0 Assigned ID: 1027 ----- Attempting Submission 1 (Fri Apr 08 23:35:05 GMT 2016) ----- HST Phase I Proposal 1027 (LyCimgGP.apt) successfully submitted. Receipt: # 1027-1 ----- Attempting Submission 2 (Fri Apr 08 23:48:38 GMT 2016) ----- HST Phase I Proposal 1027 (LyCimgGP.apt) successfully submitted. Receipt: # 1027-2 ----- Attempting Submission 3 (Fri Apr 08 23:55:18 GMT 2016) ----- POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. APT issues warning about POS_TARGs for ramp filters. We are aware of this and have planned small steps. 873165252 ----- Attempting Submission 1 (Thu Jul 21 18:07:50 GMT 2016) ----- APT issues warning about POS_TARGs for ramp filters. We are aware of this and have planned small steps. How does ionizing radiation escape from galaxies? Search for sources that reionized the Universe from z~15 to z~6 is one of the main drivers of present-day astronomy. Low-mass star-forming galaxies are the most favoured sources of ionizing photons, but the searches of escaping Lyman continuum (LyC) have not been extremely successful. Our team has recently detected prominent LyC escape from five Green Pea galaxies at redshift ~0.3, using the HST/COS spectrograph, which represents a significant breakthrough. We propose here to study the LyC escape of the strongest among these leakers, J1152, with spatial resolution. From the comparison of the ionizing and non-ionizing radiation maps, and surface brightness profiles, we will infer the major mode in which LyC is escaping: from the strongest starburst, from the galaxy edge, through a hole along our line-of-sight, through clumpy medium, or directly from all the production sites due to highly ionized medium in the entire galaxy. In parallel, we will test the predictive power of two highly debated indirect indicators of LyC leakage: the [OIII]5007/[OII]3727 ratio, and Lyman-alpha. We predict that their spatial distribution should closely follow that of the ionizing continuum if column densities of the neutral gas are low. This combined study, which relies on the HST unique capabilities, will bring crucial information on the structure of the leaking galaxies, provide constraints for hydrodynamic simulations, and will lead to efficient future searches for LyC leakers across a large range of redshifts. This program will image a compact, star-forming galaxy at z~0.3 in UV and optical filters, using ACS/SBC (9 orbits), ACS/WFC (1 orbit) and WFC3/UVIS (3 orbits). Total 13 orbits. We request the SBC visits to be scheduled so that the SBC HAS NOT BEEN IN USE FOR THE PAST 24 HOURS to minimize the dark current. We have split the SBC observations by 2 orbits per visit to prevent heatup of the detector. We require that the SBC F115LP observations be done in the SHADOW part of the orbits to minimize the effects of airglow background due to geocoronal Lyman-alpha emission. We complete the remaining part of the orbits with SBC F125LP observations. We have estimated the exposure times with ETC version 24.2. We will derive the Lyman continuum image by subtracting the signal in two adjacent ACS/SBC filters, F115LP and F125LP. We have used pysynphot to simulate the filter subtraction and derive the necessary exposure times to achieve signal-to-noise ratio of 15 in the subtracted image. We will obtain the Lyman-alpha line image from the subtraction of ACS/SBC F150LP and F165LP images. To plan the exposure times in the line and continuum filters, we have taken into account the SDSS spectroscopic fluxes, the HST COS FUV spectroscopy, and the NUV light distribution observed by HST GO 13744. We have added FLASH for WFC3/UVIS and ACS/WFC exposures as adviced by the APT and ETC. All the exposures are safe in BOT. The WFC3/UVIS visits utilise dithering to step over droplets. We use ACS/WFC ramp filters for H-alpha and H-beta, using small POS_TARGs. We use a large dithering pattern for the ACS/SBC exposures to dither over the large scale flat-field features. Galaxies 6 false true false false false false SUPPORTED GALAXY DWARF COMPACT STARBURST YES J2000 J2000 FUV=20.66+/-0.30, NUV=20.38+/-0.17 ACS/SBC Imaging No No F115LP ACS/SBC Imaging No No F125LP ACS/SBC Imaging No No F150LP ACS/SBC Imaging No No F165LP WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F763M WFC3/UVIS Imaging No No F467M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F390W ACS/WFC Imaging No No F850LP ACS/WFC RampFilter No No FR853N The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. /private/var/folders/z3/xy_g1v_s5fz9yrhzb8thz4cr0001qc/T/OPVisit6659669175983196799.xml SBC: We request that SBC NOT BE USED 24 HOURS before this visit in order to mitigate the effects of dark current. 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