Extending the earlier work of Bateman et al., we have measured the energy-integrated yield of ${}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ from the ${}^{16}\mathrm{O}{(}^{16}\mathrm{O}{,x)}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ and ${}^{16}\mathrm{O}{(}^{14}\mathrm{N}{,x)}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ reactions. We find that although the yield from the ${}^{16}\mathrm{O}{(}^{16}\mathrm{O}{,x)}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ reaction is several times larger than from the ${}^{12}\mathrm{C}{(}^{16}\mathrm{O}{,x)}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ reaction, the abundance of fossil ${}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ observed in carbonaceous chondrite meteorites could be produced by oxygen-rich cosmic rays via the ${}^{16}\mathrm{O}{(}^{16}\mathrm{O}{,x)}^{26}{\mathrm{Al}}_{\mathrm{g}.\mathrm{s}.}$ reaction only under the improbable scenario that more than 40% of the solar system oxygen was injected into the protosolar nebula as cosmic rays.