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Several concepts now exist for small, space-based missions to directlycharacterize exoplanets in reflected light. Here, we develop an instrumentnoise model suitable for studying the spectral characterization potential of acoronagraph-equipped, space-based telescope. We adopt a baseline set oftelescope and instrument parameters appropriate for near-future plannedmissions like WFIRST-AFTA, including a 2 m diameter primary aperture, anoperational wavelength range of 0.4-1.0 um, and an instrument spectralresolution of 70, and apply our baseline model to a variety of spectral modelsof different planet types, including Earth twins, Jupiter twins, and warm andcool Jupiters and Neptunes. With our exoplanet spectral models, we explorewavelength-dependent planet-star flux ratios for main sequence stars of variouseffective temperatures, and discuss how coronagraph inner and outer workingangle constraints will influence the potential to study different types ofplanets. For planets most favorable to spectroscopic characterization, we studythe integration times required to achieve moderate signal-to-noise ratiospectra. We also explore the sensitivity of the integration times required toeither detect the bottom or presence of key absorption bands to coronagraph rawcontrast performance, exozodiacal light levels, and the distance to theplanetary system. Decreasing detector quantum efficiency at longer visiblewavelengths makes the detection of water vapor in the atmospheres of Earth-likeplanets extremely challenging, and also hinders detections of the 0.89 ummethane band. Additionally, most modeled observations have noise dominated bydark current, indicating that improving CCD performance could substantiallydrive down requisite integration times. Finally, we briefly discuss theextension of our models to a more distant future Large UV-Optical-InfraRed(LUVOIR) mission.

Characterizing Rocky and Gaseous Exoplanets with 2-meter Class Space-based Coronagraphs