We have obtained ALMA Band 7 observations of the FU Ori outburst system at 0.6 \arcsec \times 0.5 \arcsec resolution to measure the link between the inner disk instability and the outer disk through sub-mm continuum and molecular line observations .
Our observations detect continuum emission which can be well modeled by two unresolved sources located at the position of each binary component .
The interferometric observations recover the entire flux reported in previous single-dish studies , ruling out the presence of a large envelope .
Assuming that the dust is optically thin , we derive disk dust masses of 2 \times 10 ^ { -4 } M _ { \odot } and 8 \times 10 ^ { -5 } M _ { \odot } , for the north and south components respectively .
We place limits on the disks ’ radii of r < 45 AU .
We report the detection of molecular emission from ^ { 12 } CO ( 3-2 ) , HCO ^ { + } ( 4-3 ) and from HCN ( 4-3 ) .
The ^ { 12 } CO appears widespread across the two binary components , and is slightly more extended than the continuum emission .
The denser gas tracer HCO ^ { + } peaks close to the position of the southern binary component , while HCN appears peaked at the position of the northern component .
This suggests that the southern binary component is embedded in denser molecular material , consistent with previous studies that indicate a heavily reddened object .
At this angular resolution any interaction between the two unresolved disk components can not be disentangled .
Higher resolution images are vital to understanding the process of star formation via rapid accretion FU Ori-type episodes .