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| − | == Help on clean task: ==
| + | {{clean}} |
| − | <pre>
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| − | Invert and deconvolve images with selected algorithm
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| − | | |
| − | The clean task has many options:
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| − |
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| − | 1) Make 'dirty' image and 'dirty' beam (psf)
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| − | 2) Multi-frequency-continuum images or spectral channel imaging
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| − | 3) Full Stokes imaging
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| − | 4) Mosaicking of several pointings
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| − | 5) Multi-scale cleaning
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| − | 6) Widefield cleaning
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| − | 7) Interactive clean boxing
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| − | 8) Use starting model (eg from single dish)
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| − |
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| − |
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| − | vis -- Name of input visibility file
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| − | default: none; example: vis='ngc5921.ms'
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| − | imagename -- Pre-name of output images:
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| − | default: none; example: imagename='m2'
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| − | output images are:
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| − | m2.image; cleaned and restored image
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| − | With or without primary beam correction
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| − | m2.psf; point-spread function (dirty beam)
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| − | m2.flux; relative sky sensitivity over field
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| − | m2.flux.pbcoverage; relative pb coverage over field
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| − | (gets created only for ft='mosaic')
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| − | m2.model; image of clean components
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| − | m2.residual; image of residuals
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| − | m2.interactive.mask; image containing clean regions
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| − | To include outlier fields:
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| − | imagename=['n5921','outlier1','outlier2']
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| − | outlierfile --- Text file name which contains image names, sizes, field
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| − | centers
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| − | field -- Select fields to image or mosaic. Use field id(s) or name(s).
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| − | ['go listobs' to obtain the list id's or names]
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| − | default: ''= all fields
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| − | If field string is a non-negative integer, it is assumed to
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| − | be a field index otherwise, it is assumed to be a
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| − | field name
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| − | field='0~2'; field ids 0,1,2
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| − | field='0,4,5~7'; field ids 0,4,5,6,7
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| − | field='3C286,3C295'; field named 3C286 and 3C295
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| − | field = '3,4C*'; field id 3, all names starting with 4C
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| − | spw -- Select spectral window/channels
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| − | NOTE: channels de-selected here will contain all zeros if
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| − | selected by the parameter mode subparameters.
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| − | Channel selection behaves differently in clean (e.g. The multiple
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| − | ranges are not supported yet).
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| − | default: ''=all spectral windows and channels
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| − | spw='0~2,4'; spectral windows 0,1,2,4 (all channels)
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| − | spw='0:5~61'; spw 0, channels 5 to 61
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| − | spw='<2'; spectral windows less than 2 (i.e. 0,1)
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| − | spw='0,10,3:3~45'; spw 0,10 all channels, spw 3,
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| − | channels 3 to 45.
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| − | spw='0~2:2~6'; spw 0,1,2 with channels 2 through 6 in each.
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| − |
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| − |
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| − | selectdata -- Other data selection parameters
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| − | default: True
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| − | | |
| − | >>> selectdata=True expandable parameters
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| − | See help par.selectdata for more on these
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| − | | |
| − | timerange -- Select data based on time range:
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| − | default: '' (all); examples,
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| − | timerange = 'YYYY/MM/DD/hh:mm:ss~YYYY/MM/DD/hh:mm:ss'
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| − | Note: if YYYY/MM/DD is missing date defaults to first
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| − | day in data set
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| − | timerange='09:14:0~09:54:0' picks 40 min on first day
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| − | timerange='25:00:00~27:30:00' picks 1 hr to 3 hr
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| − | 30min on NEXT day
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| − | timerange='09:44:00' pick data within one integration
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| − | of time
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| − | timerange='>10:24:00' data after this time
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| − | uvrange -- Select data within uvrange (default units meters)
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| − | default: '' (all); example:
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| − | uvrange='0~1000klambda'; uvrange from 0-1000 kilo-lambda
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| − | uvrange='>4klambda';uvranges greater than 4 kilo lambda
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| − | antenna -- Select data based on antenna/baseline
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| − | default: '' (all)
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| − | If antenna string is a non-negative integer, it is
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| − | assumed to be an antenna index, otherwise, it is
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| − | considered an antenna name.
