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The Ursa Major group is a nearby stellar supercluster which, while notgravitationally bound, is defined by co-moving members. DD UMa is a $\delta$Scuti star whose membership in the Ursa Major group is unclear.  The objective of this study is to confirm the membership of DD UMa in theUrsa Major group, as well as perform a detailed spectral analysis of the star.Since DD UMa is a low-amplitude $\delta$ Scuti star, we performed a frequencyanalysis. We determined fundamental parameters, chemical abundances, and derivea mass and age for the star.  For this study we observed DD UMa at the Okayama Astrophysical Observatorywith the high-resolution spectrograph HIDES, between the $27^{th}$ of Februaryand the $4^{th}$ March, 2009. Additional observations were extracted from theELODIE archive in order to expand our abundance analysis. Group membership ofDD UMa was assessed by examining the velocity of the star in Galacticcoordinates. Pulsational frequencies were determined by examining line profilevariability in the HIDES spectra. Stellar fundamental parameters and chemicalabundances were derived by fitting synthetic spectra to both the HIDES andELODIE observations.  DD UMa is found to be a member of the extended stream of the Ursa Majorgroup, based on the space motion of the star. This is supported by the chemicalabundances of the star being consistent with those of Ursa Major group members.The star is found to be chemically solar, with $T_{eff}=7450\pm150$ K and $\logg=3.98\pm0.2$. We found pulsational frequencies of 9.4 c/d and 15.0 c/d. Whilethese frequencies are insufficient to perform an asteroseismic study, DD UMa isa good bright star candidate for future study by the BRITE-constellation.

A Spectroscopic Study of DD UMa: Ursa Major Group Member and Candidate for BRITE