Nature of the gas and dust around 51 Ophiuchi^⋆

Modelling continuum and Herschel line observations

¹ UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique (IPAG), UMR 5274, 38041 Grenoble, France
e-mail: Wing-Fai.Thi@obs.ujf-grenoble.fr
² UMI – LFCA, CNRS/INSU France, and Dept. de Astronomia y Obs. Astronomico Nacional, Universidad de Chile, Casilla 36-D, Correo Central, Santiago ( UMI 3386), Chile
³ Dep. de Física Teórica, Fac. de Ciencias, UAM Campus Cantoblanco, 28049 Madrid, Spain
⁴ Centro de Astrobiologa Depto. Astrofsica (CSICINTA), ESAC Campus, PO Box 78, 28691 Villanueva de la Canada, Spain
⁵ Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
⁶ SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK
⁷ Department of Physics and Astronomy, Clemson University, USA
⁸ ALMA, Avda Apoquindo 3846, Piso 19, Edicio Alsacia, Las Condes, Santiago, Chile

Received: 24 December 2012
Accepted: 16 April 2013

Abstract

Context. Circumstellar disc evolution is paramount for the understanding of planet formation. The gas in protoplanetary discs large program (GASPS) aims at determining the circumstellar gas and solid mass around ~250 pre-main-sequence Herbig Ae and T Tauri stars.

Aims. We aim to understand the origin and nature of the circumstellar matter orbiting 51 Oph, a young (<1 Myr) luminous B9.5 star.

Methods. 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 30 m telescope. The spectral energy distribution and line fluxes were modelled using the physico-chemo radiative transfer code ProDiMo to constrain the gas and solid mass of the disc around 51 Oph. The disc vertical hydrostatic structure was computed self-consistently together with the gas thermal balance.

Results. We detected a strong emission by atomic oxygen [O i] at 63 microns using the Herschel Space Observatory. The [O i] emission at 145 microns, the [C ii] 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 [O i] emission are well explained by the emission from a compact (R_out = 10–15 AU) hydrostatic disc model with a gas mass of 5 × 10^-6 M_⊙, 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 ~10^-6 M_⊙ or free-free emission from a photoevaporative disc wind. This outer disc can either be devoid of gas and/or is too cold to emit in the [O i] line. A very flat extended disc model (R_out = 400 AU) with a fixed vertical structure and dust settling matches all photometric points and most of the [O i] flux.

Conclusions. 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.