  We show how, based on considerations on the observed form of the galaxy
2-point spatial correlation function xi(r), a very simplified -- yet
surprisingly effective -- model for the linear density fluctuations power
spectrum can be constructed. We first relate the observed large-scale shape of
xi(r) to a power-law form for the power spectrum, P(k)\propto k^{-2.2}. For a
plausible value of the bias parameter b = 1/sigma_8 ~ 1.8, one has (delta_rho /
rho)_{rms} ~ 1 r ~ 3.5/h Mpc, suggesting that the change of slope observed in
xi(r) around this scale marks the transition between the linear and nonlinear
gravitational regimes. Under this working hypothesis, we use a simple
analytical form to fit the large-scale correlations constraints together with
the COBE CMB anisotropy measurement, thus constructing a simple
phenomenological model for the linear power spectrum. Despite its simplicity,
the model fits remarkably well directly estimated power spectra from different
optical galaxy samples, and when evolved through an N-body simulation it
provides a good match to the observed galaxy correlations. One of the most
interesting features of the model is the small-scale one-dimensional velocity
dispersion produced: sigma_{1d} = 450 Km s^{-1} at 0.5/h Mpc and sigma_{1d} =
350 Km s^{-1} for separations larger than ~ 2/h Mpc.
