  Since October of 1995, employing Doppler spectroscopy astronomers have
discovered as many as 20 giant planets and brown dwarfs, including companions
to $\tau$ Boo, 51 Peg, $\upsilon$ And, 55 Cnc, $\rho$ CrB, 70 Vir, 16 Cyg B,
and 47 UMa. These discoveries have excited the planetary science community,
astronomers, and the public at large. Within hours of the announcement of the
planet 51 Peg b, the first direct detection of an unimpeachable brown dwarf,
Gl229 B, was also announced. Gl229 B is a watershed since it has methane
spectral features and a surface temperature below 1000 Kelvin, characteristics
unique to objects with substellar masses.
  During the last two years, building upon our previous experience in the
modeling of brown dwarfs and M stars, we published theoretical studies of the
evolution and spectra of extrasolar giant planets. We have recently upgraded
our capabilities and now generate non-gray spectral and color models of both
giant planets and brown dwarfs. This theory will soon encompass objects whose
effective temperatures range from 100 K to 4000 K and whose masses span three
orders of magnitude. The evolutionary, spectral, and color calculations upon
which we have embarked are in direct support of the searches now being planned
in earnest with the HST (WFPC2, NICMOS), the IRTF, the MMT 6.5-meter upgrade,
the LBT, Keck's I and II, ISO, UKIRT, NGST, the VLT, COROT, DENIS, 2MASS, and
SIRTF.
