to above 0.9. For comparison, Jupiter resides 5.2 AU from our Sun, has an orbital period of $\sim$12 years, and has an orbital eccentricity of $\sim$0.05. Table 1 provides these basic data for a representative subset of the current EGP bestiary. The extremely close-in EGPs, such as 51 Peg b, $\tau$ Boo b, HD209458b, and OGLE-TR56b[@konacki; @torres; @sasselov03], were a surprise, but no less so than was the heterogeneity of the masses and orbital properties of the emerging EGP family. To be sure, the Doppler technique selects for the closer representatives, but they must exist to be detected. As would be expected due to tidal dissipation, the close-in EGPs with orbital distances smaller than $\sim$0.06 AU all have nearly circular orbits.

There seems to be a correlation between the probability of finding an EGP and the metallicity of its parent star. The “metallicity" of a star is the mass fraction of elements, such as carbon, oxygen, nitrogen, neon, magnesium, silicon and iron, that are heavier than helium. Hydrogen and helium predominate in stars and giant planets, comprising $\sim$98% by mass of the Sun. The more super-solar the heavy-element composition of the potential parent, the more likely we are to find 