  We present a detailed study of the optical and NIR emission and absorption
line spectrum of the quasar SDSS J163345.22+512748.4. We discovered on the
newly acquired NIR spectrum a highly meta-stable neutral helium broad
absorption line (BAL) \heiozetz\ with a width of $\sim$ 2000 \kmps\ and a
blueshift of $\sim$ 7000 \kmps\ in the velocity space. The BAL system is also
significantly detected in \mgii\ and \heiteen. We estimate a column density of
$(5.0 \pm 1.7) \times 10^{14}$ cm$^{-2}$ for the HeI*(2~$^3$S) level, and infer
an ionization parameter of $U_{A} = 10^{-1.9\pm 0.2}$ for the BAL outflow
assuming that the BAL region is thick enough for a full development of an
ionization front. The total column density of the BAL outflow is constrained in
the range N$\rm _{H}$ $\sim$ 10$^{21}$-10$^{21.4}$ cm$^{-2}$. We also found
that the bulk of both MgII and UV FeII, as well as H$\alpha$ broad emission
lines (BELs) are blueshifted with a velocity of $\sim$ 2200 \kmps\ with respect
to the quasar systemic redshift. We constrain that the blueshifted BEL region
has a covering factor $C_{f}\approx 16\%$, a density n$\rm _{H}$ $\sim $
10$^{10.6}$-10$^{11.3}$ cm$^{-3}$, a column density N$\rm _{H}\gtrsim 10^{23}$
cm$^{-2}$, and an ionization parameter $U_{E}\sim 10^{-2.1}-10^{-1.5}$. The
outflow gas is located at $\sim$0.1 pc away from the central ionization source,
at a scale comparable to the BLR. A toy kinetic model has been proposed to
reproduce the profile of MgII BEL well if assuming a partial obscured
axisymmetric geometry of the outflow with a radial velocity as observed by the
BALs.
