Assigned ID: 324 ----- Attempting Submission 1 (Fri Feb 24 07:34:04 GMT 2012) ----- As discussed with my PC, an alternative for WFI2033 would be to have 2 consecutive visits if a single visit is too difficult. Both the PC (William Januszewski) and the CS (Tomas Dahlen) have been extremely helpful during this Phase II process. I am very grateful. The APT system works well, and the links to the documentation of specific entry fields are convenient. The only minor problem I had was that Aladin would crash every now and then, and require APT to restart. ----- Attempting Submission 1 (Thu Jun 28 08:54:01 GMT 2012) ----- We would like the observations of WFI2033 to be in a single visit or two consecutive visits for obtaining good PSF samplings that are required for our science goals. William Januszewski (my PC) is aware of this, and said that he would take a look at the scheduling after I submit. Accurate Cosmology from Gravitational Lens Time Delays Measuring cosmological parameters with a realistic account of the systematic errors is currently one of the principal challenges of physical cosmology. We have shown that a detailed analysis of the gravitational lens B1608+656, including systematic errors, measures the time-delay distance to 5% precision, corresponding to the Hubble constant (H0) to 7%. Combined with WMAP this yields flatness to 2% and the dark energy parameter w to 18%, comparable to BAO measurements. The results are made possible by deep HST/ACS images, showing the Einstein ring with high signal-to-noise ratio that allowed us to determine accurately the mass distribution of the deflector. We propose to extend our work to 4 additional lenses (1 archival) with exquisite time-delay measurements from the Cosmograil collaboration. New, deep WFC3/IR F160W images are needed for 3 systems to characterize fully their Einstein rings. With 5 systems in total, we will measure H0 to 3.8%, i.e., similar in precision to current distance-ladder results (3.3%). Combining these two independent measurements with upcoming Planck data yields 2.5% precision on H0, 0.5% on flatness and 13% on w. Furthermore, studying more lenses is the only way to test if unknown systematic errors are present in our approach. We will do this by performing blind analysis of each system and comparing the measurement scatter with estimated errors. With dozens of accurate time delays currently being measured by Cosmograil, the method has the potential to reach within 3 years 2% on H0 fully independent of the local ladder (and <0.3% on flatness). Eventually, PS1, DES, and LSST will discover hundreds of lenses, making 1% on H0 attainable. We will use several 4-point dither patterns with parallelogram shapes, which each has n+1/2 pixel shifts. These parallelogram patterns will have minimal overlap to avoid areas of persistence. The pixel shifts between the parallelograms are m+1/4 for two parallelograms and m+1/3 for three parallelograms, which will allow us to effectively reject cosmic rays and hot pixels and optimize the sampling of the PSF. In order to fully sample the dynamic range and avoid non-linearities at the 5 brightest pixels at the location of the lensed quasars, we will split each orbit into sequences of short and long exposures at the dither pattern positions. COSMOLOGY 12 false 0.0 0.0 false false false false SUPPORTED GALAXY EINSTEIN RING GRAVITATIONAL LENS J2000 J2000 GALAXY EINSTEIN RING GRAVITATIONAL LENS J2000 J2000 GALAXY EINSTEIN RING GRAVITATIONAL LENS J2000 J2000 WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F160W POS-TARG DITHER DITHER 4 9.132 BOX false 74.653 false 4.740 7.431 2 138.212 POS-TARG LINE 198.528 1 true POS-TARG DITHER DITHER 4 10.601 BOX false 74.653 false 5.470 8.574 3 138.212 POS-TARG LINE 198.528 2 true POS-TARG DITHER 7.431 LINE 4.740 false false 74.653 4 198.528 BOX 3 false POS-TARG DITHER DITHER 4 6.588 BOX false 74.653 false 4.740 7.431 2 138.212 POS-TARG LINE 198.528 4 true /Users/suyu/Research/ObsProposals/12-02HSTc20_proposal/PhaseII_APT_c20_proposal/OP-cache/Suyu_GLTimeDelays_c20_P2-v01.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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