  Given a redshift survey of galaxies with measurements of apparent magnitudes,
we present a novel method for measuring the growth rate $f(\Omega)$ of
cosmological linear perturbations. We use the galaxy distribution within the
survey to solve for the peculiar velocity field which depends in linear
perturbation theory on $\beta=f(\Omega)/b$, where $b$ is the bias factor of the
galaxy distribution. The recovered line-of-sight peculiar velocities are
subtracted from the redshifts to derive the distances, which thus allows an
estimate of the absolute magnitude of each galaxy. A constraint on $\beta$ is
then found by minimizing the spread of the estimated magnitudes from their
distribution function. We apply the method to the all sky $K = 11.25$ Two-MASS
Redhsift Survey (2MRS) and derive $\beta=0.35\pm 0.1$ at $z\sim 0$, remarkably
consistent with our previous estimate from the velocity-velocity comparison.
The method could easily be applied to subvolumes extracted from the SDSS survey
to derive the growth rate at $z \sim 0.1$. Further, it should also be
applicable to ongoing and future spectroscopic redshift surveys to trace the
evolution of $f(\Omega)$ to $z\sim1$. Constraints obtained from this method are
entirely independent from those obtained from the two-dimensional distortion of
$\xi(s)$ and provide an important check on $f(\Omega)$, as alternative gravity
models predict observable differences.
