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To figure out the effect of stellar mass and local environment onmorphological transformation and star formation quenching in galaxies, we usethe massive ($M_* \geq 10^{10} M_{\odot}$) galaxies at $0.5 \leq z \leq 2.5$ infive fields of 3D-HST/CANDELS. Based on the {\it UVJ} diagnosis and thepossibility of possessing spheroid, our sample of massive galaxies areclassified into four populations: quiescent early-type galaxies (qEs),quiescent late-type galaxies (qLs), star-forming early-type galaxies (sEs), andstar-forming late-type galaxies (sLs). It is found that the quiescent fractionis significantly elevated at the high ends of mass and local environmentaloverdensity, which suggests a clear dependence of quenching on both mass andlocal environment. Over cosmic time, the mass dependence of galaxy quiescencedecreases while the local environment dependence increases. The early-typefraction is found to be larger only at high-mass end, indicating a evident massdependence of morphological transformation. This mass dependence becomes moresignificant at lower redshifts. Among the four populations, the fraction ofactive galactic nucleus (AGN) in the qLs peaks at $2<z \leq 2.5$, and rapidlydeclines with cosmic time. The sEs are found to have higher AGN fractions of$20-30\%$ at $0.5\leq z<2$ . The redshift evolution of AGN fractions in the qLsand sEs suggests that the AGN feedback could have played important roles in theformation of the qLs and sEs.

Morphological Transformation and Star Formation Quenching of Massive Galaxies at 0.5 < z < 2.5 in 3D-HST/CANDELS