techniques to analyze these mock spectra. Finally, we will compare our analysis with other wind models that approximate the RT process and assess their accuracy. Galaxies and the IGM 0 Regular false true true SUPPORTED