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9 August 2016 Gemini planet imager observational calibration XIII: wavelength calibration improvements, stability, and nonlinearity
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We present improvements to the wavelength calibration for the lenslet-based Integral Field Spectrograph (IFS), that serves as the science instrument for the Gemini Planet Imager (GPI). The GPI IFS features a 2.7”×2.7” field of view and a 190 x 190 lenslet array (14.1 mas/lenslet) with spectral resolving power ranging from R ~ 35 to 78. A unique wavelength solution is determined for each lenslet characterized by a two-dimensional position, an n-dimensional polynomial describing the spectral dispersion, and the rotation of the spectrum with respect to the detector axis. We investigate the non-linearity of the spectral dispersion across all Y, J, H, and K bands through both on-sky arc lamp images and simulated IFS images using a model of the optical path. Additionally, the 10-hole non-redundant masking mode on GPI provides an alternative measure of wavelength dispersion within a datacube by cross-correlating reference PSFs with science images. This approach can be used to confirm deviations from linear dispersion in the reduced datacubes. We find that the inclusion of a quadratic term provides a factor of 10 improvement in wavelength solution accuracy over the linear solution and is necessary to achieve uncertainties of a few hundredths of a pixel in J band to a few thousands of a pixel in the K bands. This corresponds to a wavelength uncertainty of ~ 0.2 nm across all filters.
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Schuyler G. Wolff, Kimberly Ward-Duong, Joe Zalesky, Alex Z. Greenbaum, Marshall D. Perrin, and James Graham "Gemini planet imager observational calibration XIII: wavelength calibration improvements, stability, and nonlinearity", Proc. SPIE 9908, Ground-based and Airborne Instrumentation for Astronomy VI, 990838 (9 August 2016);

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