MAPPING CO GAS IN THE GG TAURI A TRIPLE SYSTEM WITH 50 au SPATIAL RESOLUTION

Journal Article · Sun Mar 20 00:00:00 EDT 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/820/1/19· OSTI ID:22518592

Tang, Ya-Wen ^[1]; Dutrey, Anne; Guilloteau, Stéphane; Di Folco, Emmanuel; Huré, Jean-Marc; Pierens, Arnaud ^[2]; Chapillon, Edwige; Pietu, Vincent; Gueth, Fréderic ^[3]; Bary, Jeff ^[4]; Beck, Tracy ^[5]; Beust, Hervé ^[6]; Boehler, Yann ^[7]; Simon, Michal ^[8]

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1. Academia Sinica, Institute of Astronomy and Astrophysics, Taipei, Taiwan (China)
2. Université de Bordeaux, Observatoire Aquitain des Sciences de l’Univers, CNRS, UMR 5804, Laboratoire d’Astrophysique de Bordeaux, 2 rue de l’Observatoire, BP 89, F-33271 Floirac Cedex (France)
3. IRAM, 300 rue de la piscine, F-38406 Saint Martin d’Hères Cedex (France)
4. Department of Physics and Astronomy, Colgate University, 13 Oak Drive, Hamilton, NY 13346 (United States)
5. Space Telescope Science Institute, 3700 San Martin Drive Baltimore, MD 21218 (United States)
6. Université de Grenoble, IPAG, Saint Martin d’Hères (France)
7. Centro de Radioastronomìa y Astrofìsica, UNAM, Apartado Postal 3-72, 58089 Morelia, Michoacàn (Mexico)
8. Stony Brook University, Stony Brook, NY 11794-3800 (United States)

We aim to unveil the observational imprint of physical mechanisms that govern planetary formation in the young, multiple system GG Tau A. We present ALMA observations of {sup 12}CO and {sup 13}CO 3–2 and 0.9 mm continuum emission with 0.″35 resolution. The {sup 12}CO 3–2 emission, found within the cavity of the circumternary dust ring (at radius <180 au) where no {sup 13}CO emission is detected, confirms the presence of CO gas near the circumstellar disk of GG Tau Aa. The outer disk and the recently detected hot spot lying at the outer edge of the dust ring are mapped both in {sup 12}CO and {sup 13}CO. The gas emission in the outer disk can be radially decomposed as a series of slightly overlapping Gaussian rings, suggesting the presence of unresolved gaps or dips. The dip closest to the disk center lies at a radius very close to the hot spot location at ∼250–260 au. The CO excitation conditions indicate that the outer disk remains in the shadow of the ring. The hot spot probably results from local heating processes. The two latter points reinforce the hypothesis that the hot spot is created by an embedded proto-planet shepherding the outer disk.

• OSTI ID: 22518592
• Journal Information: Astrophysical Journal, Vol. 820, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CARBON 12
CARBON 13
CARBON MONOXIDE
EMISSION
EXCITATION
HEATING
HOT SPOTS
HYPOTHESIS
MAPPING
PLANETS
PROTOPLANETS
SPATIAL RESOLUTION
STARS