An optical model of the wide-field imaging interferometry testbed

Leisawitz, David; Martino, Anthony J.; Thompson, Anita Kotha; Rinehart, Stephen A.; Frey, Bradley J.

doi:10.1117/12.735145

Cited by 8 publications

(5 citation statements)

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“…(13) and (14) are bandlimited by the diameters of the input apertures, and WIIT is designed to be at least Nyquist sampled according to the diameter of a single aperture. Details of WIIT's optical parameters and source capabilities can be found in other publications [3][4][5][6][7][8][9][10][11][12][13]. A typical WIIT datacube contains between two and three thousand images, one for each of the sampled delay positions L, so the act of preprocessing reduces the standard deviation of the noise in the average of Eq.…”

Section:  mentioning

confidence: 99%

“…The experimental realization that we are most concerned with is NASA's Widefield Imaging Interferometry Testbed (WIIT), which was built for the advancement of spatio-spectral interferometry in preparation for future space-based observatories [3][4][5][6][7][8][9][10][11][12][13]. This state-of-the-art testbed resides in the well-controlled environment of the Advanced Interferometry and Metrology laboratory at Goddard Space Flight Center; however, despite the quality of the environment, the light source to WIIT, known as the calibrated hyperspectral image projector (CHIP) [14][15][16], generates heat that causes mild image motion between measurements.…”

Section: Introductionmentioning

confidence: 99%

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Rotation and translation registration of bandlimited interferometric images using a chirp z-transform

2016

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Image reconstruction algorithms for wide-field spatio-spectral interferometry require knowledge of registration parameters associated with low-resolution image measurements at various baseline orientations, such that the images can be registered to within the fine resolution of the final desired image. We have developed an image registration procedure that combines a nonlinear optimization algorithm with the sub-pixel precision of chirp z-transform resampling, particularly for rotation and translation, of bandlimited images with non-radially symmetric aberrations. We show the accuracy of this image registration technique on simulated images that have a complexity comparable to scenes observed experimentally with NASA's wide-field imaging interferometry testbed. Registration to within a tenth of a pixel for translation and within three arcminutes for rotation is demonstrated at the largest simulated noise levels.

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Section:  mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Rotation and translation registration of bandlimited interferometric images using a chirp z-transform

2016

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“…Although the theoretical groundwork for double-Fourier interferometry has already been established [1][2][3][4][5] , the space-based spatio-spectral interferometric imaging technique needs further characterization before an interferometric observatory, such as the NASA proposed Space Infrared Interferometric Telescope (SPIRIT) 8 , ever becomes a reality. This prompted NASA to build the Wide-field Imaging Interferometry Testbed (WIIT) [9][10][11][12][13][14][15][16][17][18][19][20] . The WIIT was developed by NASA to further the maturation of wide-field spatio-spectral interferometry in order to meet the demands of future astronomical hyperspectral imaging missions.…”

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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“…The Wide-field Imaging Interferometry Testbed (WIIT) at GSFC was designed to explore practical limitations of the wide field-of-view "double Fourier" technique, which is currently at TRL 4. [7,8,9] …”

Section: The Spirit Origins Probe Mission Conceptmentioning

confidence: 99%

“…https://ntrs.nasa.gov/search.jsp?R=20080030265 2018-05-13T02:30:51+00:00Z (2007) [7,8] update the status of our development of the wide-field imaging interferometry technique applicable to SPIRIT, and [9] describe a model of the Wide-field Imaging Interferometry Testbed, a model which can be adapted to simulate interferometric data from SPIRIT.…”

Section: Introductionmentioning

confidence: 99%

The Space Infrared Interferometric Telescope (SPIRIT): the mission design solution space and the art of the possible

Leisawitz

Hyde

Rinehart

et al. 2008

Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter

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Although the Space Infrared Interferometric Telescope (SPIRIT) was studied as a candidate NASA Origins Probe mission, the real world presents a broader set of options, pressures, and constraints. Fundamentally, SPIRIT is a far-IR observatory for high-resolution imaging and spectroscopy designed to address a variety of compelling scientific questions. How do planetary systems form from protostellar disks, dousing some planets in water while leaving others dry? Where do planets form, and why are some ice giants while others are rocky? How did high-redshift galaxies form and merge to form the present-day population of galaxies? This paper takes a pragmatic look at the mission design solution space for SPIRIT, presents Probe-class and facility-class mission scenarios, and describes optional design changes. The costs and benefits of various mission design alternatives are roughly evaluated, giving a basis for further study and to serve as guidance to policy makers.

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An optical model of the wide-field imaging interferometry testbed

Cited by 8 publications

References 8 publications

Rotation and translation registration of bandlimited interferometric images using a chirp z-transform

Rotation and translation registration of bandlimited interferometric images using a chirp z-transform

Nonnegative matrix factorization for efficient hyperspectral image projection

The Space Infrared Interferometric Telescope (SPIRIT): the mission design solution space and the art of the possible

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