Provided by: wsclean_3.1-4_amd64 
NAME
WSClean - Fast generic widefield interferometric imager
SYNOPSIS
wsclean [options] <input-ms> [<2nd-ms> [..]]
DESCRIPTION
WSClean (w-stacking clean) is a fast generic widefield imager. It uses the w-stacking
algorithm and can make use of the w-snapshot algorithm. As of Feb 2014, it is 2-12 times
faster than CASA's w-projection, depending on the array configuration. It supports full-
sky imaging and proper beam correction for homogeneous dipole arrays such as the MWA.
WSClean allows Hogbom and Cotton-Schwab cleaning, and can clean polarizations joinedly.
All operations are performed on the CPU (it is not specialized for GPUs).
OPTIONS
GENERAL OPTIONS
-version
Print WSClean's version and exit.
-j <threads>
Specify number of computing threads to use, i.e., number of cpu cores that will be
used. Default: use all cpu cores.
-mem <percentage>
Limit memory usage to the given fraction of the total system memory. This is an
approximate value. Default: 100.
-absmem <memory limit>
Like -mem, but this specifies a fixed amount of memory in gigabytes.
-reorder, -no-reorder
Force or disable reordering of Measurement Set. This can be faster when the
measurement set needs to be iterated several times, such as with many major
iterations or in channel imaging mode. Default: only reorder when in channel
imaging mode.
-tempdir <directory>
Set the temporary directory used when reordering files. Default: same directory as
input measurement set.
-no-dirty
Do not save the dirty image.
-saveweights
Save the gridded weights in the a fits file named <image-prefix>-weights.fits.
-saveuv
Save the gridded uv plane, i.e., the FFT of the residual image. The UV plane is
complex, hence two images will be output: <prefix>-uv-real.fits and <prefix>-uv-
imag.fits.
-apply-primary-beam
Calculate and apply the primary beam and save images for the Jones components, with
weighting identical to the weighting as used by the imager. Only available for
LOFAR.
-reuse-primary-beam
If a primary beam image exists on disk, reuse those images (not implemented yet).
-use-differential-lofar-beam
Assume the visibilities have already been beam-corrected for the reference
direction.
-update-model-required (default), -no-update-model-required
These two options specify whether the model data column is required to contain
valid model data after imaging. It can save time to not update the model data
column.
-verbose (or -v)
Increase verbosity of output.
-log-time
Add date and time to each line in the output.
-quiet Do not output anything but errors.
WEIGHTING OPTIONS
-weight <weightmode>
Weightmode can be: natural, uniform, briggs. Default: uniform. When using Briggs'
weighting, add the robustness parameter, like: "-weight briggs 0.5".
-superweight <factor>
Increase the weight gridding box size, similar to Casa's superuniform weighting
scheme. Default: 1.0 The factor can be rational and can be less than one for
subpixel weighting.
-mfsweighting
In spectral mode, calculate the weights as if the image was made using MFS. This
makes sure that the sum of channel images equals the MFS weights. Otherwise, the
channel image will become a bit more naturally weighted. This is only relevant for
weighting modes that require gridding (i.e., Uniform, Briggs'). Default: off,
unless -joinchannels is specified.
-nomfsweighting
Opposite of -mfsweighting; can be used to turn off MFS weighting in -joinchannels
mode.
-weighting-rank-filter <level>
Filter the weights and set high weights to the local mean. The level parameter
specifies the filter level; any value larger than level*localmean will be set to
level*localmean.
-weighting-rank-filter-size <size>
Set size of weighting rank filter. Default: 16.
-taper-gaussian <beamsize>
Taper the weights with a Gaussian function. This will reduce the contribution of
long baselines. The beamsize is by default in asec, but a unit can be specified
("2amin").
-taper-tukey <lambda>
Taper the outer weights with a Tukey transition. Lambda specifies the size of the
transition; use in combination with -maxuv-l.
-taper-inner-tukey <lambda>
Taper the weights with a Tukey transition. Lambda specifies the size of the
transition; use in combination with -minuv-l.
-taper-edge <lambda>
Taper the weights with a rectangle, to keep a space of lambda between the edge and
gridded visibilities.
-taper-edge-tukey <lambda>
Taper the edge weights with a Tukey window. Lambda is the size of the Tukey
transition. When -taper-edge is also specified, the Tukey transition starts inside
the inner rectangle.
INVERSION OPTIONS
-name <image-prefix>
Use image-prefix as prefix for output files. Default is 'wsclean'.
