  We present sensitive observations carried out with the Atacama Large
Millimeter/Submillimeter Array (ALMA) of the dusty debris disk HD 95086. These
observations were made in bands 6 (223 GHz) and 7 (338 GHz) with an angular
resolution of about 1$''$ which allowed us to resolve well the debris disk with
a deconvolved size of 7.0$''$ $\times$ 6.0$''$ and with an inner depression of
about 2$''$. We do not detect emission from the star itself and the possible
inner 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 in
previous 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, we
computed 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 detection
of a strong submillimeter source to the northwest of the disk (ALMA-SMM1)
revealed by recent ALMA observations. This new source might be interpreted as a
planet in formation on the periphery of the debris disk HD 95086 or as a strong
impact between dwarf planets. However, given the absence of the proper motions
of ALMA-SMM1 similar to those reported in the debris disk (estimated from these
new ALMA observations) and for the optical star, this is more likely to be a
submillimeter background galaxy.
