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imager.makeimage - Function

2.5.1 Calculate images by gridding, etc.


Description

This tool function actually does gridding (and Fourier inversion if needed) of visibility data to make an image. It allows calculation of various types of image:

observed
Make the dirty image from the DATA column (default)
model
Make the dirty image from the MODEL_DATA column
corrected
Make the dirty image from the CORRECTED_DATA column
residual
Make the dirty image from the difference of the CORRECTED_DATA and MODEL_DATA columns
psf
Make the point spread function
singledish
Make a single dish image
coverage
Make a single dish coverage image
holography
Make a complex holography image
pb
Make the primary beam as defined by setvp

Note the full imager equation is not used and so, for example, the primary beam correction is not performed. Use restore to get a residual image using the full imager equation where primary beam correction is performed.

A position shift can be applied when specifying the image parameters with defineimage. If a shift is specified then the uvw coordinates are reprojected prior to gridding, and a phase rotation is applied. If the image is a PSF then no phase shift is applied but the uvw are recomputed. To see the effects of the uvw reprojected, you can use the plotuv function.

If desired, the full complex image (before conversion to stokes I,Q,U,V) may be retained. Note that the image tool cannot load a complex image directly. Instead, use the imagecalc constructor to take e.g. the real and imaginary parts of the image.

For making single dish and holography images, the data are convolved onto the grid using a one of a number of options:

gridfunction=’SF’
Circularly symmetric prolate spheroidal wavefunction. This is always the same function in pixels. To get this to match to the antenna primary beam, the optimum cellsize to use in constructing the image is the antenna primary beam half-width-half-maximum times 1.20192.
gridfunction=’BOX’
Nearest neighbor gridding.
gridfunction=’PB’
The telescope primary beam is used as the convolution function. This function is the same in arcseconds, independent of the cellsize. This choice is optimum in the least squares sense. To override the default choice of telescope primary beam for a given telescope, use the function setvp. Usually the default will be acceptable.

To make a reasonable approximation to the sky, one should divide the type=’singledish’ image by the type=’coverage’ image, thresholding at some level. For example:

 
ia.open(’scanweight’);  
 ia.statistics(s);  
threshold = s.max / 10.0;  
#  
ia.imagecalc(’sdimage’,  
      pixels=spaste(’scanimage[scanweight>’, threshold,  
    ’]/scanweight[scanweight>’, threshold, ’]’))  
###ia.view(raster=True, axislabels=True);

Arguments





Inputs

type

Type of output image

allowed:

string

Default:

observed

image

Name of output image

allowed:

string

Default:

compleximage

Name of output complex image

allowed:

string

Default:

verbose

Report things like the center frequency to the logger

allowed:

bool

Default:

true

async

Run asynchronously in the background

allowed:

bool

Default:

false

Returns
bool

Example

 
 
im.ft(model=’3C273XC1.model’, complist=’3C273XC1.complist’);  
im.makeimage(type=’residual’, image=’3C273XC1.residual’)  
im.makeimage(type=’psf’, image=’3C273XC1.psf’)  
 
 
Fill in the MODEL\_DATA column from Fourier transforming the model and  
the componentlist.  Make the residual image and write it to  
3C273XC1.residual.  

Example

 
 
im.setvp(dovp=T, usedefaultvp=T, telescope=’GBT’);  
im.makeimage(type=’pb’, image=’gbt.pb’)  
 
 
 
In the above we may want to see what the primary beam we are using  
look like. May also be useful to deconvolve single dish images in the  
deconvolver tool.  

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