Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program

Abstract Detecting planet signatures in protoplanetary disks is fundamental to understanding how and where planets form. In this work, we report dust and gas observational hints of planet formation in the disk around 2MASS J16120668-301027, as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Large Program “AGE-PRO: ALMA survey of Gas Evolution in Protoplanetary disks.” The disk was imaged with the ALMA at Band 6 (1.3 mm) in dust continuum emission and four molecular lines: 12 CO( J = 2–1), 13 CO( J = 2–1), C 18 O( J = 2–1), and H 2 CO( J = 3 (3,0) –2 (2,0) ). Resolved observations of the dust continuum emission (angular resolution of ∼150 mas, 20 au) show a ring-like structure with a peak at 0.″57 (75 au), a deep gap with a minimum at 0.″24 (31 au), an inner disk, a bridge connecting the inner disk and the outer ring, along with a spiral arm structure, and a tentative detection (to 3 σ ) of a compact emission at the center of the disk gap, with an estimated dust mass of ∼2.7−12.9 Lunar masses. We also detected a kinematic kink (not coincident with any dust substructure) through several 12 CO channel maps (angular resolution ∼200 mas, 30 au), located at a radius of ∼0.″875 (115.6 au). After modeling the 12 CO velocity rotation around the protostar, we identified a purple tentative rotating-like structure at the kink location with a geometry similar to that of the disk. We discuss potential explanations for the dust and gas substructures observed in the disk and their potential connection to signatures of planet formation.

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Publication Details

Journal
The Astrophysical Journal
Published
2024-10-01
DOI
https://doi.org/10.3847/1538-4357/ad6e73
Citations
9
Primary Topic
Stellar, planetary, and galactic studies
Type
article
Field-Weighted Citation Impact
2.98

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article

Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program

Camilo González-Ruilova, Carolina Agurto-Gangas, Aleksandra Kuznetsova, M. R. Hogerheijde et al.
9 citations
The Astrophysical Journal
Stellar, planetary, and galactic studies
2.98
article

Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program

Camilo González-Ruilova, Carolina Agurto-Gangas, Aleksandra Kuznetsova, M. R. Hogerheijde, James Miley, John M. Carpenter, Giovanni Rosotti, Dary Ruíz-Rodríguez, Lucas A. Cieza, Dingshan Deng, Paola Pinilla, Kamber R. Schwarz, Leon Trapman, N. T. Kurtovic, Benoît Tabone, Anibal Sierra, Miguel Vioque, Estephani E. TorresVillanueva, Ilaria Pascucci, Ke Zhang, Laura M. Pérez, Rossella Anania
article en
9 citations

Abstract

Abstract Detecting planet signatures in protoplanetary disks is fundamental to understanding how and where planets form. In this work, we report dust and gas observational hints of planet formation in the disk around 2MASS J16120668-301027, as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Large Program “AGE-PRO: ALMA survey of Gas Evolution in Protoplanetary disks.” The disk was imaged with the ALMA at Band 6 (1.3 mm) in dust continuum emission and four molecular lines: 12 CO( J = 2–1), 13 CO( J = 2–1), C 18 O( J = 2–1), and H 2 CO( J = 3 (3,0) –2 (2,0) ). Resolved observations of the dust continuum emission (angular resolution of ∼150 mas, 20 au) show a ring-like structure with a peak at 0.″57 (75 au), a deep gap with a minimum at 0.″24 (31 au), an inner disk, a bridge connecting the inner disk and the outer ring, along with a spiral arm structure, and a tentative detection (to 3 σ ) of a compact emission at the center of the disk gap, with an estimated dust mass of ∼2.7−12.9 Lunar masses. We also detected a kinematic kink (not coincident with any dust substructure) through several 12 CO channel maps (angular resolution ∼200 mas, 30 au), located at a radius of ∼0.″875 (115.6 au). After modeling the 12 CO velocity rotation around the protostar, we identified a purple tentative rotating-like structure at the kink location with a geometry similar to that of the disk. We discuss potential explanations for the dust and gas substructures observed in the disk and their potential connection to signatures of planet formation.

The Astrophysical JournalVol. 974(1)
Universidad de Santiago de Chile (CL), Leiden University (NL), Centre National de la Recherche Scientifique (FR), European Southern Observatory (DE), University of Wisconsin–Madison (US), University of Arizona (US), University of Milan (IT), National Radio Astronomy Observatory (US), Université Paris-Saclay (FR), Atacama Large Millimeter Submillimeter Array (CL), Chinese Academy of Science South America Center for Astronomy (CL), Institut d'Astrophysique Spatiale (FR), Max Planck Institute for Astronomy (DE), Flatiron Health (United States) (US), Flatiron Institute (US), University College London (GB), University of Chile (CL), University of Amsterdam (NL), Universidad Diego Portales (CL)
Fondo Nacional de Desarrollo Científico y Tecnológico
Openalex Percentile: Top 9%
Stellar, planetary, and galactic studies
2.98
DOIOpen Access PDFOpenAlex
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