Commit f2ab108f authored by mancini's avatar mancini

Add parameters

parent 968a5ccd
Pipeline #470 passed with stages
in 7 minutes and 50 seconds
......@@ -27,6 +27,104 @@ inputs:
type: Directory
inputBinding:
position: 2
- id: no_reorder
type: boolean?
default: false
inputBinding:
prefix: -no-reorder
- id: no_update
type: boolean?
default: false
inputBinding:
prefix: -no-update-model
- id: mgain
type: float?
inputBinding:
prefix: -mgain
doc: |
Set the major iteration gain: during every major iteration,
the peak is reduced by the given factor.
With an mgain of 0.8, the peak is reduced by 80%.
This is quite a common and safe option for cleaning.
With a reasonable good PSF, 0.9 is accettable choice without losing
accuracy but speeding up the computation. With a very bad PSF,
it might be necessary to lower the mgain parameter.
- id: mem
type: int?
inputBinding:
prefix: -mem
doc: |
Limit memory usage to the given fraction of the total system memory. This is an approximate value.
- id: n_threads
type: int?
inputBinding:
prefix: -j
doc: |
Specify number of computing threads to use, i.e., number of cpu cores that will be used.
- id: no-update-model-required
type: boolean?
doc:
Do not require the update of the data column after imaging
inputBinding:
prefix: -no-update-model-required
- id: weight
type: string?
inputBinding:
prefix: -weight
doc: |
Weightmode can be: natural, uniform, briggs. Default: uniform. When using Briggs' weighting,
add the robustness parameter, like: briggs 0.5.
- id: pol
type: string?
inputBinding:
prefix: -pol
doc: |
Default: \'I\'. Possible values: XX, XY, YX, YY, I, Q, U, V, RR, RL, LR or LL (case insensitive).
It is allowed but not necessary to separate with commas, e.g.: 'xx,xy,yx,yy'.
Two or four polarizations can be joinedly cleaned (see '-joinpolarizations'), but
this is not the default. I, Q, U and V polarizations will be directly calculated from
the visibilities, which might require correction to get to real IQUV values. The
'xy' polarization will output both a real and an imaginary image, which allows calculating
true Stokes polarizations for those telescopes.
- id: niter
type: integer?
inputBinding:
prefix: -niter
doc: |
Maximum number of clean iterations to perform. Default: 0 (=no cleaning)
- id: intervals-out
type: integer?
inputBinding:
prefix: -intervals-out
doc: |
Number of intervals to image inside the selected global interval. Default: 1
- id: interval
type: integer[]?
inputBinding:
prefix: -interval
doc: |
Only image the given time interval. Indices specify the timesteps, end index is exclusive.
Default: image all time steps.
- id: multiscale
type: boolean?
inputBinding:
prefix: -multiscale
doc: |
Clean on different scales. This is a new algorithm. Default: off.
This parameter invokes the optimized multiscale algorithm published by Offringa & Smirnov (2017).
- id: auto-threshold
type: int?
inputBinding:
prefix: -auto-threshold
doc: |
Estimate noise level using a robust estimator and stop at sigma x stddev.
- id: auto-mask
type: int
inputBinding:
prefix: -auto-mask
doc: |
Construct a mask from found components and when a threshold of sigma is reached, continue
cleaning with the mask down to the normal threshold.
outputs:
dirty_image:
type: File
......
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