tokens: the distance of the star–planet system in parsecs (PC), and Hill radius is expressed in (au). Finally, we calculate the RV semi-amplitude, K , of each planet given its estimated mass:We further assume an orbital inclination of ∼90° and e = 0. Table 2 includes each of the parameters used in our calculations which have been extracted from the HZ catalog (Kane et al. 2016 ), as well as the NASA exoplanet archive. Table 3 presents our calculations of planet mass, Hill radii (HR), estimated RV semi-amplitudes and angular separations of the planet–star systems and potential planet–moon systems at both the full HR and Hill radii ( HR). Table 2 Habitable Zone Candidates with R p > 3 R ⊕ Note. a Semimajor axis. Table 3 Radial Velocity, Hill Radius, and Angular Separation Calculations for HZ Candidates with R p > 3 R ⊕ Tables 4 and 5 then present our calculations of HR, angular separations of a potential planet–Moon systems at the full Hill radius and RV semi-amplitudes for each exoplanet with a radius of 10 R ⊕ or greater with our chosen quantified masses: one Saturn mass ( M sat ), one Jupiter mass ( M J ), and 13 Jupiter masses (13 M J ). Table 4 Radial Velocity Semi-amplitude Calculations for Category 4 HZ Candidates with R p > 10 R ⊕ Table 5 Hill Radii Calculations for Category 4 HZ Candidates with R p > 10 R ⊕ Notes. a Angular separation of exomoon at full Hill radius for . b Angular separation of exomoon at full Hill radius for M p = M J . c Angular separation of exomoon at full Hill radius for . We plot a histogram of the effective temperatures of Kepler host stars to determine if there is a similar distribution of temperatures among both the HZ candidates and the full catalog. Figure 11 shows the stellar temperature distributions for both the HZ Kepler candidates (green), as well as the full Kepler catalog (gray). The histograms show that there is a similar distribution of temperatures among both the HZ candidates and the full catalog, with the HZ host star temperatures dropping off (around) 7000 K. As the HZ of stars with greater effective temperatures will lie further away from the star, planets in this zone are harder to detect. Thus, this drop is likely a false upper limit. Figure 11. Stellar temperature distributions. Habitable zone Kepler candidates in green overlays the distribution of the full Kepler catalog in gray. The histograms show that there is a similar distribution of temperatures among both the HZ candidates and the full Kepler catalog. While the distribution of the habitable zone candidates drops off at 7000 K, this could be a false upper limit as the habitable zone of stars with greater effective temperature lies further away from the star and current transit detection methods are less sensitive to planets at these longer orbits. Using the calculations from our Tables above, we plot the Kepler magnitude of the host star of both the unconfirmed and confirmed HZ planets and their expected RV signatures to determine the
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