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The $^{14}\textrm{N(p,}\gamma\textrm{)}^{15}\textrm{O}$ reaction is theslowest reaction of the carbon-nitrogen cycle of hydrogen burning and thusdetermines its rate. The precise knowledge of its rate is required to correctlymodel hydrogen burning in asymptotic giant branch stars. In addition, it is anecessary ingredient for a possible solution of the solar abundance problem byusing the solar $^{13}$N and $^{15}$O neutrino fluxes as probes of the carbonand nitrogen abundances in the solar core. After the downward revision of itscross section due to a much lower contribution by one particular transition,capture to the ground state in $^{15}$O, the evaluated total uncertainty isstill 8\%, in part due to an unsatisfactory knowledge of the excitationfunction over a wide energy range. The present work reports precise S-factordata at twelve energies between 0.357-1.292~MeV for the strongest transition,capture to the 6.79~MeV excited state in $^{15}$O, and at ten energies between0.479-1.202~MeV for the second strongest transition, capture to the groundstate in $^{15}$O. An R-matrix fit is performed to estimate the impact of thenew data on astrophysical energies. The recently suggested slight enhancementof the 6.79~MeV transition at low energy could not be confirmed. The presentextrapolated zero-energy S-factors are $S_{6.79}(0)$~=~1.24$\pm$0.11~keV~barnand $S_{\rm GS}(0)$~=~0.19$\pm$0.05~keV~barn.

Astrophysical S-factor of the $^{14}\textrm{N(p,}\gamma\textrm{)}^{15}\textrm{O}$ reaction at 0.4 -- 1.3\,MeV