hif_makeimlist

hif_makeimlist(vis=None, imagename=None, intent=None, field=None, spw=None, stokes=None, contfile=None, linesfile=None, uvrange=None, specmode=None, outframe=None, hm_imsize=None, hm_cell=None, calmaxpix=None, phasecenter=None, nchan=None, start=None, width=None, nbins=None, robust=None, uvtaper=None, clearlist=None, per_eb=None, per_session=None, calcsb=None, datatype=None, datacolumn=None, allow_wproject=None, parallel=None) → Results[source]

Compute the list of images to be produced in the next hif_makeimages call.

Determines image parameters (cell size, image size, spectral mode, etc.) for each target/spw and populates the pipeline context imaging list. The WebLog reports the chosen parameters.

In standard ALMA interferometric recipes the task is invoked multiple times for different imaging purposes by setting the intent and specmode parameters accordingly:

  • Calibrators (intent='PHASE,BANDPASS,AMPLITUDE,POLARIZATION,DIFFGAINREF,DIFFGAINSRC'): per-spw MFS continuum images, with image dimensions limited to calmaxpix pixels.

  • Polarization calibrator (polcal recipes): per-spw MFS images of the polarization calibrator.

  • Check source: per-spw MFS image of the check source.

  • Per-spw continuum (specmode='cont'): aggregate MFS continuum images combining multiple spws.

  • Aggregate continuum (specmode='cont'): using continuum channel selections from cont.dat.

  • Spectral cube (specmode='cube'): per-spw cubes for science targets.

  • Representative bandwidth cube: cube over the representative bandwidth.

The cell size is set to the minimum consistent with the UV coverage. The image size is set from the cell size and primary beam size. If clearlist=True (default) any existing imaging list entries for the same intent are replaced.

Parameters:

  • vis --

    The list of input MeasurementSets. Defaults to the list of MeasurementSets specified in the <hifa,hifv>_importdata task. "": use all MeasurementSets in the context

    Examples: 'ngc5921.ms', ['ngc5921a.ms', ngc5921b.ms', 'ngc5921c.ms']

  • imagename -- Prefix for output image names, "" for automatic.

  • intent --

    Select intents for which associated fields will be imaged. Possible choices are PHASE, BANDPASS, AMPLITUDE, CHECK and TARGET or combinations thereof.

    Examples: 'PHASE,BANDPASS', 'TARGET'

  • field -- Select fields to image. Use field name(s) NOT id(s). Mosaics are assumed to have common source / field names. If intent is specified only fields with data matching the intent will be selected. The fields will be selected from MeasurementSets in "vis". "" Fields matching intent, one image per target source.

  • spw -- Select spectral windows to image. "": Images will be computed for all science spectral windows.

  • stokes -- Select the Stokes parameters to image. "": Stokes I will be computed except for polarization calibrators, where the automatic heuristics selects IQUV. Setting a value here will override the heuristics. Allowed values are 'I' and 'IQUV'.

  • contfile -- Name of file with frequency ranges to use for continuum images.

  • linesfile -- Name of file with line frequency ranges to exclude for continuum images.

  • uvrange --

    Select a set of uv ranges to image. "": All uv data is included

    Examples: '0~1000klambda', ['0~100klambda', 100~1000klambda]

  • specmode -- Frequency imaging mode, 'mfs', 'cont', 'cube', 'repBW'. '' defaults to 'cube' if intent parameter includes 'TARGET' otherwise 'mfs'. specmode='mfs' produce one image per source and spw specmode='cont' produce one image per source and aggregate over all specified spws specmode='cube' produce an LSRK frequency cube, channels are specified in frequency specmode='repBW' produce an LSRK frequency cube at representative channel width

  • outframe -- velocity frame of output image (LSRK, '' for automatic) (not implemented)

  • hm_imsize --

    Image X and Y size in pixels or PB level for single fields. The explicit sizes must be even and divisible by 2,3,5,7 only. The default values are derived as follows: 1. Determine phase center and spread of field centers around it. 2. Set the size of the image to cover the spread of field centers plus a border of width 0.75 * beam radius, to first null. 3. Divide X and Y extents by cell size to arrive at the number of pixels required. The PB level setting for single fields leads to an imsize extending to the specified level plus 5% padding in all directions.

