LISA is an all-sky instrument, with the sensitivity to gravitational waves only weakly depending on the location of the source in the sky. Localization of individual sources comes from two main effects. The first is the motion of the LISA constellation around the Sun, which introduces shifts in both frequency (Doppler effect) and amplitude (sweeping the LISA sensitivity pattern across the sky). These shifts encode information about the sky position of the source in the waveform that LISA observes. Since most LISA sources are observed for months or years, there is sufficient modulation to provide localization. The second effect is that, for the higher frequency sources that LISA observes, the wavelength of the gravitational waves is similar to or smaller than the size of the LISA constellation. This means that different parts of the constellation experience the gravitational wave at slightly different times, which again encodes information about the location of the source. The precision of LISA’s localization of a particular source depends on many factors including the type of source, the particular parameters of the source, and the duration of the observation. For the best-localized sources, the final localizations may be on the order of a few arcminutes. Degree-scale localization will be more typical and the more numerous faint sources will be localized less well. Interestingly, LISA’s localization of a particular source will improve over time, which will open up some novel observing strategies for potential EM counterparts of events such as mergers of massive black holes.