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hal.structure.identifierAMOR 2017
dc.contributor.authorDUTREY, Anne
hal.structure.identifierAMOR 2017
dc.contributor.authorGUILLOTEAU, S.
dc.contributor.authorPIÉTU, V.
hal.structure.identifierAMOR 2017
dc.contributor.authorCHAPILLON, E.
hal.structure.identifierAMOR 2017
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierAMOR 2017
dc.contributor.authorDI FOLCO, E.
dc.contributor.authorSTOECKLIN, T.
dc.contributor.authorDENIS-ALPIZAR, O.
dc.contributor.authorGORTI, U.
dc.contributor.authorTEAGUE, R.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, T.
dc.contributor.authorSEMENOV, D.
hal.structure.identifierObservatoire astronomique de Strasbourg [ObAS]
dc.contributor.authorGROSSO, N.
dc.date.issued2017-11
dc.identifier.issn0004-6361
dc.description.abstractEnContext. 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.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.subject.encircumstellar matter
dc.subject.enprotoplanetary disks
dc.subject.enradio lines: stars
dc.title.enThe Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201730645
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1706.02608
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA130
bordeaux.volume607
bordeaux.peerReviewedoui
hal.identifierhal-01536626
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01536626v1
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