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Direct imaging is the best detection method for exoplanets at wide separations, but it is limited by the large contrast difference between stars and planets. The most promising direct imaging surveys are conducted in near infrared wavelengths at young ages when a giant planet is still self-luminous at these wavelengths. In this talk, I summarize our survey of young stars in the Taurus Molecular Cloud and what this tells us about our experimental limits. Applying models of planet formation and brightness evolution, I also discuss how likely we are to detect accreting exoplanets with future instruments and whether we can constrain the formation conditions of directly imaged planets. |
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