Public Member Functions
def	__init__
def	result
def	__call__
def	paramgui
def	defaults
def	check_params
def	description
def	itsdefault
Public Attributes
	parameters
Static Public Attributes
	rkey
	Handle globals or user over-ride of arguments.
	i_am_a_casapy_task
list	retval
	This function sets the default values but also will return the list of parameters or the default value of a given parameter.
string	valornotval
tuple	retval
Private Attributes
	__bases__
	__doc__
	__globals__
Static Private Attributes
string	__name__
dictionary	__async__

Detailed Description

Definition at line 18 of file immath_cli.py.

Constructor & Destructor Documentation

def immath_cli.immath_cli_.__init__ ( self )

Definition at line 26 of file immath_cli.py.

Member Function Documentation

def immath_cli.immath_cli_.__call__	(	self,
		imagename = `None`,
		mode = `None`,
		outfile = `None`,
		expr = `None`,
		varnames = `None`,
		sigma = `None`,
		polithresh = `None`,
		mask = `None`,
		region = `None`,
		box = `None`,
		chans = `None`,
		stokes = `None`,
		stretch = `None`,
		async = `None`
	)

Perform math operations on images

    This task evaluates mathematical expressions involving existing
    image files. The results of the calculations are stored in the 
    designated output file.  Options are available to specify mathematical 
    expression directly or pre-defined expression for calculation of 
    spectral index image, and polarization intensity and position angle 
    images are available. The image file names imbedded in the expression or
    specified in the imagename parameter for the pre-defined calculations may
    be CASA images or FITS images.


    NOTE: Index values start at 0 Use the imhead task to see the range of
  index values for each axes.
    

    Keyword arguments:
    imagename  input image name(s)
       Default: none;
       Examples: mode='evalexpr'; imagename=['image1.im', 'image2.im' ]
       The text 'IM0' is replaced by 'image1.im' in the
       expression and 'IM1' is repalced with 'image2.im'
       mode='spix'; imagename=['image1.im','image2.im'] will calculate 
       an image of log(S1/S2)/log(f1/f2), where S1 and S2 are fluxes and 
       f1 and f2 are frequencies
       mode='pola'; imagename='multistokes.im' (where that image contains both Q and U
       stokes planes) or imagename=['imageQ.im','imageU.im'] will calculate 
       an image of polarization angle distribution, where imageQ.im and 
       imageU.im are Stokes Q and U images, respectively. Calculate 0.5*arctan(U/Q).
       mode='poli'; imagename=['imageQ.im','imageU.im','imageV.im'] will calculate
       total polarization intensity image, where imageQ.im, imageU.im, imageV.im
       are Stokes Q, U, and V images, respectively. Alternatively, with
       imagename = ['imageQ.im','imageU.im'] the linear polarization intensity
       image will be calculated. In the case where imagename is a single multi-stokes
       image, the total polarization image will be calculated if all of the Q, U, and
       V stokes planes are present, and the linear polarization intensity image will
       be calculated if the Q and U (but not V) planes are present. 

