| combine | str | Type of combination to use {average,median,minmax,sigclip} | |
| crsigma | float | Sigma rejection factor to use for cosmic ray rejection during final resampling. A zero or negative value switches cosmic ray rejection off. | |
| crtype | str | Type of statistics used for detection of cosmic rays during final resampling. "iraf" uses the variance information, "mean" uses standard (mean/stdev) statistics, "median" uses median and the median median of the absolute median deviation. {iraf,mean,median} | |
| dlambda | float | Sampling for twilight reconstruction, this should result in planes of equal wavelength coverage. | |
| hsigma | float | High sigma for pixel rejection with sigclip | |
| lambdamax | float | Maximum wavelength for twilight reconstruction. | |
| lambdamin | float | Minimum wavelength for twilight reconstruction. | |
| lsigma | float | Low sigma for pixel rejection with sigclip | |
| nhigh | int | Number of maximum pixels to reject with minmax | |
| nkeep | int | Number of pixels to keep with minmax | |
| nlow | int | Number of minimum pixels to reject with minmax | |
| overscan | str | If this is "none", stop when detecting discrepant overscan levels (see ovscsigma), for "offset" it assumes that the mean overscan level represents the real offset in the bias levels of the exposures involved, and adjusts the data accordingly; for "vpoly", a polynomial is fit to the vertical overscan and subtracted from the whole quadrant. | |
| ovscignore | int | The number of pixels of the overscan adjacent to the data section of the CCD that are ignored when computing statistics or fits. | |
| ovscreject | str | This influences how values are rejected when computing overscan statistics. Either no rejection at all ("none"), rejection using the DCR algorithm ("dcr"), or rejection using an iterative constant fit ("fit"). | |
| ovscsigma | float | If the deviation of mean overscan levels between a raw input image and the reference image is higher than |ovscsigma x stdev|, stop the processing. If overscan="vpoly", this is used as sigma rejection level for the iterative polynomial fit (the level comparison is then done afterwards with |100 x stdev| to guard against incompatible settings). Has no effect for overscan="offset". | |
| recipe_version | int | Version of the recipe | |
| resample | str | The resampling technique to use for the final output cube. {nearest,linear,quadratic,renka,drizzle,lanczos} | |
| scale | int | Scale the individual images to a common exposure time before combining them. | |
| vignmaskedges | float | Pixels on edges stronger than this fraction in the normalized image are excluded from the fit to the vignetted area. Set to non-positive number to include them in the fit. This has no effect for NFM skyflats. | |
| vignnfmmask | int | The height of the vignetted region at the top of the MUSE field in NFM. This is the region modeled separately (the final vignetting model might be smaller). | |
| vignsmooth | str | Type of smoothing to use for the vignetted region given by the VIGNETTING_MASK (for WFM, or the internal mask, for NFM); gaussian uses (vignxpar + vignypar)/2 as FWHM. {polyfit,gaussian,median} | |
| vignxpar | int | Parameter used by the vignetting smoothing: x order for polyfit (default, recommended 4), parameter that influences the FWHM for the gaussian (recommended: 10), or x dimension of median filter (recommended 5). If a negative value is found, the default is taken. | |
| vignypar | int | Parameter used by the vignetting smoothing: y order for polyfit (default, recommended 4), parameter that influences the FWHM for the gaussian (recommended: 10), or y dimension of median filter (recommended 5). If a negative value is found, the default is taken. | |
| xorder | int | Polynomial order to use in x direction to fit the full field of view. | |
| yorder | int | Polynomial order to use in y direction to fit the full field of view. | |
