Herschel-PACS observations of far-IR lines in YSOs I: [OI] and H2O at 63
  microns
  Gas plays a major role in the dynamical evolution of young stellar objects.
Its interaction with the dust is the key to our understanding planet formation
later on in the protoplanetary disc stage. Studying the gas content is a
crucial step towards understanding YSO and planet formation. Such a study can
be made through spectroscopic observations of emission lines in the
far-infrared, where some of the most important gas coolants emit. We provide a
compilation of observations of far-IR lines in 362 young stellar objects
covering all evolutionary stages, from Class 0 to Class III with debris discs.
In the present paper we focus on [OI] and o-H2O emission at 63 microns. We have
retrieved all the available Herschel -PACS spectroscopic observations at 63
microns that used the dominant observing mode, the chop-nod technique. We
provide measurements of line fluxes for the [OI] 3P1-3P2 and o-H2O 808-717
transitions at 63 microns computed using different methods. We check for
spatially extended emission and further study the presence of multiple
dynamical components in line emission. The final compilation consists of line
and continuum fluxes at 63 microns for a total of 362 young stellar objects
(YSOs). We detected [OI] line emission at 63 microns in 194 sources out of 362,
and line absorption in another five sources. o-H2O was detected in 42 sources.
We find evidence of extended [OI] emission in 77 sources, and detect 3sigma
residual emission in 71 of them. We also looked for different components
contributing to the line emission, and found evidence for multiple components
in 30 sources. We explored correlations between line emission and continuum
emission and find a clear correlation between WISE fluxes from 4.6 to 22
microns and [OI] line emission. We conclude that the observed emission is
typically a combination of disc/envelope and jet emission.
