  The spectrum of the quasar PHL 1226 is known to have a strong Mg II and
sub-damped Lyman-alpha (sub-DLA) absorption line system with
N(HI)=(5+/-2)*10^19 cm^-2 at z=0.1602. Using integral field spectra from the
Potsdam Multi Aperture Spectrophotometer (PMAS) we investigate a galaxy at an
impact parameter of 6".4 which is most probably responsible for the absorption
lines. A fainter galaxy at a similar redshift and a slightly larger distance
from the QSO is known to exist, but we assume that the absorption is caused by
the more nearby galaxy. From optical Balmer lines we estimate an intrinsic
reddening consistent with 0, and a moderate star formation rate of 0.5 M_sun
yr^-1, is inferred from the Halpha luminosity. Using nebular emission line
ratios we find a solar oxygen abundance 12+log(O/H)=8.7+/-0.1 and a solar
nitrogen to oxygen abundance ratio log(N/O)=-1.0+/-0.2. This abundance is
larger than those of all known sub-DLA systems derived from analyses of metal
absorption lines in quasar spectra. On the other hand, the properties are
compatible with the most metal rich galaxies responsible for strong Mg II
absorption systems. These two categories can be reconciled if we assume an
abundance gradient similar to local galaxies. Under that assumption we predict
abundances 12+log(O/H)=7.1 and log(N/O)=-1.9 for the sub-DLA cloud, which is
similar to high redshift DLA and sub-DLA systems. We find evidence for a
rotational velocity of ~200 km s^-1 over a length of ~7 kpc. From the geometry
and kinematics of the galaxy we estimate that the absorbing cloud does not
belong to a rotating disk, but could originate in a rotating halo.
