Protostars and Planets VI, Heidelberg, July 15-20, 2013

Poster 2S021

Herschel-PACS observation of gas lines from the disc around HD141569A

Thi, Wing-Fai (UJF-Grenoble/CNRS-INSU, IPAG)
Pinte, Christophe (UJF-Grenoble/CNRS-INSU, IPAG)
Pantin, Eric (Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, IRFU/SAP)
Augereau, Jean-Charles (UJF-Grenoble/CNRS-INSU, IPAG)
Meeus, Gwendolyn (Dep. de Física Teórica, Fac. de Ciencias, UAM Campus Cantoblanco)
Ménard, Francois (UMI – LFCA, CNRS / INSU France, and Dept. de Astronomia y Obs. Astronomico Nacional, Universidad de Chile)
Martin-Zaidi, Claire (UJF-Grenoble/CNRS-INSU, IPAG)
Woitke, Peter (SUPA, School of Physics & Astronomy, University of St. Andrews)
Riviere-Marichalar, Pablo (Kapteyn Astronomical Institute)
Kamp, Inga (Kapteyn Astronomical Institute)
Carmona, Andres (UJF-Grenoble/CNRS-INSU, IPAG)
Sandell, Goran (SOFIA-USRA, NASA Ames Research Center)
Eiroa, Carlos (Dep. de Física Teórica, Fac. de Ciencias, UAM Campus Cantoblanco)
Dent, William (ALMA,)
Montesinos, Benjamin (Dep. de Física Teórica, Fac. de Ciencias, UAM Campus Cantoblanco)
Aresu, Giambattista (Kapteyn Astronomical Institute)
Meijerink, Rowin (Kapteyn Astronomical Institute)
Spaans, Marco (Kapteyn Astronomical Institute)
White, Glenn (Astrophysics Group, Department of Physics & Astronomy, The Open University, RAL)
Ardila, David (NASA Herschel Science Center, California Institute of Technology)
Lebreton, Jeremy (UJF-Grenoble/CNRS-INSU, IPAG)
Mendigutia, Ignacio (Clemson University)
Brittain, Sean (Clemson University)

At the distance of ∼ 99–116 pc, HD141569A is one of the nearest HerbigAe stars that is surrounded by a tenuous disc, probably in transition between a massive primordial disc and a debris disc. We observed the fine-structure lines of O I at 63 and 145 μm , and the C II line at 157 μm with the PACS instrument on board the Herschel Space Telescope as part of the open-time large programme GASPS. We complemented the atomic line observations with Spitzer spectroscopic and photometric continuum data, ground-based VLT-VISIR image at 8.6 microns, and 12CO J=3–2 observations. We simultaneously modelled the continuum emission and the line fluxes with the Monte-Carlo radiative transfer code MCFOST and the thermo-chemical code ProDiMo to derive the disc gas and dust properties. We modelled the [O I] lines at 63 μm and at 145 μm, and the [C II] line at 157 μm. The models show that the oxygen lines are emitted from the inner disc around HD141569A, whereas the [C II] line emission is more extended. The CO submillimeter flux is emitted from the outer disc. Simultaneous modelling of the photometric and line data using a realistic disc structure suggests a dust mass derived from grains having a radius less than 1 mm of ∼ 2.1 × 10−7M⊙ and a total solid mass of 4.9 × 10−6 M⊙ . We constrained the PAH mass to be between 2 × 10−11 and 1.4 × 10−10 M⊙ depending on the size of the PAH. The associated PAH abundance is lower than those found in the interstellar medium by two to three orders of magnitude. The gas mass is a few 10−4M⊙. We constrained simultaneously the silicate dust grain, PAH, and gas mass in an evolved Herbig Ae disc. The uncertainty on the gas mass is large (around a factor 5) because the different gas tracers give estimates that do not agree with each other.

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