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The formation and growth of galaxy disks over cosmic time is crucial to ourunderstanding of galaxy formation. Despite steady improvements in the size andquality of disk samples over the last decade, many aspects of galaxy diskevolution remain unclear. Using two square degrees of deep, wide-field i'-bandimaging from the Canada-France-Hawaii Telescope Legacy Survey, we compute sizefunctions for 6000 disks from z=0.2 to z=1 and explore luminosity and numberdensity evolution scenarios with an emphasis on the importance of selectioneffects on the interpretation of the data. We also compute the size function ofa very large sample of disks from the Sloan Digital Sky Survey to use as alocal (z ~ 0.1) comparison. CFHTLS size functions computed with the same fixedluminosity-size selection window at all redshifts exhibit evolution thatappears to be best modelled by a pure number density evolution. The z = 0.3size function is an excellent match to the z = 0.9 one if disks at the highestredshift are a factor of 2.5 more abundant than in the local universe. The SDSSsize function would also match the z = 0.9 CFHTLS size function very well witha similar change in number density. On the other hand, the CFHTLS sizefunctions computed with a varying luminosity-size selection window withredshift remain constant if the selection window is shifted by 1.0$-$1.5 magtowards fainter magnitudes with decreasing redshift. There is a weak dependenceon disk scale length with smaller ($h \lesssim $ 4 kpc) disks requiring moreluminosity evolution than larger ones. Given that changes in number density areprimarily due to mergers and that current estimates of merger rates below z = 1are low, luminosity evolution appears to be a more plausible scenario toexplain the observations.

The Size Function of Galaxy Disks out to z ~ 1 from the Canada-France-Hawaii-Telescope Legacy Survey