A blend may consist of a background or foreground eclipsing binary (or star - planet pair) whose eclipses are attenuated by the light of the candidate and possibly other stars within
the photometric aperture.
Since we do not require spectroscopy or high - resolution imaging for validation, some of our derived parameters for a planetary system may be systematically incorrect due to dilution from light due to additional stars in
the photometric aperture.
The KELT images have a pixel scale of ~ 23 arsec per pixel (similar to TESS) and a large point spread function, and the KELT reduction pipeline uses a weighted
photometric aperture with radius 3 arcmin.
One either uses a much smaller
photometric aperture than normal, excluding the nearby star, or one uses a much wider aperture, containing both stars, and makes a correction for the dilution of the companion.
At this angular scale, multiple stars are typically blended in
the photometric apertures.