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The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk

dc.contributor.authorDutrey A.
dc.contributor.authorGuilloteau S.
dc.contributor.authorPiétu V.
dc.contributor.authorChapillon E.
dc.contributor.authorWakelam V.
dc.contributor.authorDi Folco E.
dc.contributor.authorStoecklin T.
dc.contributor.authorDenis-Alpizar O.
dc.contributor.authorGorti U.
dc.contributor.authorTeague R.
dc.contributor.authorHenning T.
dc.contributor.authorSemenov D.
dc.contributor.authorGrosso N.
dc.date.accessioned2020-09-02T22:16:45Z
dc.date.available2020-09-02T22:16:45Z
dc.date.issued2017
dc.identifier10.1051/0004-6361/201730645
dc.identifier.citation607, , -
dc.identifier.issn00046361
dc.identifier.urihttps://hdl.handle.net/20.500.12728/4322
dc.descriptionContext. 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. © ESO, 2017.
dc.language.isoen
dc.publisherEDP Sciences
dc.subjectCircumstellar matter
dc.subjectProtoplanetary disks
dc.subjectRadio lines: stars
dc.subjectDesorption
dc.subjectGases
dc.subjectStars
dc.subjectTomography
dc.subjectCircumstellar matters
dc.subjectDirect determination
dc.subjectIntensity variations
dc.subjectProtoplanetary disks
dc.subjectRadio lines: stars
dc.subjectStar-forming region
dc.subjectTemperature structure
dc.subjectVertical temperature
dc.subjectDensity of gases
dc.titleThe Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk
dc.typeArticle


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