Mass Measurements of Exoplanet Microlens Host Stars with Near Simultaneous Hubble and Keck AO Observations

A list of suggested reviewers was sent to Neill Reid several days ago. A few typos have been corrected in the resubmission. 1613121515 Assigned ID: 1643 ----- Attempting Submission 1 (Mon Mar 12 15:15:17 GMT 2018) ----- HST Phase I Proposal 1643 (HST_Keck_col_dep_cen_shift_DD.apt) successfully submitted. Receipt: # 1643-1 ----- Attempting Submission 2 (Mon Mar 12 15:47:44 GMT 2018) ----- HST Phase I Proposal 1643 (HST_Keck_col_dep_cen_shift_DD.apt) successfully submitted. Receipt: # 1643-2 0 ----- Attempting Submission 1 (Tue Apr 03 02:01:47 GMT 2018) ----- Mass Measurements of Exoplanet Microlens Host Stars with Near Simultaneous Hubble and Keck AO Observations We propose Hubble observations to detect both the photometric and astrometric signatures of host stars for 3 planets found by gravitational microlensing. These signatures will allow us to determine the masses and distances of the exoplanet host stars, and they will help us sharpen tests of the core accretion theory predictions for the exoplanet mass function beyond the snow line. We request nearly simultaneous observations with our NASA Keck Key Strategic Mission Support observing program to provide a precise comparison between optical astrometry of the Hubble images and the infrared astrometry of Keck adaptive optics (AO) images. This will allow us to detect the separation of the planetary host and source stars via the color-dependent centroid shift effect. In order to avoid systematic errors due to stellar proper motions, we request observations within 5 days of our Keck Key observing program, which is scheduled for 5 half-nights during May 21-27. This effect is maximized with the optical-infrared color difference that the combined HST and Keck AO data will provide. Our proposed observations will help us to develop and test this optical-infrared color-dependent centroid shift method for use with a larger sample of microlens planetary systems during the second year of our Keck observing program. We will want ~16 exposures per orbit in the WFC3/UVIS F814W and F555W passbands to get good spatial sampling of the effective PSFs (Anderson and King 2000), and this means that we will be unable to do parallel, full-frame buffer dumps. Fortunately, a 1024x1024 WFC3/UVIS sub-array image will contain 1600 bulge G and K-dwarfs, similar to the source stars, which can be used to construct precise PSF models. We will use the sub-array with minimal CTE degradation, but we will also use the FLASH. For OGLE-2012-BLG-0950, we will obtain 8x60 sec exposures in F814W and 8 x 110 sec exposures in F555W. We will employ a custom dither pattern designed to optimally map the effective PSF with 8 exposures. For the faintest target, OGLE-2012-BLG-0563, and the target with the lowest predicted S/N, MOA-2010-BLG-328, we request 2 orbits with 16 optimally dithered observations in each of the F814W and F555W filters. The exposure times for these two targets will be 85-92 sec. Planets and Planet Formation 0 SUPPORTED EXT-STAR EXTRA-SOLAR PLANETARY SYSTEM GRAVITATIONAL LENS J2000 J2000 I = 20.12 +- 0.05 EXT-STAR EXTRA-SOLAR PLANETARY SYSTEM GRAVITATIONAL LENS J2000 J2000 I = 19.29 +- 0.05 EXT-STAR EXTRA-SOLAR PLANETARY SYSTEM GRAVITATIONAL LENS J2000 J2000 I = 19.17 +- 0.1 WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F555W The scheduling data was generated by CASM 25.2. 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