occultations. Unlike [*HST*]{}, which takes near-infrared spectra of exoplanets at a very low spectral resolution of $R\,(\Delta\lambda/\lambda)\sim 10-20$, all of [*JWST’s*]{} spectroscopic modes will have at least R$\sim$100 and some as high as R$\sim$3000, with a possibility of R$\sim$2000 over the entire wavelength range. [*JWST*]{} has five scientific instruments, four of which will do spectroscopic observations. These are NIRCam [@2007SPIE.6693E..0GG], NIRISS [@2012SPIE.8442E..2RD], and NIRSpec [@2014SPIE.9143E..08B], all of which will observe in the near-IR between 0.6 and 5.0 $\mu m$, plus MIRI, which will observe in the mid-IR from 5 to 28.3 $\mu m$ [@2015PASP..127..623K; @2015PASP..127..646W]. The fifth instrument, FGS-Guider (0.8-5.0 $\mu m$) is a purely imaging instrument [@2012SPIE.8442E..2RD]. The angular resolution of the instruments is diffraction-limited in most configurations and ranges from 0.032 arcsec (NIRCam) to 0.11 arcsec (MIRI).

[*JWST’s*]{} capabilities will be ideal for improving our knowledge of extrasolar planets by spectroscopic observation, equaling or surpassing all prior efforts in sensitivity and spectral resolution with much greater wavelength coverage. Judicious selection of targets and robust modeling efforts will be needed to most effectively use valuable telescope time. In this paper, we specifically focus on transit spectra, not secondary eclipse emission spectra or light curves, which will be covered in 