Dust Substructures and Line Perturbations driven by a Forming Planet in J16120

@misc{sierra2026dust,
  title = {{Dust Substructures and Line Perturbations driven by a Forming Planet in J16120}},
  author = {Anibal Sierra and Andrés F. Izquierdo and Paola Pinilla and Kan Chen and Myriam Benisty and Laura Pérez and Teresa Paneque-Carreño and Carolina Agurto-Gangas and Jaehan Bae and John Carpenter and Luca Cieza and Dingshan Deng and Stefano Facchini and Camilo González-Ruilova and Nicolás Kurtovic and Aleksandra Kuznetsova and Carlo F. Manara and James Miley and Álvaro Ribas and Giovanni Rosotti and Miguel Vioque},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.05366},
  eprint = {2609.05366},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.05366},
}

TY  - UNPB
TI  - Dust Substructures and Line Perturbations driven by a Forming Planet in J16120
AU  - Anibal Sierra
AU  - Andrés F. Izquierdo
AU  - Paola Pinilla
AU  - Kan Chen
AU  - Myriam Benisty
AU  - Laura Pérez
AU  - Teresa Paneque-Carreño
AU  - Carolina Agurto-Gangas
AU  - Jaehan Bae
AU  - John Carpenter
AU  - Luca Cieza
AU  - Dingshan Deng
AU  - Stefano Facchini
AU  - Camilo González-Ruilova
AU  - Nicolás Kurtovic
AU  - Aleksandra Kuznetsova
AU  - Carlo F. Manara
AU  - James Miley
AU  - Álvaro Ribas
AU  - Giovanni Rosotti
AU  - Miguel Vioque
PY  - 2026
DA  - 2026/09/04
PB  - arXiv
DO  - 10.48550/arxiv.2609.05366
UR  - https://arxiv.org/abs/2609.05366
AB  - Hints of planet formation have been independently reported within the gap of the disc around 2MASS J16120668-301027 from millimetre continuum, infrared, and H-alpha observations. In this work, we present new evidence for ongoing planet formation based on Atacama Large Millimeter/submillimeter Array (ALMA) Band 7 observations, detecting 0.87 mm dust continuum emission together with 12CO (J=3-2) and 13CO (J=3-2) line emission. Visibility modelling of the continuum data reveals an inner disc and two dust rings peaking at 23 and 75 au. The continuum morphology is better reproduced by an eccentric disc model (e approximately 0.1) than by an axisymmetric disc. We further investigate the gas kinematics through modelling of the 12CO channel maps. The residual line-width map shows a localised increase in velocity dispersion at the position of a previously reported circumplanetary disc candidate (deprojected radius approximately 32 au, position angle approximately 170 degrees) and along its orbit. This signal is spatially coincident with kink-like features and a transition from sub-Keplerian to super-Keplerian velocities. In addition, the velocity residual map exhibits an arc-like structure extending outward from the planet candidate, while the gas kinematics, despite substantial uncertainties, is consistent with inflow towards the candidate's orbital radius. The observed increase in velocity dispersion agrees with predictions from planet-disc interaction simulations, which produce enhanced turbulence both at the planet location and along its orbital path. Taken together, the continuum morphology and gas kinematic signatures provide compelling new evidence for ongoing planet formation within the disc gap.
ER  -