A number of solvers are available in ASKAPsoft. For imaging purposes only specialized image solvers
are generally used, although generic SVD-based linear solver (see the diagram above) can be used
with (very small) images as well (some change to the code may be required as this is not a normal
use case). The *solver* parset parameter defines the type of the image solver to use with the choice
between *Dirty*, *and Clean*. The *Dirty* solver just inverts the data (takes the normal equations
and simply divides the data vector by the diagonal of the normal matrix. This is analogous to making
the dirty image or a linear mosaic of dirty images), while the Clean performs minor cycle cleaning.
If multiple beams and/or fields are present in the dataset (and mosaicing gridders (see
*Gridders* for details) are used), joint deconvolution is always preformed (individual
deconvolution is not supported).

The Restore solver is somewhat special. It is executed behind the scene with very minimal setup
required from the user (the same parameters are generally used as for the cleaning solver). Restore
solver is described separately in the *cimager*.

Parameters for all solvers:

Parameter |
Type |
Default |
Description |
---|---|---|---|

solver | string | none | Selection of solver. Specify either “Clean” or “Dirty” |

verbose | string | “true” | True enables lots of output |

tolerance | float | 0.1 | cutoff value given as a fraction of the largest diagonal
element. The linear system describing interferometric
measurement is inverted approximately, assuming that the
matrix is diagonal, i.e. the right-hand side is divided
by the appropriate diagonal element (which is a
weight). If diagonal is smaller than this tolerance
multiplied by the largest diagonal element, the
right-hand side instead is either divided by the largest
diagonal element to get the result or the result is set
to zero. This is controlled by weightcutoff
parameter. For images it means that areas with low
weight (i.e. a mosaic edge) are not boosted up. In
addition to weight truncation, all pixels with the
weight below cutoff are normally masked out. The
weightcutoff.clean parameter allows to assign mask
corresponding to weight truncation. This allows
S/N-based cleaning to happen, if the peak of S/N is
realised outside the nominal field of view. |

weightcutoff | string | truncate | Either “zero” or “truncate”. This parameter controls
what actually happens for values below cutoff defined by
the tolerance parameter. If zero is given, the
appropriate values are set to zero. For truncate,
the values are divided by the largest diagonal. |

weightcutoff.clean | bool | false | This parameter defines whether the values below cutoff are masked out or not. By default, the are masked out and so S/N-based clean never finds optima among these values. If this parameter is true, the mask is actually sqrt(tolerance), which corresponds to truncation of the diagonal during normalisation. This potentially allows cleaning to happen, if no peak of the S/N is realised among these values. |

Parameters **verbose** and **tolerance** have **solver.Clean** or **solver.Dirty** prefix. Although verbose is
understood by dirty solver, there is currently no effect. **Dirty** solver doesn’t require any additional
parameters (but one can also set up a preconditioner described in the following section with the dirty solver).
Additional parameters understood by the **Clean** solver are given in the following section.

All parameters given in the next table have **solver.Clean** prefix (i.e. Cimager.solver.Clean.algorithm) or
Cimager.solver.Clean.scales. The *Clean* solver with algorithm set to “Basisfunction” is an improved version
of the casacore *LatticeCleaner*. Most importantly, it supports use of a patch in the deconvolution. This
decreases memory use and run time by approximately the ratio of pixels in the patch to pixels in the image.

Parameter |
Type |
Default |
Description |
---|---|---|---|

algorithm | string | “MultiScale” | Valid choices are “MultiScale”, “Basisfunction”,
“Hogbom”, “MultiScaleMFS” and “BasisfunctionMFS”. Use
“Hogbom” for a single scale, non-MFS case. For the Clean
solver, the casacore’s LatticeCleaner used to do the
actual work in non-MSMFS case will be set up with
CleanEnums::HOGBOM if algorithm is Hogbom and the
single scale of 0 will be used. For the Basisfunction
algorithm, a re-implemented and improved version of the
CASA MultiScale algorithm is used |

scales | vector<string> | [0, 3, 10] | Scales to be solved (defined in pixels). Ignored if algorithm=”Hogbom” |

niter | int | 100 | Number of minor cycles |

gain | float | 0.7 | Loop gain. Fraction of the peak subtracted during one minor cycle. |

