Simple alignment procedure for a VNIR imaging spectrometer with a Shack-Hartmann wavefront sensor and a field identifier

Jun Ho Lee; Sunglyoung Hwang; Dohwan Jeong; Jinsuk Hong; Youngsoo Kim; Yeonsoo Kim; Hyunsook Kim

doi:10.1117/12.2275404

5 September 2017 Simple alignment procedure for a VNIR imaging spectrometer with a Shack-Hartmann wavefront sensor and a field identifier

Jun Ho Lee, Sunglyoung Hwang, Dohwan Jeong, Jinsuk Hong, Youngsoo Kim, Yeonsoo Kim, Hyunsook Kim

Author Affiliations +

Proceedings Volume 10402, Earth Observing Systems XXII; 104020H (2017) https://doi.org/10.1117/12.2275404
Event: SPIE Optical Engineering + Applications, 2017, San Diego, California, United States

Abstract

We report an innovative simple alignment method for a VNIR spectrometer in the wavelength region of 400–900 nm; this device is later combined with fore-optics (a telescope) to form a f/2.5 hyperspectral imaging spectrometer with a field of view of ±7.68°. The detector at the final image plane is a 640×480 charge-coupled device with a 24 μm pixel size. We first assembled the fore-optics and the spectrometer separately and then combined them via a slit co-located on the image plane of the fore-optics and the object plane of the spectrometer. The spectrometer was assembled in three steps. In the initial step, the optics was simply assembled with an optical axis guiding He-Ne laser. In the second step, we located a pin-hole on the slit plane and a Shack-Hartmann sensor on the detector plane. The wavefront errors over the full field were scanned simply by moving the point source along the slit direction while the Shack-Hartmann sensor was constantly conjugated to the pin-hole position by a motorized stage. Optimal alignment was then performed based on the reverse sensitivity method. In the final stage, the pin-hole and the Shack-Hartmann sensor were exchanged with an equispaced 10 pin-hole slit called a field identifier and a detector. The light source was also changed from the laser (single wavelength source) to a krypton lamp (discrete multi-wavelength source). We were then easily able to calculate the distortion and keystone on the detector plane without any scanning or moving optical components; rather, we merely calculated the spectral centroids of the 10 pin-holes on the detector. We then tuned the clocking angles of the convex grating and the detector to minimize the distortion and keystone. The final assembly was tested and found to have an RMS WFE < 90 nm over the entire field of view, a keystone of 0.08 pixels, a smile of 1.13 pixels and a spectral resolution of 4.32 nm.

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Jun Ho Lee, Sunglyoung Hwang, Dohwan Jeong, Jinsuk Hong, Youngsoo Kim, Yeonsoo Kim, and Hyunsook Kim "Simple alignment procedure for a VNIR imaging spectrometer with a Shack-Hartmann wavefront sensor and a field identifier", Proc. SPIE 10402, Earth Observing Systems XXII, 104020H (5 September 2017); https://doi.org/10.1117/12.2275404

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KEYWORDS

Spectroscopy

Optical fabrication

Wavefront sensors

Sensors

Mirrors

Relays

Visible radiation

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