Substep: Reduce

Defines

#define UVES_MIN_LINE_ROWS_TO_MAKE_FIT   5
#define UVES_BLAZE_DUMMY_VAL   999.

Functions

static cpl_error_code extract_ff_rebin_merge (cpl_image *back_subbed, cpl_image *backsubbed_noise, const uves_propertylist *backsubbed_header, const cpl_image *master_flat, cpl_image *mflat_noise, const cpl_table *ordertable, const polynomial *order_locations, const cpl_table *linetable, const uves_propertylist *linetable_header[3], const polynomial *dispersion_relation[3], double slit_length, double slit_offset, int window, enum uves_chip chip, bool blaze_correct, bool tilt_corr, bool DEBUG, const cpl_parameterlist *parameters, const char *context, const char *mode, flatfielding_method ff_method, extract_method ex_method, merge_method m_method,cpl_image **x, uves_propertylist **x_header, cpl_image **fx, cpl_table **cosmic_mask, cpl_image **wave_map, cpl_image **flatfielded_variance, uves_propertylist **flatfielded_variance_header, cpl_image **resampled_spectrum, cpl_image **resampled_mf, cpl_image **merged_sky, cpl_image **rebinned_spectrum, cpl_image **rebinned_noise, uves_propertylist **rebinned_header, cpl_image **merged_spectrum, cpl_image **merged_noise, uves_propertylist **merged_header, cpl_table **info_tbl, cpl_table **order_trace)
 Reduce one extraction window.
static cpl_image * subtract_sky (cpl_image *rebinned_obj, cpl_image *rebinned_obj_noise, uves_propertylist *rebinned_obj_header, const cpl_image *rebinned_sky1, const cpl_image *rebinned_sky1_noise, const uves_propertylist *rebinned_sky1_header, const cpl_image *rebinned_sky2, const cpl_image *rebinned_sky2_noise, const uves_propertylist *rebinned_sky2_header, cpl_image **merged_obj, cpl_image **merged_obj_noise, uves_propertylist *merged_obj_header, const cpl_image *merged_sky1, const cpl_image *merged_sky1_noise, const uves_propertylist *merged_sky1_header, const cpl_image *merged_sky2, const cpl_image *merged_sky2_noise, const uves_propertylist *merged_sky2_header, double obj_slit, double sky1_slit, double sky2_slit)
 Subtract sky from extracted spectrum.
static cpl_image * subtract_sky_row (cpl_image *obj, cpl_image *obj_noise, double obj_start, double obj_end, double obj_slit, const cpl_image *sky1, const cpl_image *sky1_noise, double sky1_start, double sky1_end, double sky1_slit, const cpl_image *sky2, const cpl_image *sky2_noise, double sky2_start, double sky2_end, double sky2_slit, int row, double wavestep, double *common_start, double *common_end)
 Subtract sky from 1 row of spectrum.
static double get_offset (const cpl_image *back_subbed, const cpl_table *ordertable, const polynomial *order_locations, double search_range, int nsamples, double *doffset)
 Measure object offset w.r.t. slit center.
static cpl_image * uves_get_blaze_ratio (const cpl_image *spectrum, const cpl_image *spectrum_noise)
 Get (normalized) object to flat-field blaze function ratio.
cpl_parameterlist * uves_reduce_define_parameters (void)
 Define recipe parameters used for reducing a frame.
cpl_error_code uves_reduce (const cpl_image *raw_image, const uves_propertylist *raw_header, const uves_propertylist *rotated_header, const cpl_image *master_bias, const cpl_image *master_dark, const uves_propertylist *mdark_header, const cpl_image *master_flat, const uves_propertylist *mflat_header, const cpl_table *ordertable, const polynomial *order_locations, const cpl_table *linetable[3], const uves_propertylist *linetable_header[3], const polynomial *dispersion_relation[3], enum uves_chip chip, bool DEBUG, const cpl_parameterlist *parameters, const char *rec_id, const char *mode, cpl_image **x, uves_propertylist **x_header, cpl_image **fx, cpl_table **cosmic_mask, cpl_image **wave_map, cpl_image **background, cpl_image **flatfielded_variance, uves_propertylist **flatfielded_variance_header, cpl_image **resampled_spectrum, cpl_image **resampled_mf, cpl_image **merged_sky, cpl_image **rebinned_spectrum, cpl_image **rebinned_noise, uves_propertylist **rebinned_header, cpl_image **merged_spectrum, cpl_image **merged_noise, uves_propertylist **merged_header, cpl_image **reduced_rebinned_spectrum, cpl_image **reduced_rebinned_noise, cpl_image **reduced_spectrum, cpl_image **reduced_noise, cpl_table **info_tbl, double *extraction_slit, cpl_table **order_trace)
 Reduce a science frame.
static polynomialinterpolate_wave (const polynomial *dispersion_relation[3], const uves_propertylist *linetable_header[3], double objoffset)
 1st order line tilt correction
cpl_image * uves_normalize_spectrum (const cpl_image *spectrum, const cpl_image *spectrum_error, const uves_propertylist *spectrum_header, const uves_propertylist *raw_header, int n_traces, enum uves_chip chip, const cpl_table *atm_extinction, bool correct_binning, cpl_image **scaled_error)
 Normalize a spectrum.

