A Multi-wavelength Analysis of Dust and Gas in the SR 24S Transition Disk
Andrews, S. M.
van der Marel, N.
van Dishoeck, E. F.
AffiliationUniv Arizona, Dept Astron Steward Observ
Keywordsaccretion, accretion disks
planet and satellites: formation
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationA Multi-wavelength Analysis of Dust and Gas in the SR 24S Transition Disk 2017, 839 (2):99 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 firstname.lastname@example.org.
AbstractWe present new Atacama Large Millimeter/sub-millimeter Array (ALMA) 1.3 mm continuum observations of the SR 24S transition disk with an angular resolution less than or similar to 0'.18 (12 au radius). We perform a multi-wavelength investigation by combining new data with previous ALMA data at 0.45 mm. The visibilities and images of the continuum emission at the two wavelengths are well characterized by a ring-like emission. Visibility modeling finds that the ring-like emission is narrower at longer wavelengths, in good agreement with models of dust-trapping in pressure bumps, although there are complex residuals that suggest potentially asymmetric structures. The 0.45 mm emission has a shallower profile inside the central cavity than the 1.3 mm emission. In addition, we find that the (CO)-C-13 and (CO)-O-18 (J = 2-1) emission peaks at the center of the continuum cavity. We do not detect either continuum or gas emission from the northern companion to this system (SR 24N), which is itself a binary system. The upper limit for the dust disk mass of SR 24N is less than or similar to 0.12 M-circle plus, which gives a disk mass ratio in dust between the two components of M-dust,M-SR 24S/M-dust,M-SR 24N greater than or similar to 840. The current ALMA observations may imply that either planets have already formed in the SR 24N disk or that dust growth to millimeter sizes is inhibited there and that only warm gas, as seen by rovibrational CO emission inside the truncation radii of the binary, is present.
VersionFinal published version
SponsorsNASA through Hubble Fellowship [HST-HF2-51380.001-A]; Space Telescope Science Institute; NASA [NAS 5-26555]; European Union A-ERC grant ; Netherlands Research School for Astronomy (NOVA); Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program ; Science Foundation of Ireland [13/ERC/I2907]