  [Abridged] Recently, there have been a series of detections of molecules in
the atmospheres of extrasolar planets using high spectral resolution
(R~100,000) observations, mostly using the CRyogenic high-resolution InfraRed
Echelle Spectrograph (CRIRES) on the Very Large Telescope. These measurements
are able to resolve molecular bands into individual absorption lines. Observing
many lines simultaneously as their Doppler shift changes with time allows the
detection of specific molecules in the atmosphere of the exoplanet. We
performed simulations of high-resolution CRIRES observations of a planet's
thermal emission and transit between 1-5 micron and performed a
cross-correlation analysis on these results to assess how well the planet
signal can be extracted. We also simulated day-side and night-side spectra at
high spectral resolution for planets with and without a day-side temperature
inversion, based on the cases of HD 189733b and HD 209458b. Several small
wavelength regions in the L-band promise to yield cross-correlation signals
from the thermal emission of hot Jupiters that can exceed those of the current
detections by up to a factor of 2-3 for the same integration time. For transit
observations, the H-band is also attractive, with the H, K, and L-band giving
cross-correlation signals of similar strength. High-resolution night-side
spectra of hot Jupiters can give cross-correlation signals as high as the
day-side, or even higher. We show that there are many new possibilities for
high-resolution observations of exoplanet atmospheres that have expected planet
signals at least as high as those already detected. Hence, high-resolution
observations at well-chosen wavelengths and at different phases can improve our
knowledge about hot Jupiter atmospheres significantly, already with currently
available instrumentation.
