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 Besançon 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 .