MUSE Pipeline Reference Manual  0.18.5
Data Structures | Typedefs
Recipe muse_skyflat: Combine several separate (twilight) sky flat-fields into one master skyflat, and compute the integrated flux within the given wavelength range of the IFU.

Data Structures

struct  muse_skyflat_params_s
 Structure to hold the parameters of the muse_skyflat recipe. More...
 

Typedefs

typedef struct
muse_skyflat_params_s 
muse_skyflat_params_t
 Structure to hold the parameters of the muse_skyflat recipe. More...
 

Detailed Description

Author
Peter Weilbacher
  Processing trims the raw data and records the overscan statistics,
  subtracts the bias (taking account of the overscan, if --overscan is not
  "none"), and optionally, the dark from each raw input image, converts
  them from adu to count, and combines the exposures using input
  parameters. Bad pixels are then interpolated from surrounding good ones
  before computing the integrated flux in all slices by summing the pixel
  values of all within the boundaries given by the trace table and the
  --lambdamin and --lambdamax parameters.

  The integrated flux value is then later used as estimate for the
  relative throughput of each IFU, to scale values to a common flux level.

  Since twilight sky flat-fields will have an illumination similar to that
  of science exposures, they should preferably be used as input to this
  recipe. Normal lamp flat-fields can be used, if twilight sky flats are
  not available.

  The output image is not further used by the pipeline, only the FITS
  header with the integrated flux is propagated to the science data.

Typedef Documentation

Structure to hold the parameters of the muse_skyflat recipe.

This structure contains the parameters for the recipe that may be set on the command line, in the configuration, or through the environment.