First Millimeter Detection of the Disk around a Young, Isolated, Planetary-mass Object

• Main Authors: Bayo, Amelia, Joergens, Viki, Liu, Yao, Brauer, Robert, Olofsson, Johan, Arancibia, Javier, Pinilla, Paola, Wolf, Sebastian, Ruge, Jan Philipp, Henning, Thomas, Natta, Antonella, Johnston, Katharine G., Bonnefoy, Mickael, Beuther, Henrik, Chauvin, Gael
• Other Authors: Univ Arizona, Dept Astron, Steward Observ
• Language: en
• Published: IOP PUBLISHING LTD 2017
• Subjects: brown dwarfs; stars: formation; stars: low-mass; stars: pre-main sequence
• Online Access: http://hdl.handle.net/10150/624481; http://arizona.openrepository.com/arizona/handle/10150/624481

OTS44 is one of only four free-floating planets known to have a disk. We have previously shown that it is the coolest and least massive known free-floating planet (similar to 12 M-Jup) with a substantial disk that is actively accreting. We have obtained Band 6 (233 GHz) ALMA continuum data of this very young disk-bearing object. The data show a clear unresolved detection of the source. We obtained disk-mass estimates via empirical correlations derived for young, higher-mass, central (substellar) objects. The range of values obtained are between 0.07 and 0.63 M-circle plus (dust masses). We compare the properties of this unique disk with those recently reported around higher-mass (brown dwarfs) young objects in order to infer constraints on its mechanism of formation. While extreme assumptions on dust temperature yield disk-mass values that could slightly diverge from the general trends found for more massive brown dwarfs, a range of sensible values provide disk masses compatible with a unique scaling relation between M-dust and M* through the substellar domain down to planetary masses.