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To understand the role that planet formation history has on the observableatmospheric carbon-to-oxygen ratio (C/O) we have produced a population ofastrochemically evolving protoplanetary disks. Based on the parameters used ina pre-computed population of growing planets their combination allows us totrace the molecular abundances of the gas that is being collected intoplanetary atmospheres. We include atmospheric pollution of incoming (icy)planetesimals as well as the effect of refractory carbon erosion noted to existin our own solar system. We find that the carbon and oxygen content ofNeptune-mass planets are determined primarily through solid accretion andresult in more oxygen-rich (by roughly two orders of magnitude) atmospheresthan Hot-Jupiters, whose C/O are primarily determined by gas accretion.Generally we find a `main-sequence' between the fraction of planetary massaccreted through solid accretion and the resulting atmospheric C/O - withplanets of higher solid accretion fraction having lower C/O. Hot-Jupiters whoseatmospheres have been chemically characterized agree well with our populationof planets, and our results suggest that Hot Jupiter formation typically beginsnear the water ice line. Lower mass hot-Neptunes are observed to be much morecarbon-rich (with 0.33 $\lesssim$ C/O $\lesssim$ 1) than is found in our models(C/O $\sim 10^{-2}$), and suggest that some form of chemical processing mayaffect their observed C/O over the few Gyrs between formation and observation.Our population reproduces the general mass-metallicity trend of the solarsystem and qualitatively reproduces the C/O-metallicity anti-correlation thathas been inferred for the population of characterized exoplanetary atmospheres.

Connecting planet formation and astrochemistry: A main sequence for C/O in hot-exoplanetary atmospheres