Enabling imaging astrometry detection and mass measurement of Earth-like planets

Accurate measurement of exoplanetary masses is a critical step in addressing key aspects of NASA's science vision. New technologies to implement an astrometric instrument capable of measuring masses of earth-analog planets aboard as a part of NASA's future mission portfolio will be required: this is simply the only viable avenue to attaining these data. Here we propose to advance Diffractive Pupil (DP) technology, capable of performing mass measurements down to 1 Earth mass, to TRL-5. This will immediately empower the possibility for dedicated astrometric missions, and perhaps most enticing, it will enable astrometric observing modes to be added (with relatively low cost and impact) to any mission boasting a sufficiently stable direct imaging platform. Astrometry is the only technique that can unequivocally measure exoplanet masses regardless of the system alignment, and serves to independently confirm direct imaging detections, yielding more precise planet orbits than direct imaging alone. Most critically, detection noise floors make it uniquely suited to habitable zone orbits for Earth-mass objects around sun-like stars: true Earth-analogs. Therefore, this technology can confer unique scientific benefits to future flagship missions. In particular, because these missions are expected to yield one or two dozen exoearths, measurements of mass add very significant value to the science of habitability in the solar neighborhood. The proposed work has three areas that complement each other to develop an efficient and reliable technology: 1) Data reduction and calibration algorithms will be fully developed (including those for a diffractive pupil optimized for single and binary stars). To fully benchmark the methodology, confronting the signal recovery with real data from an optical laboratory testbench is essential. 2) A prototype instrument that performs an end-to-end astrometry demonstration in air and in vacuum will be built and tested. This astrometric instrument will include a star simulator with capability to inject simulated planetary orbital signals, together with a telescope equipped with a diffractive pupil, and laser metrology for detector calibration. 3) A study of implementation aboard the HabEx mission in which the diffractive pupil is implemented at an intermediate location in the optical path (not on the telescope primary mirror) will be performed. Such a scenario calls for calibration of the upstream path by way of the telescope metrology system. During year 1 we will improve existing distortion calibration algorithms (Ames and Sydney) and integrate and test the instrument in air at Ames. In parallel, JPL will build the laser metrology system and calibrate the camera. During year 2 the data reduction pipeline will be tested using real data, and the instrument moved to JPL where the laser metrology will be integrated and the system ready for full vacuum testing. In parallel, the HABEX implementation analysis will be initiated. In year 3, vacuum tests will be undertaken at JPL, while simultaneously the HABEX analysis will be finalized. This proposal leverages successful execution of APRA-09 and TDEM-13 that brought the DP technology to TRL-4. Ames Research Center and JPL will partner for the execution of this proposal utilizing previous investments and expertise in laser metrology from JPL and distortion calibration at Ames.

The Astrophysics Research and Analysis program (APRA) supports suborbital and suborbital-class investigations, development of detectors and supporting technology, laboratory astrophysics, and limited ground

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