    mode       mode for mathematical operation
       Default: evalexpr
       Options: 'evalexpr' : evalulate a mathematical expression defined in 'expr' 
        'spix' : spectalindex image 
        'pola' : polarization position angle image 
        'poli' : polarization intesity image 
      >>> mode expandable parameters
      sigma       (for mode='poli') standard deviation of noise of Stokes images with unit such as
          Jy/beam to correct for bias 
          Default: '0.0Jy/beam' (= no debiasing)
      polithresh  (for mode='pola') Quantity (eg '30uJy/beam') describing the linear (not total;
          the stokes V contribution is not included) polarization threshold. A mask ('mask0')
          is written to the output image and is False for all corresponding linear polarization
          values below this threshold. This parameter overrides the mask input parameter
          (below). Default ('') means use the value given in mask, or no masking if that
          value is empty as well.
      expr        (for mode='evalexpr') A LEL expression with images.
              Image file names are specified in the imagenames paramter, and
          the variables IM0, IM1, ... (or optionally via the varnames parameter, see below)
          are used to represent these files
          in the expression. Explicit notations of file names in the 
          expression are also supported, in which cases the file names must
          be enclosed in double quotes (") and imagename is ignored.
              Examples:
          Make an image that is image1.im - image2.im
          expr=' (IM0 - IM1 )'
          or with an explicit notation, 
          expr='("image1.im" - "image2.im")'
          Clip an image below a value (0.5 in this case)
          expr = ' iif( IM0 >=0.5, IM0, 0.0) '
          Note: iif (a, b, c)   a is the boolean expression
                                b is the value if true
                                c is the value if false
          Take the rms value of two images
          expr = ' sqrt(IM0 * IM0 + IM1 * IM1) '
          Note: No exponentiaion available?
          Build an image pixel by pixel from the minimum of (image2.im, 2*image1.im)
          expr='min(IM1,2*max(IM0))'
       varnames   For mode="evalexpr". Instead of the default variable names IM0, IM1, ..., use
          the names in this array to represent the input images.
    outfile    The output image. Overwriting an existing outfile is not permitted.
   Default: immath_results.im;  Example: outfile='results.im'
    mask       Mask to use. See help par.mask. Default is none. Also see polithresh.
    stretch    Stretch the input mask if necessary and possible. See below.
    region     Name of region file, region text description, or region dictionary.
    box        A rectangular region on the directional plane expressed in pixels.
       Example: box='10,10,50,50'
    chans      Channel ranges to use, expressed in pixels. Example: chans='3~20'   
    stokes     Stokes parameters. Example: stokes='IQUV';
       Options: 'I','Q','U','V','RR','RL','LR','LL','XX','YX','XY','YY', ... 
       Not used in for cases of mode='poli' or mode='pola'

    Available functions in the expr and mask paramters:
    pi(), e(), sin(), sinh(), asinh(), cos(), cosh(), tan(), tanh(),
    atan(), exp(), log(), log10(), pow(), sqrt(), complex(), conj()
    real(), imag(), abs(), arg(), phase(), aplitude(), min(), max()
    round(), isgn(), floor(), ceil(), rebin(), spectralindex(), pa(), 
    iif(), indexin(), replace(), ...

    If the mask has fewer dimensions than the image and if the shape
    of the dimensions the mask and image have in common are the same,
    the mask will automatically have the missing dimensions added so
    it conforms to the image.

    For a full description of the allowed syntax see the 
    Lattice Expression Language (LEL) documentation on the at:
    http://aips2.nrao.edu/docs/notes/223/223.html

    NOTE: where indexing and axis numbering are used in the above
    functions they are 1-based, ie. numbering starts at 1.

    If stretch is true and if the number of mask dimensions is less than
    or equal to the number of image dimensions and some axes in the
    mask are degenerate while the corresponding axes in the image are not,
    the mask will be stetched in the degenerate axis dimensions. For example,
    if the input image has shape [100, 200, 10] and the input
    mask has shape [100, 200, 1] and stretch is true, the mask will be
    stretched along the third dimension to shape [100, 200, 10]. However if
    the mask is shape [100, 200, 2], stretching is not possible and an
    error will result.

    CAUTION: Note that when multiple image are used in the expression, there is
    no garauntee about which of those images will be used to create the header
    of the output image. Therefore, one may have to modify the output header as
    needed if the input headers differ.

    Examples:
    # Double all values in an image.
    immath( imagesname='myimage.im', expr='IM0*2', outfile='double.im' )
    # or with an explicit notation, 
    immath( expr='"myimage.im"*2', outfile='double.im' )

    # Taking the sin of an image and adding it to another
    # Note that the images need to be the same size
    immath(images=['image1.im', 'image2.im'], expr='sin(IM1)+IM0;',outfile='newImage.im')

    # Adding only the plane associated with the 'V' stokes value and
    # the 1st channel together in two images
    immath(imagename=[image1', 'image2'], expr='IM0+IM1',chans='1',stokes='V')


