Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 502, Issue 4, Pages 5779-5796Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab313
Keywords
techniques: interferometric; planet-disc interactions; stars: pre-main sequence
Categories
Funding
- Australian Government Research Training Program (RTP) Scholarship
- Australian Research Council [FT170100040, DP180104235, FT100100495]
- Banting Postdoctoral Fellowships programme
- STFC consolidated grant [ST/S000623/1]
- European Union [823823]
- ANR (Agence Nationale de la Recherche) of France [ANR-16-CE31-0013]
- LABEX Lyon Institute of Origins of the Universite de Lyon within the programme 'Investissements d'Avenir' of the French government [ANR-10-LABX-0066, ANR-11-IDEX-0007]
- Commonwealth of Australia
- Australian Research Council [FT100100495] Funding Source: Australian Research Council
- STFC [ST/S000623/1] Funding Source: UKRI
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The origin of inner dust cavities in transition discs remains unclear, with differences expected based on the clearing mechanism. Observations with ATCA and ALMA show that the brightness distributions of 8.8mm and sub-mm dust grains in transition discs peak at the same radius, suggesting a common cavity size possibly induced by a dust trap.
The origin of the inner dust cavities observed in transition discs remains unknown. The segregation of dust and size of the cavity is expected to vary depending on which clearing mechanism dominates grain evolution. We present the results from the Discs Down Under program, an 8.8-mm continuum Australia Telescope Compact Array (ATCA) survey targeting 15 transition discs with large (greater than or similar to 20 au) cavities and compare the resulting dust emission to Atacama Large millimetre/sub-millimetre Array (ALMA) observations. Our ATCA observations resolve the inner cavity for 8 of the 14 detected discs. We fit the visibilities and reconstruct 1D radial brightness models for 10 sources with a S/N > 5 sigma. We find that, for sources with a resolved cavity in both wavebands, the 8.8 mm and sub-mm brightness distributions peak at the same radius from the star. We suggest that a similar cavity size for 8.8 mm and sub-mm dust grains is due to a dust trap induced by the presence of a companion.
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