    Examples: '0.3pb', [120, 120]

  • hm_cell --

    Image X and Y cell sizes. "" computes the cell size based on the UV coverage of all the fields to be imaged and uses a 5 pix per beam sampling. The pix per beam specification ('<number>ppb') uses the above default cell size ('5ppb') and scales it accordingly. The cells can also be specified as explicit measures.

    Examples: '3ppb', ['0.5arcsec', '0.5arcsec']

  • calmaxpix -- Maximum image X or Y size in pixels if a calibrator is being imaged ('PHASE', 'BANDPASS', 'AMPLITUDE' or 'FLUX' intent).

  • phasecenter --

    Direction measure or field id of the image center. The default phase center is set to the mean of the field directions of all fields that are to be image together.

    Examples: 'J2000 19h30m00 -40d00m00', 0

  • nchan -- Total number of channels in the output image(s) -1 selects enough channels to cover the data selected by spw consistent with start and width.

  • start -- Start of image frequency axis as frequency or velocity. "" selects start frequency automatically.

  • width -- Output channel width. Difference in frequency between 2 selected channels for frequency mode images. 'pilotimage' for 15 MHz / 8 channel heuristic

  • nbins --

    Channel binning factors for each spw. Format: 'spw1:nb1,spw2:nb2,...' with optional wildcards: '*:nb'

    Examples: '9:2,11:4,13:2,15:8', '*:2'

  • robust -- Briggs robustness parameter Values range from -2.0 (uniform) to 2.0 (natural)

  • uvtaper -- uv-taper on outer baselines

  • clearlist -- Clear any existing target list

  • per_eb -- Make an image target per EB

  • per_session -- Make an image target per session

  • calcsb -- Force (re-)calculation of sensitivities and beams

  • datatype --

    Data type(s) to image. The default '' selects the best available data type (e.g. selfcal over regcal) with an automatic fallback to the next available data type. With the datatype parameter one can force the use of only given data type(s) without a fallback. The data type(s) are specified as comma separated string of keywords. Accepted values are the standard data types such as 'REGCAL_CONTLINE_ALL', 'REGCAL_CONTLINE_SCIENCE', 'SELFCAL_CONTLINE_SCIENCE', 'REGCAL_LINE_SCIENCE', 'SELFCAL_LINE_SCIENCE'. The shortcuts 'regcal' and 'selfcal' are also accepted. They are expanded into the full data types using the specmode parameter and the available data types for the given MSes. In addition the strings 'best' and 'all' are accepted, where 'best' means the above mentioned automatic mode and 'all' means all available data types for a given specmode. The data type strings are case insensitive.

    Examples: 'selfcal', 'regcal, 'selfcal,regcal', 'REGCAL_LINE_SCIENCE,selfcal_line_science'

  • datacolumn -- Data column to image. Only to be used for manual overriding when the automatic choice by data type is not appropriate.

  • allow_wproject -- Allow the wproject heuristics for imaging

  • parallel --

    Use the CASA imager parallel processing when possible.

    Options: 'automatic', 'true', 'false', True, False

    Default: 'automatic'

Notes

QA = fraction of images successfully added to the list compared to the total expected.

Returns:

The results object for the pipeline task is returned.

Examples

  1. Make a list of science target images to be cleaned, one image per science spw:

>>> hif_makeimlist()

  1. Make a list of PHASE and BANDPASS calibrator targets to be imaged, one image per science spw:

>>> hif_makeimlist(intent='PHASE,BANDPASS')

  1. Make a list of PHASE calibrator images observed in spw 1, images limited to 50 pixels on a side:

>>> hif_makeimlist(intent='PHASE', spw='1', calmaxpix=50)