Nature of the gas and dust around 51 Oph
  Circumstellar disc evolution is paramount for the understanding of planet
formation. The GASPS program aims at determining the circumstellar gas and
solid mass around ~250 pre-main-sequence Herbig Ae and TTauri stars. We aim to
understand the origin and nature of the circumstellar matter orbiting 51 Oph, a
young (<1 Myr) luminous B9.5 star. We obtained continuum and line observations
with the PACS instrument on board the Herschel Space Observatory and continuum
data at 1.2 mm with the IRAM 30m telescope. The SED and line fluxes were
modelled using the physico-chemo radiative transfer code ProDiMo. We detected a
strong emission by OI at 63 microns using the Herschel Space Observatory. The
[OI] emission at 145 microns, the [CII] emission at 158 microns, the high-J CO
emissions, and the warm water emissions were not detected. Continuum emission
was detected at 1.2 mm. The continuum from the near- to the far-infrared and
the [OI] emission are well explained by the emission from a compact hydrostatic
disc model with a gas mass of 5E-6 MSun, 100 times that of the solid mass.
However, this model fails to match the continuum millimeter flux, which hints
at a cold outer disc with a mass in solids of 1E-6 MSun or free-free emission
from a photoevaporative disc wind. This outer disc can either be devoid of gas
and/or is to cold to emit in the [OI] line. A very flat extended disc model
(Rout=400 AU) with a fixed vertical structure and dust settling matches all
photometric points and most of the [O I] flux. The observations can be
explained by an extended flat disc where dust grains have settled. However, a
flat gas disc cannot be reproduced by hydrostatic disc models. The low mass of
the 51 Oph inner disc in gas and dust may be explained either by the fast
dissipation of an initial massive disc or by a very small initial disc mass.
