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Caption: Figure 24.
Kempton et al. (2018) metrics of signal-to-noise for hypothetical observations of exoplanet atmospheres in transmission (during primary transit) on the vertical axis and emission (during secondary eclipse) on the horizontal axis for a subset of TOIs detected as of the end of 2021 September (NASA Exoplanet Archive; Akeson et al. 2013). Only planets smaller than Neptune, with T eq < 1300 K, and that are predicted to impart a Doppler RV signal K > 3 ms−1 are shown. The points’ sizes are scaled with radius and the color scaled to estimated equilibrium temperature, with the color bar on the right. Increased metric means higher S/N, and the dashed lines indicate the boundary above and to the right of which systems are suitable for JWST observations (Kempton et al. 2018). TOIs 560 b and c are labeled immediately to the right of their data points.
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