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dc.contributor.authorVan Terwisga, SE
dc.contributor.authorVan Dishoeck, EF
dc.contributor.authorCazzoletti, P
dc.contributor.authorFacchini, S
dc.contributor.authorTrapman, L
dc.contributor.authorWilliams, JP
dc.contributor.authorManara, CF
dc.contributor.authorMiotello, A
dc.contributor.authorVan Der Marel, N
dc.contributor.authorAnsdell, M
dc.contributor.authorHogerheijde, MR
dc.contributor.authorTazzari, Marco
dc.contributor.authorTesti, L
dc.date.accessioned2019-01-18T00:30:40Z
dc.date.available2019-01-18T00:30:40Z
dc.date.issued2019-03-01
dc.identifier.issn0004-6361
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/288151
dc.description.abstractThe cyanide radical CN is abundant in protoplanetary disks, with line fluxes often comparable to those of 13CO. It is known to be sensitive to UV irradiation of the upper disk atmosphere, with models predicting ring-shaped emission. Aims. We seek to characterize the CN emission from 94 Class-II disks in the Lupus star-forming region, compare it to observations in other regions, and interpret our observations with a grid of models. The CN emission morphology is discussed for two primordial disks, Sz 71 and Sz 98, and is modeled in more detail. Methods. ALMA observed CN N = 32 in Lupus disks down to sensitivities better than previous surveys. Models constructed with the physico-chemical code DALI are used to study the integrated fluxes of the disks and resolved emission of CN in disks without (dust) substructures. Results. CN N = 32 is bright, and detected in 38% of sources, but its disk-integrated flux is not strongly correlated to either 13CO or continuum flux. Compared to pre-ALMA single-dish surveys, no significant difference in the CN flux distributions in Lupus and Taurus-Auriga is found, although Ophiuchus disks may be fainter on average. We find ring-shaped CN emission with peak radii of 50AU in two resolved disks. Conclusions. A large fraction of sources are faint in CN; only exponential gas surface density cutoffs at Rc 15AU can reconcile observations with models. This is the first observational evidence of such a compact gas disk population in Lupus. bsolute intensities and the emission morphology of CN are reproduced by DALI models without the need for any continuum substructure; they are unrelated to the CO snowline location. The observations presented here, together with the modeling of these rings, provide a new probe of the structure and conditions in disks, and particularly their incident UV radiation field, if disk size is determined from the data.
dc.publisherEDP Sciences
dc.rightsAll rights reserved
dc.titleThe ALMA Lupus protoplanetary disk survey: Evidence for compact gas disks and molecular rings from CN
dc.typeArticle
prism.numberA150
prism.publicationDate2019
prism.publicationNameAstronomy and Astrophysics: a European journal
prism.volume623
dc.identifier.doi10.17863/CAM.35467
dcterms.dateAccepted2018-11-06
rioxxterms.versionofrecord10.1051/0004-6361/201834257
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2019-03-01
dc.contributor.orcidTazzari, Marco [0000-0003-3590-5814]
dc.identifier.eissn1432-0746
dc.publisher.urlhttp://dx.doi.org/10.1051/0004-6361/201834257
rioxxterms.typeJournal Article/Review
pubs.funder-project-idEuropean Research Council (341137)
pubs.funder-project-idScience and Technology Facilities Council (ST/N000927/1)
cam.issuedOnline2019-03-25
cam.orpheus.successMon Jul 20 07:55:39 BST 2020 - The item has an open VoR version.
rioxxterms.freetoread.startdate2100-01-01


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