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dc.contributor.authorPodio, L.
dc.contributor.authorKamp, I.
dc.contributor.authorCodella, C.
dc.contributor.authorNisini, B.
dc.contributor.authorAresu, G.
dc.contributor.authorBrittain, S.
dc.contributor.authorCabrit, S.
dc.contributor.authorDougados, C.
dc.contributor.authorGrady, C.
dc.contributor.authorMeijerink, R.
dc.contributor.authorSandell, G.
dc.contributor.authorSpaans, M.
dc.contributor.authorThi, W.-F.
dc.contributor.authorWhite, G.J.
dc.contributor.authorWoitke, P.
dc.date.accessioned2014-09-02T10:01:02Z
dc.date.available2014-09-02T10:01:02Z
dc.date.issued2014-03-10
dc.identifier.citationPodio , L , Kamp , I , Codella , C , Nisini , B , Aresu , G , Brittain , S , Cabrit , S , Dougados , C , Grady , C , Meijerink , R , Sandell , G , Spaans , M , Thi , W-F , White , G J & Woitke , P 2014 , ' Probing the gaseous disk of T Tau N with CN 5-4 lines ' , Astrophysical Journal Letters , vol. 783 , no. 2 , L26 . https://doi.org/10.1088/2041-8205/783/2/L26en
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 145268872
dc.identifier.otherPURE UUID: 8b41643a-5396-4a20-8c4c-574e61b5425f
dc.identifier.otherScopus: 84895161016
dc.identifier.otherWOS: 000332516300002
dc.identifier.urihttp://hdl.handle.net/10023/5321
dc.descriptionL.P. and S.D.B. acknowledge funding from the European FP7 (PIEF-GA-2009-253896) and the National Science Foundation (AST-0954811).en
dc.description.abstractWe present spectrally resolved observations of the young multiple system T Tau in atomic and molecular lines obtained with the Heterodyne Instrument for the Far Infrared on board Herschel. While CO, H2O, [C II], and SO lines trace the envelope and the outflowing gas up to velocities of 33 km s-1 with respect to systemic, the CN 5-4 hyperfine structure lines at 566.7, 566.9 GHz show a narrow double-peaked profile centered at systemic velocity, consistent with an origin in the outer region of the compact disk of T Tau N. Disk modeling of the T Tau N disk with the thermo-chemical code ProDiMo produces CN line fluxes and profiles consistent with the observed ones and constrain the size of the gaseous disk (Rout 110+10-20 AU) and its inclination (i = 25°± 5°). The model indicates that the CN lines originate in a disk upper layer at 40-110 AU from the star, which is irradiated by the stellar UV field and heated up to temperatures of 50-700 K. With respect to previously observed CN 2-1 millimeter lines, the CN 5-4 lines appear to be less affected by envelope emission, due to their larger critical density and excitation temperature. Hence, high-J CN lines are a unique confusion-free tracer of embedded disks, such as the disk of T Tau N.
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectAstrochemistryen
dc.subjectISM: moleculesen
dc.subjectProtoplanetary disksen
dc.subjectStars: individual (T Tau)en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleProbing the gaseous disk of T Tau N with CN 5-4 linesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/2041-8205/783/2/L26
dc.description.statusPeer revieweden


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