We present high resolution ( \sim 0.1 \arcsec ) , very high Strehl ratio ( 0.97 \pm 0.03 ) mid-infrared ( IR ) adaptive optics ( AO ) images of the AGB star RV Boo utilizing the MMT adaptive secondary AO system .
RV Boo was observed at a number of wavelengths over two epochs ( 9.8 \mu m in May 2003 , 8.8 , 9.8 and 11.7 \mu m in February 2004 ) and appeared slightly extended at all wavelengths .
While the extension is very slight at 8.8 and 11.7 \mu m data , the extension is somewhat more pronounced at 9.8 \mu m. With such high Strehls we can achieve super-resolutions of 0.1 \arcsec by deconvolving RV Boo with a point-spread function ( PSF ) derived from an unresolved star .
We tentatively resolve RV Boo into a 0.16 \arcsec FWHM extension at a position angle of 120 degrees .
At a distance of 390 ^ { +250 } _ { -100 } pc , this corresponds to a FWHM of 60 ^ { +40 } _ { -15 } AU .
We measure a total flux at 9.8 \mu m of 145 \pm 24 Jy for the disk and star .
Based on a dust thermal emission model for the observed IR spectral energy distribution and the 9.8 \mu m AO image , we derive a disk dust mass of 1.6 \times 10 ^ { -6 } M _ { \sun } and an inclination of 30 to 45 ^ { \circ } from edge-on .
We discuss whether the dust disk observed around RV Boo is an example of the early stages in the formation of asymmetric structure in planetary nebula .