TY - JOUR
T1 - Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region
AU - Long, Feng
AU - Pinilla, Paola
AU - Herczeg, Gregory J.
AU - Harsono, Daniel
AU - Dipierro, Giovanni
AU - Pascucci, Ilaria
AU - Hendler, Nathan
AU - Tazzari, Marco
AU - Ragusa, Enrico
AU - Salyk, Colette
AU - Edwards, Suzan
AU - Lodato, Giuseppe
AU - Van De Plas, Gerrit
AU - Johnstone, Doug
AU - Liu, Yao
AU - Boehler, Yann
AU - Cabrit, Sylvie
AU - Manara, Carlo F.
AU - Menard, Francois
AU - Mulders, Gijs D.
AU - Nisini, Brunella
AU - Fischer, William J.
AU - Rigliaco, Elisabetta
AU - Banzatti, Andrea
AU - Avenhaus, Henning
AU - Gully-Santiago, Michael
N1 - Funding Information:
We thank the anonymous referee for useful comments. F.L. thanks Sean Andrews for discussions on comparing ALMA fluxes to past interferometer fluxes, and Zhaohuan Zhu, Kaitlin Kratter, and Andrew Youdin for insightful discussions. F.L. and G.J.H. thank Subo Dong for discussions of planet mass functions and radial distributions. F.L. and G.J.H. are supported by general grants 11473005 and 11773002 awarded by the National Science Foundation of China. P.P. acknowledges support by NASA through Hubble Fellowship grant HST-HF2-51380.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. G.D. acknowledges financial support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement no. 681601). D.H. is supported by European Union A-ERC grant 291141 CHEMPLAN, NWO, and by a KNAW professor prize awarded to E. van Dishoeck. C.F.M. acknowledges support through the ESO Fellowship. M.T. has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG. F.M., G.v.d.P., and Y.B. acknowledge funding from ANR of France under contract no. ANR-16-CE31-0013 (Planet-Forming-Disks). D.J. is supported by NRC Canada and by an NSERC Discovery Grant. B.N. and G.L. thank the support by the project PRIN-INAF 2016 The Cradle of Life—GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA). Y.L. acknowledges support by the Natural Science Foundation of Jiangsu Province of China (grant no. BK20181513) and by the Natural Science Foundation of China (grant no. 11503087). This paper makes use of the following ALMA data: 2016.1.01164.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/ gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC,https://www.cosmos.esa.int/web/gaia/ dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/12/10
Y1 - 2018/12/10
N2 - Rings are the most frequently revealed substructure in Atacama Large Millimeter/submillimeter Array (ALMA) dust observations of protoplanetary disks, but their origin is still hotly debated. In this paper, we identify dust substructures in 12 disks and measure their properties to investigate how they form. This subsample of disks is selected from a high-resolution (∼0.″12) ALMA 1.33 mm survey of 32 disks in the Taurus star-forming region, which was designed to cover a wide range of brightness and to be unbiased to previously known substructures. While axisymmetric rings and gaps are common within our sample, spiral patterns and high-contrast azimuthal asymmetries are not detected. Fits of disk models to the visibilities lead to estimates of the location and shape of gaps and rings, the flux in each disk component, and the size of the disk. The dust substructures occur across a wide range of stellar mass and disk brightness. Disks with multiple rings tend to be more massive and more extended. The correlation between gap locations and widths, the intensity contrast between rings and gaps, and the separations of rings and gaps could all be explained if most gaps are opened by low-mass planets (super-Earths and Neptunes) in the condition of low disk turbulence (α = 10-4). The gap locations are not well correlated with the expected locations of CO and N2 ice lines, so condensation fronts are unlikely to be a universal mechanism to create gaps and rings, though they may play a role in some cases.
AB - Rings are the most frequently revealed substructure in Atacama Large Millimeter/submillimeter Array (ALMA) dust observations of protoplanetary disks, but their origin is still hotly debated. In this paper, we identify dust substructures in 12 disks and measure their properties to investigate how they form. This subsample of disks is selected from a high-resolution (∼0.″12) ALMA 1.33 mm survey of 32 disks in the Taurus star-forming region, which was designed to cover a wide range of brightness and to be unbiased to previously known substructures. While axisymmetric rings and gaps are common within our sample, spiral patterns and high-contrast azimuthal asymmetries are not detected. Fits of disk models to the visibilities lead to estimates of the location and shape of gaps and rings, the flux in each disk component, and the size of the disk. The dust substructures occur across a wide range of stellar mass and disk brightness. Disks with multiple rings tend to be more massive and more extended. The correlation between gap locations and widths, the intensity contrast between rings and gaps, and the separations of rings and gaps could all be explained if most gaps are opened by low-mass planets (super-Earths and Neptunes) in the condition of low disk turbulence (α = 10-4). The gap locations are not well correlated with the expected locations of CO and N2 ice lines, so condensation fronts are unlikely to be a universal mechanism to create gaps and rings, though they may play a role in some cases.
KW - circumstellar matter
KW - planets and satellites: formation
KW - protoplanetary disks
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U2 - 10.3847/1538-4357/aae8e1
DO - 10.3847/1538-4357/aae8e1
M3 - Article
AN - SCOPUS:85058465221
SN - 0004-637X
VL - 869
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 17
ER -