[OIII] Emission Line Properties in a New Sample of Heavily Reddened
  Quasars at $z>2$
  We present VLT-SINFONI near infra-red spectra of 26 new heavily reddened
quasar candidates selected from the UKIDSS-LAS, VISTA VHS and VIKING imaging
surveys. This new sample extends our reddened quasar search to both brighter
and fainter luminosities. 25 of the 26 candidates are confirmed to be broad
line quasars with redshifts $0.7<z<2.6$ and dust extinctions $0.5<E(B-V)<3.0$.
Combining with previously identified samples, we study the H$\alpha$, H$\beta$
and [OIII] emission line properties in 22 heavily reddened quasars with
$L_{bol}\approx 10^{47}$ erg/s and $z>2$. We present the first comparison of
the [OIII] line properties in high luminosity obscured quasars to a large
sample of 111 unobscured quasars in the same luminosity and redshift range.
Broad wings extending to velocities of 2500 km/s are seen in the [OIII]
emission line profiles of our reddened quasars, suggesting that strong outflows
are affecting the ionised gas kinematics. However, we find no significant
difference between the kinematics of the [OIII] emission in reddened and
unobscured quasars when the two samples are matched in luminosity and redshift.
Our results are consistent with a model where quasar-driven outflows persist
for some time after the obscuring dust has been cleared from along the line of
sight. Assuming the amount of ionised gas in obscured and unobscured quasars is
similar, we use the equivalent width distribution of the [OIII] emission to
constrain the location of the obscuring dust in our reddened quasars. We find
that the dust is most likely to be located on galactic scales, outside the
[OIII] emitting region.
