MUSE Pipeline Reference Manual  2.1.1
Data Structures | Typedefs
Recipe muse_scipost: Prepare reduced and combined science products.

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. More...
 

Detailed Description

Author
Peter Weilbacher
  Sort input pixel tables into lists of files per exposure, merge pixel
  tables from all IFUs of each exposure.

  Correct each exposure for differential atmospheric refraction (unless
  --lambdaref is far outside the MUSE wavelength range).
  Then the flux calibration is carried out, if a response 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 logarithmically (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 Documentation

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.