CALPRODUCT-NS-008: NISP-S Wavelength Dispersion with Planetary Nebulae¶
Parent requirement¶
Scheduling¶
Once during PV phase. Once during routine phase, after 1 year or later at a time when unallocated time would become large later in the survey.
Time-critical¶
Yes. See dependencies.
Dependencies¶
Objective¶
Observe a compact planetary nebula (PN) with strong emission lines as a function of position for each NISP detector, to obtain the wavelength dispersion solution. The dispersion solution is transfered to the Self-cal field to establish a set of standards that can be used to monitor for drifts. The Self-cal must be observed immediately after (or before) the PN observations, without grism wheel movements in between.
Fulfilled by¶
Data volume¶
NISP-S: (80*2*5 + 9*2*5)*NS = 145070 MB for the PN and Self-cal NISP-S exposures
NISP-P: 3*4*4*NP = 4224 MB for the astrometric NISP-P exposures
VIS: 16*VS = 7232 MB for the VIS astrometric exposures
Processing input¶
Ground Processing Input Data: All calibration products to run the standard science pipeline (BPM, darks, flat, nonlinearity etc), ground-based dispersion data/model.
Data Description: NISP: 320 spectro-MACC images (5*16*4), 162 photo-MACC images (144 for the 2x2 grid, and a total of 18 for the first and last dither position), VIS: 320 images (5*16*4)
Processing output¶
Dispersion solution as a function of detector position for all detectors and all grisms.
Required accuracy, constraints¶
Emission line centroids successfully extracted from all PN measurements
Processing tools¶
L1 science pipeline and line measurement pipeline (?), additional offline trend analysis of dispersion combined with ground data/model
Quality control parameters¶
DataModel: https://gitlab.euclid-sgs.uk/
Contact person¶
NISP-S calibration scientist