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Molecules with ALMA at Planet-forming Scales. XX. The massive disk around GM aurigae
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Schwarz_2021_ApJS_257_20.pdf
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Author
Schwarz, K.R.Calahan, J.K.
Zhang, K.
Alarcón, F.
Aikawa, Y.
Andrews, S.M.
Bae, J.
Bergin, E.A.
Booth, A.S.
Bosman, A.D.
Cataldi, G.
Cleeves, L.I.
Czekala, I.
Huang, J.
Ilee, J.D.
Law, C.J.
Le Gal, R.
Long, F.
Loomis, R.A.
Macías, E.
Liu, Y.
McClure, M.
Ménard, F.
Öberg, K.I.
Teague, R.
van Dishoeck, E.
Walsh, C.
Wilner, D.J.
Affiliation
Lunar and Planetary Laboratory, University of ArizonaIssue Date
2021
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American Astronomical SocietyCitation
Schwarz, K. R., Calahan, J. K., Zhang, K., Alarcón, F., Aikawa, Y., Andrews, S. M., Bae, J., Bergin, E. A., Booth, A. S., Bosman, A. D., Cataldi, G., Cleeves, L. I., Czekala, I., Huang, J., Ilee, J. D., Law, C. J., Le Gal, R., Long, F., Loomis, R. A., … Wilner, D. J. (2021). Molecules with ALMA at Planet-forming Scales. XX. The massive disk around GM aurigae. Astrophysical Journal, Supplement Series.Rights
Copyright © 2021. The American Astronomical Society. All rights reserved.Collection Information
This 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.Abstract
Gas mass remains one of the most difficult protoplanetary disk properties to constrain. With much of the protoplanetary disk too cold for the main gas constituent, H2, to emit, alternative tracers such as dust, CO, or the H2 isotopologue HD are used. However, relying on disk mass measurements from any single tracer requires assumptions about the tracer's abundance relative to H2 and the disk temperature structure. Using new Atacama Large Millimeter/submillimeter Array (ALMA) observations from the Molecules with ALMA at Planet-forming Scales (MAPS) ALMA Large Program as well as archival ALMA observations, we construct a disk physical/chemical model of the protoplanetary disk GM Aur. Our model is in good agreement with the spatially resolved CO isotopologue emission from 11 rotational transitions with spatial resolution ranging from 0 15 to 0 46 (24-73 au at 159 pc) and the spatially unresolved HD J = 1-0 detection from Herschel. Our best-fit model favors a cold protoplanetary disk with a total gas mass of approximately 0.2 Me, a factor of 10 reduction in CO gas inside roughly 100 au and a factor of 100 reduction outside of 100 au. Despite its large mass, the disk appears to be on the whole gravitationally stable based on the derived Toomre Q parameter. However, the region between 70 and 100 au, corresponding to one of the millimeter dust rings, is close to being unstable based on the calculated Toomre Q of <1.7. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement. © 2021. The American Astronomical Society. All rights reserved.Note
Immediate accessISSN
0067-0049Version
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4365/ac143b