Kavli Affiliate: Gregory J. Herczeg
| First 5 Authors: Camilo González-Ruilova, Lucas A. Cieza, Antonio S. Hales, Sebastián Pérez, Alice Zurlo
| Summary:
ISO-Oph 2 is a wide-separation (240 au) binary system where the primary star
harbors a massive (M$_{dust}$ $sim$40 M$_{oplus}$) ring-like disk with a dust
cavity $sim$50 au in radius and the secondary hosts a much lighter (M$_{dust}$
$sim$0.8 M$_{oplus}$) 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 0”02 (3
au) resolution. We resolve the disk around the primary into two
non-axisymmetric rings and find that the disk around the secondary is only
$sim$7 au across and also has a dust cavity (r $sim$2.2 au). Based on the
infrared flux ratio of the system and the M0 spectral type of the primary, we
estimate the mass of the companion to be close to the brown dwarf limit. Hence,
we conclude that the ISO-Oph 2 system contains the largest and smallest
cavities, the smallest measured disk size, and the resolved cavity around the
lowest mass object (M$_{star}$ $sim$0.08 M$_odot$) 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.
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