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ISO-Oph 2 is a wide-separation (240 au) binary system where the primary starharbors a massive (M$_{dust}$ $\sim$40 M$_{\oplus}$) ring-like disk with a dustcavity $\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 mmcontinuum and $^{12}$CO molecular line observations of the system at 0''02 (3au) resolution. We resolve the disk around the primary into twonon-axisymmetric rings and find that the disk around the secondary is only$\sim$7 au across and also has a dust cavity (r $\sim$2.2 au). Based on theinfrared flux ratio of the system and the M0 spectral type of the primary, weestimate the mass of the companion to be close to the brown dwarf limit. Hence,we conclude that the ISO-Oph 2 system contains the largest and smallestcavities, the smallest measured disk size, and the resolved cavity around thelowest mass object (M$_{\star}$ $\sim$0.08 M$_\odot$) in Ophiuchus. From the$^{12}$CO data, we find a bridge of gas connecting both disks. While themorphology of the rings around the primary might be due to an unseen disturberwithin the cavity, we speculate that the bridge might indicate an alternativescenario in which the secondary has recently flown by the primary star causingthe azimuthal asymmetries in its disk. The ISO-Oph 2 system is therefore aremarkable laboratory to study disk evolution, planet formation, andcompanion-disk interactions.

the astrophysical journal. letters

A Tale of Two Transition Disks: ALMA long-baseline observations of  ISO-Oph 2 reveal two closely packed non-axisymmetric rings and a $\sim$2 au  cavity