1 / 6

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

tausiq
Download Presentation

Euclid slitless calibrations

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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)

More Related