    # Selecting a single plane (5th channel), of the 3-D cube and  
    # adding it to the original image.  In this example the 2-D plane
    # gets expanded out and the values are applied to each plane in the 
    # 3-D cube. 
    default('immath')
    imagename='ngc7538.image'
    outfile='chanFive.im'
    expr='IM0'
    chans='5'
    go
    default('immath')
    imagename=['ngc7538.image', chanFive.im']
    outfile='ngc7538_chanFive.im'
    expr='IM0+IM1'
    go

    # Selecting and saving the inner 3/4 of an image for channels 40,42,44
    # as well as channels less than 10
    default('immath')
    imagename='my_image.im'
    expr='IM0'
    box='25,25,123,123'
    chans='<10;40,42,44'
    outfile='my_image_inner.im' )
    go

    # Dividing an image by another, making sure we aren't dividing by zero
    default('immath')
    imagename=['orion.image', 'my.image']
    expr='IM0/iif(IM1==0,1.0,IM1)'
    outfile='my_orion.image'
    go

    # Applying a mask to all of the images in the expression
    default('immath')
    imagename=['ngc7538.image','ngc7538_clean.image']
    expr='(IM0*10)+IM1'
    mask='"ngc7538.mask"'
    outfile='really_noisy_ngc7538.image'
    go


    # Applying a pixel mask contained in the image information
    default('immath')
    imagename='ngc5921.image'
    expr='IM0*10'
    mask='mask("ngc5921.mask")'
    outfile='ngc5921.masked.image'
    go

    # Creating a total polarization intensity image from an multi-stokes image
    # containing IQUV.
    default('immath')
    outfile='pol_intensity'
    stokes=''
    # in imagename, you can also specify a list containing single stokes images
    # of Q and U (for linear polarization intensity) and V (for total
    # polarization intensity)
    imagename='3C138_pcal'
    mode='poli'
    go

    # Creating a polarization position angle image 
    default('immath')
    outfile='pol_angle.im'
    mode='pola'
    # you can also do imagename=['Q.im','U.im'] for single stokes images, order of
    # the two Stokes images does not matter
    imagename='3C138_pcal' # multi-stokes image containing at least Q and U stokes 
    go 

    # same as before but write a mask with values of False for pixels for which the
    # corresponding linear polarization ( sqrt(Q*Q+U*U)) is less than 30 microJy/beam
    polithresh='30uJy/beam'
    go

    # Creating a spectral index image from the images at two different observing frequencies
    default('immath')
    outfile='mySource_sp.im'
    mode='spix'
    imagename=['mySource_5GHz.im','mySource_8GHz.im']
    go
    
    TEMPORARY IMAGES

    At this time, it is usually necessary for this task to create intermediate, temporary disk images.
    The names of these images start with '_immath' and are created in the directory in which the task
    is run. The task makes reasonable attempts to remove these images before it exits, but there are
    conceivably instances where the temporary images may not be automatically deleted. It is generally
    safe to delete them by hand, assuming no immath instance is currently in progress.

    The hope and plan is that the necessity of these images will decrease in the future (ie the computations
    will require only RAM and not temporary persistent storage of intermediate results).

Definition at line 46 of file immath_cli.py.

def immath_cli.immath_cli_.check_params	(	self,
		param = `None`,
		value = `None`,
		ipython_globals = `None`
	)

Definition at line 498 of file immath_cli.py.

def immath_cli.immath_cli_.defaults	(	self,
		param = `None`,
		ipython_globals = `None`,
		paramvalue = `None`,
		subparam = `None`
	)

Definition at line 437 of file immath_cli.py.

def immath_cli.immath_cli_.description	(	self,
		key = `'immath'`,
		subkey = `None`
	)

Definition at line 529 of file immath_cli.py.

def immath_cli.immath_cli_.itsdefault	(	self,
		paramname
	)

Definition at line 555 of file immath_cli.py.

