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A New Technique for Solar Imaging Spectro-polarimetry using Shack-Hartmann and Fabry-Perot

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dc.contributor.author Placco, V. M
dc.contributor.author Beers, T. C
dc.contributor.author Rossi, S
dc.contributor.author Kennedy, C
dc.contributor.author Christlieb, N
dc.contributor.author Lee, Y. S
dc.contributor.author Sivarani, T
dc.date.accessioned 2020-11-11T01:17:58Z
dc.date.available 2020-11-11T01:17:58Z
dc.date.issued 2012-02
dc.identifier.citation ASP conference series; Vol. 463, pp. 301- 306 en_US
dc.identifier.isbn 978-1-58381-808-4
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6846
dc.description Restricted Access © Astronomical Society of the Pacific http://www.aspbooks.org/a/volumes/article_details?paper_id=34849 en_US
dc.description.abstract A new technique for solar imaging spectro-polarimetry is presented. Using the combination of a Shack-Hartmann (SH) and a Fabry-Pérot (FP) interferometer, high-cadence spectroscopic observations can be obtained at discrete wavelength positions simultaneously, thereby avoiding errors due to non-simultaneity of the wavelength scans. A SH mask is used to generate multiple images of the same field-of-view (FOV). These multiple images when passed through the FP in a collimated-beam arrangement are shifted in wavelength due to the angular dependence of the FP filter transmission profile. Thus, by re-imaging one obtains multiple images of the FOV which are tuned to different wavelength points across the spectral line, in a single exposure. The schematic of the setup and the laboratory simulation of such a configuration is presented. The technique has an advantage of simultaneity over conventional wavelength scanning filtergraphs and has potential for observing highly-dynamic phenomena like solar flares. Also, one can exploit the method to perform snapshot spectropolarimetry by designing a special polarization modulator. The limitation of this technique is that it downgrades the spatial resolution due to the downsampling of the pupil into smaller sub-apertures. However, for large aperture telescopes like 4 meter class telescopes (ATST) this is not a major issue and one can still work at sub-arcsec resolution, though not at the diffraction limit of the full aperture. en_US
dc.language.iso en en_US
dc.publisher Astronomical Society of the Pacific en_US
dc.title A New Technique for Solar Imaging Spectro-polarimetry using Shack-Hartmann and Fabry-Perot en_US
dc.type Book en_US


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