resolution (R$\sim$100). The NIRSpec Prism mode is also uniquely suited for faint targets ($J>11$), while brighter targets will saturate it.

It is important to select observing modes for JWST to make efficient use of observing time. Each observing mode (except MIRI MRS) requires one visit, consisting of one or more transits (in the case of transit spectroscopy). Therefore, we wish to cover as large a wavelength range as possible with as few visits as possible. Four particular observing modes together, NIRISS GR700XD, NIRCam F322W2, NIRCam F444W, and MIRI LRS, are the fewest modes that can achieve complete coverage of the wavelength range of interest (0.6 to 14 $\mu m$) for planets orbiting bright stars. The additional range covered by MIRI MRS (the 14.0 to 28.3 $\mu m$ range not covered by LRS) has not been frequently considered, but is likely to yield useful diagnostics to trace molecular species.

We summarize seven model observing programs in Table \[FilterCombos\] and plot their throughput functions with major molecular opacities in Figure \[ComboPlot\]. In all cases, MIRI LRS refers to the Slitless model, which we find to be more informative for our simple, three-parameter model, based on our analysis in Section \[LRS\]. Program 1 