Referenced by rmtables_cli.rmtables_cli_.defaults(), listfits_cli.listfits_cli_.defaults(), listhistory_cli.listhistory_cli_.defaults(), importfitsidi_cli.importfitsidi_cli_.defaults(), uvsub_cli.uvsub_cli_.defaults(), importgmrt_cli.importgmrt_cli_.defaults(), uvcontsub2_cli.uvcontsub2_cli_.defaults(), plotweather_cli.plotweather_cli_.defaults(), importuvfits_cli.importuvfits_cli_.defaults(), imreframe_cli.imreframe_cli_.defaults(), plotants_cli.plotants_cli_.defaults(), importfits_cli.importfits_cli_.defaults(), smoothcal_cli.smoothcal_cli_.defaults(), listsdm_cli.listsdm_cli_.defaults(), tclean_cli.tclean_cli_.defaults(), splattotable_cli.splattotable_cli_.defaults(), sdflagmanager_cli.sdflagmanager_cli_.defaults(), testconcat_cli.testconcat_cli_.defaults(), sdlist_cli.sdlist_cli_.defaults(), msview_cli.msview_cli_.defaults(), viewer_cli.viewer_cli_.defaults(), imregrid_cli.imregrid_cli_.defaults(), listpartition_cli.listpartition_cli_.defaults(), sdscale_cli.sdscale_cli_.defaults(), imsubimage_cli.imsubimage_cli_.defaults(), impbcor_cli.impbcor_cli_.defaults(), msmoments_cli.msmoments_cli_.defaults(), slsearch_cli.slsearch_cli_.defaults(), peel_cli.peel_cli_.defaults(), predictcomp_cli.predictcomp_cli_.defaults(), uvcontsub_cli.uvcontsub_cli_.defaults(), wvrgcal_cli.wvrgcal_cli_.defaults(), ssoflux_cli.ssoflux_cli_.defaults(), vishead_cli.vishead_cli_.defaults(), uvcontsub3_cli.uvcontsub3_cli_.defaults(), sdimprocess_cli.sdimprocess_cli_.defaults(), virtualconcat_cli.virtualconcat_cli_.defaults(), listobs_cli.listobs_cli_.defaults(), sdsmooth_cli.sdsmooth_cli_.defaults(), visstat_cli.visstat_cli_.defaults(), imview_cli.imview_cli_.defaults(), widebandpbcor_cli.widebandpbcor_cli_.defaults(), sdcoadd_cli.sdcoadd_cli_.defaults(), uvmodelfit_cli.uvmodelfit_cli_.defaults(), listvis_cli.listvis_cli_.defaults(), sdsave_cli.sdsave_cli_.defaults(), simanalyze_cli.simanalyze_cli_.defaults(), sdmath_cli.sdmath_cli_.defaults(), listcal_cli.listcal_cli_.defaults(), sdgrid_cli.sdgrid_cli_.defaults(), importasdm_cli.importasdm_cli_.defaults(), sdtpimaging_cli.sdtpimaging_cli_.defaults(), sdstat_cli.sdstat_cli_.defaults(), makemask_cli.makemask_cli_.defaults(), split_cli.split_cli_.defaults(), sdimaging_cli.sdimaging_cli_.defaults(), statwt_cli.statwt_cli_.defaults(), sdflag_cli.sdflag_cli_.defaults(), importevla_cli.importevla_cli_.defaults(), partition_cli.partition_cli_.defaults(), simalma_cli.simalma_cli_.defaults(), sdfit_cli.sdfit_cli_.defaults(), sdcal_cli.sdcal_cli_.defaults(), simobserve_cli.simobserve_cli_.defaults(), polcal_cli.polcal_cli_.defaults(), sdbaseline_cli.sdbaseline_cli_.defaults(), setjy_cli.setjy_cli_.defaults(), mosaic_cli.mosaic_cli_.defaults(), widefield_cli.widefield_cli_.defaults(), pclean_cli.pclean_cli_.defaults(), plotxy_cli.plotxy_cli_.defaults(), specfit_cli.specfit_cli_.defaults(), plotms_cli.plotms_cli_.defaults(), and sdreduce_cli.sdreduce_cli_.defaults().

def immath_cli.immath_cli_.paramgui	(	self,
		useGlobals = `True`,
		ipython_globals = `None`
	)

Opens a parameter GUI for this task.  If useGlobals is true, then any relevant global parameter settings are used.

