  Using the Harvard College Observatory Photographic Plate Collection and
recent CCD observations by the ASAS project we have reconstructed the light
variations of the southern pulsating red giant star VZ Velorum between 1890 and
early 2006. Contrary to an early report on its low-amplitude semiregular
nature, we found a relatively stable Mira-like light curve with a mean period
of 318 days and amplitude up to 7 magnitudes. The latest observations show
evidence for a slightly shorter period (312 days). However, the difference does
not exceed the intrinsic period jitter often seen in Mira type variables.
