A three-dimensional view of Gomez’s hamburger

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dc.citation.issue1
dc.citation.rankM21
dc.citation.spage451-459
dc.citation.volume495
dc.contributor.authorTeague, Richard
dc.contributor.authorJankovic, Marija R.
dc.contributor.authorHaworth, Thomas J.
dc.contributor.authorQi, Chunhua
dc.contributor.authorIlee, John D.
dc.date.accessioned2023-05-09T11:14:46Z
dc.date.available2023-05-09T11:14:46Z
dc.date.issued2020-04-30
dc.description.abstractUnravelling the three-dimensional physical structure, the temperature and density distribution, of protoplanetary discs is an essential step if we are to confront simulations of embedded planets or dynamical instabilities. In this paper, we focus on submillimeter array observations of the edge-on source, Gomez’s Hamburger, believed to host an overdensity hypothesized to be a product of gravitational instability in the disc, GoHam b. We demonstrate that, by leveraging the well-characterized rotation of a Keplerian disc to deproject observations of molecular lines in position-position-velocity space into disc-centric coordinates, we are able to map out the emission distribution in the (r,z) plane and (⁠x,|y|,z) space. We show that 12CO traces an elevated layer of z/r∼0.3⁠, while 13CO traces deeper in the disc at z/r≲0.2⁠. We identify an azimuthal asymmetry in the deprojected 13CO emission coincident with GoHam b at a polar angle of ≈30○. At the spatial resolution of ∼1.5 arcsec, GoHam b is spatially unresolved, with an upper limit to its radius of <190 au.
dc.identifier.doi10.1093/mnras/staa1167
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.scopus2-s2.0-85093697604
dc.identifier.urihttps://pub.ipb.ac.rs/handle/123456789/15
dc.identifier.wos000539101400036
dc.language.isoen
dc.publisherOxford University Press (OUP)
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsrestrictedAccess
dc.titleA three-dimensional view of Gomez’s hamburger
dc.typejournal-article
dc.type.versionpublishedVersion
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