Detailed Description

This module is for reducing a science frame.


Function Documentation

static cpl_error_code extract_ff_rebin_merge ( cpl_image *  back_subbed,
cpl_image *  backsubbed_noise,
const uves_propertylist backsubbed_header,
const cpl_image *  master_flat,
cpl_image *  mflat_noise,
const cpl_table *  ordertable,
const polynomial order_locations,
const cpl_table *  linetable,
const uves_propertylist linetable_header[3],
const polynomial dispersion_relation[3],
double  slit_length,
double  slit_offset,
int  window,
enum uves_chip  chip,
bool  blaze_correct,
bool  tilt_corr,
bool  DEBUG,
const cpl_parameterlist *  parameters,
const char *  context,
const char *  mode,
flatfielding_method  ff_method,
extract_method  ex_method,
merge_method  m_method,
cpl_image **  x,
uves_propertylist **  x_header,
cpl_image **  fx,
cpl_table **  cosmic_mask,
cpl_image **  wave_map,
cpl_image **  flatfielded_variance,
uves_propertylist **  flatfielded_variance_header,
cpl_image **  resampled_spectrum,
cpl_image **  resampled_mf,
cpl_image **  merged_sky,
cpl_image **  rebinned_spectrum,
cpl_image **  rebinned_noise,
uves_propertylist **  rebinned_header,
cpl_image **  merged_spectrum,
cpl_image **  merged_noise,
uves_propertylist **  merged_header,
cpl_table **  info_tbl,
cpl_table **  order_trace 
) [static]

Reduce one extraction window.

Parameters:
back_subbed The de-biased, dark subtracted, background subtracted, possibly already flat-fielded image in (pixel, pixel)-space
backsubbed_noise Noise of back_subbed
backsubbed_header FITS header of back_subbed
master_flat The master flat frame. May be NULL if flatfielding is not performed.
mflat_noise Noise of master_flat
ordertable Order table describing the order locations on the raw image
order_locations The polynomial describing the order positions
linetable Line table used for the current extraction window
linetable_header Line table header containing offsets for previously obtained dispersion relations
dispersion_relation The dispersion relations, will be interpolated depending on offset
slit_length Length (in spatial direction, in pixels) of current extraction window.
slit_offset Offset of current extraction window (applies only to linear/average, not optimal/2d extraction)
window Extraction window number. Must be 1, 2, 3, for lower sky, object, upper sky, respectively. Not used in optimal/2d extraction modes.
chip The CCD chip id
blaze_correct Correct (empirically) for the different shapes of object/flat-field blaze function?
tilt_corr Correct for line tilt? If not, the appropriate dispersion solutions are used for object/sky (without interpolation)
DEBUG If true, intermediate results are saved to the current directory
parameters Parameters used for extraction and rebinning.
context Use parameters belonging to this context
ff_method The flat-fielding method.
ex_method Extraction method.
m_method The order merging method.
x (Output) If non-NULL, this will contain the extracted spectrum (recipe product only in 2d mode)
x_header (Output) If non-NULL, the header belonging to x
fx (Output) If non-NULL, the extracted, flat-fielded spectrum (recipe product only in 2d mode)
cosmic_mask (Output) Used only for optimal extraction
flatfielded_variance (Output) If non-NULL, variance of ff. spectrum
flatfielded_variance_header (Output) Header of flatfielded_variance
resampled_spectrum (Output) Extracted + rebinned. Not ff. May be NULL
resampled_mf (Output) Extracted + rebinned master flat-field. May be NULL
merged_sky (Output) For optimal extraction, the merged sky spectrum
rebinned_spectrum (Output) Extracted, flat-fielded, rebinned spectrum
rebinned_noise (Output) Error (1 sigma) of rebinned_spectrum
rebinned_header (Output) Header describing geometry of rebinned_spectrum and rebinned_noise
merged_spectrum (Output) The merged spectrum
merged_noise (Output) Noise (1 sigma) of merged_spectrum
merged_header (Output) Header belonging to merged_spectrum and merged_noise
info_tbl table with information on object location, FWHM, and S/N
Returns:
CPL_ERROR_NONE iff okay

