ORCID Profile
0000-0001-8764-1780
Current Organisation
UCL Academy
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Publisher: American Astronomical Society
Date: 14-10-2015
Publisher: EDP Sciences
Date: 06-2015
Publisher: American Astronomical Society
Date: 10-2020
Abstract: ISO-Oph 2 is a wide-separation (240 au) binary system where the primary star harbors a massive ( M dust ∼ 40 M ⊕ ) ring-like disk with a dust cavity ∼50 au in radius and the secondary hosts a much lighter ( M dust ∼ 0.8 M ⊕ ) disk. As part of the high-resolution follow-up of the “Ophiuchus Disk Survey Employing ALMA” (ODISEA) project, we present 1.3 mm continuum and 12 CO molecular line observations of the system at 002 (3 au) resolution. We resolve the disk around the primary into two nonaxisymmetric rings and find that the disk around the secondary is only ∼7 au across and also has a dust cavity ( r ∼ 2.2 au). Based on the infrared flux ratio of the system and the M0 spectral type of the primary, we estimate the mass of the companion to be close to the brown-dwarf limit. Hence, we conclude that the ISO-Oph 2 system contains the largest and smallest cavities, the smallest measured disk size, and the resolved cavity around the lowest-mass object ( M ⋆ ∼ 0.08 M ⊙ ) in Ophiuchus. From the 12 CO data, we find a bridge of gas connecting both disks. While the morphology of the rings around the primary might be due to an unseen disturber within the cavity, we speculate that the bridge might indicate an alternative scenario in which the secondary has recently flown by the primary star causing the azimuthal asymmetries in its disk. The ISO-Oph 2 system is therefore a remarkable laboratory to study disk evolution, planet formation, and companion–disk interactions.
Publisher: Oxford University Press (OUP)
Date: 10-12-2020
Abstract: We present 1.3 mm continuum ALMA long-baseline observations at 3–5 au resolution of 10 of the brightest discs from the Ophiuchus DIsc Survey Employing ALMA (ODISEA) project. We identify a total of 26 narrow rings and gaps distributed in 8 sources and 3 discs with small dust cavities (r & au). We find that two discs around embedded protostars lack the clear gaps and rings that are ubiquitous in more evolved sources with Class II SEDs. Our s le includes five objects with previously known large dust cavities (r & au). We find that the 1.3 mm radial profiles of these objects are in good agreement with those produced by numerical simulations of dust evolution and planet–disc interactions, which predict the accumulation of mm-sized grains at the edges of planet-induced cavities. Our long-baseline observations resulted in the largest s le of discs observed at ∼3–5 au resolution in any given star-forming region (15 objects when combined with Ophiuchus objects in the DSHARP Large Program) and allow for a demographic study of the brightest $\\sim\\! 5{{\\ \\rm per\\ cent}}$ of the discs in Ophiuchus (i.e. the most likely formation sites of giant planets in the cloud). We use this unique s le to propose an evolutionary sequence and discuss a scenario in which the substructures observed in massive protoplanetary discs are mainly the result of planet formation and dust evolution. If this scenario is correct, the detailed study of disc substructures might provide a window to investigate a population of planets that remains mostly undetectable by other techniques.
Publisher: Oxford University Press (OUP)
Date: 13-08-2015
Location: United Kingdom of Great Britain and Northern Ireland
Location: United States of America
No related grants have been discovered for Paola Pinilla.