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dc.contributor.authorBoyden, Ryan D.
dc.contributor.authorEisner, Josh A.
dc.date.accessioned2020-11-07T02:35:47Z
dc.date.available2020-11-07T02:35:47Z
dc.date.issued2020-05-07
dc.identifier.citationBoyden, R. D., & Eisner, J. A. (2020). Protoplanetary Disks in the Orion Nebula Cluster: Gas-disk Morphologies and Kinematics as Seen with ALMA. The Astrophysical Journal, 894(1), 74.en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab86b7
dc.identifier.urihttp://hdl.handle.net/10150/648158
dc.description.abstractWe present Atacama Large Millimeter Array CO(3 - 2) and HCO+(4 - 3) observations covering the central 15 x 15 region of the Orion Nebula Cluster (ONC). The unprecedented level of sensitivity (similar to 0.1 mJy beam(-1)) and angular resolution (similar to 009 40 au) of these line observations enable us to search for gas-disk detections toward the known positions of submillimeter-detected dust disks in this region. We detect 23 disks in gas: 17 in CO(3 - 2), 17 in HCO+(4 - 3), and 11 in both lines. Depending on where the sources are located in the ONC, we see the line detections in emission, in absorption against the warm background, or in both emission and absorption. We spectrally resolve the gas with 0.5 km s(-1) channels and find that the kinematics of most sources are consistent with Keplerian rotation. We measure the distribution of gas-disk sizes and find typical radii of similar to 50-200 au. As such, gas disks in the ONC are compact in comparison with the gas disks seen in low-density star-forming regions. Gas sizes are universally larger than the dust sizes. However, the gas and dust sizes are not strongly correlated. We find a positive correlation between gas size and distance from the massive star (1) Ori C, indicating that disks in the ONC are influenced by photoionization. Finally, we use the observed kinematics of the detected gas lines to model Keplerian rotation and infer the masses of the central pre-main-sequence stars. Our dynamically derived stellar masses are not consistent with the spectroscopically derived masses, and we discuss possible reasons for this discrepancy.en_US
dc.description.sponsorshipNSFen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rights© 2020. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectProtoplanetary disksen_US
dc.subjectCircumstellar disksen_US
dc.subjectProplydsen_US
dc.subjectCircumstellar gasen_US
dc.subjectYoung star clustersen_US
dc.subjectYoung stellar objectsen_US
dc.subjectPre-main sequence starsen_US
dc.subjectPlanet formationen_US
dc.subjectRadio astronomyen_US
dc.subjectMillimeter astronomyen_US
dc.titleProtoplanetary Disks in the Orion Nebula Cluster: Gas-disk Morphologies and Kinematics as Seen with ALMAen_US
dc.typeArticleen_US
dc.identifier.eissn1538-4357
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume894
dc.source.issue1
dc.source.beginpage74
refterms.dateFOA2020-11-07T02:35:57Z


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