Gas in the protoplanetary disc of HD 169142: Herschel's view

TL;DR

This study uses Herschel far-IR observations and modeling to analyze the gas and dust components of the protoplanetary disc around HD 169142, constraining its gas mass, composition, and structure.

Contribution

It provides the first combined gas and dust analysis of HD 169142 using Herschel data and advanced modeling, offering new constraints on disc properties.

Findings

Detected [OI] 63.2 micron line; other lines are upper limits.

Gas mass estimated at approximately 5.0 +/- 2.0 x 10^-3 solar masses.

Disc is consistent with well-mixed gas and dust in a continuous structure from 20 to 200 AU.

Abstract

In an effort to simultaneously study the gas and dust components of the disc surrounding the young Herbig Ae star HD 169142, we present far-IR observations obtained with the PACS instrument onboard the Herschel Space Observatory. This work is part of the Open Time Key Project GASPS, which is aimed at studying the evolution of protoplanetary discs. To constrain the gas properties in the outer disc, we observed the star at several key gas-lines, including [OI] 63.2 and 145.5 micron, [CII] 157.7 micron, CO 72.8 and 90.2 micron, and o-H2O 78.7 and 179.5 micron. We only detect the [OI] 63.2 micron line in our spectra, and derive upper limits for the other lines. We complement our data set with PACS photometry and 12/13CO data obtained with the Submillimeter Array. Furthermore, we derive accurate stellar parameters from optical spectra and UV to mm photometry. We model the dust continuum with the 3D radiative transfer code MCFOST and use this model as an input to analyse the gas lines with the thermo-chemical code ProDiMo. Our dataset is consistent with a simple model in which the gas and dust are well-mixed in a disc with a continuous structure between 20 and 200 AU, but this is not a unique solution. Our modelling effort allows us to constrain the gas-to-dust mass ratio as well as the relative abundance of the PAHs in the disc by simultaneously fitting the lines of several species that originate in different regions. Our results are inconsistent with a gas-poor disc with a large UV excess; a gas mass of 5.0 +/- 2.0 times 10^(-3) Msun is still present in this disc, in agreement with earlier CO observations.