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backest -- background or mask image for a slitless image
backest grism config
- Name of grism/prism image.
- Filename of grism/prism extraction configuration file.
- (np) [integer]
- The number of points to use in computing the medianed/averaged/fitted background.
- (interp) [integer]
- The type of interpolation to perform. The permitted values and their meaning are given below in the description.
- (niter_med) [integer]
- Number of kappa-sigma iterations around the sample median.
- (niter_fit) [integer]
- Number of kappa-sigma iterations around the fit.
- (kappa) [float]
- Kappa to use in the kappa-sigma iterations.
- (smooth_length) [int]
- Smoothing length?
- (smooth_fwhm) [float]
- FWHM in background smoothing?
- (old_bck = false) [boolean]
- Create a background in the old, aXe-1.4 format .
- (mask = false) [boolean]
- Create a mask image where the pixels at the beam positions have a characteristic value rather than interpolated values.
- (in_af = "") [string]
- Name to use for the input aperture file instead of the default. aXe default file naming conventions are described below.
- (out_back = "") [string]
- Name to use for the output background file instead of the default. aXe default file naming conventions are described below.
This task uses the input slitless image and a Background Aperture File (BAF) to generate a Background Estimate File (BEF). In the BEF the beams listed in the BAF file are either masked (mask="YES") or replaced by background pixel values derived from intepolating the borders of the beam areas.
If a background image is requested, the number of points to use (np) and the order of the interpolation (interp) to be used when computing the background balues can be set. The values in the regions within each of the BEAMs listed in the BAF are replaced by the median, average, linear, or nth order interpolation of pixels which are immediately above and below a BEAM (but not within any other BEAM). The number of pixels to use for this is by default set to 10 both below and above each BEAM. The np option can be used to change this default value. The type of interpolation is controlled by the interp parameter:
interp= -1 Median interp= 0 Average interp= 1 Linear fit interp= n>1 nth order polynomial fit
If a mask image is requested, the pixels within the beams are replaced with the value -1000000. With the mask option set this task is used by the axetask AXEPREP.
If the cosmic ray hits are not flagged in the dq-extensions, the background estimates are usually very bad due to the large data numbers in the cosmic ray affected pixels. To get also in those circumstances acceptable background estimates the task can perform a kappa-sigma rejection to eject the cosmics from the assembly of background pixels. backest offers a kappa sigma rejection based on deviations from the median data value as well as a rejection based on the deviations from the fit to the data points. The number of iterations is given in niter_med for median based rejection and niter_fit for fit based rejection, respectively. While the median based rejection is executed prior to the fit based, both use the identical value given in kappa to identify pixels to be rejected.
The number of pixels used for the interpolation (np) can be limited due to for example crowding in dense fields. In such situations the background may show stripes in the interpolation direction. backest offers to smooth with a Gaussian the background areas in the dispersion direction (x-direction) to eliminate these features. The parameters smooth_length and smooth_fwhm give the number of pixels and the FWHM of the Gaussian used to compute the smoothed value of each background pixel. By default, no smoothing is applied (smooth_length=0 and smooth_fwhm=0.0). With e.g. smooth_length=5, for each pixel the background pixels in a distance of <=5 pixels in x-direction (that is at most 10) are used to compute the smoothed background value. When smoothing close to the border of the beam areas, the non-interpolated outside pixels are not used, hence the number of pixels is lower (down to 5).
aXe tasks use default names for input and output files based on the given name of the "grism" image. For this task the default input BAF would be called <grism-rootname>_<science extension>.BAF and the output BEF would be <grism-rootname>_<science extension>.BCK.fits for the background computation. If the beams are only masked out, the resulting file would be <grism-rootname>_<science extension>.MSK.fits
1. Generate a background estimate file (BEF) from the image test_grism_1.fits using a background aperture file (BAF) with the standard default name. 10 points will be used and cubic (3rd order) interpolation will be performed.
ax> backest test_grism_1.fits np=10 interp=3
2. As in 1., but reject cosmic rays using first 2 kappa-sigma iterations around the median and then 3 iterations around the (cubic) fit with kappa=3.0 before doing the final, cubic fit.
ax> backest test_grism_1.fits np=10 interp=3 niter_med=2 niter_fit=3 kapp=3.0
Refer to manual for more detailed information about using this aXe task: