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While high-resolution cross-correlation spectroscopy (HRCCS) techniques haveproven effective at characterizing the atmospheres of transiting andnon-transiting hot Jupiters, the limitations of these techniques are not wellunderstood. We present a series of simulations of one HRCCS technique, whichcombines the cross-correlation functions from multiple epochs, to placetemperature and contrast limits on the accessible exoplanet population for thefirst time. We find that planets approximately Saturn-size and larger within$\sim$0.2 AU of a Sun-like star are likely to be detectable with currentinstrumentation in the $L$-band, a significant expansion compared with thepreviously-studied population. Cooler ($ \rm T_{eq} \leq 1000$ K) exoplanetsare more detectable than suggested by their photometric contrast alone as aresult of chemical changes which increase spectroscopic contrast. The $L$-bandCH$_4$ spectrum of cooler exoplanets enables robust constraints on theatmospheric C/O ratio at $\rm T_{eq} \sim 900K$, which have proven difficult toobtain for hot Jupiters. These results suggest that the multi-epoch approach toHRCCS can detect and characterize exoplanet atmospheres throughout the innerregions of Sun-like systems with existing high-resolution spectrographs. Wefind that many epochs of modest signal-to-noise ($\rm S/N_{epoch} \sim 1500$)yield the clearest detections and constraints on C/O, emphasizing the need forhigh-precision near-infrared telluric correction with short integration times.

Contrast and Temperature Dependence of Multi-Epoch High-Resolution Cross-Correlation Exoplanet Spectroscopy