Volume 607, November 2017
|Number of page(s)||14|
|Section||Interstellar and circumstellar matter|
|Published online||27 November 2017|
The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk
1 Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, 33615 Pessac, France
2 IRAM, 300 rue de la piscine, 38406 Saint Martin d’Hères, France
3 Institut des Sciences Moléculaires, UMR5255-CNRS, 351 Cours de la libération, 33405 Talence, France
4 Universidad Autónoma de Chile, Instituto de Ciencias Quimicas Aplicadas, Theoretical and Quantum Chemistry Center, 2801 El Llano Subercaseaux, San Miguel, Santiago, Chile
5 SETI Institute/NASA Ames Research Center, Mail Stop 245-3, Moffett Field, CA 94035-1000, USA
6 Max-Planck-Institute für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
7 Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, 67000 Strasbourg, France
Received: 17 February 2017
Accepted: 5 June 2017
Context. Determining the gas density and temperature structures of protoplanetary disks is a fundamental task in order to constrain planet formation theories. This is a challenging procedure and most determinations are based on model-dependent assumptions.
Aims. We attempt a direct determination of the radial and vertical temperature structure of the Flying Saucer disk, thanks to its favorable inclination of 90 degrees.
Methods. We present a method based on the tomographic study of an edge-on disk. Using ALMA, we observe at 0.5″ resolution the Flying Saucer in CO J = 2–1 and CS J = 5–4. This edge-on disk appears in silhouette against the CO J = 2–1 emission from background molecular clouds in ρ Oph. The combination of velocity gradients due to the Keplerian rotation of the disk and intensity variations in the CO background as a function of velocity provide a direct measure of the gas temperature as a function of radius and height above the disk mid-plane.
Results. The overall thermal structure is consistent with model predictions, with a cold (<12−15 K) CO-depleted mid-plane and a warmer disk atmosphere. However, we find evidence for CO gas along the mid-plane beyond a radius of about 200 au, coincident with a change of grain properties. Such behavior is expected in the case of efficient rise of UV penetration re-heating the disk and thus allowing CO thermal desorption or favoring direct CO photo-desorption. CO is also detected at up to 3–4 scale heights, while CS is confined to around 1 scale height above the mid-plane. The limits of the method due to finite spatial and spectral resolutions are also discussed.
Conclusions. This method appears to be a very promising way to determine the gas structure of planet-forming disks, provided that the molecular data have an angular resolution which is high enough, on the order of 0.3−0.1″ at the distance of the nearest star-forming regions.
Key words: circumstellar matter / protoplanetary disks / radio lines: stars
© ESO, 2017
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