Radio pulsars are highly magnetized, rapidly rotating neutron stars that emit synchrotron radiation along the magnetic axes at their spin frequencies. A compact, strongly gravitating object that emits narrow, regular pulses 1-1000 times per second provides us with a laboratory to test Einstein’s general relativity by, for instance, long-term observations of pulse arrival times. Pulsars in tight binaries are of particular interests as they are important sources of gravitational waves. For example, NS-NS binaries are one of the prime targets for the advanced gravitational-wave detectors on Earth. Since the first discovery made by Jocelyn Bell Burnell and Antony Hewish in 1967, more than 2000 radio pulsars are known to-date in our Galaxy. Discoveries of new population and precision timings made in the past decade not only shed light on existing questions, but also arose new ones. Radio pulsar spectrum follows a power-law with a negative slope of -2. Hence, observations have often been done at low frequencies (MHz up to a few GHz). More recently, high-frequency pulsar observations (several GHz and above) have been practically possible, when a broad-band spectrometer and fast computers became available. The main driving force toward higher frequencies is to find pulsars in the vicinity of Sgr A*, which is one of the holy grails of pulsar astronomy. In this talk, I will overview the Galactic pulsar population and discuss how we can utilize the Korean VLBI Network for pulsar observations. I will also present the on-going efforts at KASI.