-size <width> <height>
Default: 2048 x 2048
-trim <width> <height>
After inversion, trim the image to the given size.
-scale <pixel-scale>
Scale of a pixel. Default unit is degrees, but can be specificied, e.g. -scale
20asec. Default: 0.01deg.
-nwlayers <nwlayers>
Number of w-layers to use. Default: minimum suggested #w-layers for first MS.
-nwlayers-for-size <width> <height>
Use the minimum suggested w-layers for an image of the given size. Can e.g. be used
to increase accuracy when predicting small part of full image.
-channelsout <count>
Splits the bandwidth and makes count nr. of images. Default: 1.
-predict
Only perform a single prediction for an existing image. Doesn't do any imaging or
cleaning. The input images should have the same name as the model output images
would have in normal imaging mode.
-predict-channels <nchannels>
Interpolate from a given number of images to the number of channels that are
predicted as specified by -channelsout. Will interpolate using the frequencies of
the images. Use one the -fit-spectral-... options to specify the interpolation
method / freedom. Only used when -predict is specified.
-subtract-model
Subtract the model from the data column in the first iteration. This can be used to
reimage an already cleaned image, e.g. at a different resolution.
-nosmallinversion, -smallinversion
Perform inversion at the Nyquist resolution and upscale the image to the requested
image size afterwards. This speeds up inversion considerably, but makes aliasing
slightly worse. This effect is in most cases <1%. Default: on.
-gridmode <"nn", "kb" or "rect">
Kernel and mode used for gridding: kb = Kaiser-Bessel (default with 7 pixels), nn =
nearest neighbour (no kernel), rect = rectangular window. Default: kb.
-gkernelsize <size>
Gridding antialiasing kernel size. Default: 7.
-oversampling <factor>
Oversampling factor used during gridding. Default: 63.
-make-psf
Always make the psf, even when no cleaning is performed.
-make-psf-only
Only make the psf, no images are made.
-savegridding
Save the gridding correction image. This shows the effect of the antialiasing
filter. Default: not saved.
-dft-prediction
Predict via a direct Fourier transform. This is slow, but can account for
direction-dependent effects. This has only effect when -mgain is set or -predict is
given.
-dft-with-beam
Apply the beam during DFT. Currently only works for LOFAR.
-visibility-weighting-mode [normal/squared/unit]
Specify visibility weighting modi. Affects how the weights (normally) stored in
WEIGHT_SPECTRUM column are applied. Useful for estimating e.g. EoR power spectra
errors. Normally one would use this in combination with -no-normalize-for-
weighting.
-no-normalize-for-weighting
Disable the normalization for the weights, which makes the PSF's peak one. See
-visibility-weighting-mode. Only useful with natural weighting.
DATA SELECTION OPTIONS
-pol <list>
Default: 'I'. Possible values: XX, XY, YX, YY, I, Q, U, V, RR, RL, LR or LL (case
insensitive). Multiple values can be separated 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 is not appropriate for telescopes with non-orthogonal
feeds, such as MWA and LOFAR. The 'xy' polarization will output both a real and an
imaginary image, which allows calculating true Stokes polarizations for those
telescopes.
-interval <start-index> <end-index>
Only image the given time interval. Indices specify the timesteps, end index is
exclusive. Default: image all time steps.
-intervalsout <count>
Number of intervals to image inside the selected global interval. Default: 1
-channelrange <start-channel> <end-channel>
Only image the given channel range. Indices specify channel indices, end index is
exclusive. Default: image all channels.
-field <fieldid>
Image the given field id. Default: first field (id 0).
-datacolumn <columnname>
Default: CORRECTED_DATA if it exists, otherwise DATA will be used.
-maxuvw-m <meters>, -minuvw-m <meters>
Set the min/max baseline distance in meters.
-maxuv-l <lambda>, -minuv-l <lambda>
Set the min/max uv distance in lambda.
-maxw <percentage>
Do not grid visibilities with a w-value higher than the given percentage of the max
w, to save speed. Default: grid everything
DECONVOLUTION OPTIONS
-niter <niter>
Maximum number of clean iterations to perform. Default: 0
-threshold <threshold>
Stopping clean thresholding in Jy. Default: 0.0
-gain <gain>
Cleaning gain: Ratio of peak that will be subtracted in each iteration. Default:
0.1
-mgain <gain>
Cleaning gain for major iterations: Ratio of peak that will be subtracted in each
major iteration. To use major iterations, 0.85 is a good value. Default: 1.0
-joinpolarizations
Perform cleaning by searching for peaks in the sum of squares of the polarizations,
but subtract components from the individual images. Only possible when imaging two
or four Stokes or linear parameters. Default: off.
