  The CNO cycle is one of the most important nuclear energy sources in stars.
At temperatures of hydrostatic H-burning (20 MK $<$ T $<$ 80 MK) the
$^{17}$O(p,$\gamma$)$^{18}$F reaction rate is dominated by the poorly
constrained 64.5~keV resonance. Here we report on the first direct measurements
of its resonance strength and of the direct capture contribution at 142 keV,
performed with a new high sensitivity setup at LUNA. The present resonance
strength of $\omega\gamma_{(p, \gamma)}$\textsuperscript{bare} = (30 $\pm$
6\textsubscript{stat} $\pm$ 2\textsubscript{syst})~peV is about a factor of 2
higher than the values in literature, leading to a
$\Gamma$\textsubscript{p}\textsuperscript{bare} = (34 $\pm$
7\textsubscript{stat} $\pm$ 3\textsubscript{syst})~neV, in agreement with LUNA
result from the (p,$\alpha$) channel. Such agreement strengthen our
understanding of the oxygen isotopic ratios measured in red giant stars and in
O-rich presolar grains.
