We present far-infrared and submillimeter maps from the Herschel Space Observatory and the James Clerk Maxwell Telescope of the debris disk host star AU Microscopii .
Disk emission is detected at 70 , 160 , 250 , 350 , 450 , 500 and 850 µm .
The disk is resolved at 70 , 160 and 450 µm .
In addition to the planetesimal belt , we detect thermal emission from AU Mic ’ s halo for the first time .
In contrast to the scattered light images , no asymmetries are evident in the disk .
The fractional luminosity of the disk is 3.9 \times 10 ^ { -4 } and its mm-grain dust mass is 0.01 M _ { \oplus } ( \pm 20 % ) .
We create a simple spatial model that reconciles the disk SED as a blackbody of 53 \pm 2 K ( a composite of 39 and 50 K components ) and the presence of small ( non-blackbody ) grains which populate the extended halo .
The best fit model is consistent with the “ birth ring ” model explored in earlier works , i.e. , an edge-on dust belt extending from 8.8-40 AU , but with an additional halo component with an r ^ { -1.5 } surface density profile extending to the limits of sensitivity ( 140 AU ) .
We confirm that AU Mic does not exert enough radiation force to blow out grains .
For stellar mass loss rates of 10-100x solar , compact ( zero porosity ) grains can only be removed if they are very small ; consistently with previous work , if the porosity is 0.9 , then grains approaching 0.1 µm can be removed via corpuscular forces ( i.e. , the stellar wind ) .