The Sizes and Depletions of the Dust and Gas Cavities in the Transitional Disk J160421.7-213028
Marel, Nienke van der
Liu, Hauyu Baobab
Knapp, Gillian R.
AffiliationUniv Arizona, Steward Observ
planets and satellites: formation
stars: individual ([PZ99] J160421.7-213028)
stars: pre-main sequence
stars: variables: T Tauri, Herbig Ae/Be
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PublisherIOP PUBLISHING LTD
CitationThe Sizes and Depletions of the Dust and Gas Cavities in the Transitional Disk J160421.7-213028 2017, 836 (2):201 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2017. The American Astronomical Society. All rights reserved.
Collection InformationThis 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 email@example.com.
AbstractWe report ALMA Cycle 2 observations of 230 GHz (1.3 mm) dust continuum emission, and (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 2-1 line emission, from the Upper Scorpius transitional disk [PZ99] J160421.7-213028, with an angular resolution of similar to 0''.25 (35 au). Armed with these data and existing H-band scattered light observations, we measure the size and depth of the disk's central cavity, and the sharpness of its outer edge, in three components: sub-mu m-sized "small" dust traced by scattered light, millimeter-sized "big" dust traced by the millimeter continuum, and gas traced by line emission. Both dust populations feature a cavity of radius similar to 70 au that is depleted by factors of at least 1000 relative to the dust density just outside. The millimeter continuum data are well explained by a cavity with a sharp edge. Scattered light observations can be fitted with a cavity in small dust that has either a sharp edge at 60 au, or an edge that transitions smoothly over an annular width of 10 au near 60 au. In gas, the data are consistent with a cavity that is smaller, about 15 au in radius, and whose surface density at 15 au is 10(3 +/- 1) times smaller than the surface density at 70 au; the gas density grades smoothly between these two radii. The CO isotopologue observations rule out a sharp drop in gas surface density at 30 au or a double-drop model, as found by previous modeling. Future observations are needed to assess the nature of these gas and dust cavities (e.g., whether they are opened by multiple as-yet-unseen planets or photoevaporation).
VersionFinal published version
SponsorsNASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF-51320.01-A]; NASA [NAS 5-26555]; UC Berkeley Vice Chancellor for Research; Berkeley Center for Integrative Planetary Science