-joinchannels
Perform cleaning by searching for peaks in the MFS image, but subtract components
from individual channels. This will turn on mfsweighting by default. Default: off.
-multiscale
Clean on different scales. This is a new algorithm. Default: off. This parameter
invokes the v1.9 multiscale algorithm, which is slower but more accurate compared
to the older algorithm, and therefore the recommended one to use. The older
algorithm is now invoked with -fast-multiscale.
-fast-multiscale
Clean on different scales. This is a new fast experimental algorithm. Default: off.
This method used to be invoked with -multiscale before v1.9, but the newer
multiscale algorithm is somewhat more accurate and therefore recommended.
-multiscale-threshold-bias
Parameter to lower the threshold for larger scales. The used threshold for a scale
is threshold(scale)=pointsource_threshold x tbias^scale. A lower bias will clean
larger scales deeper. Default: 0.7
-multiscale-scale-bias
Parameter to prevent cleaning small scales in the large-scale iterations. A higher
bias will give more focus to larger scales. Default: 0.6
-multiscale-scales <comma-separated list of sizes in pixels>
Sets a list of scales to use in multi-scale cleaning. If unset, WSClean will select
the delta (zero) scale, scales starting at four times the synthesized PSF, and
increase by a factor of two until the maximum scale is reached. Example:
-multiscale-scales 0,5,12.5
-iuwt Use the IUWT deconvolution algorithm.
-moresane-ext <location>
Use the MoreSane deconvolution algorithm, installed at the specified location.
-moresane-arg <arguments>
Pass the specified arguments to moresane. Note that multiple parameters have to be
enclosed in quotes.
-moresane-sl <sl1,sl2,...>
MoreSane --sigmalevel setting for each major loop iteration. Useful to start at
high levels and go down with subsequent loops, e.g. 20,10,5
-cleanborder <percentage>
Set the border size in which no cleaning is performed, in percentage of the
width/height of the image. With an image size of 1000 and clean border of 1%, each
border is 10 pixels. Default: 5 (%).
-fitsmask <mask>
Use the specified fits-file as mask during cleaning.
-casamask <mask>
Use the specified CASA mask as mask during cleaning.
-smallpsf
Resize the psf to speed up minor clean iterations. Not the default.
-nonegative
Do not allow negative components during cleaning. Not the default.
-negative
Default on: opposite of -nonegative.
-stopnegative
Stop on negative components. Not the default.
-fit-spectral-pol <nterms>
Fit a polynomial over frequency to each clean component. This has only effect when
the channels are joined with -joinchannels.
-fit-spectral-log-pol <nterms>
Like fit-spectral-pol, but fits a logarithmic polynomial over frequency instead.
-deconvolution-channels <nchannels>
Decrease the number of channels as specified by -channelsout to the given number
for deconvolution. Only possible in combination with one of the -fit-spectral
options. Proper residuals/restored images will only be returned when mgain < 1.
-squared-channel-joining
Use with -joinchannels to perform peak finding in the sum of squared values over
channels, instead of the normal sum. This is useful for imaging QU polarizations
with non-zero rotation measures, for which the normal sum is insensitive.
-force-dynamic-join
Use alternative joined clean algorithm (feature for testing).
RESTORATION OPTIONS
-beamsize <arcsec>
Set the FWHM beam size in arcsec for restoring the clean components. Default:
longest projected baseline defines restoring beam.
-beamshape <maj in arcsec> <min in arcsec> <position angle in deg>
Set the FWHM beam shape for restoring the clean components. Defaults units for maj
and min are arcsec, and degrees for PA. Can be overridden, e.g. '-beamshape 1amin
1amin 3deg'.
-fitbeam
Determine beam shape by fitting the PSF (default if PSF is made).
-nofitbeam
Do not determine beam shape from the PSF.
-theoreticbeam
Write the beam in output fits files as calculated from the longest projected
baseline. This method results in slightly less accurate integrated fluxes, but in
simple imaging provide a beam size even without making the PSF. Default: off.
-circularbeam
Force the beam to be circular: bmin will be set to bmaj.
-ellipticalbeam
Allow the beam to be elliptical. Default.
AUTHOR
André Offringa <offringa@gmail.com>