  Sub-milliarcsecond imaging of nearby main sequence stars and binary systems
can provide critical information on stellar phenomena such as rotational
deformation, accretion effects, and the universality of starspot (sunspot)
cycles. Achieving this level of resolution in optical wavelength bands (U/V)
requires use of a sparse array of interferometric telescopes with kilometer
scale baseline separations. Current ground based VHE gamma-ray observatories,
such as VERITAS, HESS, and MAGIC, employ arrays of > 10 m diameter optical
Imaging Atmospheric Cherenkov Telescopes (IACTs) with >80 m telescope
separations, and are therefore well suited for sub-milliarcsecond astronomical
imaging in the U/V bands using Hanbury Brown and Twiss (HBT) interferometry
[1,2]. We describe the development of instrumentation for the augmentation of
IACT arrays to perform Stellar Intensity Interferometric (SII) imaging.
Laboratory tests are performed using pseudo-random and thermal (blackbody)
light to demonstrate the ability of high speed (250 MHz) digitizing electronics
to continuously record photon intensity over long periods (minutes to hours)
and validate the use of offline software correlation to calculate the squared
degree of coherence . We then use as the interferometric observable to populate
the Fourier reciporical image plane, and apply standard inversion techniques to
recover the original 2-D source image. The commercial availability of
inexpensive fiber-optic based sub-nanosecond multi-crate (White Rabbit[3])
synchronization timing enables the extension of SII to baselines greater than
10 km, theoretically allowing U/V band imaging with resolution <100 $\mu$
arc-seconds. This article provides a description of typical designs of
practical SII instrumentation for the VERITAS IACT observatory array (Amado,
Arizona) and the future CTA IACT Observatory (Canary Islands, Spain and
Paranal, Chile).
