  Photometric observations made by the NASA Kepler Mission have led to a
dramatic increase in the number of main-sequence and subgiant stars with
detected solar-like oscillations. We present an ensemble asteroseismic analysis
of 76 solar-type stars. Using frequencies determined from the Kepler
time-series photometry, we have measured three asteroseismic parameters that
characterize the oscillations: the large frequency separation (\Delta \nu), the
small frequency separation between modes of l=0 and l=2 (\delta \nu_02), and
the dimensionless offset (\epsilon). These measurements allow us to construct
asteroseismic diagrams, namely the so-called C-D diagram of \delta \nu_02
versus \Delta \nu, and the recently re-introduced {\epsilon} diagram. We
compare the Kepler results with previously observed solar-type stars and with
theoretical models. The positions of stars in these diagrams places constraints
on their masses and ages. Additionally, we confirm the observational
relationship between {\epsilon} and T_eff that allows for the unambiguous
determination of radial order and should help resolve the problem of mode
identification in F stars.
