CALPRODUCT-NS-003: NISP-S Focal Plane Distortion¶
Parent requirement¶
Scheduling¶
At least every 6 months, using secondary wavelengh calibrators (absorption line systems) in the SelfCal field. The full wavelengtj dispersion solution based on PN is done once during PV, and repeated once after 1 year in flight.
Time-critical¶
no
Objective¶
Determine the Distortion Pattern across the NISP Spectro Focal Plane. This calibration is based on three mappings:
From sky (Gaia references) to 0th order using bright stars.
From 0th order to a reference wavelength in the 1st order.
Reconstruction of the wavelength dispersion solution (based on PN observations)
Fulfilled by¶
CALBLOCK-PV-009: NISP Wavelength Dispersion and VIS BFE
Data volume¶
No dedicated observations needed!
Processing input¶
Ground Processing Input Data: All calibration products to run the standard science pipeline (BPM, darks, flat, nonlinearity etc), astrometric reference catalog (Gaia), offline analysis
Data Description: No dedicated observations needed!
Processing method¶
Distortion pattern is derived by comparing source positions against known (Gaia) astrometric positions (compared to 0th order centroids?), or by a self-cal approach utilizing the multiply dithered observations.
Processing output¶
Distortion map of NISP-S focal plane, WCS solution for NISP spectro images, evaluation of impact of GWA position uncertainty
Required accuracy, constraints¶
accurate source position measurements
Processing tools¶
L1 science pipeline, source position measurements
Quality control parameters¶
DataModel: https://gitlab.euclid-sgs.uk/
Contact person¶
NISP-S calibration scientist