Massive stars play important roles in the star-forming history of galaxies throughout cosmic time. They end their lives by producing a violent explosion caused by the gravitational collapse of the iron core, called core-collapse supernovae(CCSNe). They give rise to bright optical emission, thereby making them an important tool to investigating star-forming activities of distant galaxies. One of the fundamental questions on massive star evolution is how to connect massive stars born in a specific environment to various types of CCSNe and compact remnants. This problem is still difficult to solve because of the complex interplay of various physical processes involved in massive star evolution and the explosion mechanism of core-collapse supernova themselves. Therefore, it appears that we still have a long way to go. However, recent observational and theoretical progresses, such as, progenitor detections in HST archival images and numerical modelings of CCSNe by massively parallel supercomputers, have gradually made important steps toward the ultimate goal. In this talk, I review observational features CCSNe and discuss recent topics.