Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud
Long,Feng1,2; Herczeg,Gregory J.1; Harsono,Daniel3; Pinilla,Paola4,5; Tazzari,Marco6; Manara,Carlo F.7; Pascucci,Ilaria8,9; Cabrit,Sylvie10,11; Nisini,Brunella12; Johnstone,Doug13,14; Edwards,Suzan15; Salyk,Colette16; Menard,Francois11; Lodato,Giuseppe17; Boehler,Yann11,18; Mace,Gregory N.19; Liu,Yao20,21; Mulders,Gijs D.9,22; Hendler,Nathanial8; Ragusa,Enrico23; Fischer,William J.24; Banzatti,Andrea8; Rigliaco,Elisabetta25; van de Plas,Gerrit11; Dipierro,Giovanni23; Gully-Santiago,Michael26; Lopez-Valdivia,Ricardo19
Source PublicationThe Astrophysical Journal
AbstractAbstract 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 (Reff,95%???50 au). In contrast, all disks with Reff,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.
Keywordcircumstellar matter planets and satellites: formation protoplanetary disks stars: pre-main sequence
WOS IDIOP:0004-637X-882-1-ab2d2d
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People’s Republic of China
2.Department of Astronomy, School of Physics, Peking University, Beijing 100871, People’s Republic of China
3.Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands
4.Department of Astronomy/Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
5.Max-Planck-Institut für Astronomie, K?nigstuhl 17, D-69117, Heidelberg, Germany
6.Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
7.European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany
8.Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
9.Earths in Other Solar Systems Team, NASA Nexus for Exoplanet System Science, USA
10.Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, LERMA, F-75014 Paris, France
11.Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France
12.INAF–Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monte Porzio Catone, Italy
13.NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada
14.Department of Physics and Astronomy, University of Victoria, Victoria, BC, V8P 5C2, Canada
15.Five College Astronomy Department, Smith College, Northampton, MA 01063, USA
16.Vassar College Physics and Astronomy Department, 124 Raymond Avenue, Poughkeepsie, NY 12604, USA
17.Dipartimento di Fisica, Universita Degli Studi di Milano, Via Celoria, 16, I-20133 Milano, Italy
18.Rice University, Department of Physics and Astronomy, Main Street, 77005 Houston, USA
19.McDonald Observatory and Department of Astronomy, University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA
20.Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748, Garching, Germany
21.Purple Mountain Observatory, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, People’s Republic of China
22.Department of the Geophysical Sciences, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
23.Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
24.Space Telescope Science Institute Baltimore, MD 21218, USA
25.INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy
26.NASA Ames Research Center and Bay Area Environmental Research Institute, Moffett Field, CA 94035, USA
Recommended Citation
GB/T 7714
Long,Feng,Herczeg,Gregory J.,Harsono,Daniel,et al. Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud[J]. The Astrophysical Journal,2019,882(1).
APA Long,Feng.,Herczeg,Gregory J..,Harsono,Daniel.,Pinilla,Paola.,Tazzari,Marco.,...&Lopez-Valdivia,Ricardo.(2019).Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud.The Astrophysical Journal,882(1).
MLA Long,Feng,et al."Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud".The Astrophysical Journal 882.1(2019).
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