TY - JOUR
T1 - Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud
AU - Long, Feng
AU - Herczeg, Gregory J.
AU - Harsono, Daniel
AU - Pinilla, Paola
AU - Tazzari, Marco
AU - Manara, Carlo F.
AU - Pascucci, Ilaria
AU - Cabrit, Sylvie
AU - Nisini, Brunella
AU - Johnstone, Doug
AU - Edwards, Suzan
AU - Salyk, Colette
AU - Menard, Francois
AU - Lodato, Giuseppe
AU - Boehler, Yann
AU - Mace, Gregory N.
AU - Liu, Yao
AU - Mulders, Gijs D.
AU - Hendler, Nathanial
AU - Ragusa, Enrico
AU - Fischer, William J.
AU - Banzatti, Andrea
AU - Rigliaco, Elisabetta
AU - Van De Plas, Gerrit
AU - Dipierro, Giovanni
AU - Gully-Santiago, Michael
AU - Lopez-Valdivia, Ricardo
N1 - Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/9/1
Y1 - 2019/9/1
N2 - We present a high-resolution (∼0.″12, ∼16 au, mean sensitivity of 50 μJy 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,95% ≲ 50 au). In contrast, all disks with R eff,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.
AB - We present a high-resolution (∼0.″12, ∼16 au, mean sensitivity of 50 μJy 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,95% ≲ 50 au). In contrast, all disks with R eff,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.
KW - circumstellar matter
KW - planets and satellites: formation
KW - protoplanetary disks
KW - stars: pre-main sequence
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U2 - 10.3847/1538-4357/ab2d2d
DO - 10.3847/1538-4357/ab2d2d
M3 - Article
AN - SCOPUS:85072341472
SN - 0004-637X
VL - 882
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 49
ER -