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| − | antenna='5&6'; baseline between antenna index 5 and
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| − | index 6.
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| − | antenna='VA05&VA06'; baseline between VLA antenna 5
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| − | and 6.
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| − | antenna='5&6;7&8'; baselines 5-6 and 7-8
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| − | antenna='5'; all baselines with antenna index 5
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| − | antenna='05'; all baselines with antenna number 05
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| − | (VLA old name)
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| − | antenna='5,6,9'; all baselines with antennas 5,6,9
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| − | index numbers
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| − | scan -- Scan number range.
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| − | default: '' (all)
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| − | example: scan='1~5'
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| − | Check 'go listobs' to insure the scan numbers are in order.
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| − | mode -- Frequency Specification:
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| − | NOTE: Channels deselected with spw parameter will contain all
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| − | zeros.
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| − | See examples below.
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| − | default: 'mfs'
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| − | mode = 'mfs' means produce one image from all
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| − | specified data.
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| − | mode = 'channel'; Use with nchan, start, width to specify
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| − | output image cube.
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| − | mode = 'velocity', channels are specified in velocity.
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| − | mode = 'frequency', channels are specified in frequency.
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| − | | |
| − | >>> mode='mfs' expandable parameters
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| − | Make a continuum image from the selected frequency
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| − | channels/range using Multi-frequency synthesis
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| − | algorithm for wide-band narrow field imaging. nterms
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| − | is the number of Taylor terms to be used to model the
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| − | frequency dependence of the sky emission. nterms=1 is
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| − | equivalent to assuming no frequency dependence.
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| − | nterms=2 is equivalent to the Sault-Wieringa algorithm
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| − | (AandAS, 1994) reffreq is the reference frequency about
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| − | which the Taylor expansion is done. ** Note that the
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| − | software implementation of the algorithm for nterms>1
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| − | is still experimental and will be fully available in a
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| − | later release. **
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| − | | |
| − | >>> mode='channel', 'velocity', and 'frequency' expandable parameters
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| − | nchan -- Total number of channels in the output image.
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| − | Example: nchan=100.
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| − | Default: -1; Automatically selects enough channels to cover
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| − | data selected by 'spw' and consistent with 'start' and 'width'.
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| − | It is often easiest to leave nchan at the default value.
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| − | start -- First channel, velocity, or frequency.
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| − | For mode='channel'; This selects the channel index number
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| − | from the MS (0 based) that you want to correspond to the first
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| − | channel of the output cube. The output cube will be in frequency
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| − | space with the first channel having the frequency of the
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| − | MS channel selected by start. start=0 refers to the first
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| − | channel in the first selected spw, even if that channel
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| − | is de-selected in the spw parameter. Channels de-selected by
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| − | the spw parameter will be filled with zeros if included by
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| − | the start parameter. For example, spw=3~8:3~100 and start=2
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| − | will produce a cube that starts on the third channel (recall 0
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| − | based) of spw index 3, and the first channel will be blank.
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| − | example:start=5
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| − | For mode='velocity' or 'frequency': default='';
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| − | starts at first input channel of first input spw
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| − | examples: start='5.0km/s', or start='22.3GHz'.
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| − | width -- Output channel width
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| − | For mode='channel', default=1; >1 indicates channel averaging
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| − | example: width=4.
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| − | For mode=' 'velocity' or 'frequency', default=''; width of
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| − | first input channel, or more precisely, the difference
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| − | in frequencies between the first two selected channels.
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| − | (for example if channels 1 and 3 are selected with spw,
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| − | then the default width will be the difference between their
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| − | frequencies, and not the width of channel 1)
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| − | When not using the default, one must give units
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| − | examples: width='1.0km/s', or width='24.2kHz'.
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| − | Setting width>0 gives channels of increasing frequency for
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| − | mode='frequency', and increasing velocity for mode='velocity'.
