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The goal is to determine the composition of Pluto's atmosphere and toconstrain the nature of surface-atmosphere interactions.  We perform high--resolution spectroscopic observations in the 2.33--2.36$\mu$m range, using CRIRES at the VLT.  We obtain (i) the first detection of gaseous methane in this spectral range,through lines of the $\nu_3$ + $\nu_4$ and $\nu_1$ + $\nu_4$ bands (ii) strongevidence (6-$\sigma$ confidence) for gaseous CO in Pluto. For an isothermalatmosphere at 90 K, the CH$_4$ and CO column densities are 0.75 and 0.07 cm-am,within factors of 2 and 3, respectively. Using a physically--based thermalstructure model of Pluto's atmosphere also satisfying constraints from stellaroccultations, we infer CH$_4$ and CO mixing ratios q$_{CH_4}$=0.6$^{+0.6}_{-0.3}$% (consistent with results from the 1.66 $\mu$m range) andq$_{CO}$ = 0.5$^{+1}_{-0.25}$$\times10^{-3}$. The CO atmospheric abundance isconsistent with its surface abundance. As for Triton, it is probably controlledby a thin, CO-rich, detailed balancing layer resulting from seasonal transportand/or atmospheric escape.

High resolution spectroscopy of Pluto's atmosphere: detection of the 2.3 $\mu$m CH$_4$ bands and evidence for carbon monoxide