  We have carried out a search for the 2.14 micron spectroscopic signature of
the close orbiting extrasolar giant planet, HD 179949b. High cadence time
series spectra were obtained with the CRIRES spectrograph at VLT1 on two
closely separated nights. Deconvolution yielded spectroscopic profiles with
mean S/N ratios of several thousand, enabling the near infrared contrast ratios
predicted for the HD 179949 system to be achieved.
  Recent models have predicted that the hottest planets may exhibit spectral
signatures in emission due to the presence of TiO and VO which may be
responsible for a temperature inversion high in the atmosphere. We have used
our phase dependent orbital model and tomographic techniques to search for the
planetary signature under the assumption of an absorption line dominated
atmospheric spectrum, where T and V are depleted from the atmospheric model,
and an emission line dominated spectrum, where TiO and VO are present.
  We do not detect a planet in either case, but the 2.120 - 2.174 micron
wavelength region covered by our observations enables the deepest near infrared
limits yet to be placed on the planet/star contrast ratio of any close orbiting
extrasolar giant planet system. We are able to rule out the presence of an
atmosphere dominated by absorption opacities in the case of HD 179949b at a
contrast ratio of F_p/F_* ~ 1/3350, with 99 per cent confidence.