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| − | interpolation -- Interpolation type for spectral gridding onto
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| − | the uv-plane. Options: 'nearest', 'linear', or 'cubic'.
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| − | default = 'linear'
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| − | chaniter -- specify how spectral CLEAN is performed,
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| − | default: chaniter=False;
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| − | example: chaniter=True; step through channels
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| − | WARNING: The interactive clean with chaniter=True for
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| − | optical velocity mode
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| − | (mode='velocity' and veltype='optical') is
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| − | NOT YET IMPLEMENTED.
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| − | outframe -- For mode='velocity', 'frequency', or 'channel': velocity
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| − | reference frame of output image
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| − | Options: '','LSRK','LSRD','BARY','GEO','TOPO','GALACTO',
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| − | 'LGROUP','CMB'
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| − | default: ''; same as input data
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| − | example: frame='bary' for Barycentric frame
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| − | veltype -- for mode='velocity' gives the velocity definition
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| − | Options: 'radio','optical'
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| − | default: 'radio'
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| − | NOTE: the viewer always defaults to displaying the 'radio'
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| − | frame, but that can be changed in the position tracking
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| − | pull down.
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| − | mode='mfs' examples:
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| − | spw = '0,1'; mode = 'mfs'
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| − | will produce one image made from all channels in spw
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| − | 0 and 1
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| − | spw='0:5~28^2'; mode = 'mfs'
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| − | will produce one image made with channels
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| − | (5,7,9,...,25,27)
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| − | | |
| − | mode='channel' examples:
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| − | spw = '0'; mode = 'channel': nchan=3; start=5; width=4
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| − | will produce an image with 3 output planes
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| − | plane 1 contains data from channels (5+6+7+8)
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| − | plane 2 contains data from channels (9+10+11+12)
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| − | plane 3 contains data from channels (13+14+15+16)
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| − | spw = '0:0~63^3'; mode='channel'; nchan=21; start = 0;
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| − | width = 1
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| − | will produce an image with 20 output planes
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| − | Plane 1 contains data from channel 0
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| − | Plane 2 contains date from channel 2
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| − | Plane 21 contains data from channel 61
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| − | spw = '0:0~40^2'; mode = 'channel'; nchan = 3; start =
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| − | 5; width = 4
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| − | will produce an image with three output planes
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| − | plane 1 contains channels (5,7)
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| − | plane 2 contains channels (13,15)
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| − | plane 3 contains channels (21,23)
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| − | | |
| − | psfmode -- method of PSF calculation to use during minor cycles:
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| − | default: 'clark': Options: 'clark','clarkstokes', 'hogbom'
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| − | 'clark' use smaller beam (faster, usually good enough);
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| − | for stokes images clean components peaks are searched
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| − | in the I^2+Q^2+U^2+V^2 domain
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| − | 'clarkstokes' locate clean components independently in
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| − | each stokes image
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| − | 'hogbom' full-width of image (slower, better for poor
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| − | uv-coverage)
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| − | Note: psfmode will also be used to clean if imagermode = ''
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| − | imagermode -- Advanced imaging e.g. mosaic or Cotton-Schwab clean
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| − | default: imagermode='': Options: '', 'csclean', 'mosaic'
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| − | default '' => psfmode cleaning algorithm used
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| − | | |
| − | >>> gridmode='' expandable parameters
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| − | The default value of '' has no effect.
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| − |
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| − | >>> gridmode='widefield' expandable parameters
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| − | Apply corrections for non-coplanar effects during imaging
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| − | using the W-Projection algorithm (Cornwell et al. IEEE JSTSP
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| − | (2008)) or faceting or a combination of the two.
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| − | | |
| − | wprojplanes is the number of pre-computed w-planes used for
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| − | the W-Projection algorithm. wprojplanes=1 disables
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| − | correction for non-coplanar effects.
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| − | facets is the number of facets used. W-Projection is done
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| − | for each facet.
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| − | | |
| − | >>> gridmode='aprojection' expandable parameters
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| − | Corrects for the (E)VLA polarization squint using the
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| − | A-Projection algorithm (Bhatnagar et al., AandA (2008)).
