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DH Tau is a young ($\sim$1 Myr) classical T Tauri star. It is one of the fewyoung PMS stars known to be associated with a planetary mass companion, DH Taub, orbiting at large separation and detected by direct imaging. DH Tau b isthought to be accreting based on copious H${\alpha}$ emission and exhibitsvariable Paschen Beta emission. NOEMA observations at 230 GHz allow us to placeconstraints on the disk dust mass for both DH Tau b and the primary in a regimewhere the disks will appear optically thin. We estimate a disk dust mass forthe primary, DH Tau A of $17.2\pm1.7\,M_{\oplus}$, which gives a disk-to-starmass ratio of 0.014 (assuming the usual Gas-to-Dust mass ratio of 100 in thedisk). We find a conservative disk dust mass upper limit of 0.42$M_{\oplus}$for DH Tau b, assuming that the disk temperature is dominated by irradiationfrom DH Tau b itself. Given the environment of the circumplanetary disk,variable illumination from the primary or the equilibrium temperature of thesurrounding cloud would lead to even lower disk mass estimates. A MCFOSTradiative transfer model including heating of the circumplanetary disk by DHTau b and DH Tau A suggests that a mass averaged disk temperature of 22 K ismore realistic, resulting in a dust disk mass upper limit of 0.09$M_{\oplus}$for DH Tau b. We place DH Tau b in context with similar objects and discuss theconsequences for planet formation models.

An upper limit on the mass of the circumplanetary disk for DH Tau b