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Rings and gaps in the disc around Elias 24 revealed by ALMA

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posted on 29.01.2018, 17:14 by G. Dipierro, L. Ricci, L. Pérez, G. Lodato, R. D. Alexander, G. Laibe, S. Andrews, J. M. Carpenter, C. J. Chandler, J. A. Greaves, C. Hall, T. Henning, W. Kwon, H. Linz, L. Mundy, A. Sargent, M. Tazzari, L. Testi, D. Wilner
We present Atacama Large Millimeter/sub-millimeter Array (ALMA) Cycle 2 observations of the 1.3 mm dust continuum emission of the protoplanetary disc surrounding the T Tauri star Elias 24 with an angular resolution of ∼0.2″ (∼28 au). The dust continuum emission map reveals a dark ring at a radial distance of 0.47″ (∼65 au) from the central star, surrounded by a bright ring at 0.58″ (∼81 au). In the outer disc, the radial intensity profile shows two inflection points at 0.71″ and 0.87″ (∼99 and 121 au respectively). We perform global three-dimensional smoothed particle hydrodynamic gas/dust simulations of discs hosting a migrating and accreting planet. Combining the dust density maps of small and large grains with three dimensional radiative transfer calculations, we produce synthetic ALMA observations of a variety of disc models in order to reproduce the gap- and ring-like features observed in Elias 24. We find that the dust emission across the disc is consistent with the presence of an embedded planet with a mass of ∼0.7MJ at an orbital radius of ∼ 60 au. Our model suggests that the two inflection points in the radial intensity profile are due to the inward radial motion of large dust grains from the outer disc. The surface brightness map of our disc model provides a reasonable match to the gap- and ring-like structures observed in Elias 24, with an average discrepancy of ∼ 5% of the observed fluxes around the gap region.

Funding

referee for constructive comments that improved this manuscript. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00498.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research used the ALICE High Performance Computing Facility at the University of Leicester. Some resources on ALICE form part of the DiRAC Facility jointly funded by STFC and the Large Facilities Capital Fund of BIS. The authors are grateful to C. P. Dullemond for making RADMC-3D available. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 681601). J.M.C. acknowledges support from the National Aeronautics and Space Administration under Grant No. 15XRP15 20140 issued through the Exoplanets Research Program. M.T. has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC- 2013-ADG. We used SPLASH (Price 2007).

History

Citation

Monthly Notices of the Royal Astronomical Society, 2018, sty181

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP), Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Acceptance date

17/01/2018

Copyright date

2018

Available date

29/01/2018

Publisher version

https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/sty181/4822167

Language

en

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