Data Structures | |
| struct | muse_scipost_params_s |
| Structure to hold the parameters of the muse_scipost recipe. More... | |
Typedefs | |
| typedef struct muse_scipost_params_s | muse_scipost_params_t |
| Structure to hold the parameters of the muse_scipost recipe. | |
Sort input pixel tables into lists of files per exposure, merge pixel tables from all IFUs of each exposure.
Correct each exposure for differential atmopheric refraction (unless --lambdaraf is far outside the MUSE wavelength range). Then the flux calibration is carried out, if a respnse curve was given in the input; it includes a correction of telluric absorption, if a telluric absorption correction file was given. Then the sky subtraction is carried out (unless --skymethod="none"), either directly subtracting an input sky continuum and an input sky emission lines (for --skymethod="subtract-model"), or (--skymethod="model") create a sky spectrum from the darkest fraction (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as artifacts) of the field of view, then fitting and subtracting sky emission lines using an initial estimate of the input sky lines; then the continuum (residuals after subtracting the sky lines from the sky spectrum) is subtracted as well. If --save contains "skymodel", all sky-related products are saved for each exposure. Afterwards the data is corrected for the radial velocity of the observer (--rvcorr), before the input (or a default) astrometric solution is applied. Now each individual exposure is fully reduced; the pixel tables at this stage can be saved by setting "individual" in --save.
If multiple exposures were given, they are then combined. If --save contains "combined", this final merged pixel table is saved.
Finally (if --save contains "cube"), the data is resampled into a datacube, using all parameters given to the recipe. The extent and orientation of the cube is normally computed from the data itself, but this can be overridden by passing a file with the output world coordinate system (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample the wavelength axis logorithmically (in that file set "CTYPE3='AWAV-LOG'"). As a last step, the computed cube is integrated over all filter functions given (--filter) that are also present in the input filter list table.
| typedef struct muse_scipost_params_s muse_scipost_params_t |
Structure to hold the parameters of the muse_scipost recipe.
This structure contains the parameters for the recipe that may be set on the command line, in the configuration, or through the environment.
1.6.1