Direct Imaging: Observation, Measurement & Evidence

Direct-imaging systems use adaptive optics, coronagraphs or starshades, precise wavefront control, and post-processing to suppress starlight. Current detections are biased toward young, massive, warm planets at relatively wide separations.

Systems such as HR 8799 show multiple planets tracked over years of orbital motion. Infrared spectra and photometry of directly imaged worlds reveal temperatures, clouds, molecules, and surface gravity.

A coronagraph blocks or destructively suppresses the star's diffraction pattern while preserving off-axis planet light. Adaptive optics corrects atmospheric distortion for ground-based observations, and differential imaging separates stable instrumental speckles from real astrophysical companions.

Multi-epoch observations confirm common proper motion and orbital change. Planet spectra and colors constrain temperature, clouds, molecular composition, and surface gravity.