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| − | cfcache is the name of the directory to be used to cache the
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| − | convolution functions. These functions can be reused
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| − | again if the image parameters are unchanged. If the image
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| − | parameters change, a new cache must be created (or the
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| − | existing one removed).
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| − | painc (in degrees) is the Parallactic Angle increment used to
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| − | compute the convolution functions.
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| − | | |
| − | >>> imagermode='mosaic' expandable parameter(s):
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| − | Make a mosaic of the different pointings (uses csclean style
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| − | too)
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| − | mosweight -- Individually weight the fields of the mosaic
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| − | default: False; example: mosweight=True
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| − | This can be useful if some of your fields are more
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| − | sensitive than others (i.e. due to time spent
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| − | on-source); this parameter will give more weight to
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| − | higher sensitivity fields in the overlap regions.
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| − | ftmachine -- Gridding method for the mosaic;
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| − | Options: 'ft' (standard interferometric gridding), 'sd'
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| − | (standard single dish),
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| − | and 'mosaic' (grid using PB as convolution function).
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| − | default: 'mosaic';
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| − | ONLY if imagermode='mosaic' is chosen and
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| − | ftmachine='mosaic', is heterogeneous imaging (CARMA, ALMA)
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| − | possible using the right convolution of primary beams for
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| − | each baseline.
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| − | scaletype -- Controls scaling of pixels in the image plane.
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| − | (Not fully implemented...for now only controls
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| − | what is seen if interactive=True...but in the future will
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| − | control the image on which clean components are searched)
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| − | default='SAULT'; example: scaletype='PBCOR'
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| − | Options: 'PBCOR','SAULT'
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| − | 'SAULT' when interactive=True shows the residual
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| − | with constant noise across the mosaic.
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| − | be acheived by setting pbcor=True.
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| − | 'PBCOR' uses the SAULT scaling scheme for
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| − | deconvolution, but if interactive=True shows the
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| − | primary beam corrected image during interactive.
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| − | | |
| − | >>> imagermode='csclean' expandable parameter(s):
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| − | Image using the Cotton-Schwab algorithm in between major cycles
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| − | cyclefactor -- Change the threshold at which the deconvolution
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| − | cycle will stop, degrid and subtract from the visibilities
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| − | For poor PSFs, reconcile often (cyclefactor=4 or 5);
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| − | For good PSFs, use cyclefactor 1.5 to 2.0.
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| − | Note: threshold = cyclefactor * max sidelobe * max residual
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| − | default: 1.5; example: cyclefactor=4
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| − | cyclespeedup -- Cycle threshold doubles in this number of
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| − | iterations
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| − | default: -1;
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| − | example: cyclespeedup=3
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| − | try cyclespeedup = 50 to speed up cleaning
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| − | | |
| − | multiscale -- set of scales to use in deconvolution. If set,
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| − | cleans with several resolutions using hobgom clean. The
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| − | scale sizes are in units of cellsize. So if
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| − | cell='2arcsec', a multiscale scale=10 = 20arcsec. First
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| − | scale should always be 0 (point), we suggest second on
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| − | the order of synthesized beam, third 3-5 times
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| − | synthesized beam, etc. For example if synthesized beam
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| − | is 10" and cell=2", try multscale = [0,5,15]. Note,
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| − | multiscale is currently a bit slow.
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| − | default: multiscale=[] (standard CLEAN with psfmode algorithm,
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| − | no multi-scale). Example: multiscale = [0,5,15]
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| − | | |
| − | >>> multiscale expandable parameter(s):
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| − | negcomponent -- Stop component search when the largest scale
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| − | has found this number of negative components;
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| − | -1 means continue component search even if the largest
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| − | component is negative. default: -1; example: negcomponent=50
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| − | smallscalebias -- A bias toward smaller scales.
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| − | The peak flux found at each scale is weighted by
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| − | a factor = 1 - smallscalebias*scale/max_scale, so
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| − | that Fw = F*factor.
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| − | Typically the values range from 0.2 to 1.0.
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| − | default: 0.6
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| − | | |
| − | imsize -- Image pixel size (x,y). DOES NOT HAVE TO BE A POWER OF 2
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| − | default = [256,256]; example: imsize=[350,350]
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| − | imsize = 500 is equivalent to [500,500]
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| − | If include outlier fields, e.g., [[400,400],[100,100]] or
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| − | use outlierfile.
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| − | Avoid odd-numbered imsize.
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| − | cell -- Cell size (x,y)
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| − | default= '1.0arcsec';
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| − | example: cell=['0.5arcsec,'0.5arcsec'] or
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| − | cell=['1arcmin', '1arcmin']
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| − | cell = '1arcsec' is equivalent to ['1arcsec','1arcsec']
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| − | NOTE:cell = 2.0 => ['2arcsec', '2arcsec']
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| − | phasecenter -- direction measure or fieldid for the mosaic center
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| − | default: '' => first field selected ; example: phasecenter=6
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| − | or phasecenter='J2000 19h30m00 -40d00m00'
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| − | If include outlier fields,
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| − | e.g. ['J2000 19h30m00 -40d00m00',J2000 19h25m00 -38d40m00']
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| − | or use outlierfile.
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| − | restfreq -- Specify rest frequency to use for output image
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| − | default='' Occasionally it is necessary to set this (for
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| − | example some VLA spectral line data). For example for
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| − | NH_3 (1,1) put restfreq='23.694496GHz'
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| − | stokes -- Stokes parameters to image
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| − | default='I'; example: stokes='IQUV';
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| − | Options: 'I','IV''QU','IQUV','RR','LL','XX','YY','RRLL','XXYY'
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| − | niter -- Maximum number iterations,
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| − | if niter=0, then no CLEANing is done ("invert" only)
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| − | default: 500; example: niter=5000
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| − | gain -- Loop gain for CLEANing
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| − | default: 0.1; example: gain=0.5
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| − | threshold -- Flux level at which to stop CLEANing
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| − | default: '0.0mJy';
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| − | example: threshold='2.3mJy' (always include units)
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| − | threshold = '0.0023Jy'
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| − | threshold = '0.0023Jy/beam' (okay also)
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| − | interactive -- use interactive clean (with GUI viewer)
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| − | default: interactive=False
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| − | example: interactive=True
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| − | interactive clean allows the user to build the cleaning
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| − | mask interactively using the viewer. The viewer will
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| − | appear every npercycle interation, but modify as needed
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| − | The final interactive mask is saved in the file
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| − | imagename_interactive.mask. The initial masks use the
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| − | union of mask and cleanbox (see below).
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| − | | |
| − | >>> interactive=True expandable parameters
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| − | npercycle -- this is the number of iterations between each
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| − | interactive update of the mask. It is important to modify
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| − | this number interactively during the cleaning, starting with
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| − | a low number like 20, but then increasing as more extended
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| − | emission is encountered.
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| − | | |
| − | mask -- Specification of cleanbox(es), mask image(s), and/or
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| − | region(s) to be used for CLEANing. As long as the image has
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| − | the same shape (size), mask images from a previous
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| − | interactive session can be used for a new execution. NOTE:
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| − | the initial clean mask actually used is the union of what
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| − | is specified in mask and <imagename>.mask default: [] (no
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| − | masking); Possible specification types: (a) Explicit
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| − | cleanbox pixel ranges example: mask=[110,110,150,145] clean
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| − | region with blc=110,100; trc=150,145 (pixel values) (b)
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| − | Filename with cleanbox pixel values with ascii format:
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| − | example: mask='mycleanbox.txt' <fieldid blc-x blc-y
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| − | trc-x trc-y> on each line
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| − | 1 45 66 123 124
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| − | 2 23 100 300 340
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| − | (c) Filename for image mask example: mask='myimage.mask'
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| − | (d) Filename for region specification (e.g. from viewer)
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| − | example: mask='myregion.rgn' (e) Combinations of any of the
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| − | above example: mask=[[110,110,150,145],'mycleanbox.txt',
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| − | 'myimage.mask','myregion.rgn']
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| − | If include outlier fields, then mask need to be specified in
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| − | nested lists:
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| − | e.g. mask=[[[110,110,150,145],'myimage.mask'],[],[20,20,40,40]]
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| − | (A clean box with [110,110,150,145] and a image mask for main
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| − | field, no mask for 1st outlier field, 1 clean box for second
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| − | outlier field.)
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| − | uvtaper -- Apply additional uv tapering of the visibilities.
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| − | default: uvtaper=False; example: uvtaper=True
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| − | >>> uvtaper=True expandable parameters
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| − | outertaper -- uv-taper on outer baselines in uv-plane
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| − | [bmaj, bmin, bpa] taper Gaussian scale in uv or
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| − | angular units. NOTE: the on-sky FWHM in arcsec is roughly
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| − | the uv taper/200 (klambda).
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| − | default: outertaper=[]; no outer taper applied
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| − | example: outertaper=['5klambda'] circular taper
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| − | FWHM=5 kilo-lambda
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| − | outertaper=['5klambda','3klambda','45.0deg']
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| − | outertaper=['10arcsec'] on-sky FWHM 10 arcseconds
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| − | outertaper=['300.0'] default units are meters
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| − | in aperture plane
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| − | innertaper -- uv-taper in center of uv-plane
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| − | [bmaj,bmin,bpa] Gaussian scale at which taper falls to
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| − | zero at uv=0
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| − | default: innertaper=[]; no inner taper applied
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| − | NOT YET IMPLEMENTED
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| − | modelimage -- Name of model image(s) to initialize cleaning. If
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| − | multiple images, then these will be added together to
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| − | form initial staring model NOTE: these are in addition
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| − | to any initial model in the <imagename>.model image file
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| − | default: '' (none); example: modelimage='orion.model'
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| − | modelimage=['orion.model','sdorion.image'] Note: if the
| |
| − | units in the image are Jy/beam as in a single-dish
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| − | image, then it will be converted to Jy/pixel as in a
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| − | model image, using the restoring beam in the image
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| − | header
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| − | weighting -- Weighting to apply to visibilities:
| |
| − | default='natural'; example: weighting='uniform';
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| − | Options: 'natural','uniform','briggs',
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| − | 'superuniform','briggsabs','radial'
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| − | | |
| − | >>> Weighting expandable parameters
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| − | For weighting='briggs' and 'briggsabs'
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| − | robust -- Brigg's robustness parameter
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| − | default=0.0; example: robust=0.5;
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| − | Options: -2.0 to 2.0; -2 (uniform)/+2 (natural)
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| − | For weighting='briggsabs'
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| − | noise -- noise parameter to use for Briggs "abs"
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| − | weighting
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| − | example noise='1.0mJy'
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| − | npixels -- uv-cell area used for weight calculation
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| − | example npixels=1
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| − | Default = 0
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| − | superuniform: 0 Means 3x3 cells for weighting
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| − | the cell weight is proportional to the weight of
| |
| − | the 3x3 cells centered on it.
| |
| − | superuniform = F means 1x1 cell for averaging weights.
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| − | briggs/briggsabs: 0 is similar to 1x1 cell weight.
| |
| − | 1 may? be similar to 3X3 cells.
| |
| − | Only npixels 0 or 1 recommended
| |
| − |
| |
| − | restoringbeam -- Output Gaussian restoring beam for CLEAN image
| |
| − | [bmaj, bmin, bpa] elliptical Gaussian restoring beam
| |
| − | default units are in arc-seconds for bmaj,bmin, degrees
| |
| − | for bpa default: restoringbeam=[]; Use PSF calculated
| |
| − | from dirty beam.