As its name sort of implies, this function

  • extracts the spectrum (optimally, 2d or simple). If optimal extraction, also the sky is extracted.
  • divides by flat-field iff method is FF_EXTRACT. If method is FF_PIXEL the input is assumed to have been already flat-fielded.
  • rebins to (order, wavelength)-space the extracted spectrum/spectra.
  • merges the rebinned spectrum/spectra.

Definition at line 1687 of file uves_reduce.c.

References check, check_nomsg, interpolate_wave(), passure, uves_extract(), uves_flatfielding(), uves_get_blaze_ratio(), uves_get_wave_map(), uves_image_mflat_detect_blemishes(), uves_merge_orders(), uves_msg, uves_msg_debug, uves_msg_low, uves_msg_warning, uves_pfits_get_firstabsorder(), uves_pfits_get_lastabsorder(), uves_polynomial_convert_to_table(), uves_polynomial_delete(), uves_polynomial_duplicate(), uves_propertylist_copy_property_regexp(), uves_propertylist_duplicate(), uves_rebin(), and uves_round_double().

Referenced by uves_reduce().

static cpl_image * subtract_sky ( cpl_image *  rebinned_obj,
cpl_image *  rebinned_obj_noise,
uves_propertylist rebinned_obj_header,
const cpl_image *  rebinned_sky1,
const cpl_image *  rebinned_sky1_noise,
const uves_propertylist rebinned_sky1_header,
const cpl_image *  rebinned_sky2,
const cpl_image *  rebinned_sky2_noise,
const uves_propertylist rebinned_sky2_header,
cpl_image **  merged_obj,
cpl_image **  merged_obj_noise,
uves_propertylist merged_obj_header,
const cpl_image *  merged_sky1,
const cpl_image *  merged_sky1_noise,
const uves_propertylist merged_sky1_header,
const cpl_image *  merged_sky2,
const cpl_image *  merged_sky2_noise,
const uves_propertylist merged_sky2_header,
double  obj_slit,
double  sky1_slit,
double  sky2_slit 
) [static]

Subtract sky from extracted spectrum.

Parameters:
rebinned_obj The rebinned object spectrum
rebinned_obj_noise Noise of rebinned object spectrum
rebinned_obj_header Header of rebinned object spectrum
rebinned_sky1 The rebinned lower sky spectrum
rebinned_sky1_noise Noise of rebinned lower sky spectrum
rebinned_sky1_header Header of rebinned lower sky spectrum
rebinned_sky2 The rebinned upper sky spectrum
rebinned_sky2_noise Noise of rebinned upper sky spectrum
rebinned_sky2_header Header of rebinned upper sky spectrum
merged_obj The merged object spectrum
merged_obj_noise Noise of merged object spectrum
merged_obj_header Header of merged object spectrum
merged_sky1 The merged lower sky spectrum
merged_sky1_noise Noise of merged lower sky spectrum
merged_sky1_header Header of merged lower sky spectrum
merged_sky2 The merged upper sky spectrum
merged_sky2_noise Noise of merged upper sky spectrum
merged_sky2_header Header of merged upper sky spectrum
obj_slit Extraction slit length (object)
sky1_slit Extraction slit length (lower sky)
sky2_slit Extraction slit length (upper sky)
Returns:
The merged sky spectrum which was subtracted, or NULL if the provided sky windows had no good pixels

Due to (slightly) different dispersion relations, the ranges of sky and object spectra might not be exactly identical. This function takes care of subtracting the sky from rebinned and merged spectra while aligning the proper wavelengths bin with each other.

Definition at line 2600 of file uves_reduce.c.

