sinfo_stectrum_ima2table |
convert an image in a table spectrum
- Parameters:
-
| spc | input image spectrum |
| filename | input filename |
| tbl | output table |
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int | sinfo_stectrum_ima2table (const cpl_image *spc, const char *filename, cpl_table **tbl) |
| convert an image in a table spectrum
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sinfo_new_vector() |
allocates memory for a new sinfo_vector
- Parameters:
-
| n_elements | number of sinfo_vector elements |
- Returns:
- Vector
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Vector * | sinfo_new_vector (ulong32 n_elements) |
sinfo_free_svector() |
frees memory of a sinfo_vector
- Parameters:
-
- Returns:
- nothing
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void | sinfo_free_svector (Vector **svector) |
sinfo_new_destroy_vector() |
frees memory of a sinfo_vector
- Parameters:
-
- Returns:
- nothing
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void | sinfo_new_destroy_vector (Vector *sinfo_vector) |
sinfo_new_vector_to_image() |
converts a spectral sinfo_vector to a fits image
- Parameters:
-
| spectral | sinfo_vector that should be converted to a fits image |
- Returns:
- image with lx = 1 and ly = length of sinfo_vector
- Note:
- sinfo_vector object spectrum is destroyed
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cpl_image * | sinfo_new_vector_to_image (Vector *spectrum) |
sinfo_new_image_to_vector() |
converts a fits image to a spectral sinfo_vector
- Parameters:
-
| 1-D | Fits image that should be converted to a spectral sinfo_vector |
- Returns:
- spectral sinfo_vector with length ly
- Note:
- input image is destroyed
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Vector * | sinfo_new_image_to_vector (cpl_image *spectrum) |
sinfo_new_extract_spectrum_from_resampled_flat() |
extracts a spectrum from an image image
- Parameters:
-
| resflat,: | resampled halogen lamp frame, bad pixel corrected |
| loreject,@param | hireject: percentage of extreme low and high intensity values to be rejected from averaging |
- Returns:
- fits image that contains the final halogen lamp spectrum builds one spectrum in a fits image out of a resampled flatfield frame by taking a clean mean along the spatial pixels
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cpl_image * | sinfo_new_extract_spectrum_from_resampled_flat (cpl_image *resflat, float loreject, float hireject) |
sinfo_new_multiply_image_with_spectrum() |
multiplies a resampled image with a resampled spectrum in the same spectral range
- Parameters:
-
| image,: | resampled image |
| spectrum,: | resampled spectrum in image format |
- Returns:
- resulting image multiplys a resampled image with a resampled spectrum (calibrated halogen lamp spectrum) in the same spectral range that means all image columns are multiplied with the same spectrum
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cpl_image * | sinfo_new_multiply_image_with_spectrum (cpl_image *image, cpl_image *spectrum) |
sinfo_new_optimal_extraction_from_cube() |
does the optimal extraction of a standard star spectrum
- Parameters:
-
| cube,: | input data cube |
| llx,@param | lly: lower left sinfo_edge points of the 2d Gaussian fitting box |
| halfbox_x,@param | halfbox_y: half width of a box inside which a 2D-Gaussian fit is carried out |
| fwhm_factor,: | factor applied to the found fwhms of a 2D-Gaussian fit, defines the radius of the aperture inside which the spectral extraction is carried out (default: 0.6). |
| backvariance,: | (readnoise^2 + sinfo_dark current variance) needed to determine the noise variance of the background. Must be given in counts/sec. |
| sky,: | estimated sky variance in counts/sec |
| gain,: | conversion factor electrons/count |
| exptime,: | total exposure time |
- Returns:
- resulting spectrum stored in a 1D-image does the optimal extraction of a standard star spectrum according to the equation: S = sum { (P^2 / V) * (I - B) / P } / sum{ P^2 / V } S: spectral flux at a particular wavelength P: normalized PSF (determined by a 2D-Gaussian fit) I: pixel value B: background pixel value determined by the background parameter of the 2D-Gaussian fit V: estimated variance of a pixel: V = [R^2 + D + sky + I,c/exptime]/gain where R is the read noise, and D the sinfo_dark current variance. backvariance is R^2 + D in counts/sec. I,c is the source intensity in counts
- Note:
- : sigma,e[e-] = gain[e/count] * sigma,c [counts] = sqrt(I,e) = sqrt(gain*I,c) => V,c = sigma,c^2 = sigma,e^2/gain^2 => sigma,c = sqrt(I,c/gain) => V,c = I,c/gain
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cpl_image * | sinfo_new_optimal_extraction_from_cube (cpl_imagelist *cube, int llx, int lly, int halfbox_x, int halfbox_y, float fwhm_factor, float backvariance, float sky, float gain, float exptime, const char *name, cpl_table **spectrum, int qc_info, int *check2) |
sinfo_new_extract_sky_from_cube() |
extracts a sky spectrum from a data cube
- Parameters:
-
| cube,: | reduced cube from sky spider observation |
| loReject,@param | hiReject: fraction (percentage) of the extreme high and low sky spectrum values that are rejected before averaging the found sky spectra. |
| position,: | end pixel positions of the straight line in the image dividing the sky from the object pixels. |
| tolerance,: | pixel tolerance which are not considered and subtracted from the diagonal line to be sure to get a clean sky, default: 2 |
| posindicator,: | indicates in which sinfo_edge of the field of view the sky is projected. output of spiffi_get_spiderposindex() in fitshead.c |
- Returns:
- resulting averaged sky spectrum extracts a sky spectrum from a reduced sky spider observation, that means from a data cube. Therefore, the position of the sky within the field of view must be first read from the fits header. A pixel tolerance is subtracted. The found sky spectra are averaged by rejecting the extreme high and low values.
