Difference between revisions of "Using QL outputs"
(→Important Notes) |
(→Important Notes) |
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The exact values for these are stored in: | The exact values for these are stored in: | ||
/usr/local/etc/qlgui/pars.json<br /> | /usr/local/etc/qlgui/pars.json<br /> | ||
| − | |||
"badMax0": 98, <br /> | "badMax0": 98, <br /> | ||
| − | |||
"badMin1": 2145, <br /> | "badMin1": 2145, <br /> | ||
| − | |||
in python 0-based numbering.<br /> | in python 0-based numbering.<br /> | ||
i.e. in python, to reproduce the same transformation, one would do:<br /> | i.e. in python, to reproduce the same transformation, one would do:<br /> | ||
| − | |||
from astropy.io import fits<br /> | from astropy.io import fits<br /> | ||
| − | |||
im2D = fits.getdata('image.fits')<br /> | im2D = fits.getdata('image.fits')<br /> | ||
| − | |||
im2D = im2D[:,-:] # flip x<br /> | im2D = im2D[:,-:] # flip x<br /> | ||
| − | |||
im2D = im2D[:,98:2145] # trim<br /> | im2D = im2D[:,98:2145] # trim<br /> | ||
| − | |||
fits.writeto('outimage.fits',im2D)<br /> | fits.writeto('outimage.fits',im2D)<br /> | ||
This image could then be used for a fresh extraction using IRAF or the user's preffered package, and will be one-to-one pixel aligned with the [approximate] WLC from the 1D extracted arc. | This image could then be used for a fresh extraction using IRAF or the user's preffered package, and will be one-to-one pixel aligned with the [approximate] WLC from the 1D extracted arc. | ||
| Line 33: | Line 25: | ||
In IRAF, the equivalent would be:<br /> | In IRAF, the equivalent would be:<br /> | ||
imcopy a0361665[-*,*] test.fits<br /> | imcopy a0361665[-*,*] test.fits<br /> | ||
| − | imcopy test.fits[99:2146,*] out65.fits< | + | imcopy test.fits[99:2146,*] out65.fits<br /> |
[Note the 1-based indexing] | [Note the 1-based indexing] | ||
Revision as of 10:25, 22 December 2016
Overview
The QL Tool produces quick-look products, but there are some straightforward steps allowing users to use these as a starting point for their science quality reductions
Important Notes
In going from the raw 2D images to the 1D extractions produce by the QL Tool:
- The x axis is flipped so that increasing wavelength runs in the same direction as increasing x
- The spectra are then trimmed to remove overscan, etc.
The exact values for these are stored in:
/usr/local/etc/qlgui/pars.json
"badMax0": 98,
"badMin1": 2145,
in python 0-based numbering.
i.e. in python, to reproduce the same transformation, one would do:
from astropy.io import fits
im2D = fits.getdata('image.fits')
im2D = im2D[:,-:] # flip x
im2D = im2D[:,98:2145] # trim
fits.writeto('outimage.fits',im2D)
This image could then be used for a fresh extraction using IRAF or the user's preffered package, and will be one-to-one pixel aligned with the [approximate] WLC from the 1D extracted arc.
In IRAF, the equivalent would be:
imcopy a0361665[-*,*] test.fits
imcopy test.fits[99:2146,*] out65.fits
[Note the 1-based indexing]
