0 Assigned ID: 1248 ----- Attempting Submission 1 (Wed Sep 30 23:07:28 GMT 2020) ----- HST Phase I Proposal 1248 successfully submitted. Receipt: # 1248-1 ----- Attempting Submission 2 (Wed Sep 30 23:38:36 GMT 2020) ----- HST Phase I Proposal 1248 successfully submitted. Receipt: # 1248-2 ----- Attempting Submission 3 (Wed Sep 30 23:40:08 GMT 2020) ----- 0 ----- Attempting Submission 1 (Tue Dec 01 05:59:30 GMT 2020) ----- Mapping the Porous Neutral Gas Reservoir in an Extremely High Ionization Galaxy We do not empirically know how the first galaxies reionized the early universe. In particular, how does neutral gas transmit ionizing photons from gas-rich star-forming regions into the intergalactic medium? One solution is that small regions of ionized gas preferentially funnel ionizing photons out of galaxies. However, this anisotropic escape dramatically changes the morphology of cosmic reionization and the subsequent structure of the universe. The James Webb Space Telescope aims to provide the empirical foundation of the epoch of reionization, but it will not sufficiently resolve the morphology of neutral gas nor the isotropy of the escape of ionizing photons. Here, we propose 15 orbits of HST mid-cycle observations to obtain 35 pc spatial resolution WFC3 images of the neutral resonant Mg II emission line. The proposed high-ionization emission line galaxy has recently been discovered to have a massive, but porous, neutral gas reservoir. Regions of bright resonant Mg II emission will trace the low column density holes through which the newly observed Lyman Alpha must propagate through. These Mg II maps will test where photons are transmitted out of this galaxy to answer how isotropically ionizing photons stream into the intergalactic medium. We will complement the Mg II maps with optical emission line maps to determine whether strong optical lines trace these low column density holes. These observations are crucial for understanding upcoming JWST observations and will illuminate one of the key empirical obstacles towards understanding cosmic reionization. Here we aim to image the Mg II emission from an extreme emission line galaxy with WFC3/UVIS. We then aim to understand why this resonant emission escapes the extreme emission line galaxy. To do this we will image the galaxy in 9 different filters: Mg II emission (F275W)m Mg II continuum (F280N), [O II] (F373N), [O II] continuum (F343N), [O III] (F502N), H-beta (F487N), the H-beta + [O III] continuum (F467N), H-alpha (F665N) and the H-alpha continuum (F645N). We use previous SDSS and MUSE spatially resolved imaging to determine the surface brightnesses that we must integrate down to and the WFC3/UVIS ETC to determine the required exposure times. We will break the individual visits up into 3 orbit visits. Where possible, we will try to have as long of visits as possible to increase the background and the CTE, while reducing the pre-flash required. We calculate the pre-flash required for each exposure using the WFC3 ETC and determining the flash required to reach a total background of 20 e-. We will use the WFC3 Dither-line pattern, which will allow us to do 2 exposures per filter set up to account for bad pixels and sub-sample the PSF. In order to avoid large buffer dump issues, we include some of our shorter orbits (e.g. H-alpha and O III) with some of our longer orbits. This enables the buffer dump to occur during the longer exposure. The proposed team is made up of a subset of the CLASSY team. CLASSY is a Large Hubble Space Telescope Project that has taken HST/COS spectra of 48 local star-forming galaxies to compile an atlas of high-quality ultra-violet spectra of star-forming galaxies in the local universe. J1418+2102, the subject of this proposed observation, is one of the CLASSY targets. Our team has extensive history of narrow-band imaging, rest-frame UV, and optical spectroscopy (e.g. Hayes et al. 2014). Galaxies Large Scale Structure of the Universe 0 false false true false true false false SUPPORTED GALAXY EMISSION LINE NEBULA STARBURST YES J2000 J2000 WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F373N WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F467M WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F645N POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 1 false /Users/johnchisholm/Documents/Mg2/OP-cache/J14_HST-v01.xml The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 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