References check, passure, subtract_sky_row(), uves_pfits_get_cdelt1(), uves_pfits_get_crval1(), uves_pfits_get_wend(), uves_pfits_get_wstart(), uves_pfits_set_crval1(), uves_pfits_set_wend(), uves_pfits_set_wstart(), and uves_round_double().

Referenced by uves_reduce().

static cpl_image * subtract_sky_row ( cpl_image *  obj,
cpl_image *  obj_noise,
double  obj_start,
double  obj_end,
double  obj_slit,
const cpl_image *  sky1,
const cpl_image *  sky1_noise,
double  sky1_start,
double  sky1_end,
double  sky1_slit,
const cpl_image *  sky2,
const cpl_image *  sky2_noise,
double  sky2_start,
double  sky2_end,
double  sky2_slit,
int  row,
double  wavestep,
double *  common_start,
double *  common_end 
) [static]

Subtract sky from 1 row of spectrum.

Parameters:
obj The object spectrum
obj_noise Noise of object spectrum
obj_start Wavelength of first bin of row
obj_end Wavelength of last bin to consider
obj_slit Object slit length
sky1 The lower sky spectrum (or NULL if not extracted)
sky1_noise Noise of lower sky spectrum
sky1_start Wavelength of first bin of row
sky1_end Wavelength of last bin to consider
sky1_slit Lower sky slit length
sky2 The upper sky spectrum (or NULL if not extracted)
sky2_noise Noise of upper sky spectrum
sky2_start Wavelength of first bin of row
sky2_end Wavelength of last bin to consider
sky2_slit Upper sky slit length
row Row (order number) of spectrum images to process
wavestep Width of one win (same for obj/sky spectra)
common_start (output) Minimum common wavelength
common_end (output) Maximum common wavelength
Returns:
The merged sky spectrum, or NULL if provided sky images had no good pixels

This function subtracts sky from (only) the specified row of the input spectrum. Before subtraction, the fluxes are properly scaled according to extraction slit lengths.

Definition at line 2847 of file uves_reduce.c.

References check, uves_average_images(), uves_max_double(), uves_min_double(), uves_msg_debug, uves_msg_low, and uves_round_double().

Referenced by subtract_sky().

static double get_offset ( const cpl_image *  back_subbed,
const cpl_table *  ordertable,
const polynomial order_locations,
double  search_range,
int  nsamples,
double *  doffset 
) [static]

Measure object offset w.r.t. slit center.

Parameters:
back_subbed The input image
ordertable The order table. Used to get min/max order numbers
order_locations Polynomial describing the order locations
search_range The half search window height (in pixels)
nsamples Number of sample points per order
doffset (out) If non-null, the measured width (1 sigma) of the object is returned.
Returns:
The average object offset in relation to the center of the order

This function finds the flux centroid (in y-direction) of nsamples median collapsed chunks in each order and returns the mean centroid position (average of all orders).

Definition at line 3069 of file uves_reduce.c.

References passure, uves_max_int(), uves_min_int(), uves_polynomial_evaluate_2d(), and uves_round_double().

Referenced by uves_reduce().

static cpl_image * uves_get_blaze_ratio ( const cpl_image *  spectrum,
const cpl_image *  spectrum_noise 
) [static]

Get (normalized) object to flat-field blaze function ratio.

Parameters:
spectrum The extracted, flat-fielded spectrum in (pixel, order)-space
spectrum_noise Noise associated with spectrum
Returns:
The correction factor

Due to the different blaze function profile of flat/science spectra (for unknown reason) there will be order scale ripples when merging. This function

This function

  • Normalizes in each order the flux to 1: norm(x) = f(x) / median_x(f).
  • Fits for each x0 a low-order polynomial to norm(x0, order). The result is a correction factor close to 1 that corrects for the different shape of blaze functions (but doesn't change the overall normalization)

Definition at line 3191 of file uves_reduce.c.

References assure_mem, check, check_nomsg, passure, uves_error_reset, uves_filter_image_median(), uves_polynomial_delete(), uves_polynomial_evaluate_1d(), and uves_polynomial_regression_1d().

Referenced by extract_ff_rebin_merge().

cpl_parameterlist* uves_reduce_define_parameters ( void   ) 

Define recipe parameters used for reducing a frame.

Returns:
Newly allocated parameter list for this sub-step

See source code or 'esorex --man-page' for a description of each parameter.

