Cross Section Measurements for 34S($\alpha $,$\gamma )$

Some massive stars will go through a stage of~explosive oxygen burning which commences with conversion of $^{16}$O and $^{24}$Mg to~$^{28}$Si. When the $^{24}$Mg becomes exhausted, a network of reactions ranging from $^{28}$Si to $^{40}$Ca is initiated. Final abundances of most of the neutron-rich nuclides in this mass region depend in varying amounts on the cross sections of reactions involving $^{34}$S and $^{38}$Ar, particularly those of $\alpha $-capture. Astrophysical reaction rates are dominated by the isolated resonances within the Gamow windows. Often statistical modeling is used instead for reaction rate calculations though there is typically a large discrepancy between these calculations and experimental determinations. For $\alpha $-capture onto $^{34}$S there are discrepancies between experimental measurements that have never been resolved. Also, unstudied states exist around the Gamow window that could be resonances for alpha capture. A recent measurement was done using DRAGON at TRIUMF to resolve these discrepancies and to search for new resonances. Experimental data will be shown and preliminary results discussed.