  High-resolution Doppler spectroscopy provides an avenue to study the
atmosphere of both transiting and non-transiting planets. This powerful method
has also yielded some of the most robust atmospheric detections to date.
Currently, high-resolution Doppler spectroscopy detects atmospheric signals by
cross-correlating observed data with a model atmospheric spectrum. This
technique has been successful in detecting various molecules such as H2O, CO,
HCN and TiO, as well as several atomic species. Here we present an alternative
method of performing high-resolution Doppler spectroscopy, using a technique
known as Doppler tomography. We present an analysis of HD 179949 b using
Doppler tomography and provide Doppler tomograms confirming previous detections
of CO at 2.3 microns, and H2O at both 2.3 microns, and 3.5 microns within the
atmosphere of HD 179949 b, showing significantly lower background noise levels
when compared to cross-correlation methods applied to the same data. We also
present a novel detection of H2O at 2.1 microns, as well as a tentative
detection of CO on the night side of the planet at 2.3 microns. This represents
the first observational evidence for molecular absorption in the night-side
emission spectrum of an exoplanet using Doppler spectroscopy.
