Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud
Herczeg, Gregory J.
Manara, Carlo F.
Mace, Gregory N.
Mulders, Gijs D.
Fischer, William J.
van de Plas, Gerrit
AffiliationUniv Arizona, Steward Observ, Dept Astron
Univ Arizona, Lunar & Planetary Lab
planets and satellites: formation
stars: pre-main sequence
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationFeng Long et al 2019 ApJ 882 49
RightsCopyright © 2019. 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 a high-resolution (similar to 0 ''.12, similar to 16 au, mean sensitivity of 50 mu Jy beam(-1) at 225 GHz) snapshot survey of 32 protoplanetary disks around young stars with spectral type earlier than M3 in the Taurus star-forming region using the Atacama Large Millimeter Array. This sample includes most mid-infrared excess members that were not previously imaged at high spatial resolution, excluding close binaries and objects with high extinction, thereby providing a more representative look at disk properties at 1-2 Myr. Our 1.3 mm continuum maps reveal 12 disks with prominent dust gaps and rings, 2 of which are around primary stars in wide binaries, and 20 disks with no resolved features at the observed resolution (hereafter smooth disks), 8 of which are around the primary star in wide binaries. The smooth disks were classified based on their lack of resolved substructures, but their most prominent property is that they are all compact with small effective emission radii (R-eff,R-95% less than or similar to 50 au). In contrast, all disks with R-eff,R-95% of at least 55 au in our sample show detectable substructures. Nevertheless, their inner emission cores (inside the resolved gaps) have similar peak brightness, power-law profiles, and transition radii to the compact smooth disks, so the primary difference between these two categories is the lack of outer substructures in the latter. These compact disks may lose their outer disk through fast radial drift without dust trapping, or they might be born with small sizes. The compact dust disks, as well as the inner disk cores of extended ring disks, that look smooth at the current resolution will likely show small-scale or low-contrast substructures at higher resolution. The correlation between disk size and disk luminosity correlation demonstrates that some of the compact disks are optically thick at millimeter wavelengths.
VersionFinal published version
SponsorsNational Science Foundation of ChinaNational Natural Science Foundation of China [11773002, 11473005]; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF251380.001-A]; European Union A-ERCEuropean Union (EU) [291141 CHEMPLAN]; NWONetherlands Organization for Scientific Research (NWO); KNAW professor prize; ESO Fellowship; Deutsche Forschungs-Gemeinschaft (DFG, German Research Foundation)German Research Foundation (DFG) [FOR 2634/1 TE1024/1-1]; DISCSIM project; European Research CouncilEuropean Research Council (ERC) [341137, ERC-2013-ADG]; UK Science and Technology Research Council (STFC); ANR of FranceFrench National Research Agency (ANR) [ANR-16-CE31-0013]; NRC Canada; NSERC Discovery GrantNatural Sciences and Engineering Research Council of Canada; European UnionEuropean Union (EU) ; Natural Science Foundation of Jiangsu Province of ChinaNatural Science Foundation of Jiangsu Province [BK20181513]; Natural Science Foundation of ChinaNational Natural Science Foundation of China ; European Research Council (ERC) under the European UnionEuropean Research Council (ERC) ; LSSTC Data Science Fellowship Program - LSSTC, NSF ; Brinson Foundation ; Moore FoundationGordon and Betty Moore Foundation; US National Science Foundation (NSF)National Science Foundation (NSF); Korea Astronomy and Space Science Institute (KASI); US NSFNational Science Foundation (NSF) [AST-1229522]; Korean GMT Project of KASI; NASANational Aeronautics & Space Administration (NASA) [NAS 5-26555]