speedup | float | no speed up | Relevant for “MultiScale” and “MultiScaleMFS” only. If defined, the value will be passed as a speed up factor to the lattice cleaners doing the minor cycle. According to casacore’s manual, this will speed up clean by raising the threshold (could help if the threshold set too low for the given dataset). The physical meaning of the parameter is the number of iterations required to double the threshold. |

padding | float | 1.0 | Optional padding of all images in the solver (minor
cycle will be done on an image this factor times larger
on both axes, e.g. to alleviate the fact that FFT is
used to compute convolutions). Default value means no
padding. At this stage this option is understood by
MultiScale cleaner only |

logevery | int | 1 | How frequently to log progress in the minor cycle. Every
nth iteration is reported (ie. if logevery=100,
every 100th iteration is reported), providing the
iteration number, the peak residual, the objective
function and the total flux. |

saveintermediate | bool | true | Save intermediate images (residuals and preconditioned PSF) at the end of each majorcycle. |

The following parameters are available for the Basisfunction and BasisfunctionMFS algorithms.

Parameter |
Type |
Default |
Description |
---|---|---|---|

psfwidth | int | 0 | Sets the width of the psf patch used in the minor cycle. This decreases memory use and run time by approximately the ratio of pixels in the patch to pixels in the image. |

All parameters given in the next table **do not** have **solver.Clean** prefix (i.e. Cimager.threshold.minorcycle).

Parameter |
Type |
Default |
Description |
---|---|---|---|

threshold.minorcycle | vector<string> | no threshold | If defined, the parameter can be either a single string or a vector of two strings. A number without units is interpreted as a fractional stopping threshold (with respect to the peak residual) as well as the number with the percentage sign. An absolute flux given in Jy or related units is interpreted as an absolute threshold. Either one or both of these thresholds can be given in the same time. Undefined parameter means no minor cycle thresholding is done |

threshold.majorcycle | string | -1Jy | The target peak residual. Use negative value to ensure all requested major cycles are done. |

threshold.masking | float | -1 | If the value is negative (default), a
signal-to-noise based cleaning is done. In other
words, a peak of S/N is searched at every minor
cycle, rather than a flux peak. A positive value
reverts the algorithm back to the traditional
absolute flux peak-based clean. In this case, the
value is the threshold used for masking on the
basis of the weight. For example, a value of 0.9
(btw, this is the default in the casacore’s
LatticeCleaner, and, therefore, could be
implicitly adopted in casa imager) means that all
pixels with less than 90% weight (defined as
square root from the ratio of matrix diagonal to
the maximum diagonal element) will be masked out
for cleaning purposes. |

preconditioner.Names | vector<string> | empty vector | List of preconditioners to be applied (in the
order they are given in the list). Preconditioners
are ASKAPsoft equivalents of visibility weighting
(i.e. uniform, robust, natural), which do not
require multiple passes over the
dataset. Preconditioners can be viewed as
operators applied to equation matrix before it is
solved. Having the normal matrix as close to the
diagonal as possible (a diagonal form is actually
assumed during the inversion process) makes the
inversion more accurate. By default, no
transformation to the normal matrix is done. This
is equivalent to the natural weighting. The
following preconditioners are currently
implemented: Wiener, NormWiener,
Robust and GaussianTaper. In addition, the
word None is understood as an empty
preconditioner which does nothing. Each
preconditioner requires a specific set of
parameters described in a separate section. These
parameters are given after the name of the
preconditioner,
e.g. preconditioner.Wiener.noisepower (see
below) |

preconditioner.name.xxx | Use this form to define parameter xxx for
preconditioner name. Note, this preconditioner
will only be instantiated and used if its name
appears in the list given in
preconditioner.Names. Description of individual
parameters are given in a separate section. |
||

preconditioner.preservecf | bool | false | Use a modified PSF to generate any preconditioner
that is derived from the uv sampling function
(e.g. Wiener and Robust). This option
takes a running mean over an approximate
nearest-neighbour sampling function
with a box width that is proportional to the
support size of the gridding kernels. This enables
post-gridding density weighting while preserving
the gridding convolutions.
Note that this is currently only used with the
Wiener preconditioner and the WProject
gridder. |

The normal matrix can optionally be transformed by a preconditioning operator before equations are solved.
This step can regularise the matrix and improve the quality of the solution. It is the ASKAPsoft way of
implementing visibility weighting for the PSF (e.g. uniform, robust), and does not require an additional
pass over the data. The following preconditioners are currently implemented: **Wiener**, **NormWiener**,
**Robust** and **GaussianTaper**.

