  High-contrast adaptive optics imaging is a powerful technique to probe the
architectures of planetary systems from the outside-in and survey the
atmospheres of self-luminous giant planets. Direct imaging has rapidly matured
over the past decade and especially the last few years with the advent of
high-order adaptive optics systems, dedicated planet-finding instruments with
specialized coronagraphs, and innovative observing and post-processing
strategies to suppress speckle noise. This review summarizes recent progress in
high-contrast imaging with particular emphasis on observational results,
discoveries near and below the deuterium-burning limit, and a practical
overview of large-scale surveys and dedicated instruments. I conclude with a
statistical meta-analysis of deep imaging surveys in the literature. Based on
observations of 384 unique and single young ($\approx$5--300~Myr) stars
spanning stellar masses between 0.1--3.0~\Msun, the overall occurrence rate of
5--13~\Mjup \ companions at orbital distances of 30--300~AU is
0.6$^{+0.7}_{-0.5}$\% assuming hot-start evolutionary models. The most massive
giant planets regularly accessible to direct imaging are about as rare as hot
Jupiters are around Sun-like stars. Dividing this sample into individual
stellar mass bins does not reveal any statistically-significant trend in planet
frequency with host mass: giant planets are found around 2.8$^{+3.7}_{-2.3}$\%
of BA stars, $<$4.1\% of FGK stars, and $<$3.9\% of M dwarfs. Looking forward,
extreme adaptive optics systems and the next generation of ground- and
space-based telescopes with smaller inner working angles and deeper detection
limits will increase the pace of discovery to ultimately map the demographics,
composition, evolution, and origin of planets spanning a broad range of masses
and ages.
