Resolving the planetesimal belt of HR 8799 with ALMA
Author
Abstract
The star HR 8799 hosts one of the largest known debris discs and at least four giant planets. Previous observations have found evidence for a warm belt within the orbits of the planets, a cold planetesimal belt beyond their orbits and a halo of small grains. With the infrared data, it is hard to distinguish the planetesimal belt emission from that of the grains in the halo. With this in mind, the system has been observed with ALMA in band 6 (1.34 mm) using a compact array format. These observations allow the inner edge of the planetesimal belt to be resolved for the first time. A radial distribution of dust grains is fitted to the data using an MCMC method. The disc is best fitted by a broad ring between 145(12)(+12) au and 429(32)(+37) au at an inclination of 40(6)(+5)degrees and a position angle of 51(8)(+8)degrees. A disc edge at similar to 145 au is too far out to be explained simply by interactions with planet b, requiring either a more complicated dynamical history or an extra planet beyond the orbit of planet b
Patrocinador
FONDECYT 3140479 3150106 1130857 1130949 1141175
Millennium Nucleus (Chilean Ministry of Economy) RC130007
BASAL CATA PFB-06
Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio IC 120009
STFC
ESO
European Union through ERC 279973
CONICYT-PCHA/Doctorado Nacional
Indexation
Artículo de publicación ISI
Quote Item
MNRAS 460, L10–L14 (2016)
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