the frame.[]{data-label="fig:keck"}](her99b_fig_v2.eps){width="45.00000%"}

To try and resolve this issue we obtained an adaptive optics image of 99 Her at L’ (3.8 $\mu$m) using the NIRC2 camera at Keck II on July 27, 2011, shown in Figure \[fig:keck\]. We adopted the narrow camera (10 mas/pixel) and used a five-point dither pattern with three images obtained at each position consisting of 25 coadds of 0.181 seconds integration. The cumulative integration time for the final co-registered and coadded image is 67.875 seconds. The core of the A component point-spread-function is highly saturated, which degrades the achievable astrometry. We estimate the position of 99 Her A by determining the geometric center of the first diffraction ring. The position of 99 Her B is taken from the centroid of the unsaturated core. The PA and separation are quoted above.

There is no detection of the putative 99 Her C within 1.6” of the primary in the combined image if it is only a factor 2.4 fainter than the B component, because it would appear 20 times brighter than the brightest speckles. However, if it were closer to the primary than 0.2” it would currently be too close to detect. If the object was fixed on the 