Kavli Affiliate: Ruobing Dong
| Summary:
GQ Lup B is a massive (10-40 M$_textJup$) companion orbiting the young T-Tauri star GQ Lup A at a projected distance of $sim$110 au (0.7”). It is outside the circumprimary disk in the submm continuum, but its $sim,63^circ$ inclined orbit intersects the primary’s gas disk twice per period. We report a 5.8$σ$ detection of continuum emission at the location of GQ Lup B, obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 0.89 mm (band 7). We associate this emission with a dusty disk around the companion, already detected by VLT/NACO and JWST/MIRI in the mid-Infrared. To date, this is the third disk observed at mm wavelengths around a companion spanning the brown dwarf and planetary mass regimes, following PDS 70 c, a gas giant embedded in the parent circumstellar disk, and SR 12 c, a planetary-mass companion at 1200 au from the primary. We retrieve a point source with peak intensity $54.5pm9.4,μrm Jy, beam^-1$, co-spatial with GRAVITY astrometry. The emission is spatially unresolved, placing an upper limit on the source radius of 2.3 au (from a synthesized beam of $sim,29times25$ mas). For comparison, this is smaller than 1/3 of the Hill’s radius (3-5 au for GQ Lup B, depending on the assumed mass), the theoretical upper limit for circum-planetary disks. Assuming optically thin thermal emission from mm-size grains in a disk-like structure, we infer a mass of 0.0032 M$_oplus$, while the optically thick limit yields an emission radius of 0.2 au. Assuming a gas to dust ratio of 100, our results indicate a very low disk mass to accretion rate ratio, of the order of $sim10^4$ years, analogously to the highest accretors in the stellar mass regime. In the case of GQ Lup B, this can be explained by its periodic crossings of the circumprimary disk, which could deliver a substantial amount of gas to the companion’s disk over a long timescale.
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