Definition at line 413 of file immath_cli.py.

def immath_cli.immath_cli_.result	(	self,
		key = `None`
	)

Definition at line 33 of file immath_cli.py.

References accum_cli.accum_cli_.__async__, immath_cli.immath_cli_.__async__, imhead_cli.imhead_cli_.__async__, imfit_cli.imfit_cli_.__async__, imcontsub_cli.imcontsub_cli_.__async__, imcollapse_cli.imcollapse_cli_.__async__, hanningsmooth_cli.hanningsmooth_cli_.__async__, gencal_cli.gencal_cli_.__async__, gaincal_cli.gaincal_cli_.__async__, ft_cli.ft_cli_.__async__, fluxscale_cli.fluxscale_cli_.__async__, flagmanager_cli.flagmanager_cli_.__async__, flagdata_cli.flagdata_cli_.__async__, flagcmd_cli.flagcmd_cli_.__async__, fixvis_cli.fixvis_cli_.__async__, fixplanets_cli.fixplanets_cli_.__async__, find_cli.find_cli_.__async__, feather_cli.feather_cli_.__async__, exportuvfits_cli.exportuvfits_cli_.__async__, exportfits_cli.exportfits_cli_.__async__, exportasdm_cli.exportasdm_cli_.__async__, delmod_cli.delmod_cli_.__async__, deconvolve_cli.deconvolve_cli_.__async__, cvel_cli.cvel_cli_.__async__, csvclean_cli.csvclean_cli_.__async__, conjugatevis_cli.conjugatevis_cli_.__async__, concat_cli.concat_cli_.__async__, clearstat_cli.clearstat_cli_.__async__, clearplot_cli.clearplot_cli_.__async__, clearcal_cli.clearcal_cli_.__async__, clean_cli.clean_cli_.__async__, caltabconvert_cli.caltabconvert_cli_.__async__, calstat_cli.calstat_cli_.__async__, browsetable_cli.browsetable_cli_.__async__, boxit_cli.boxit_cli_.__async__, blcal_cli.blcal_cli_.__async__, bandpass_cli.bandpass_cli_.__async__, autoclean_cli.autoclean_cli_.__async__, asdmsummary_cli.asdmsummary_cli_.__async__, and applycal_cli.applycal_cli_.__async__.

Member Data Documentation

dictionary immath_cli.immath_cli_.__async__ [static, private]

Definition at line 20 of file immath_cli.py.

