  The atmospheric chemical composition of a hot Jupiter can lead to insights
into where in its natal protoplanetary disk it formed and its subsequent
migration pathway. We use a 1-D chemical kinetics code to compute a suite of
models across a range of elemental abundances to investigate the resultant
abundances of key molecules in hot jupiter atmospheres. Our parameter sweep
spans metallicities between 0.1x and 10x solar values for the C/H, O/H and N/H
ratios, and equilibrium temperatures of 1000K and 2000K. We link this parameter
sweep to the formation and migration models from previous works to predict
connections between the atmospheric molecular abundances and formation
pathways, for the molecules \ce{H2O}, \ce{CO}, \ce{CH4}, \ce{CO2}, \ce{HCN} and
\ce{NH3}. We investigate atmospheric \ce{H2O} abundances in eight hot Jupiters
reported in the literature. All eight planets fall within our predicted ranges
for various formation models, however six of them are degenerate between
multiple models and, hence, require additional molecular detections for
constraining their formation histories. The other two planets, HD 189733~b and
HD 209458~b, have water abundances that fall within ranges expected from
planets that formed beyond the \ce{CO2} snowline. Finally, we investigate the
detections of \ce{H2O}, \ce{CO}, \ce{CH4}, \ce{CO2}, \ce{HCN} and \ce{NH3} in
the atmosphere of HD 209458~b and find that, within the framework of our model,
the abundances of these molecules best match with a planet that formed between
the \ce{CO2} and \ce{CO} snowlines and then underwent disk-free migration to
reach its current location.
