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        Herschel-PACS observation of the 10 Myr old T Tauri disk TW Hya Constraining the disk gas mass

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        Author
        Thi, W. -F.
        Mathews, G.
        Menard, F.
        Woitke, P.
        Meeus, G.
        Riviere-Marichalar, P.
        Pinte, C.
        Howard, C. D.
        Roberge, A.
        Sandell, G.
        Pascucci, I.
        Riaz, B.
        Grady, C. A.
        Dent, W. R. F.
        Kamp, I.
        Duchene, G.
        Augereau, J. -C.
        Pantin, E.
        Vandenbussche, B.
        Tilling, I.
        Williams, J. P.
        Eiroa, C.
        Barrado, D.
        Alacid, J. M.
        Andrews, S.
        Ardila, D. R.
        Aresu, G.
        Brittain, S.
        Ciardi, D. R.
        Danchi, W.
        Fedele, D.
        de Gregorio-Monsalvo, I.
        Heras, A.
        Huelamo, N.
        Krivov, A.
        Lebreton, J.
        Liseau, R.
        Martin-Zaidi, C.
        Mendigutia, I.
        Montesinos, B.
        Mora, A.
        Morales-Calderon, M.
        Nomura, H.
        Phillips, N.
        Podio, L.
        Poelman, D. R.
        Ramsay, S.
        Rice, K.
        Solano, E.
        Walker, H.
        White, G. J.
        Wright, G.
        Attention
        2299/7278
        Abstract
        Planets are formed in disks around young stars. With an age of similar to 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 (12) CO 3-2 and (CO)-C-13 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 mu m. The other lines that were observed, [OI] at 145 mu m and [CII] at 157 mu m, are not detected. No extended emission has been found. Preliminary modeling of the photometric and line data assuming [(CO)-C-12]/[(CO)-C-13] = 69 suggests a dust mass for grains with radius < 1 mm of similar to 1.9 x 10(-4) M-circle dot (total solid mass of 3 x 10(-3) M-circle dot) and a gas mass of (0.5-5) x 10(-3) M-circle dot. The gas-to-dust mass may be lower than the standard interstellar value of 100.
        Publication date
        2010
        Published in
        Astronomy and Astrophysics
        Published version
        https://doi.org/10.1051/0004-6361/201014578
        Other links
        http://hdl.handle.net/2299/7278
        Relations
        School of Physics, Astronomy and Mathematics
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