Abstract
Astronomical spectropolarimeters require high accuracy polarizers with large aperture and stringent uniformity requirements. In solar applications, wire grid polarizers are often used as performance is maintained under high heat loads and temperatures over 200°C. DKIST is the NSF’s new 4-m aperture solar telescope designed to deliver accurate spectropolarimetric solar data across a wide wavelength range, covering a large field of view simultaneously using multiple facility instruments. Polarizers at 120 mm diameter are used to calibrate DKIST instruments but vary spatially in transmission, extinction ratio, and orientation of maximum extinction. We combine new spatial and spectral metrology for polarizers and retarders to simulate the accuracy losses with field angle and wavelength caused simultaneously by spatial variation of several optical parameters including beam decenter from misalignments. We also present testing of a new crystal sapphire substrate polarizer designed and fabricated to improve DKIST long wavelength calibrations. We assess spatial thickness variation of sapphire and fused silica wafer substrates using spectral interference fringes.
Highlights
Daniel K. Inouye Solar Telescope (DKIST) and Polarization Models for CalibrationThe National Science Foundation’s Daniel K
We show some examples of contrast, extinction, Mueller matrix elements, and the degree of polarization (DoP) in Appendix E
We presented new metrology for the DKIST polarizers and retarders on apertures larger than 90 mm diameter with thousands to tens of thousands of spatial sampling points at spectral resolving powers over a few thousand covering 390 to 1600 nm
Summary
This variation was included in the DKIST optical model to show polarization calibration errors as functions of field angle and wavelength. We include spatial variation across individual beam footprints in a Mueller matrix propagation simulation This simulation creates synthetic modulated data as a function of field angle and wavelength as the footprints sample the calibration optics well away from the optical bore sight. For the optical path to our NCSP and the Cryo-NIRSP, the aO and AO systems are not simultaneously sampling the coudé beam This leads to temporal drifts in the beam centering and preliminary polarization calibration errors at levels we simulate in this paper. We compile here additional information about the interference fringe properties anticipated for our polarizers
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More From: Journal of Astronomical Telescopes, Instruments, and Systems
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