DH Tau is a young ( \sim 1 Myr ) classical T Tauri star .
It is one of the few young PMS stars known to be associated with a planetary mass companion , DH Tau b , orbiting at large separation and detected by direct imaging .
DH Tau b is thought to be accreting based on copious H { \alpha } emission and exhibits variable Paschen Beta emission .
NOEMA observations at 230 GHz allow us to place constraints on the disk dust mass for both DH Tau b and the primary in a regime where the disks will appear optically thin .
We estimate a disk dust mass for the primary , DH Tau A of 17.2 \pm 1.7 M _ { \oplus } , which gives a disk-to-star mass ratio of 0.014 ( assuming the usual Gas-to-Dust mass ratio of 100 in the disk ) .
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 irradiation from DH Tau b itself .
Given the environment of the circumplanetary disk , variable illumination from the primary or the equilibrium temperature of the surrounding cloud would lead to even lower disk mass estimates .
A MCFOST radiative transfer model including heating of the circumplanetary disk by DH Tau b and DH Tau A suggests that a mass averaged disk temperature of 22 K is more 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 the consequences for planet formation models .