Issue |
A&A
Volume 648, April 2021
|
|
---|---|---|
Article Number | A19 | |
Number of page(s) | 16 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202039469 | |
Published online | 07 April 2021 |
A highly non-Keplerian protoplanetary disc
Spiral structure in the gas disc of CQ Tau★
1
Max-Planck-Institut für extraterrestrische Physik,
Gießenbachstr. 1,
85748
Garching bei München,
Germany
e-mail: woelfer@mpe.mpg.de
2
Universitäts-Sternwarte München,
Scheinerstr. 1,
81679
München, Germany
3
European Southern Observatory,
Karl-Schwarzschild-Str. 2,
85748
Garching bei München,
Germany
4
Departamento de Astronomía, Universidad de Chile,
Camino El Observatorio 1515,
Las Condes,
Santiago, Chile
5
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg, Germany
6
Center for Astrophysics | Harvard & Smithsonian,
60 Garden Street,
Cambridge,
MA
02138, USA
7
Leiden Observatory, Leiden University,
PO Box 9513,
2300 RA
Leiden, The Netherlands
8
Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS,
UMI
3386, Chile
9
Univ. Grenoble Alpes, CNRS, IPAG,
38000
Grenoble, France
10
Excellence Cluster Origin and Structure of the Universe,
Boltzmannstr. 2,
85748
Garching bei München, Germany
11
Dipartimento di Fisica, Università degli Studi di Milano,
Via Giovanni Celoria 16,
20133
Milano, Italy
12
INAF – Osservatorio Astrofisico di Arcetri,
Largo E. Fermi 5,
50125
Firenze, Italy
Received:
18
September
2020
Accepted:
8
December
2020
Context. In recent years high-angular-resolution observations have revealed that circumstellar discs appear in a variety of shapes with diverse substructures being ubiquitous. This has given rise to the question of whether these substructures are triggered by planet–disc interactions. Besides direct imaging, one of the most promising methods to distinguish between different disc-shaping mechanisms is to study the kinematics of the gas disc. In particular, the deviations of the rotation profile from Keplerian velocity can be used to probe perturbations in the gas pressure profile that may be caused by embedded (proto-) planets.
Aims. In this paper we aim to analyse the gas brightness temperature and kinematics of the transitional disc around the intermediate-mass star CQ Tau in order to resolve and characterise substructure in the gas caused by possible perturbers.
Methods. For our analysis we used spatially resolved ALMA observations of the three CO isotopologues 12CO, 13CO, and C18O (J = 2−1) from the disc around CQ Tau. We further extracted robust line centroids for each channel map and fitted a number of Keplerian disc models to the velocity field.
Results. The gas kinematics of the CQ Tau disc present non-Keplerian features, showing bent and twisted iso-velocity curves in 12CO and 13CO. Significant spiral structures are detected between ~10 and 180 au in both the brightness temperature and the rotation velocity of 12CO after subtraction of an azimuthally symmetric model, which may be tracing planet–disc interactions with an embedded planet or low-mass companion. We identify three spirals, two in the brightness temperature and one in the velocity residuals, spanning a large azimuth and radial extent. The brightness temperature spirals are morphologically connected to spirals observed in near-infrared scattered light in the same disc, indicating a common origin. Together with the observed large dust and gas cavity, these spiral structures support the hypothesis of a massive embedded companion in the CQ Tau disc.
Key words: accretion, accretion disks / protoplanetary disks / planet–disk interactions / submillimeter: planetary systems / stars: individual: CQ Tau
The reduced datacubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/648/A19
© L. Wölfer et al. 2021
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Open Access funding provided by Max Planck Society.
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