Referenced by immath_cli.immath_cli_.result(), wvrgcal_cli.wvrgcal_cli_.result(), widefield_cli.widefield_cli_.result(), widebandpbcor_cli.widebandpbcor_cli_.result(), visstat_cli.visstat_cli_.result(), vishead_cli.vishead_cli_.result(), virtualconcat_cli.virtualconcat_cli_.result(), viewer_cli.viewer_cli_.result(), uvsub_cli.uvsub_cli_.result(), uvmodelfit_cli.uvmodelfit_cli_.result(), uvcontsub_cli.uvcontsub_cli_.result(), uvcontsub3_cli.uvcontsub3_cli_.result(), uvcontsub2_cli.uvcontsub2_cli_.result(), testconcat_cli.testconcat_cli_.result(), tclean_cli.tclean_cli_.result(), statwt_cli.statwt_cli_.result(), ssoflux_cli.ssoflux_cli_.result(), split_cli.split_cli_.result(), splattotable_cli.splattotable_cli_.result(), specfit_cli.specfit_cli_.result(), smoothcal_cli.smoothcal_cli_.result(), slsearch_cli.slsearch_cli_.result(), simobserve_cli.simobserve_cli_.result(), simanalyze_cli.simanalyze_cli_.result(), simalma_cli.simalma_cli_.result(), setjy_cli.setjy_cli_.result(), sdtpimaging_cli.sdtpimaging_cli_.result(), sdstat_cli.sdstat_cli_.result(), sdsmooth_cli.sdsmooth_cli_.result(), sdscale_cli.sdscale_cli_.result(), sdsave_cli.sdsave_cli_.result(), sdreduce_cli.sdreduce_cli_.result(), sdplot_cli.sdplot_cli_.result(), sdmath_cli.sdmath_cli_.result(), sdlist_cli.sdlist_cli_.result(), sdimprocess_cli.sdimprocess_cli_.result(), sdimaging_cli.sdimaging_cli_.result(), sdgrid_cli.sdgrid_cli_.result(), sdflagmanager_cli.sdflagmanager_cli_.result(), sdflag_cli.sdflag_cli_.result(), sdfit_cli.sdfit_cli_.result(), sdcoadd_cli.sdcoadd_cli_.result(), sdcal_cli.sdcal_cli_.result(), sdbaseline_cli.sdbaseline_cli_.result(), rmtables_cli.rmtables_cli_.result(), predictcomp_cli.predictcomp_cli_.result(), polcal_cli.polcal_cli_.result(), plotxy_cli.plotxy_cli_.result(), plotweather_cli.plotweather_cli_.result(), plotuv_cli.plotuv_cli_.result(), plotms_cli.plotms_cli_.result(), plotcal_cli.plotcal_cli_.result(), plotants_cli.plotants_cli_.result(), peel_cli.peel_cli_.result(), pclean_cli.pclean_cli_.result(), partition_cli.partition_cli_.result(), msview_cli.msview_cli_.result(), msmoments_cli.msmoments_cli_.result(), mosaic_cli.mosaic_cli_.result(), makemask_cli.makemask_cli_.result(), listvis_cli.listvis_cli_.result(), listsdm_cli.listsdm_cli_.result(), listpartition_cli.listpartition_cli_.result(), listobs_cli.listobs_cli_.result(), listhistory_cli.listhistory_cli_.result(), listfits_cli.listfits_cli_.result(), listcal_cli.listcal_cli_.result(), imview_cli.imview_cli_.result(), imval_cli.imval_cli_.result(), imtrans_cli.imtrans_cli_.result(), imsubimage_cli.imsubimage_cli_.result(), imstat_cli.imstat_cli_.result(), imsmooth_cli.imsmooth_cli_.result(), imregrid_cli.imregrid_cli_.result(), imreframe_cli.imreframe_cli_.result(), importvla_cli.importvla_cli_.result(), importuvfits_cli.importuvfits_cli_.result(), importgmrt_cli.importgmrt_cli_.result(), importfitsidi_cli.importfitsidi_cli_.result(), importfits_cli.importfits_cli_.result(), importevla_cli.importevla_cli_.result(), importasdm_cli.importasdm_cli_.result(), impbcor_cli.impbcor_cli_.result(), and immoments_cli.immoments_cli_.result().

immath_cli.immath_cli_.__bases__ [private]

Definition at line 27 of file immath_cli.py.

immath_cli.immath_cli_.__doc__ [private]

Definition at line 28 of file immath_cli.py.

immath_cli.immath_cli_.__globals__ [private]

Definition at line 284 of file immath_cli.py.

string immath_cli.immath_cli_.__name__ [static, private]

Definition at line 19 of file immath_cli.py.

immath_cli.immath_cli_.i_am_a_casapy_task [static]

Definition at line 22 of file immath_cli.py.

immath_cli.immath_cli_.parameters

Definition at line 30 of file immath_cli.py.

tuple immath_cli.immath_cli_.retval [static]

This function sets the default values but also will return the list of parameters or the default value of a given parameter.

Definition at line 477 of file immath_cli.py.

tuple immath_cli.immath_cli_.retval [static]

Definition at line 490 of file immath_cli.py.

immath_cli.immath_cli_.rkey [static]

Handle globals or user over-ride of arguments.

Definition at line 21 of file immath_cli.py.

string immath_cli.immath_cli_.valornotval [static]

Definition at line 480 of file immath_cli.py.

The documentation for this class was generated from the following file:

immath_cli.py

Public Member Functions

Public Attributes

Static Public Attributes

Private Attributes

Static Private Attributes

Detailed Description

Constructor & Destructor Documentation

Member Function Documentation

Member Data Documentation