The ${}^{13}\mathrm{C}(p,\gamma ){}^{14}\mathrm{N}$ reaction is the second reaction of the CNO cycle. This cycle takes place in our Sun and fuels massive, red, and asymptotic giant branch stars. The ${}^{13}\mathrm{C}(p,\gamma ){}^{14}\mathrm{N}$ rate affects the final abundances of ${}^{12,13}\mathrm{C}$ and ${}^{19}\mathrm{F}$ nuclides, with impact on our understanding of the $i$ and $s$ process, giant star nucleosynthesis and mixing processes, and ultimately the chemical evolution of the galaxy. Here, we report on a new measurement of the ${}^{13}\mathrm{C}(p,\gamma ){}^{14}\mathrm{N}$ cross section, which has been performed at the Felsenkeller shallow underground laboratory in Dresden (Germany). The present $S$-factor results agree at low energy with LUNA data but are about 20% lower than previous literature data over the whole energy range explored, $E=310-680\mathrm{keV}$. The narrow resonance corresponding to the 7966.9(5) keV excited state has been investigated and we report a new resonance strength, $\omega \gamma =18\left(2\right)\mathrm{meV}$. In addition, a new $R$-matrix fit is presented, from which new parameters for the broad resonance corresponding to the 8062.0(10) keV excited state are derived and a new extrapolation for the total $S$ factor down to zero energy is obtained, $S_{\mathrm{tot}}\left(0\right)=6.4\left(4\right)\mathrm{keV}$ b. Finally a new reaction rate is calculated and reported here.

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• Hydrostatic stellar nucleosynthesis
• Nuclear astrophysics
• Nuclear reactions
• Radiative capture
• Resonance reactions
• S-factor
• 6 ≤ A ≤ 19