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The  γ -ray strength function ( γ SF) is a nuclear quantity that governs photoabsorption in ( γ, n ) and photoemission in ( n, γ ) reactions. Within the framework of the  γ -ray strength function method, we use ( γ, n ) cross sections as experimental constraints on the  γ SF from the Hartree-Fock-Bogolyubov plus quasiparticle-random phase approximation based on the Gogny D1M interaction for E1 and M1 components. The experimentally constrained  γ SF is further supplemented with the zero-limit  M 1 and  E 1 strengths to construct the downward  γ SF with which ( n, γ ) cross sections are calculated. We investigate ( n, γ ) cross sections in the context of astrophysical applications over the nickel and barium isotopic chains along the s-process path.

γ-ray strength function for astrophysical applications in the IAEA-CRP