Control de aberraciones del telescopio de 2.1-m del OAN por medio de la codificación del frente de onda
Wave-front coding is a known technique for correcting defocus-like aberrations by introducing an aspherical phase distribution in to a standard clear aperture system, resulting in a near diffracted limited image by using deconvolution techniques. With this technology, we want to improve the image qu...
| Autor: | |
|---|---|
| Tipo de recurso: | tesis doctoral |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2016 |
| País: | México |
| Institución: | Instituto Nacional de Astrofísica, Óptica y Electrónica |
| Repositorio: | Repositorio Institucional del INAOE |
| Idioma: | español |
| OAI Identifier: | oai:inaoe.repositorioinstitucional.mx:1009/842 |
| Acceso en línea: | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/842 |
| Access Level: | acceso abierto |
| Palabra clave: | info:eu-repo/classification/Codificación de frente de onda/Wavefront coding info:eu-repo/classification/Restauración de imagen/Image restoration info:eu-repo/classification/Célula activa/Active cell info:eu-repo/classification/Telescopios/Telescopes info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/22 info:eu-repo/classification/cti/2209 info:eu-repo/classification/cti/331111 |
| Sumario: | Wave-front coding is a known technique for correcting defocus-like aberrations by introducing an aspherical phase distribution in to a standard clear aperture system, resulting in a near diffracted limited image by using deconvolution techniques. With this technology, we want to improve the image quality of the 2.1-m telescope at the San Pedro Mártir Observatory using the primary mirror's active cell as the wave-front coder element. The active cells functionality and control is studied in order to understand how it works and whether is it possible to use it as the wave-front coding element. The characterization of the telescope's point-spread function (PSF) with and without the wave-front coding element is performed, and an extended analysis in the frequency domain is done to fit the design criterion enabling image processing in order to improve image quality. The parameters used in the active cell and the benefits of using this technique in the Astronomy field will be discussed. |
|---|