Discovery of An au-scale Excess in Millimeter Emission from the Protoplanetary Disk around TW Hya

We report the detection of an excess in dust continuum emission at 233 GHz (1.3 mm in wavelength) in the protoplanetary disk (PPD) around TW Hya revealed through high-sensitivity observations at ∼3 au resolution with the Atacama Large Millimeter/submillimeter Array. The sensitivity of the 233 GHz im...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2019-06, Vol.878 (1), p.L8
Main Authors: Tsukagoshi, Takashi, Muto, Takayuki, Nomura, Hideko, Kawabe, Ryohei, Kanagawa, Kazuhiro D., Okuzumi, Satoshi, Ida, Shigeru, Walsh, Catherine, Millar, Tom J., Takahashi, Sanemichi Z., Hashimoto, Jun, Uyama, Taichi, Tamura, Motohide
Format: Article
Language:English
Subjects:
Celestial bodies
Continuum radiation
Dust
Emission
Flux density
Protoplanetary disks
Radio telescopes
Sensitivity
stars: individual (TW Hya)
Visibility
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Summary:We report the detection of an excess in dust continuum emission at 233 GHz (1.3 mm in wavelength) in the protoplanetary disk (PPD) around TW Hya revealed through high-sensitivity observations at ∼3 au resolution with the Atacama Large Millimeter/submillimeter Array. The sensitivity of the 233 GHz image has been improved by a factor of 3 with regard to that of our previous cycle 3 observations. The overall structure is mostly axisymmetric, and there are apparent gaps at 25 and 41 au as previously reported. The most remarkable new finding is a few astronomical-unit-scale excess emission in the southwest part of the PPD. The excess emission is located at 52 au from the disk center and is 1.5 times brighter than the surrounding PPD at a significance of 12 . We performed a visibility fitting to the extracted emission after subtracting the axisymmetric PPD emission and found that the inferred size and the total flux density of the excess emission are 4.4 × 1.0 au and 250 Jy, respectively. The dust mass of the excess emission corresponds to 0.03 M⊕ if a dust temperature of 18 K is assumed. Because the excess emission can also be marginally identified in the Band 7 image at almost the same position, the feature is unlikely to be a background source. The excess emission can be explained by a dust clump accumulated in a small elongated vortex or a massive circumplanetary disk around a Neptune-mass-forming planet.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ab224c