MUSE Pipeline Reference Manual  2.1.1
Data Fields

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

#include <muse_standard_z.h>

Data Fields

int profile
 Type of flux integration to use. "gaussian" and "moffat" use 2D profile fitting, circle and square are non-optimal flux integrators.
 
const char * profile_s
 Type of flux integration to use. "gaussian" and "moffat" use 2D profile fitting, circle and square are non-optimal flux integrators. (as string)
 
int select
 How to select the star for flux integration, "flux" uses the brightest star in the field, "distance" uses the detection nearest to the approximate coordinates of the reference source.
 
const char * select_s
 How to select the star for flux integration, "flux" uses the brightest star in the field, "distance" uses the detection nearest to the approximate coordinates of the reference source. (as string)
 
int smooth
 How to smooth the response curve before writing it to disk. "none" does not do any kind of smoothing (such a response curve is only useful, if smoothed externally; "median" does a median-filter of 15 Angstrom half-width; "ppoly" fits piecewise cubic polynomials (each one across 2x150 Angstrom width) postprocessed by a sliding average filter of 15 Angstrom half-width.
 
const char * smooth_s
 How to smooth the response curve before writing it to disk. "none" does not do any kind of smoothing (such a response curve is only useful, if smoothed externally; "median" does a median-filter of 15 Angstrom half-width; "ppoly" fits piecewise cubic polynomials (each one across 2x150 Angstrom width) postprocessed by a sliding average filter of 15 Angstrom half-width. (as string)
 
double lambdamin
 Cut off the data below this wavelength after loading the pixel table(s).
 
double lambdamax
 Cut off the data above this wavelength after loading the pixel table(s).
 
double lambdaref
 Reference wavelength used for correction of differential atmospheric refraction. The R-band (peak wavelength ~7000 Angstrom) that is usually used for guiding, is close to the central wavelength of MUSE, so a value of 7000.0 Angstrom should be used if nothing else is known. A value less than zero switches DAR correction off.
 
int darcheck
 Carry out a check of the theoretical DAR correction using source centroiding. If "correct" it will also apply an empirical correction.
 
const char * darcheck_s
 Carry out a check of the theoretical DAR correction using source centroiding. If "correct" it will also apply an empirical correction. (as string)
 
const char * filter
 The filter name(s) to be used for the output field-of-view image. Each name has to correspond to an EXTNAME in an extension of the FILTER_LIST file. If an unsupported filter name is given, creation of the respective image is omitted. If multiple filter names are given, they have to be comma separated. If the zeropoint QC parameters are wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I".
 

Detailed Description

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.

Definition at line 48 of file muse_standard_z.h.


The documentation for this struct was generated from the following file: