not yet known, absorbs in the blue and creates the reddish cast of both Jupiter and Saturn, lowering their albedos shortward of 0.55 by a factor of $\sim$1.5–2. (Chromophores were not modelled to produce Fig. 2.)

As Fig. 2 suggests, the planet/star contrast ratio is better in the mid- to far-infrared, particularly at wide separations. For such separations, the contrast ratio in the optical can sink to 10$^{-10}$. For the closest-in EGPs, such as HD209458b, OGLE-TR56b, 51 Peg b, and $\tau$ Boo b, the contrast ratio in the optical is between 10$^{-5}$ and 10$^{-6}$ and is more favorable. Such EGPs are not shown in Fig. 2; there are in fact about 20 known EGPs with orbital distances less than 0.08 AU. Due to the possible formation of iron clouds in their atmospheres, HD209458b and OGLE-TR56b may be brighter in the optical than 51 Peg b and may have higher reflection albedos. Figure 3 portrays a generic absolute flux spectrum at 10 parsecs of a close-in EGP (“Class V" in the nomenclature of Sudarsky et al.[@Sudarsky00]), not unlike HD209458b. Highlighted are the positions of some of the important spectral features. Since modern telescopes can easily detect fluxes at the milliJansky level, 