A Wiener filter, which is constructed from the PSF, is the preferred preconditioner. This preconditioner is somewhat analogous to robust weighting.

The preconditioners are described below along with the available parameters. The parameters need a
**preconditioner.preconditionerName** prefix, but not the **solver** prefix (e.g.
**Cimager.preconditioner.Wiener.noisepower**), although technically preconditioning is done in the
solver. When defined this way, the same parameters can be reused in the *restore solver* (described in
the *cimager* documentation). One exception to this is the *restore solver* itself, which can
have an additional preconditioner specified for the final restore step (e.g.
**Cimager.restore.preconditioner.Wiener.robustness**). The additional restored files will have the
**.alt.restored** suffix.

The table below contains the description of individual parameters (names starts with **preconditionerName**).

Parameter |
Type |
Default |
Description |
---|---|---|---|

Wiener.noisepower | float | none | If the Wiener filter is defined with noisepower,
this exact value of noise power will be used to
construct the filter. Optionally, the PSF can be
normalised before the filter is constructed (see
normalise option – this is a replacement for
the NormWiener preconditioner).
Note that the Wiener filter must be specified with
either noisepower or robustness, and it is
recommended that preservecf is set to true. |

Wiener.normalise | bool | false | This is an additional option for a Wiener
preconditioner being constructed from an explicit
value of the noise power (i.e. noisepower). If
set to true, the PSF will be normalised to 1.0
before the filter is constructed, easing
interpretation. Note, this option is incompatible
with robustness, because in that case the PSF
is always normalised). |

Wiener.robustness | float | none | The noise power is derived from the given value of
robustness to have roughly the same effect as the
analogous parameter in Robust (i.e., -2.0 close to
uniform weighting, +2.0 close to natural weighting).
Note that the Wiener filter must be specified with
either noisepower or robustness. |

Wiener.taper | float | none | If defined, the FFT of the uv sampling function used to generate the Wiener filter (effectively the PSF) will be tapered with a Gaussian. The value of the parameter is the FWHM of the taper in image pixels. Restricting the filter size to approximately that of the primary beam size is of particular importance when imaging over fields that are larger than the primary beam. There is little point to tapering if preservecf = true. |

NormWiener.robustness | float | 0.0 | Roughly the same effect as the same parameter in Robust. |

Robust.robustness | float | 0.0 | Post-gridding version of robust weighting is
applied. It is recommended that preservecf
is set to true. |

GaussianTaper | vector<string> | None | A Gaussian taper is applied to the visibilities.
The parameter should be either a single string with
the FWHM of a circular gaussian taper, or a vector
of three strings for an elliptical taper: the major
and minor axis FWHM and the position angle. String
values may contain units, e.g.
[10arcsec,10arcsec,34deg]. If no units are
given, radians are assumed. GaussianTaper
currently conflicts with different uv-cell sizes
for different images. An exception is thrown if
such a condition exists. |

```
Cimager.solver = Clean
Cimager.solver.Clean.algorithm = MultiScale
Cimager.solver.Clean.scales = [0, 3, 10]
Cimager.solver.Clean.niter = 10000
Cimager.solver.Clean.gain = 0.1
Cimager.solver.Clean.tolerance = 0.1
Cimager.solver.Clean.verbose = True
Cimager.threshold.minorcycle = [0.27mJy, 10%]
Cimager.threshold.majorcycle = 0.3mJy
Cimager.preconditioner.Names = [Wiener,GaussianTaper]
Cimager.preconditioner.GaussianTaper = [30arcsec, 8arcsec, 10deg]
Cimager.preconditioner.Wiener.noisepower = 100.0
Cimager.ncycles = 5
Cimager.restore = True
Cimager.restore.beam = [30arcsec, 30arcsec, 0deg]
```

```
Cimager.solver = Dirty
Cimager.solver.Dirty.tolerance = 0.1
Cimager.solver.Dirty.verbose = True
Cimager.ncycles = 0
```