  Imaging the direct light signal from a faint exoplanet against the
overwhelming glare of its host star presents one of the fundamental challenges
to modern astronomical instrumentation. Achieving sufficient signal-to-noise
for detection by direct imaging is limited by three basic physical processes:
aberration of the wavefronts (both instrumental and atmospheric), photon noise,
and detector noise. In this paper, we advance a novel optical setup which
synthesizes the advantages of two different techniques: nulling interferometry
to mitigate photon noise, and closure phase to combat optical aberrations. Our
design, which employs technology from integrated optics and photonics, is
intended to combine the advantageous aspects of both a coronagraph and a
non-redundant interferometer inside a single optical device. We show that such
an instrument would have a dynamic range limited either by i) the readout noise
(if perfect co-phasing), or ii) the photon noise due to stellar flux leakage
(in the case of imperfect nulling). This concept is optimal when the readout
noise is not the main limitation, ie, for space interferometry or for ground
based observations of bright stellar hosts (apparent magnitude brighter than
10).
