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− | <pre>
| + | {{clean}} |
− | Deconvolve an image with selected algorithm
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− | | |
− | This is the main clean deconvolution task. It contains many functions
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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) Interactive clean boxing
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− | 7) 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 in mosaic. Use field id(s) or field 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: This selects the data passed as the INPUT to mode
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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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− | spw='0:0~10;15~60'; spectral window 0 with channels
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− | 0-10,15-60
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− | spw='0:0~10,1:20~30,2:1;2;3'; spw 0, channels 0-10,
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− | spw 1, channels 20-30, and spw 2, channels, 1,2 and 3
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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: 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. See examples below
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− | mode = 'velocity', means channels are specified in
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− | velocity.
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− | mode = 'frequency', means channels are specified in
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− | 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.
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− | nterms is the number of Taylor terms to be used to
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− | model the frequency dependence of the sky emission.
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− | nterms=1 is equivalent to assuming no frequency
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− | dependence. nterms=2 is equivalent to the
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− | Sault-Wieringa algorithm (AandAS, 1994)
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− | reffreq is the reference frequency about which the
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− | Taylor expansion is done.
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− | | |
− | >>> mode expandable parameters (for modes other than 'mfs')
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− | Start, width are given in units of channels, frequency
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− | or velocity as indicated by mode (note: only nearest neighbour
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− | interpolation is available at this time).
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− | nchan -- Number of channels (planes) in output image
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− | default: 1; example: nchan=3
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− | start -- Start input channel (relative-0)
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− | default=0; example: start=5
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− | width -- Output channel width in units of the input
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− | channel width (>1 indicates channel averaging)
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− | default=1; example: width=4
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− | interpolation -- Interpolation type of spectral data when gridded on
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− | the uv-plane
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− | default = 'nearest'
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− | HOWEVER, 'linear' is recommended
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− | outframe -- velocity reference frame of output image (for mode='velocity' or 'frequency')
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− | Options: '','LSRK','LSRD','BARY','GEO','TOPO','GALACTO','LGROUP','CMB'
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− | default: ''; same as input data; example: frame='bary' for Barycentric frame
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− | veltype -- (for mode='velocity') velocity definition
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− | Options: 'radio','optical','true' (='relativistic')
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− | veltype='true' (or equivalently 'relativistic')
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− | for velocity defined without approximations using the relativistic expression
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− | default: 'radio'
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− | 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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− | 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 in the I^2+Q^2+U^2+V^2 domain
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− | 'clarkstokes' locate clean components independently in 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 be used to clean is 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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− | | |
− | Correct 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 again if
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− | the image parameters are unchanged. If the image parameters
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− | change, a new cache must be created (or the existing one
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− | 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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− | Image as a mosaic of the different pointings (uses csclean style 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 image;
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− | Options: ft (standard interferometric gridding), sd
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− | (standard single dish) both (ft and sd as appropriate),
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− | mosaic (gridding use PB as convolution function)
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− | default: 'mosaic'; example: ftmachine='ft'
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− | if imagermode mosaic is chosen and ftmachine is mosaic,
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− | heterogenous arrays like Carma or Alma are recognized
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− | and the right Primary Beam (depending on the size of the dish)
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− | is used for 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. If
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− | pbcor=False, the final output image is NOT
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− | corrected for the PB pattern, and therefore is
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− | not "flux correct". Division of SAULT
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− | <imagename>.image by the <imagename>.flux image
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− | will produce a "flux correct image", can also
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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; the final PBCOR
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− | image is "flux correct" if pbcor=True.
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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 using 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 has
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− | found this number of negative components; -1 means continue
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− | component search even if the largest component is
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− | 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 clean
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− | to update mask interactively. It is important to modify
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− | this number interactively during the cleaning, starting wiht
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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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− | chaniter -- specify how interactive CLEAN is performed,
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− | either by stepping through channels or do jointly for all channel
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− | default: chaniter='joint';
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− | example: chaniter='channel'; step through channels
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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 field,
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− | no mask for 1st outlier field, 1 clean box for second 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: uv taper in (klambda) is roughly on-sky
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− | FWHM(arcsec/200)
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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"
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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
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− | 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:
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− | 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
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− | the 3x3 cells centered on it.
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− | superuniform = F means 1x1 cell for averaging weights.
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− | briggs/briggsabs: 0 is similar to 1x1 cell weight.
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− | 1 may? be similar to 3X3 cells.
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− | Only npixels 0 or 1 recommended
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− |
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− | restoringbeam -- Output Gaussian restoring beam for CLEAN image
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− | [bmaj, bmin, bpa] elliptical Gaussian restoring beam
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− | default units are in arc-seconds for bmaj,bmin, degrees
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− | for bpa default: restoringbeam=[]; Use PSF calculated
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− | from dirty beam.
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− | example: restoringbeam=['10arcsec'] circular Gaussian
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− | FWHM 10" example:
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− | restoringbeam=['10.0','5.0','45.0deg'] 10"x5"
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− | at 45 degrees
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− | pbcor -- Output primary beam-corrected image
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− | default: pbcor=False; output un-corrected image
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− | example: pbcor=True; output pb-corrected image (masked outside
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− | minpb) Note: if you set pbcor=False, you can later
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− | recover the pbcor image by dividing by the .flux image
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− | (e.g. using immath)
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− | minpb -- Minimum PB level to use default=0.1;
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− | The flux image is used to determine this
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− | except for the case of mosaic with ft='mosaic'
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− | where the flux.pbcoverage image is used.
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− | example:
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− | minpb=0.01 Note: this minpb is always in effect
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− | (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.
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− | async -- Run asynchronously
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− | 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,
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− | an outlier file more convenient.
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− | | |
− | Direct Method:
| |
− | | |
− | cell = ['1.0arcsec', '1.0arcsec']
| |
− | imagename = ['M1_0','M1_1','M1_2]
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− | imsize = [[1024,1024],[128,128],[128,128]]
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− | 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
| |
− | 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>
| |