Location
University of Richmond, Richmond, Virginia
Document Type
Poster
Description
Imaging telescopes with asymmetric antenna patterns that vary with wavelength can create time-ordered data that may be processed into multiple images corresponding to different bands of wavelengths from just a single set of scans. The imaging telescope named QUBIC has this property and is the inspiration behind this project. Our goal is to quantify, both statistically and analytically, the ability of these telescopes to perform such a reconstruction given different cases. In the case that the telescope is observing the full sky, we reconstruct our maps via a spherical harmonic basis. In this way, the reconstructed images are described as a set of spherical harmonic coefficients, whose properties can be analyzed and computed relatively easily. In the case that the telescope is only observing part of the sky, we must reconstruct maps with a value assigned to each discretized point in the sky, and thus more computation and analysis is required. In each case, we find eigenvectors in wavelength space that maximize the reconstructed signal-to-noise ratio, and use these to quantify the number of maps that can be reconstructed accurately. This project is inspired by the instrument QUBIC, whose antenna pattern consists of a large central Gaussian peak, along with many smaller Gaussian peaks that are both asymmetrically distributed and separated by a distance that is dependent on wavelength.
Included in
Polychromatic Map Reconstruction Using Telescopes with Asymmetric Antenna Patterns
University of Richmond, Richmond, Virginia
Imaging telescopes with asymmetric antenna patterns that vary with wavelength can create time-ordered data that may be processed into multiple images corresponding to different bands of wavelengths from just a single set of scans. The imaging telescope named QUBIC has this property and is the inspiration behind this project. Our goal is to quantify, both statistically and analytically, the ability of these telescopes to perform such a reconstruction given different cases. In the case that the telescope is observing the full sky, we reconstruct our maps via a spherical harmonic basis. In this way, the reconstructed images are described as a set of spherical harmonic coefficients, whose properties can be analyzed and computed relatively easily. In the case that the telescope is only observing part of the sky, we must reconstruct maps with a value assigned to each discretized point in the sky, and thus more computation and analysis is required. In each case, we find eigenvectors in wavelength space that maximize the reconstructed signal-to-noise ratio, and use these to quantify the number of maps that can be reconstructed accurately. This project is inspired by the instrument QUBIC, whose antenna pattern consists of a large central Gaussian peak, along with many smaller Gaussian peaks that are both asymmetrically distributed and separated by a distance that is dependent on wavelength.
Comments
Faculty Mentor: Dr. Emory F. Bunn