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26 April 2024

» arxiv » 1005.3830

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Herschel-PACS observation of the 10 Myr old T Tauri disk TW Hya: Constraining the disk gas mass
W.F. Thi ; G. Mathews ; F. Ménard ; P. Woitke ; G. Meeus ; P. Riviere-Marichalar ; C. Pinte ; C. D. Howard ; A. Roberge ; G. Sandell ; I. Pascucci ; B. Riaz ; C. A. Grady ; W.R.F. Dent ; I. Kamp ; G. Duchêne ; J.C. Augereau ; E. Pantin ; B. Vandenbussche ; I. Tilling ; J. P. Williams ; C. Eiroa ; D. Barrado ; J. M. Alacid ; S. Andrews ; D.R. Ardila ; G. Aresu ; S. Brittain ; D.R. Ciardi ; W. Danchi ; D. Fedele ; I. de Gregorio-Monsalvo ; A. Heras ; N. Huelamo ; A. Krivov ; J. Lebreton ; R. Liseau ; C. Martin-Zaidi ; I. Mendigutía ; B. Montesinos ; A. Mora ; M. Morales-Calderon ; H. Nomura ; N. Phillips ; L. Podio ; D.R. Poelman ; S. Ramsay ; K. Rice ; E. Solano ; H. Walker ; G.J. White ; G. Wright ;
Date:	20 May 2010
Abstract:	Planets are formed in disks around young stars. With an age of ~10 Myr, TW Hya is one of the nearest T Tauri stars that is still surrounded by a relatively massive disk. In addition a large number of molecules has been found in the TW Hya disk, making TW Hya the perfect test case in a large survey of disks with Herschel-PACS to directly study their gaseous component. We aim to constrain the gas and dust mass of the circumstellar disk around TW Hya. We observed the fine-structure lines of [OI] and [CII] as part of the Open-time large program GASPS. We complement this with continuum data and ground-based 12CO 3-2 and 13CO 3-2 observations. We simultaneously model the continuum and the line fluxes with the 3D Monte-Carlo code MCFOST and the thermo-chemical code ProDiMo to derive the gas and dust masses. We detect the [OI] line at 63 micron. The other lines that were observed, [OI] at 145 micron and [CII] at 157 micron, are not detected. No extended emission has been found. Preliminary modeling of the photometric and line data assuming [12CO]/[13CO]=69 suggests a dust mass for grains with radius < 1 mm of ~1.9 times 10^-4 Msun (total solid mass of 3 times 10^-3 Msun) and a gas mass of (0.5--5) times 10^-3 Msun. The gas-to-dust mass may be lower than the standard interstellar value of 100.
Source:	arXiv, 1005.3830
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