Testing a New Method for Finding Leaky Galaxies: Implications for the Epoch of Reionization

0 Assigned ID: 477 ----- Attempting Submission 1 (Fri Apr 07 11:05:36 GMT 2017) ----- HST Phase I Proposal 477 (leaky_v4.apt) successfully submitted. Receipt: # 477-1 ----- Attempting Submission 5 (Fri Apr 07 19:48:42 GMT 2017) ----- HST Phase I Proposal 477 (leaky_v5.apt) successfully submitted. Receipt: # 477-5 ----- Attempting Submission 6 (Fri Apr 07 20:03:38 GMT 2017) ----- The number of orbits used exceeds the number allocated Visit 06 is a HOPR repeat of visit 05. 830584777 ----- Attempting Submission 1 (Mon Jul 17 15:32:11 GMT 2017) ----- HST Phase II Proposal 15341 (15341_PhaseII.apt) successfully submitted. Receipt: # 15341-1 ----- Attempting Submission 2 (Wed Jul 19 19:14:01 GMT 2017) ----- HST Phase II Proposal 15341 (15341_PhaseII-DS2_dark.apt) successfully submitted. Receipt: # 15341-2 ----- Attempting Submission 3 (Wed Jul 19 21:09:21 GMT 2017) ----- ----- Attempting Submission 4 (Thu May 24 16:06:40 GMT 2018) ----- Testing a New Method for Finding Leaky Galaxies: Implications for the Epoch of Reionization One of the core missions of JWST will be understanding the Epoch of Reionization (EOR), which traces the formation of the earliest progenitors of present-day galaxies. A major uncertainty is the relative amount of ionizing Lyman Continuum (LyC) photons that can escape from these early galaxies. Unfortunately, it is not possible to directly measure the leakage of LyC photons from galaxies during the EOR. The best strategy is to find lower redshift galaxies that are leaking LyC photons, and to use these analogs to both understand the physical processes that make this leakage possible and to identify reliable indirect signposts of leaky galaxies that could be measured with JWST. We propose to test one such promising signpost: the relative weakness of the [SII]6717,6731 emission-lines. The lines are produced near and just beyond the outer edge of a Stromgren sphere. In conditions when the gas is optically-thin to LyC photons (allowing leakage) these lines therefore become weak. Our specific goal is to directly observe the rest-frame LyC in five galaxies chosen to have unusually weak SII. If we succeed, this would provide a new signpost for JWST to characterize leaky galaxies during the EOR. We are observing the four target with G140L segment 1105 A. The idea is to get to the Lyman edge at 912A in the rest frame and measure the Lyman continuum flux. We will proceed by acquiring acquisition images with MIRROR A at S/N =40. Then we will observe with G140 L in each of the 4 FP-POS. These are supplemented by DARK observations at the end of each orbital visible range. Galaxies and the IGM Cosmology 0 false false true false true false false SUPPORTED GALAXY STARBURST NO J2000 J2000 2e-16 erg/s/cm2/A [FUV flux density within the COS aperture GALAXY STARBURST NO J2000 J2000 4e-16 erg/s/cm2/A [FUV flux density within the COS aperture GALAXY STARBURST NO J2000 J2000 3e-16 erg/s/cm2/A [FUV flux density within the COS aperture GALAXY STARBURST NO J2000 J2000 5e-16 erg/s/cm2/A [FUV flux density within the COS aperture GALAXY STARBURST NO J2000 J2000 3e-16 erg/s/cm2/A [FUV flux density within the COS aperture] COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 1500498113983 The scheduling data was generated by CASM 25.2. 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