  The Herschel Space Observatory was used to observe ~ 120 pre-main-sequence
stars in Taurus as part of the GASPS Open Time Key project. PACS was used to
measure the continuum as well as several gas tracers such as [OI] 63 \mu m,
[OI] 145 \mu m, [CII] 158 \mu m, OH, H2O and CO. The strongest line seen is
[OI] at 63 \mu m. We find a clear correlation between the strength of the [OI]
63 \mu m line and the 63 \mu m continuum for disk sources. In outflow sources,
the line emission can be up to 20 times stronger than in disk sources,
suggesting that the line emission is dominated by the outflow. The tight
correlation seen for disk sources suggests that the emission arises from the
inner disk ($<$ 50 AU) and lower surface layers of the disk where the gas and
dust are coupled. The [OI] 63 \mu m is fainter in transitional stars than in
normal Class II disks. Simple SED models indicate that the dust responsible for
the continuum emission is colder in these disks, leading to weaker line
emission. [CII] 158 \mu m emission is only detected in strong outflow sources.
The observed line ratios of [OI] 63 \mu m to [OI] 145 \mu m are in the regime
where we are insensitive to the gas-to-dust ratio, neither can we discriminate
between shock or PDR emission. We detect no Class III object in [OI] 63 \mu m
and only three in continuum, at least one of which is a candidate debris disk.
