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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
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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 arcseconds 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
| |
| 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>
| |