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| − | example: restoringbeam=['10arcsec'] circular Gaussian
| |
| − | FWHM 10 arcseconds example:
| |
| − | restoringbeam=['10.0','5.0','45.0deg'] 10"x5"
| |
| − | at 45 degrees
| |
| − | pbcor -- Output primary beam-corrected image
| |
| − | If pbcor=False, the final output image is NOT corrected for the
| |
| − | PB pattern (particularly important for mosaics), and therefore is
| |
| − | not "flux correct". Correction can also be done after the
| |
| − | fact using immath to divide <imagename>.image by
| |
| − | the <imagename>.flux image.
| |
| − | default: pbcor=False; output un-corrected image
| |
| − | example: pbcor=True; output pb-corrected image (masked outside
| |
| − | minpb)
| |
| − | minpb -- Minimum PB level to use default=0.2;
| |
| − | The flux image is used to determine this
| |
| − | except for the case of mosaic with ftmachine='mosaic'
| |
| − | where the flux.pbcoverage image is used.
| |
| − | example: minpb=0.01 Note: this minpb is always in effect
| |
| − | (regardless of pbcor=True/False)
| |
| − | calready -- if True will create scratch columns if they are
| |
| − | not there. And after clean completes the predicted model
| |
| − | visibility is from the clean components are written to the ms.
| |
| − | async -- Run asynchronously
| |
| − | default = False; do not run asychronously
| |
| − | | |
| − | | |
| − | ======================================================================
| |
| − | | |
| − | HINTS ON CLEAN WITH FLANKING FIELDS
| |
| − | | |
| − | 1. Decide if the images will be specified directly in the
| |
| − | inputs or with an outlier file. For more than a few fields,
| |
| − | an outlier file more convenient.
| |
| − | | |
| − | Direct Method:
| |
| − | | |
| − | cell = ['1.0arcsec', '1.0arcsec']
| |
| − | imagename = ['M1_0','M1_1','M1_2]
| |
| − | imsize = [[1024,1024],[128,128],[128,128]]
| |
| − | phasecenter = ['J2000 13h27m20.98 43d26m28.0',
| |
| − | 'J2000 13h30m52.159 43d23m08.02', 'J2000 13h24m08.16 43d09m48.0']
| |
| − | | |
| − | Text file method (in outlier.txt)
| |
| − | | |
| − | imagename = 'M1'
| |
| − | outlierfile = 'outlier.txt'
| |
| − | [phasecenter, imsize ignored]
| |
| − | | |
| − | Contents of outlier.txt
| |
| − | C 0 1024 1024 13 27 20.98 43 26 28.0
| |
| − | C 1 128 128 13 30 52.158 43 23 08.00
| |
| − | C 2 128 128 13 24 08.163 43 09 48.00
| |
| − | | |
| − | In both cases the following images will be made:
| |
| − | M1_0.image, M1_1.image, M1_2.image cleaned images
| |
| − | M1.0.model, M1_1.model, M1_2.model model images
| |
| − | M1.0.residual, M1_1.residual, M1_2.residual residual images
| |
| − | | |
| − | 2. Masks for flanking fields are specified in same way as
| |
| − | in the single output field case, but need extra '[ ]' to
| |
| − | distinguish each field.
| |
| − | mask=[['myregion.rg',[100,100,150,150]],['myimage1.mask'],[]]
| |
| − | would apply masks:
| |
| − | for the first field (main field),
| |
| − | myregion.rg and a box defined by [100,100,150,150] in pixels
| |
| − | for the seconf field (first outlier), myimage1.mask
| |
| − | for the third field (second outlier), no mask (produce a mask for
| |
| − | whole field)
| |
| − | However, if boxfiles are given, ids in the first column of the files
| |
| − | are used to match with fields (using order given imagename or
| |
| − | outlierfile.
| |
| − | So, if the content of a boxfile looks like this,
| |
| − | 0 45 66 123 124
| |
| − | 1 23 100 300 340
| |
| − | 2 20 20 40 40
| |
| − | then [45 66 123 124] is assigned to first field (imagename[0], or first line
| |
| − | of outlierfile).
| |
| − |
| |
| − |
| |
| − | </pre>
| |