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Vector * | sinfo_new_extract_sky_from_cube (cpl_imagelist *cube, float loReject, float hiReject, int *position, int tolerance, int posindicator) |
sinfo_new_sum_rectangle_of_cube_spectra() |
summing routine for a reduced data to get a better spectral S/N only for a rectangular aperture
- Parameters:
-
| cube,: | 1 allocated cube, |
| llx,@param | lly, |
| urx,@param | ury: lower left and upper right position of rectangle in x-y plane , image coordinates 0... |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_sum_rectangle_of_cube_spectra (cpl_imagelist *cube, int llx, int lly, int urx, int ury) |
sinfo_new_sum_circle_of_cube_spectra() |
summing routine for a reduced data to get a better spectral S/N only for a circular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| centerx,@param | centery: center pixel of circular aperture in image coordinates |
| radius,: | integer radius of circular aperture |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_sum_circle_of_cube_spectra (cpl_imagelist *cube, int centerx, int centery, int radius) |
sinfo_new_mean_rectangle_of_cube_spectra() |
averaging routine for a reduced data to get a better spectral S/N only for a rectangular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| llx,@param | lly, |
| urx,@param | ury: lower left and upper right position of rectangle in x-y plane , image coordinates 0... |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_mean_rectangle_of_cube_spectra (cpl_imagelist *cube, int llx, int lly, int urx, int ury) |
sinfo_new_mean_circle_of_cube_spectra() |
averaging routine for a reduced data to get a better spectral S/N only for a circular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| centerx,@param | centery: center pixel of circular aperture in image coordinates |
| radius,: | integer radius of circular aperture |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_mean_circle_of_cube_spectra (cpl_imagelist *cube, int centerx, int centery, int radius) |
sinfo_new_blackbody_spectrum() |
computes a blackbody spectral intensity distribution (W/(m^2 lambda ster))
- Parameters:
-
| templateSpec,: | spectrum of a standard star (1-d image with fits header) |
| temp,: | blackbody temperature in Kelvin (standard Star temp), |
- Returns:
- resulting spectrum sinfo_vector
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Vector * | sinfo_new_blackbody_spectrum (char *templateSpec, double temp) |
sinfo_new_median_rectangle_of_cube_spectra() |
sinfo_median routine for a reduced data to get a better spectral S/N only for a rectangular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| llx,@param | lly, |
| urx,@param | ury: lower left and upper right position of rectangle in x-y plane , image coordinates 0... |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_median_rectangle_of_cube_spectra (cpl_imagelist *cube, int llx, int lly, int urx, int ury) |
sinfo_new_median_circle_of_cube_spectra() |
sinfo_median routine for a reduced data to get a better spectral S/N only for a circular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| centerx,@param | centery: center pixel of circular aperture in image coordinates |
| radius,: | integer radius of circular aperture |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_median_circle_of_cube_spectra (cpl_imagelist *cube, int centerx, int centery, int radius) |
sinfo_new_cleanmean_rectangle_of_cube_spectra() |
clean averaging routine for a reduced data to get a better spectral S/N only for a rectangular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| llx,@param | lly, |
| urx,@param | ury: lower left and upper right position of rectangle in x-y plane , image coordinates 0... |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_cleanmean_rectangle_of_cube_spectra (cpl_imagelist *cube, int llx, int lly, int urx, int ury, float lo_reject, float hi_reject) |
sinfo_new_cleanmean_circle_of_cube_spectra() |
clean averaging routine for a reduced data to get a better spectral S/N only for a circular aperture.
- Parameters:
-
| cube,: | 1 allocated cube, |
| centerx,@param | centery: center pixel of circular aperture in image coordinates |
| radius,: | integer radius of circular aperture |
- Returns:
- result spectrum sinfo_vector
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Vector * | sinfo_new_cleanmean_circle_of_cube_spectra (cpl_imagelist *cube, int centerx, int centery, int radius, float lo_reject, float hi_reject) |
sinfo_new_shift_array() |
shifts an array by a sub-pixel shift value using a tanh interpolation kernel
- Parameters:
-
| input,: | input array, |
| n_elements,: | number of elements in input array |
| shift,: | sub-pixel shift value (must be < 1.) |
| ker,: | interpolation kernel |
- Returns:
- resulting float array
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float * | sinfo_new_shift_array (float *input, int n_elements, float shift, double *ker) |
sinfo_new_div_image_by_spectrum() |
divides a resampled image with a resampled spectrum in the same spectral range
- Parameters:
-
| image,: | resampled image |
| spectrum,: | resampled spectrum in image format |
- Returns:
- resulting image divides a resampled image with a resampled spectrum in the same spectral range that means all image columns are multiplied with the same spectrum
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cpl_image * | sinfo_new_div_image_by_spectrum (cpl_image *image, cpl_image *spectrum) |
Vector * | sinfo_new_clean_mean_circle_of_cube_spectra (cpl_imagelist *cube, int centerx, int centery, int radius, float lo_reject, float hi_reject) |
Vector * | sinfo_new_clean_mean_rectangle_of_cube_spectra (cpl_imagelist *cube, int llx, int lly, int urx, int ury, float lo_reject, float hi_reject) |