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We present sensitive observations carried out with the Atacama LargeMillimeter/Submillimeter Array (ALMA) of the dusty debris disk HD 95086. Theseobservations were made in bands 6 (223 GHz) and 7 (338 GHz) with an angularresolution of about 1$''$ which allowed us to resolve well the debris disk witha deconvolved size of 7.0$''$ $\times$ 6.0$''$ and with an inner depression ofabout 2$''$. We do not detect emission from the star itself and the possibleinner dusty belt. We also do not detect CO (J=2-1) and (J=3-2) emission,excluding the possibility of an evolved gaseous primordial disk as noted inprevious studies of HD95086. We estimated a lower limit for the gas mass of$\leq$0.01 M$_\oplus$ for the debris disk of HD95086. From the mm. emission, wecomputed a dust mass for the debris disk HD95086 of 0.5$\pm$0.2 M$_\oplus$,resulting in a dust-to-gas ratio of $\geq$50. Finally, we confirm the detectionof a strong submillimeter source to the northwest of the disk (ALMA-SMM1)revealed by recent ALMA observations. This new source might be interpreted as aplanet in formation on the periphery of the debris disk HD 95086 or as a strongimpact between dwarf planets. However, given the absence of the proper motionsof ALMA-SMM1 similar to those reported in the debris disk (estimated from thesenew ALMA observations) and for the optical star, this is more likely to be asubmillimeter background galaxy.

A Submillimeter Galaxy Projected on the Debris Disk of HD 95086