0 Assigned ID: 1287 ----- Attempting Submission 1 (Sat Oct 01 00:13:39 GMT 2016) ----- HST Phase I Proposal 1287 (hst_z10.apt) successfully submitted. Receipt: # 1287-1 ----- Attempting Submission 2 (Sat Oct 01 00:16:06 GMT 2016) ----- HST Phase I Proposal 1287 (hst_z10.apt) successfully submitted. Receipt: # 1287-2 ----- Attempting Submission 3 (Sat Oct 01 00:32:46 GMT 2016) ----- HST Phase I Proposal 1287 (hst_z10.apt) successfully submitted. Receipt: # 1287-3 0 ----- Attempting Submission 1 (Mon Dec 12 21:16:29 GMT 2016) ----- 0 Confirmation of ultra-luminous z~9 galaxies We propose to confirm the robustness of 5 ultrabright (24.2 < H < 25.0) candidate galaxies at redshift z = 8.5 - 9.5. The sources were unexpectedly found over the wide area (~ 1sq degree) groundbased UltraVISTA near-infrared survey. If these are truly ultraluminous galaxies at z~9 then the UV luminosity function has a power-law-like shape at very early times rather than the familiar Schechter function at lower redshift. This information places strong constraints on models for feedback and duty cycles in the earliest phases of galaxy formation during the epoch of reionization. In addition, the confirmation of a population of ultra-bright sources impacts survey strategies for JWST in 2017, while providing compelling targets for early cycle JWST studies. Given how little is known about the brightest, most massive galaxies at z~9 we propose to immediately verify or reject these candidates in this Mid Cycle, before targeting them with deep dedicated observations in HST cycle 25. The H-band magnitude of sources in our bright sample range from ~24.2 to 25.0. Since we desire the measure a break of 3 magnitudes (at 1 sigma), we need to reach 28.0 at 1 sigma. HST is capable of reaching those limits in 0.65 orbits / object. We note also that the z ~ 9-10 range is not particularl well suited for groundbased spectroscopic follow up due to poor transmission around 1.4 micron. We also devote a small fraction (0.35 orbits) of the minimum 1-orbit integration time on each source to obtaining imaging at 1.25 micron and 1.55 micron in the F125W and F160W bands, respectively. Not only will this ensure that we can connect our new HST photometry at 1, 1.25, and 1.55 microns to the ground-based photometry to obtain maximally robust results, but this will greatly improve our estimates of the redshifts for the individual sources assuming they are at z > 8. For H~24.2-25.0 sources, a S/N of 8-10 can be obtained in just a 500 second exposure. 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