Definition at line 187 of file uves_reduce.c.

cpl_error_code uves_reduce ( const cpl_image *  raw_image,
const uves_propertylist raw_header,
const uves_propertylist rotated_header,
const cpl_image *  master_bias,
const cpl_image *  master_dark,
const uves_propertylist mdark_header,
const cpl_image *  master_flat,
const uves_propertylist mflat_header,
const cpl_table *  ordertable,
const polynomial order_locations,
const cpl_table *  linetable[3],
const uves_propertylist linetable_header[3],
const polynomial dispersion_relation[3],
enum uves_chip  chip,
bool  DEBUG,
const cpl_parameterlist *  parameters,
const char *  rec_id,
const char *  mode,
cpl_image **  x,
uves_propertylist **  x_header,
cpl_image **  fx,
cpl_table **  cosmic_mask,
cpl_image **  wave_map,
cpl_image **  background,
cpl_image **  flatfielded_variance,
uves_propertylist **  flatfielded_variance_header,
cpl_image **  resampled_spectrum,
cpl_image **  resampled_mf,
cpl_image **  merged_sky,
cpl_image **  rebinned_spectrum,
cpl_image **  rebinned_noise,
uves_propertylist **  rebinned_header,
cpl_image **  merged_spectrum,
cpl_image **  merged_noise,
uves_propertylist **  merged_header,
cpl_image **  reduced_rebinned_spectrum,
cpl_image **  reduced_rebinned_noise,
cpl_image **  reduced_spectrum,
cpl_image **  reduced_noise,
cpl_table **  info_tbl,
double *  extraction_slit,
cpl_table **  order_trace 
)

Reduce a science frame.

Parameters:
raw_image the image to reduce (pre and overscan are already removed)
raw_header FITS header of raw image
rotated_header Header describing the geometry of the raw image after rotation and removal of pre- and overscan areas
master_bias The master bias image. If NULL, no bias subtraction is done.
master_dark The master dark image. If NULL, no dark subtraction is done.
mdark_header The master dark header containing the master dark exposure time.
master_flat Master flat image. May be NULL, but only if no flatfielding is requested.
mflat_header The master flat header. Contains the number of input flat frames which is needed to generate the master flat noise image.
ordertable Order table describing the order locations on the raw image
order_locations The polynomial describing the order positions
linetable Length 3 array of linetable for sky, object, sky.
linetable_header Length 3 array of linetable headers for sky, object, sky.
dispersion_relation Length 3 array of dispersion relations for sky, object, sky.
chip The CCD chip id
DEBUG If true, intermediate results are saved to the current directory
parameters Parameters used for background subtraction, flat-fielding, extraction and rebinning. Add parameters to the caller recipe by calling uves_propagate_parameters_step() from the recipe_create() function
rec_id Use parameters belonging to this recipe
mode mode to set different default params (efficiencY)
x (Output) In 2d extraction mode, the extracted spectrum
x_header (Output) In 2d extraction mode, header of extracted spectrum
fx (Output) In 2d extraction mode, the flat-fielded, extracted spectrum
cosmic_mask (Output) In optimal extraction mode, the list of hot pixels
background (Output) The background that was subtracted from the raw image
flatfielded_variance (Output) If non-NULL variance of extracted+flatfielded (not resampled) object
flatfielded_variance_header (Output) If non-NULL header of flatfielded_variance
resampled_spectrum (Output) Extracted + resampled but not FF object. If input is NULL, this is not produced
resampled_mf (Output) Extracted + resampled master flat. If input is NULL, this is not produced
merged_sky (Output) Input pointer must be non-NULL. Returned is the sky spectrum, or NULL if no sky was extracted (image slicer or 2d modes)
rebinned_spectrum (Output) The resampled 2d spectrum (non sky-subtracted)
rebinned_noise (Output) Noise (1 sigma) of rebinned_spectrum
rebinned_header (Output) Header describing geometry of rebinned_spectrum (and of course rebinned_noise)
merged_spectrum (Output) The merged spectrum (non sky-subtracted)
merged_noise (Output) Noise (1 sigma) of merged_spectrum
merged_header (Output) Header belonging to merged_spectrum and merged_noise
reduced_rebinned_spectrum (Output) The sky subtracted spectrum rebinned to (wavelength, order) space (i.e. non-merged).
reduced_rebinned_noise (Output) Noise (1 sigma) of reduced_rebinned_spectrum
reduced_spectrum (Output) Merged, sky-subtracted spectrum
reduced_noise (Output) Noise (1 sigma) of reduced_spectrum
info_tbl (output) table with information on object location, FWHM, and S/N
extraction_slit (output) extraction slit actually used
order_trace (Output) In optimal extraction mode, table describing the measured spatial profile
Returns:
CPL_ERROR_NONE iff okay.

