  We present ALMA 12-m, 7-m & Total Power (TP) Array observations of the FU
Orionis outbursting system, covering spatial scales ranging from 160 to 25,000
au. The high-resolution interferometric data reveals an elongated
$^{12}$CO(2-1) feature previously observed at lower resolution in
$^{12}$CO(3-2). Kinematic modeling indicates that this feature can be
interpreted as an accretion streamer feeding the binary system. The mass infall
rate provided by the streamer is significantly lower than the typical stellar
accretion rates (even in quiescent states), suggesting that this streamer alone
is not massive enough to sustain the enhanced accretion rates characteristic of
the outbursting class prototype. The observed streamer may not be directly
linked to the current outburst but rather a remnant of a previous, more massive
streamer that may have contributed enough to the disk mass to render it
unstable and trigger FU Ori's outburst. The new data detects, for the first
time, a vast, slow-moving carbon monoxide molecular outflow emerging from this
object. To accurately assess the outflow properties (mass, momentum, kinetic
energy), we employed $^{13}$CO(2-1) data to correct for optical depth effects.
The analysis indicates that the outflow corresponds to swept-up material not
associated with the current outburst, similar to slow-molecular outflows
observed around other FUor and Class I protostellar objects.
