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The origin of fluorine is a widely debated issue. Nevertheless, the^{15}N({\alpha},{\gamma})^{19}F reaction is a common feature among the variousproduction channels so far proposed. Its reaction rate at relevant temperaturesis determined by a number of narrow resonances together with the DC componentand the tails of the two broad resonances at E_{c.m.} = 1323 and 1487 keV.Measurement through the direct detection of the 19F recoil ions with theEuropean Recoil separator for Nuclear Astrophysics (ERNA) were performed. Thereaction was initiated by a 15N beam impinging onto a 4He windowless gastarget. The observed yield of the resonances at Ec.m. = 1323 and 1487 keV isused to determine their widths in the {\alpha} and {\gamma} channels. We showthat a direct measurement of the cross section of the^{15}N({\alpha},{\gamma})^{19}F reaction can be successfully obtained with theRecoil Separator ERNA, and the widths {\Gamma}_{\gamma} and {\Gamma}_{\alpha}of the two broad resonances have been determined. While a fair agreement isfound with earlier determination of the widths of the 1487 keV resonance, asignificant difference is found for the 1323 keV resonance {\Gamma}_{\alpha} .The revision of the widths of the two more relevant broad resonances in the15N({\alpha},{\gamma})19F reaction presented in this work is the first steptoward a more firm determination of the reaction rate. At present, the residualuncertainty at the temperatures of the ^{19}F stellar nucleosynthesis isdominated by the uncertainties affecting the Direct Capture component and the364 keV narrow resonance, both so far investigated only through indirectexperiments.

Measurement of 1323 and 1487 keV resonances in 15N({\alpha}, {\gamma})19F with the recoil separator ERNA