Spectral Optical Transfer Function of a Wide-Field Double-Fourier Interferometer

Iacchetta, Alexander S.; Fienup, James R.; Leisawitz, David

doi:10.1364/isa.2015.it2a.2

Cited by 1 publication

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“…The optical path following one of the mirrors is kept fixed while the other can vary, resulting in a measured datacube for each baseline separation. Taking the Fourier transform of these datacubes over the delay dimension results in a set of high-pass filtered images, where the passband in the spatial frequency domain is related to both the baseline and wavelength 7 . A single high-spatial-resolution hyperspectral image can be recovered from the set of high-pass filtered images using an image synthesis algorithm, such as the algorithm developed by Lyon et al 4,5 .…”

Section: Introductionmentioning

confidence: 99%

Nonnegative matrix factorization for efficient hyperspectral image projection

et al. 2015

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Hyperspectral imaging for remote sensing has prompted development of hyperspectral image projectors that can be used to characterize hyperspectral imaging cameras and techniques in the lab. One such emerging astronomical hyperspectral imaging technique is wide-field double-Fourier interferometry. NASA's current, state-of-the-art, Wide-field Imaging Interferometry Testbed (WIIT) uses a Calibrated Hyperspectral Image Projector (CHIP) to generate test scenes and provide a more complete understanding of wide-field double-Fourier interferometry. Given enough time, the CHIP is capable of projecting scenes with astronomically realistic spatial and spectral complexity. However, this would require a very lengthy data collection process. For accurate but time-efficient projection of complicated hyperspectral images with the CHIP, the field must be decomposed both spectrally and spatially in a way that provides a favorable trade-off between accurately projecting the hyperspectral image and the time required for data collection. We apply nonnegative matrix factorization (NMF) to decompose hyperspectral astronomical datacubes into eigenspectra and eigenimages that allow time-efficient projection with the CHIP. Included is a brief analysis of NMF parameters that affect accuracy, including the number of eigenspectra and eigenimages used to approximate the hyperspectral image to be projected. For the chosen field, the normalized mean squared synthesis error is under 0.01 with just 8 eigenspectra. NMF of hyperspectral astronomical fields better utilizes the CHIP's capabilities, providing time-efficient and accurate representations of astronomical scenes to be imaged with the WIIT.

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Section: Introductionmentioning

confidence: 99%