Comparing Non-Redundant Masking and Filled-Aperture Kernel Phase for Exoplanet Detection and Characterization. (arXiv:1901.01266v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sallum_S/0/1/0/all/0/1">Steph Sallum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skemer_A/0/1/0/all/0/1">Andy Skemer</a>
The limitations of adaptive optics and coronagraph performance make exoplanet
detection close to {lambda}/D extremely difficult with conventional imaging
methods. The technique of non-redundant masking (NRM), which turns a filled
aperture into an interferometric array, has pushed the planet detection
parameter space to within {lambda}/D. For high Strehl, the related
filled-aperture kernel phase technique can achieve resolution comparable to
NRM, without the associated dramatic decrease in throughput. We present
non-redundant masking and kernel phase contrast curves generated for ground-
and space-based instruments. We use both real and simulated observations to
assess the performance of each technique, and discuss their capabilities for
different exoplanet science goals such as broadband detection and spectral
characterization.
The limitations of adaptive optics and coronagraph performance make exoplanet
detection close to {lambda}/D extremely difficult with conventional imaging
methods. The technique of non-redundant masking (NRM), which turns a filled
aperture into an interferometric array, has pushed the planet detection
parameter space to within {lambda}/D. For high Strehl, the related
filled-aperture kernel phase technique can achieve resolution comparable to
NRM, without the associated dramatic decrease in throughput. We present
non-redundant masking and kernel phase contrast curves generated for ground-
and space-based instruments. We use both real and simulated observations to
assess the performance of each technique, and discuss their capabilities for
different exoplanet science goals such as broadband detection and spectral
characterization.
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