MUSE Pipeline Reference Manual  2.1.1
Data Structures | Typedefs
Recipe muse_standard: Create a flux response curve from a standard star exposure.

Data Structures

struct  muse_standard_params_s
 Structure to hold the parameters of the muse_standard recipe. More...
 

Typedefs

typedef struct muse_standard_params_s muse_standard_params_t
 Structure to hold the parameters of the muse_standard recipe. More...
 

Detailed Description

Author
Peter Weilbacher
  Merge pixel tables from all IFUs and correct for differential
  atmospheric refraction.

  To derive the flux response curve, integrate the flux of all objects
  detected within the field of view using the given profile. Select one
  object as the standard star (either the brightest or the one nearest
  one, depending on --select) and compare its measured fluxes to
  tabulated fluxes to derive the sensitivity over wavelength. Postprocess
  this sensitivity curve to mark wavelength ranges affected by telluric
  absorption. Interpolate over the telluric regions and derive a telluric
  correction spectrum for them. The final response cuve is then linearly
  extrapolated to the largest possible MUSE wavelength range and smoothed
  (with the method given by --smooth). The derivation of the telluric
  correction spectrum assumes that the star has a smooth spectrum within
  the telluric regions.

  If there are more than one exposure given in the input data, the
  derivation of the flux response and telluric corrections are done
  separately for each exposure. For each exposure, an image containing
  the extracted stellar spectra and the datacube used for
  flux integration are saved, together with collapsed images for each given
  filter.

Typedef Documentation

Structure to hold the parameters of the muse_standard recipe.

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