I investigate the possibility of constraining the flux of the lens ( i.e. , host star ) for the types of planetary systems the Korean Microlensing Telescope Network is predicted to find .
I examine the potential to obtain lens flux measurements by 1 ) imaging a lens once it is spatially resolved from the source , 2 ) measuring the elongation of the point spread function of the microlensing target ( lens+source ) when the lens and source are still unresolved , and 3 ) taking prompt follow-up photometry .
In each case I simulate observing programs for a representative example of current ground-based adaptive optics ( AO ) facilities ( specifically NACO on VLT ) , future ground-based AO facilities ( GMTIFS on GMT ) , and future space telescopes ( NIRCAM on JWST ) .
Given the predicted distribution of relative lens-source proper motions , I find that the lens flux could be measured to a precision of \sigma _ { H _ { \ell } } \leq 0.1 for \gtrsim 60 \% of planet detections \geq 5 years after each microlensing event , for a simulated observing program using GMT that images resolved lenses .
NIRCAM on JWST would be able to carry out equivalently high-precision measurements for \sim 28 \% of events \Delta t = 10 years after each event by imaging resolved lenses .
I also explore the effects various blend components would have on the mass derived from prompt follow-up photometry , including companions to the lens , companions to the source , and unassociated interloping stars .
I find that undetected blend stars would cause catastrophic failures ( i.e. , > 50 \% fractional uncertainty in the inferred lens mass ) for \lesssim ( 16 \cdot f _ { bin } ) \% of planet detections , where f _ { bin } is the binary fraction , with the majority of these failures occurring for host stars with mass \lesssim 0.3 M _ { \odot } .