IIINSTRUMENT Pipeline Reference Manual
1.5.13
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Functions | |
cpl_polynomial * | sofi_wavelength_engine (const cpl_image *in, const char *table_name, const char *oh, const char *xe, const char *ne, const cpl_polynomial *phdisprel, double slit_width, int degree, double wl_err, int nsamples, int use_ppm, int plot, double *xcorr) |
Compute a dispersion relation. More... | |
double | sofi_get_slitwidth (const char *filename) |
Find out the slit width. More... | |
cpl_polynomial * | sofi_get_disprel_estimate (const char *filename, int poly_deg) |
Estimate the instrument dispersion relation. More... | |
cpl_polynomial* sofi_get_disprel_estimate | ( | const char * | filename, |
int | poly_deg | ||
) |
Estimate the instrument dispersion relation.
filename | input file name |
poly_deg | polynomial degree |
Definition at line 313 of file sofi_wavelength.c.
References sofi_pfits_get_mode(), and sofi_pfits_get_naxis2().
double sofi_get_slitwidth | ( | const char * | filename | ) |
Find out the slit width.
filename | SOFI fits file name |
Definition at line 263 of file sofi_wavelength.c.
References sofi_pfits_get_opti1_id(), and sofi_pfits_get_pixscale().
cpl_polynomial* sofi_wavelength_engine | ( | const cpl_image * | in, |
const char * | table_name, | ||
const char * | oh, | ||
const char * | xe, | ||
const char * | ne, | ||
const cpl_polynomial * | phdisprel, | ||
double | slit_width, | ||
int | degree, | ||
double | wl_err, | ||
int | nsamples, | ||
int | use_ppm, | ||
int | plot, | ||
double * | xcorr | ||
) |
Compute a dispersion relation.
in | Allocated spectroscopic image |
table_name | Spectral table name (see below) |
oh | the oh lines catalog |
xe | the xe lines catalog |
ne | the ne lines catalog |
phdisprel | first guess polynomial (phys. mod.?) |
slit_width | Width in pixels of the slit used |
degree | Degree of the polynomial to fit the matched lines |
wl_err | the wl error |
nsamples | Number of samples for wavelength computation |
use_ppm | Use the point pattern matching at the end |
plot | Flag for plots |
xcorr | the cross correlation factor (computed) |
Compute a dispersion relation from a spectroscopic image showing some strong emission lines. A vital assumption is that strong emission lines can be seen in the image. The removal of thermal background will attempt to remove from the spectroscopic image any low-frequency components, i.e. any features that are a lot wider than the slit width.
The spectral table name is a character string. Possible values are:
"oh" : OH lines "Xe" : Xenon lines "Ar" : Argon lines "Xe+Ar" : Xenon and Argon lines
Definition at line 150 of file sofi_wavelength.c.