| darcheck | str | Carry out a check of the theoretical DAR correction using source centroiding. If "correct" it will also apply an empirical correction. {none,check,correct} | |
| filter | str | The filter name(s) to be used for the output field-of-view image. Each name has to correspond to an EXTNAME in an extension of the FILTER_LIST file. If an unsupported filter name is given, creation of the respective image is omitted. If multiple filter names are given, they have to be comma separated. If the zeropoint QC parameters are wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I". | |
| lambdamax | float | Cut off the data above this wavelength after loading the pixel table(s). | |
| lambdamin | float | Cut off the data below this wavelength after loading the pixel table(s). | |
| lambdaref | float | Reference wavelength used for correction of differential atmospheric refraction. The R-band (peak wavelength ~7000 Angstrom) that is usually used for guiding, is close to the central wavelength of MUSE, so a value of 7000.0 Angstrom should be used if nothing else is known. A value less than zero switches DAR correction off. | |
| profile | str | Type of flux integration to use. "gaussian", "moffat", and "smoffat" use 2D profile fitting, "circle" and "square" are non-optimal aperture flux integrators. "smoffat" uses smoothing of the Moffat parameters from an initial fit, to derive physically meaningful wavelength-dependent behavior. "auto" selects the smoothed Moffat profile for WFM data and circular flux integration for NFM. {gaussian,moffat,smoffat,circle,square,auto} | |
| recipe_version | int | Version of the recipe | |
| select | str | How to select the star for flux integration, "flux" uses the brightest star in the field, "distance" uses the detection nearest to the approximate coordinates of the reference source. {flux,distance} | |
| smooth | str | How to smooth the response curve before writing it to disk. "none" does not do any kind of smoothing (such a response curve is only useful, if smoothed externally; "median" does a median-filter of 15 Angstrom half-width; "ppoly" fits piecewise cubic polynomials (each one across 2x150 Angstrom width) postprocessed by a sliding average filter of 15 Angstrom half-width. {none,median,ppoly} | |
