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default_reduction [2013/09/05 06:06]
mjc |
default_reduction [2013/09/05 06:26] (current)
mjc |
| | //CAL// | 'superbias' | imcombine, generate_wifes_bias_fit | Creates super-bias from bias frame co-add, then fits a smooth model of the bias shape across entire detector. | | | //CAL// | 'superbias' | imcombine, generate_wifes_bias_fit | Creates super-bias from bias frame co-add, then fits a smooth model of the bias shape across entire detector. | |
| | **02** | 'bias_sub' | imarith | Subtracts master bias (or local bias) from science frames. | | | **02** | 'bias_sub' | imarith | Subtracts master bias (or local bias) from science frames. | |
| | //CAL// | 'superflat'<sup>A</sup> | imcombine | Co-adds all flats (standard: median coadd). | | | //CAL// | 'superflat' | imcombine | Co-adds all flats (standard: median coadd).<sup>A</sup> | |
| | //CAL// | 'slitlet_profile' | derive_slitlet_profiles | Uses flat lamp to measure slitlet locations. | | | //CAL// | 'slitlet_profile' | derive_slitlet_profiles | Uses flat lamp to measure slitlet locations. | |
| | //CAL// | 'flat_cleanup' | interslice_cleanup | Corrects contamination of flat lamp and sky flat data for internal light reflections inside the instrument. | | | //CAL// | 'flat_cleanup' | interslice_cleanup | Corrects contamination of flat lamp and sky flat data for internal light reflections inside the instrument. | |
| | //CAL// | 'wire_soln' | derive_wifes_wire_solution | Derives spatial zeropoint in the y-direction (along slitlet) from a wire frame. | | | //CAL// | 'wire_soln' | derive_wifes_wire_solution | Derives spatial zeropoint in the y-direction (along slitlet) from a wire frame. | |
| | //CAL// | 'flat_response' | wifes_2dim_response | Uses lamp flat, sky flat, and wavelength solution to [[data_reduction#flat-fielding|derive flatfield response function]] for all slitlet. | | | //CAL// | 'flat_response' | wifes_2dim_response | Uses lamp flat, sky flat, and wavelength solution to [[data_reduction#flat-fielding|derive flatfield response function]] for all slitlet. | |
| | **04** | 'cosmic_rays' | x | x | | | **04** | 'cosmic_rays' | lacos_wifes | Identify and correct cosmic rays using the [[http://adsabs.harvard.edu/abs/2001PASP..113.1420V|LA Cosmic]] procedure developed by Pieter van Dokkum, as adapted to work with WiFeS data. | |
| | **05** | 'sky_sub'<sup>B</sup> | x | x | | | **05** | 'sky_sub' | imarith | Raw subtraction of sky frame from science frame, or sky pixels from object pixels in nod-and-shuffle (appropriately scaled for exposure time).<sup>B</sup> | |
| | **06** | 'obs_coadd' | x | x | | | **06** | 'obs_coadd' | imcombine | Co-add multiple observations of the same object or field, as defined by the metadata structure. | |
| | **07** | 'flatfield' | x | x | | | **07** | 'flatfield' | imarith | Divide science data by the flatfield response function. | |
| | **08** | 'cube_gen' | x | x | | | **08** | 'cube_gen' | generate_wifes_cubes | Rectify data onto square (x,y,λ) grid to [[data_reduction#data_cube_generation|create final data cube]]. | |
| | //CAL// | x | x | x | | | //CAL// | 'extract_stars' | extract_wifes_stdstar | Automatically extract standard star spectrum from WiFeS data cube (uncalibrated). | |
| | **09** | 'flux_calib' | x | x | | | //CAL// | 'derive_calib' | derive_wifes_calibration | Derive instrument sensitivity function from comparison of observed standard star fluxes to reference spectra.<sup>C</sup> | |
| | **10** | 'telluric_corr' | x | x | | | **09** | 'flux_calib' | calibrate_wifes_cube | Flux calibrate the data by applying instrument sensitivity function to science frames. | |
| | **11** | 'save_3dcube' | x | x | | | //CAL// | 'extract_stars' | extract_wifes_stdstar | Automatically extract standard star spectrum from WiFeS data cube (calibrated, but not telluric-corrected). | |
| | | //CAL// | 'derive_telluric' | derive_wifes_telluric | Derive telluric feature corrections from flux-calibrated spectra of smooth-spectrum standard stars. | |
| | | **10** | 'telluric_corr' | apply_wifes_telluric | Correct telluric absorption in all science frames. | |
| | | **11** | 'save_3dcube' | generate_wifes_3dcube | Convert fully calibrated data into standard 3D fits data format, as preferred for ds9. | |
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| <sup>A</sup> "Superflat" procedures performed for both spectral (quartz lamp) flats and spatial (twilight) flats. | <sup>A</sup> "Superflat" procedures performed for both spectral (quartz lamp) flats and spatial (twilight) flats. |
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| <sup>B</sup> Currently this step is a strict subtraction of object data and sky data (either "point-and-stare" or "nod-and-shuffle"). This is planned to be moved to after flat-fielding once a sophisticated sky-subtraction model procedure has been devised (part of PyWiFeS "Phase 2"). | <sup>B</sup> Currently this step is a strict subtraction of object data and sky data (either "point-and-stare" or "nod-and-shuffle"). This is planned to be moved to after flat-fielding once a sophisticated sky-subtraction model procedure has been devised (part of PyWiFeS "Phase 2"). |
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| | <sup>C</sup> Identification of standard star spectra is done automatically by name matching from the 'OBJECT' header field to the list of stars in 'wifes_calib.py'. Alternatively users can set the name of the standard stars in their calibration list manually. Plans for PyWiFeS "Phase 2" include automatic identification based on target coordinates. |
