A Bayesian analysis of the astrophysical factor for the fusion reaction is presented using available low-energy information at carbon–carbon relative energies , including direct measurements and recent inverse-kinematics data. The goal of the global Bayesian fit is not to reproduce the local resonance-by-resonance structure of the system, but rather to constrain the smooth global component of using the direct and inverse-kinematics constraints. The resulting posterior lies systematically below the traditional FCZ75 reference normalization over the energy interval considered. For example, at the median posterior value is , whereas the Fowler–Caughlan–Zimmerman reference value is [W.~A. Fowler, G.~R. Caughlan, and B.~A. Zimmerman, Annu. Rev. Astron. Astrophys. , 69 (1975)]. Thus, the updated posterior favors a lower smooth low-energy trend and does not support a sharp increase of as the energy decreases. The astrophysical consequence of the analysis is assessed through the thermonuclear reaction rate . The resulting median rate is lower than the CF88 analytic rate [G.~R. Caughlan and W.~A. Fowler, At. Data Nucl. Data Tables , 283 (1988)] over the temperature interval considered, with – for . At higher temperatures, where the Gamow window extends above the upper end of the adopted integration interval, the calculated rate should be regarded as a truncated rate rather than a complete stellar rate.

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