0 Assigned ID: 882 ----- Attempting Submission 1 (Fri Feb 24 23:05:03 GMT 2012) ----- HST Phase I Proposal 882 (cy20_faint_quasars.apt) successfully submitted. PSF calibration targets have been changed for visits 02, 04, 06. These targets have been confirmed (via coordinated Gemini AO imaging) to be non-binary at WFC3 IR resolution. ON HOLD has been removed from Visits 01-06. These visits may now be scheduled. Use of F126N in Visits 02, 04, 06 is simply as a low-throughput filter to create dummy exposures, in order to ensure matched orbital phasing of quasar and star dithers. -1435319916 ----- Attempting Submission 1 (Mon Jul 09 21:09:15 GMT 2012) ----- HST Phase II Proposal 12974 (cy20_faint_quasars.apt) successfully submitted. ----- Attempting Submission 2 (Tue Apr 30 01:20:01 GMT 2013) ----- ----- Attempting Submission 3 (Tue Sep 03 00:37:48 GMT 2013) ----- Errors are in completed visits (07-10) WFC3IR Imaging of UV-Faint z=6 Quasars: Star-Forming Host Galaxies of AGN in the Early Universe We propose to study the star-forming host galaxies of AGN at z~6 with WFC3/IR in F125W and F160W. Recently, far-infrared (FIR) continuum has been detected in five UV-faint (rest-frame m_1450>20.2) quasars at z~6, suggesting that they have star formation rates (SFRs) of ~1000 MSun/yr, comparable to UV-bright z~6 quasars. Such SFRs imply a significant young, UV-bright stellar population. These host galaxies have yet to be seen in starlight, however, since light from the AGN still dominates the rest-frame UV emission. We successfully subtracted the point source in the UV-bright (m_1450=19.03) quasar J1148+5251 down to mu_J>24.4, mu_H>24.9 mag arcsec^-2, giving upper limits of m_1680>22.5, m_2160>23.0 mag for the host galaxy (Program 12332, PI Windhorst). Uncertainties in the PSF model remain the dominant source of residuals. Since these uncertainties scale with brightness, low-contrast quasars with UV-faint point sources and UV-bright hosts are the best targets for this method. Using the observing and subtraction methods we developed, we propose to observe all 5 FIR-detected, UV-faint z~6 quasars with WFC3/IR in F125W and F160W. We request 5 orbits per quasar, for a total of 25 orbits. This program is beyond the capability of ground-based AO facilities, due to depth and PSF stability required. Observations of these host galaxies are critical to determine: (a) The existence of a luminous stellar component (b) Luminosity and color profiles, to constrain star formation histories (c) Morphologies and sizes, to look for mergers and hierarchical formation processes (d) Stellar mass, to understand formation and co-evolution of SMBHs and galaxy bulges We will observe each z=6 quasar for 4 orbits, as well as 1 final orbit for an accompanying PSF measurement star. Each 1-orbit PSF star visit will be executed directly following the 4-orbit quasar visit to ensure a consistent thermal environment for measuring the time- and thermal-dependent PSF. We use a 4-point dither pattern to recover (via drizzling) Nyquist sampling of the PSF at 1.25 microns. Persistence effects are avoided through careful dithering, by avoiding chip areas that have been exposed to high fluxes from other targets in the field, and by waiting to observe the bright PSF stars (which will saturate the inner ~9 pixels, but with an acceptable count rate read by using STEP25 sample sequence) until the final, 5th orbit. Spacecraft breathing effects on the PSF are mitigated by: 1) selecting PSF stars that have similar celestial coordinates (<5 deg away) to the quasars, to minimize orientation-based effects. 2) fully time-sampling the PSF variability within an orbit by taking exposures of the same subpixel dither point at the same orbital phase to sample variability induced by the orbital day-night cycle. Wavelength-based PSF differences are minimized by selecting PSF stars that match the quasar J-H and H-K colors, thus avoiding halo-like residuals seen when PSF stars are not color-matched. Each 5-orbit package of quasar+PSF star will be marked ON HOLD awaiting the results of coordinated Gemini observations (approved by the TAC) to pre-select non-binary PSF stars from a list of color- and coordinate-matched candidates. As soon as a suitable PSF star is vetted by Gemini, the quasar/PSF star pair will have their ON HOLD requirement removed. AGN/QUASARS 12 false false 0.0 1.25 false false false SUPPORTED GALAXY HIGH REDSHIFT GALAXY QUASAR J2000 J2000 z=21.78 GALAXY HIGH REDSHIFT GALAXY QUASAR J2000 J2000 z=22.8 GALAXY HIGH REDSHIFT GALAXY QUASAR J2000 J2000 z=20.97 GALAXY HIGH REDSHIFT GALAXY QUASAR J2000 J2000 z=20.62 CALIBRATION POINT SPREAD FUNCTION This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 J 15.45, H 14.89 GALAXY HIGH REDSHIFT GALAXY QUASAR J2000 J2000 z=20.6 CALIBRATION POINT SPREAD FUNCTION This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 g 17.95, r 16.68, i 16.23, z 15.92, J 14.79, H 14.24 CALIBRATION POINT SPREAD FUNCTION This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 H 14.33 CALIBRATION POINT SPREAD FUNCTION This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 H 13.33 CALIBRATION POINT SPREAD FUNCTION This object was generated by the targetselector and retrieved from the SIMBAD database. 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