2010/05/20 by G. Meeus, C. Pinte, P. Woitke +70 · 48 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Infrared #Molecular Spectroscopy and Structure #Optics #Photometry (optics) #Physics #Radiative transfer #Space observatory #Spectral line #Star formation #Stars #Stellar, planetary, and galactic studies #Submillimeter Array #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201014557
published in Astronomy and Astrophysics 518, L124 (EDP Sciences) · 5 pages, 3 Postscript figures, accepted for publication in the A&A Herschel special issue
arxiv created 2010/05/20 · openalex publication_date 2010/07/01 · arxiv updated 2015/05/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 <i>Herschel<i/> Space Observatory. This work is part of the open time key program 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 <i>μ<i/>m, [CII] 157.7 <i>μ<i/>m, CO 72.8 and 90.2 <i>μ<i/>m, and o-H<sub>2<sub/>O 78.7 and 179.5 <i>μ<i/>m. We only detect the [OI] 63.2 <i>μ<i/>m line in our spectra, and derive upper limits for the other lines. We complement our data set with PACS photometry and <sup>12/13<sup/>CO 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 <i>±<i/> 2.0 × 10<sup>-3<sup/> is still present in this disc, in agreement with earlier CO observations.