WFIRST microlensing observations will return high-precision parallaxes, σ(π) . 0.3 μas, for the roughly 1 million stars with H < 14 in its 2.8 deg2 field toward the Galactic bulge. Combined with its 40,000 epochs of high precision photometry (∼ 0.7 mmag at Hvega = 14 and ∼ 0.1 mmag at H = 8), this will yield a wealth of asteroseismic data of giant stars, primarily in the Galactic bulge but including a substantial fraction of disk stars at all Galactocentric radii interior to the Sun. For brighter stars, the astrometric data will yield an external check on the radii derived from the two asteroseismic parameters, the large-frequency separation h
νnli and the frequency of maximum oscillation power νmax, while for the fainter ones, it will enable a mass measurement from the single measurable asteroseismic parameter νmax. Simulations based on Kepler data indicate that WFIRST will be capable of detecting oscillations in stars from slightly less luminous than the red clump to the tip of the red giant branch, yielding roughly 1 million detections.

Abstract
1. INTRODUCTION
2. ASTROMETRIC AND PHOTOMETRIC PRECISIONSATURATED STARS IN THE PHOTON-NOISE LIMIT
    2.1. Astrometric Precision of Saturated Broad BandAiry Disk
    2.2. Photometric Precision of Saturated Broad BandAiry Disk
    2.3. Utility of Analytic Formulae
3. FROM ASTROMETRIC MEASUREMENTS TOPARALLAXES
4. SYSTEMATIC ERRORS
    4.1. Random Systematics
    4.2. Correlated Systematics
    4.3. Angular Radii
5. SIMULATED WFIRST ASTEROSEISMO
    5.1. Amplitude Adjustment
    5.2. Spectral Frequency Response Function
    5.3. Photometric Noise Estimates
    5.4. Simulated WFIRST Asteroseimology
    5.5. Availability of Asteroseismic Targets
REFERENCES

• Andrew Gould(Department of Astronomy, Ohio State University) Corresponding author
• Daniel Huber(NASA Ames Research Center/SETI Institute/Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney)
• Matthew Penny(Department of Astronomy, Ohio State University/Sagan Fellow)
• Dennis Stello(Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney/Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University)