Provenance information as activity list

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.

The data is then cut to a useful wavelength range (if --crop=true).

If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice is multiplied by the normalized median flux of that slice in the ILLUM exposure.

As last step, the data is divided by the normalized twilight cube (if given), using the 3D coordinate of each pixel in the pixel table to interpolate the twilight correction onto the data.

This pre-reduced pixel table for each exposure is then saved to disk.

Processing handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not "none"), optionally detects cosmic rays (note that by default cosmic ray rejection is handled in the post processing recipes while the data is reformatted into a datacube, so that the default setting is cr="none" here), converts the images from adu to count, subtracts the dark, divides by the flat-field, and (optionally) propagates the integrated flux value from the twilight-sky cube.

[For special cases, users can choose to combine all input files at the image level, so that the pixel table is only created once, for the combined data. This is not recommended for science data, where the combination should take place after correcting for atmospheric effects, before the creation of the final cube.]

The reduced image is then saved (if --saveimage=true).

The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table for each exposure.

If --skylines contains one or more wavelengths for (bright and isolated) sky emission lines, these lines are used to correct the wavelength calibration using an offset.