MUSE Pipeline Reference Manual
2.1.1
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Functions | |
int | muse_cosmics_dcr (muse_image *aImage, unsigned int aXBox, unsigned int aYBox, unsigned int aPasses, float aThres) |
Quickly mark cosmic rays in an image using the DCR algorithm. More... | |
This group implements a few functions to be used to remove artifacts from MUSE data at the level of single CCDs.
int muse_cosmics_dcr | ( | muse_image * | aImage, |
unsigned int | aXBox, | ||
unsigned int | aYBox, | ||
unsigned int | aPasses, | ||
float | aThres | ||
) |
Quickly mark cosmic rays in an image using the DCR algorithm.
aImage | image on which to replace cosmic rays |
aXBox | search box size in x |
aYBox | search box size in y |
aPasses | maximum number of cleaning passes |
aThres | detection gap threshold in factors of standard deviation |
This uses the DCR algorithm of Pych, 2004, PASP, 116, 148. From Sect. 2 ("The Algorithm") of the paper:
In each subframe:
set CPL_ERROR_NULL_INPUT, return -1 | input image is NULL |
set CPL_ERROR_ILLEGAL_INPUT, return -2 | aThres is not positive |
set CPL_ERROR_ILLEGAL_INPUT, return -3 | aPasses is not positive |
set CPL_ERROR_ILLEGAL_INPUT, return -4 | aXBox is larger than the horizontal image size |
set CPL_ERROR_ILLEGAL_INPUT, return -5 | aYBox is larger than the horizontal image size |
print warning | size of a subframe is less than 100pix |
Definition at line 275 of file muse_artifacts.c.
References muse_image::data.
Referenced by muse_basicproc_params_delete(), and muse_quadrants_overscan_stats().