This function pre-processes the input image:

  • subtracts master bias if provided,
  • subtracts master dark if provided,
  • subtracts background (see uves_backsub_spline()),
  • gets extraction slit length
  • divides by master flat if FF_METHOD is FF_PIXEL.

Then, if optimal extraction:

  • extracts (including sky subtraction), optionally flat-field corrects and merges the object window (see extract_ff_rebin_merge()).

If linear/average extraction,

  • extracts, optionally flat-field corrects and merges the object and both sky windows, then
  • subtracts the sky spectra from the object spectrum (after normalizing to the object slit length)

If 2d extraction,

  • extracts, optionally flat-field corrects and merges each of the spatial traces (see extract_ff_rebin_merge()). In 2d extraction mode, no sky subtraction can be performed as the object position is not defined.

Definition at line 574 of file uves_reduce.c.

References assure_nomsg, check, extract_ff_rebin_merge(), get_offset(), passure, subtract_sky(), uves_define_noise(), uves_flatfielding(), uves_get_extract_method(), uves_get_flatfield_method(), uves_get_merge_method(), uves_max_double(), uves_max_int(), uves_min_double(), uves_msg, uves_msg_low, uves_msg_warning, uves_pfits_get_datancom(), uves_pfits_get_exptime(), uves_pfits_get_slit1_name(), uves_pfits_get_slitlength_pixels(), uves_pfits_set_hs(), uves_propertylist_append_c_double(), uves_propertylist_contains(), uves_propertylist_get_double(), uves_round_double(), uves_subtract_bias(), and uves_subtract_dark().

Referenced by uves_response_efficiency(), and uves_scired_process_chip().

static polynomial* interpolate_wave ( const polynomial dispersion_relation[3],
const uves_propertylist linetable_header[3],
double  objoffset 
) [static]

1st order line tilt correction

Parameters:
dispersion_solution calibration solutions
linetable_header describing where dispersion solutions were obtained
objoffset object slit position
Returns:
interpolated dispersion solution at the specified object position

Definition at line 1509 of file uves_reduce.c.

References uves_msg, uves_msg_debug, uves_pfits_get_offset(), uves_polynomial_add_2d(), uves_polynomial_delete(), uves_polynomial_duplicate(), and uves_polynomial_rescale().

Referenced by extract_ff_rebin_merge().

cpl_image* uves_normalize_spectrum ( const cpl_image *  spectrum,
const cpl_image *  spectrum_error,
const uves_propertylist spectrum_header,
const uves_propertylist raw_header,
int  n_traces,
enum uves_chip  chip,
const cpl_table *  atm_extinction,
bool  correct_binning,
cpl_image **  scaled_error 
)

Normalize a spectrum.

Parameters:
spectrum The 1d (merged) or 2d (non-merged or 2d extracted+merged) spectrum to be normalized
spectrum_error Error (1 sigma) of spectrum, or NULL.
spectrum_header Header describing the geometry of the input spectrum
raw_header Header of the raw frame
n_traces Number of spatial bins (1 unless 2d extracted)
chip CCD chip
atm_extinction The table of extinction coefficients
correct_binning Flag indicating whether or not to divide by the x-binning factor
scaled_error (output) If non-NULL, error of output spectrum
Returns:
The normalized spectrum

The spectrum is divided by exposure time, gain and (optionally) binning. Also corrected for atmospheric extinction using the provided table of extinction coefficients.

Bad pixels are propagated.

Definition at line 122 of file uves_reduce_utils.c.

References assure_nomsg, check, uves_msg, uves_pfits_get_airmass_end(), uves_pfits_get_airmass_start(), uves_pfits_get_biny(), uves_pfits_get_cdelt1(), uves_pfits_get_crval1(), uves_pfits_get_exptime(), uves_pfits_get_gain(), uves_pfits_get_wstart(), and uves_spline_hermite_table().

Referenced by uves_response_efficiency(), and uves_scired_process_chip().


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