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Euclid slitless calibrations

Euclid slitless calibrations. Jeremy R. Walsh Harald Kuntschner Martin Kümmel Space Telescope European Co-ordinating Facility, ESO. Slitless Spectroscopy. HST NICMOS, ACS and most recently WFC3 provided slitless spectroscopy WFC3 has similar λ coverage to Euclid 0.8-1.7µm

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Euclid slitless calibrations

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  1. Euclid slitless calibrations Jeremy R. Walsh Harald Kuntschner Martin Kümmel Space Telescope European Co-ordinating Facility, ESO

  2. Slitless Spectroscopy • HST NICMOS, ACS and most recently WFC3 provided slitless spectroscopy • WFC3 has similar λ coverage to Euclid 0.8-1.7µm • Typical features: • Spectra of all objects in field → contamination • Multiple orders • Individual λ zero points → require direct image to determine WFC3 G141 (1.1-1.7µm) slitless image WFC3 G141 point source spectrum

  3. Calibrations for slitless spectroscopy • Wavelength – dispersion and zero point • λ-dependent flat field • Sensitivity (flux calibration) • Dispersed sky background

  4. Wavelength calibration • Compact Galactic planetary nebulae provide excellent sky wavelength calibration sources • Expect that dispersion solution varies across field → calibrate with multiple sources • Map transfer of zero point

  5. Wavelength error budget • In order to achieve Δλ/λ ≤ 0.001 for measurement of emission lines. Following systematics to control: • Dispersion solution variation across field • Estimation of object positions on direct image • Transfer of wavelength zero point to grism image • Determination of emission line position

  6. Flat fielding • Any pixel can receive any λ so require a flat field cube • On ground construct mono-chromatic flat fields then fits as function of λ for flat field cube • In-orbit correct for large scale illumination with rastered star field (L-flat)

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