  Abridged: Subaru Deep Field line-emitting galaxies in four narrow-band
filters at low and intermediate redshifts are presented. Broad-band colors,
follow-up optical spectroscopy, and multiple NB filters are used to distinguish
Ha, [O II], and [O III] emitters between redshifts of 0.07 and 1.47 to
construct their luminosity functions (LFs). These LFs are derived down to faint
magnitudes, which allows for a more accurate determination of the faint end
slope. With a large (N~200-900) sample for each redshift interval, a Schechter
profile is fitted to each LF. Prior to dust extinction corrections, the [O III]
and [O II] LFs reported in this paper agree reasonably well with those of
Hippelein et al. The z=0.08 Ha LF, which reaches two orders of magnitude
fainter than Gallego et al., is steeper by 25%. This indicates that there are
more low luminosity star-forming galaxies for z<0.1. The faint end slope \alpha
and \phi_{\star} show a strong evolution with redshift while L_{\star} show
little evolution. The evolution in \alpha indicates that low-luminosity
galaxies have a stronger evolution compared to brighter ones. Integrated star
formation rate densities are derived via Ha, [O III], and [O II] for
0.07<z<1.47. A steep increase in the star-formation rate density, as a function
of redshift, is seen for 0.4<z<0.9. For z>1, the star-formation rate densities
are more or less constant. The latter is consistent with previous UV and [O II]
measurements. Below z<0.4, the SFR densities are consistent with several Ha, [O
II], and UV measurements, but other measurements are a factor of two higher.
For example, the z=0.066-0.092 Ha LF agrees with those of Jones &
Bland-Hawthorn, but at z=0.24 and 0.40, their number density is higher by a
factor of two. This discrepancy can be explained by cosmic variance.
