Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science . Specifically , eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models . By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry , we find two new eclipsing binaries , TYC 0272-00458-1 and TYC 1422-01328-1 , which we use as case studies to develop a general approach to eclipsing binaries in survey data . TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques . For a primary mass of M _ { 1 } = 0.92 \pm 0.1 ~ { } M _ { \odot } , we find M _ { 2 } = 0.610 \pm 0.036 ~ { } M _ { \odot } , R _ { 1 } = 0.932 \pm 0.076 ~ { } R _ { \odot } and R _ { 2 } = 0.559 \pm 0.102 ~ { } R _ { \odot } , and find that both stars have masses and radii consistent with model predictions . TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair . We find that the eclipsing pair consists of an evolved primary star ( M _ { 1 } = 1.163 \pm 0.034 ~ { } M _ { \odot } , R _ { 1 } = 2.063 \pm 0.058 ~ { } R _ { \odot } ) and a G-type dwarf secondary ( M _ { 2 } = 0.905 \pm 0.067 ~ { } M _ { \odot } , R _ { 2 } = 0.887 \pm 0.037 ~ { } R _ { \odot } ) . We provide the framework necessary to apply this analysis to much larger datasets .