Linearized Field Deblending: Point-spread Function Photometry for Impatient Astronomers

NASA's Kepler, K2 and TESS missions employ Simple Aperture Photometry (SAP) to derive time-series photometry, where an aperture is estimated for each star, pixels containing star are summed create a single light curve. This method simple, but in crowded fields the derived can be highly contaminated. The alternate of fitting Point Spread Function (PSF) data able account crowding, computationally expensive. In this paper, we present new approach extracting photometry from these missions, which fits PSF directly, makes simplifying assumptions order greatly reduce computation expense. Our fixes scene field image, estimates shape instrument with linear model, allows only source flux position vary. We demonstrate that our separate blended targets Kepler dataset separated by less than pixel. fast compute, fully accounts uncertainties degeneracies due fields. name described work Linearized Field Deblending (LFD). on false positive target \koi. two sources data, contaminating transiting signal consistent small, sub-stellar companion radius $2.67R_{jup}$ ($0.27R_{sol}$). equally applicable mission.