0Assigned ID: 228
----- Attempting Submission 1 (Thu Apr 10 18:36:39 GMT 2014) -----
HST Phase I Proposal 228 (udlaes_grism.apt) successfully submitted.SAME POS MAY NOT BE APPROPRIATE
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SAME POS MAY NOT BE APPROPRIATE0----- Attempting Submission 1 (Fri Jul 18 04:35:33 GMT 2014) -----Two adjacent direct/grism exposures will have the same coordinate
(no offset).Stellar Populations and Ionization States of Lyman Alpha Emitters During the Epoch of Peak Star FormationLow luminosity galaxies contribute significantly to the mass and star-formation density of the early Universe. Ly-alpha emitting galaxies (LAEs) are powerful probes of the faint-end of the luminosity function and early mass assembly. LAE studies at z>2 have typically used stacked optical and/or Spitzer data to discern their median properties, but the actual distribution of stellar masses and ionization states of LAEs remain largely unconstrained. To advance our understanding of this important population, we have successfully identified large samples of LAEs (~900 in four 0.33 deg^2 fields) at z~1.9, and have spectroscopically confirmed our selection using Keck. Here we propose to leverage our existing deep HST near-IR and Spitzer/IRAC imaging with the WFC3 G141 grism to measure [OIII]+H-beta for 76 LAE candidates from our sample, 13 of which are already spectroscopically confirmed at z=1.9+/-0.1. Combined with [OII] measurements from the ground, we will: (1) correct the emission line contribution to the HST broadband photometry and thus more accurately measure stellar masses and ages of LAEs; (2) measure ionization states with [OIII]/[OII] to discern the physical conditions in the ISM of these faint, low-mass galaxies; and (3) use systemic velocities derived from [OIII]+Hb, combined with our rest-UV spectra of the Ly-alpha and interstellar absorption lines, to deduce the kinematics of the ISM and the prevalence of galaxy-scale outflows. An economical investment of 16 orbits will enable robust stellar population, ionization, and ISM structure measurements for LAEs, thus illuminating their significance at a time when galaxies were forming most of their stars.We will be targeting 8 distinct targets with the WFC3/IR G141 grism. Each target will have a single visit consisting of two orbits. Each orbit will be split into 4 exposures. For the first orbit, the first exposure is a ~200 sec direct image in F140W at POS_TARG = (0.000,0.000). The second exposure is a ~1103 sec G141 image with the same POS_TARG as exposure 1. The third exposure is a 1203 sec G141 image at POS_TARG=(0.542,0.182). The fourth exposure isa direct image in F140W with the same POS_TARG as exposure 3. For the second orbit, the first exposure is a ~200 sec direct image in F140W at POS_TARG = (0.339,0.485). The second exposure is a ~1103 sec G141 image with the same POS_TARG as exposure 1. The third exposure is a 1203 sec G141 image at POS_TARG=(-0.203,0.303). The fourth exposure isa direct image in F140W with the same POS_TARG as exposure 3. The purpose of this sequence and POS_TARG offsets is to do a 4 point box dither with a short direct and long grism exposure at each position of the box.UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTUREDefaultfalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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