${}^{26}\mathrm{Al}$ remains an intriguing target for observational $\gamma$-ray astronomy, thanks to its characteristic decay. The ${}^{25}\mathrm{Al}\left(p,\gamma \right){}^{26}\mathrm{Si}$ reaction is the crucial link in a sequence that bypasses the production of the observable ${}^{26}\mathrm{Al}^g$ in favor of the short-lived isomeric state; determining its astrophysical reaction rate across a range of stellar environments has been the focus of many studies. A reanalysis of previous work, utilizing recent improvements in excitation energies and ground state masses, is presented to reduce the ambiguities in the literature and provide focus to future measurements.

• Received 23 April 2015
• Revised 13 November 2015

DOI:https://doi.org/10.1103/PhysRevC.93.035801