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We present a study on structures and physical properties of massive ($M_*>10^{10} M_{\sun} $) compact galaxies at $1.0<z<2.0$ in five 3D--{\itHST}/CANDELS fields. Compared with the extended star-forming galaxies (eSFGs),compact star-forming galaxies (cSFGs) are found to have the lower level of starformation, and mainly distribute in the quiescent region of the {\it UVJ}diagram. The distributions of dust attenuation and S{\'e}rsic index supportthat the progenitors of cQGs are cSFGs, and cSFGs are at a transitional phasebetween eSFGs and cQGs. The prevalence of X-ray selected AGNs ($\sim 28\%$) isconfirmed in the cSFGs at $1<z<2$ which indicates that the violent gas-richprocesses such as merger and disk instability could drive the structure to bemore compact, and trigger both star formation and black hole growth in thecentral regions. Our results support the "two-step" scenario that the cSFGs at$1<z<2$ are the intermediate population after compaction but before a quickquenching. Our analysis of parametric and nonparametric morphologies shows thatcQGs (eQGs) are more concentrated and have less substructures than cSFGs(eSFGs), and quenching and compactness should be associated with each other.The cSFGs at $1.5<z<2$ ($1<z<1.5$) prefer to be in higher (lower) densityenvironment, similar as cQGs (eSFGs). It suggests that merger or stronginteraction might be the main driving mechanism of compaction at higherredshifts, whereas the disk instability of individual galaxies might play amore important role on the formation of cSFGs at lower redshifts.

Structures, stellar population properties, AGN fractions, and environments of massive compact galaxies at $1 < z < 2$ in 3D--{\it HST}/CANDELS