  We investigate the giant planet-metallicity correlation for a homogeneous,
unbiased set of 217 hot Jupiters taken from nearly 15 years of wide-field
ground-based surveys. We compare the host star metallicity to that of field
stars using the Besan\c{c}on Galaxy model, allowing for a metallicity
measurement offset between the two sets. We find that hot Jupiters
preferentially orbit metal rich stars. However, we find the correlation
consistent, though marginally weaker, for hot Jupiters
($\beta=0.71^{+0.56}_{-0.34}$) than it is for other longer period gas giant
planets from radial velocity surveys. This suggests that the population of hot
Jupiters probably formed in a similar process to other gas giant planets, and
differ only in their migration histories.
