  The Ursa Major group is a nearby stellar supercluster which, while not
gravitationally 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 the
Ursa 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 frequency
analysis. We determined fundamental parameters, chemical abundances, and derive
a mass and age for the star.
  For this study we observed DD UMa at the Okayama Astrophysical Observatory
with the high-resolution spectrograph HIDES, between the $27^{th}$ of February
and the $4^{th}$ March, 2009. Additional observations were extracted from the
ELODIE archive in order to expand our abundance analysis. Group membership of
DD UMa was assessed by examining the velocity of the star in Galactic
coordinates. Pulsational frequencies were determined by examining line profile
variability in the HIDES spectra. Stellar fundamental parameters and chemical
abundances were derived by fitting synthetic spectra to both the HIDES and
ELODIE observations.
  DD UMa is found to be a member of the extended stream of the Ursa Major
group, based on the space motion of the star. This is supported by the chemical
abundances 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 $\log
g=3.98\pm0.2$. We found pulsational frequencies of 9.4 c/d and 15.0 c/d. While
these frequencies are insufficient to perform an asteroseismic study, DD UMa is
a good bright star candidate for future study by the BRITE-constellation.
