Exoplanet direct imaging separates planetary light from the host star's light on the sky. The two central obstacles are small angular separation and a large brightness contrast. Diffraction spreads stellar light into the surrounding image, and imperfect optics add structure that can resemble or hide a faint companion. Adaptive optics reduces blurring from the terrestrial atmosphere, improving the concentration and stability of the image.
Young giant planets on wide orbits are favourable targets because their intrinsic thermal radiation can be substantial. Measuring their light at several wavelengths constrains the exoplanet atmosphere; repeated positions trace the orbit. Brightness alone does not directly measure mass: converting it into mass requires an age and an evolutionary cooling model. Doppler spectroscopy or orbital dynamics can supply independent constraints.
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