.ec _
.ll 80
.ad b
.in 4
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1 Language
.nf
  PIPELINE    Pipeline processing of all UV tables
  REPORT      Report data properties & Pipeline results
  SIMULATE    Simulation pipeline from model data
  TIPS        Give Random tip about IMAGER

  CLARK       Shortcut to CLEAN with CLARK Method
  HOGBOM      Shortcut to CLEAN with HOGBOM Method
  GCLEAN      Shortcut to CLEAN with GAUSS method
  MRC         Shortcut to CLEAN with MRC Method
  MULTISCALE  Shortcut to CLEAN with MULTISCALE Method
  SDI         Shortcut to CLEAN with SDI Method
.fi

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1 TIPS
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    [IMAGER_\]TIPS [Number]

    Without argument, print out a random tip about IMAGER.
  With an argument, give the corresponding tip number.

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1 REPORT
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  [IMAGER_\]REPORT ?|COVERAGE|SUMMARY|RESULTS
  
  REPORT is associated to the PIPELINE command. It will create
PDF reports of the properties of data prepared by the PIPELINE ORGANIZE
command.  The resulting PDF files are located in a sub-directory
named REPORT.

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2 COVERAGE
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  [IMAGER_\]REPORT COVERAGE
  
  Create a PDF summary of the data, that contains a preview of all
  spectral windows, with spectral lines from the catalog overplotted.
  
  Wide band spectral windows include the continuum, while Narrow band
  windows have been baseline subtracted to better illustrate spectral
  line detections.

  The report is available under REPORT/coverage.pdf
    
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2 RESULTS
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  [IMAGER_\]REPORT RESULTS
  
  Create a PDF summary of the data, that contains a preview of 
  tentatively detected spectral lines from the catalog overplotted,
  and a VIEW of the corresponding data cubes.
  
  The VIEW uses the last VIEW parameters defined by the user (size,
  spectral range, support, ...)
  
  The report is available under REPORT/views.pdf
      
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2 SUMMARY
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  [IMAGER_\]REPORT SUMMARY
  
  Create a PDF summary of the data, that contains Spectral configuration
  information and Imaging suggestions.
  
  Spectral configuration:
.nf
  - A list of Wide band tables suitable (or not...) for self-calibration
  - A list of higheresolution band tables suitable for spectral line imaging.
  - A list of spectral lines covered by the data (among those in the CATALOG)
.fi  
  Imaging suggestions:
.nf
  - An estimate of a Robust parameter when this makes sense
  - A feasibility estimate about self-calibration based on the widest band.
    This includes a plot of the resulting self-calibrated continuum image.
.fi
  The report is available under REPORT/summary.pdf
 
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1 PIPELINE 
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    [IMAGER_\]PIPELINE [Arg1 [Arg2]] [/MODE Type] [/WIDGET]
    
    PIPELINE is a command activating the Imaging Pipeline. The pipeline contains 
all processing steps for high fidelity imaging (Self-calibration, continuum
extraction, line identification, etc...) 
  
    With no /WIDGET option, PIPELINE run in unattended mode (no SIC_\PAUSE statement), 
one step after the other. 
.nf
    PIPELINE ?      will display the Pipeline input parameters
    PIPELINE *      will run the whole Pipeline with the current input parameters    
    PIPELINE NEXT   runs the next following step
    PIPELINE LAST   will repeat the last step.  
.fi    
PIPELINE with no argument stands for PIPELINE LAST. The /MODE option controls
the operating mode (default: last selected mode).

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2 /MODE
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    [IMAGER_\]PIPELINE [Arg1 [Arg2]] /MODE All|Continuum|Split|Survey

Specifdy in which mode the Pipeline will run. 4 modes are possible

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  CONTINUUM
.br
  Only produce continuum images, no data cube. In this mode, the emission is assumed
to be purely continuum, with no significant line contamination.

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  SURVEY
.br 
  Only produce line+continuum data cubes. No attempt to separate line emission from
continuum emission is made. The complete spectral coverage is imaged, at the velocity
resolution specified by the user. This mode is especially adapted for extra-galactic
work, or sources with lines close to the spectral confusion limit.

  A "continuum" image is also produced, but a more elaborate evaluation using 
MAP__CONTINUUM on the full data cubes is recommended after imaging.

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  ALL
.br
  Produce data cubes that contains line and continuum emission together. Spectral line
identification will be performed if a Catalog is present, with the user-specified
velocity range and spectral resolution around each spectral line in the band.

If no Catalog is present, the complete spectral coverage is imaged, at the velocity
resolution specified by the user (this case is equivalent to the SURVEY mode). 
  
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  SPLIT
.br
  Similar to ALL, but produce data cubes that contains line and continuum emission 
separately. The separation is based on filtering performed by UV__PREVIEW. 
  
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2 /WIDGET
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  PIPELINE /WIDGET 
  
  Activates the widget that simplifies the interactive control of the Pipeline steps.
  
  Each step is controlled by a separate button. In this mode, the Self-Calibration
related button requires user interaction. Some buttons are duplicated on top of the widget,
which also contains a  SELF-CALIBRATION button that can execute all Self-Calibration related
steps in sequence.
  
    The PIPELINE button (as the GO button) will run the full Pipeline without
any further user interaction, like the PIPELINE * command.
  
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2 STOP
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  The symbol STOP is used to control whether the Pipeline actions run unattended, or
require a user input.  In Widget mode, symbol STOP is defined by default as being
command PAUSE, requiring user input to continue.  In pure pipeline mode 
(PIPELINE *  command), symbol STOP is defined as CONTINUE, so that action proceed
without any user intervention.

  The user may override these default behviours by defining STOP either as
.nf
  SYMBOL STOP CONTINUE
or
  SYMBOL STOP PAUSE
.fi
before pipeline actions.

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2 Arguments:
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    PIPELINE supports the following arguments when not used in Widget mode,
given here in sequential order of actions
.nf    
  ORGANIZE      Prepare the UV tables and directory layout
  SETUP         Basic setup, composed of the 4 following sub-steps:
    FIND          Locate the UV tables
    SELECT        Select the Wide bands vs Narrow bands
    EXPLORE       Explore imaging parameters
    SCAN          Explore covered spectral lines
  CHECK         Check if Self-Calibration is possible
  COMPUTE (or SELF)   Compute Self-calibration
  COLLECT       Collect all Self-calibration solutions
  APPLY         Apply Self-calibration
  TIME          Time average to gain space
  TABLES        Create per-line UV tables
  IMAGE         Image all data
  SHOW          Show self-calibration results
  SAVE          Save parameters
.fi
Argument SCAN is a special case to built a sub-catalog of spectral
lines adapted to the current selection.

As post-processing (after IMAGING and TABLES), additional actions
are possible
.nf 
  CONTINUUM     Collect all Continuum data in one Multi-frequency set.
  SED or INDEX  Compute Spectral Index and Flux from continuum tables.
  SKY           Apply primary  beam correction to existing images. 
.fi

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2 ORGANIZE
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  [IMAGER_\]PIPELINE ORGANIZE

    Automatically re-arrange the set of UV tables or UVFITS files in the current
directory to a directory tree that is suitable for the Pipeline / Widget use.

    This is Step 1, NEXT step is SETUP (or FIND)
    
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2 SETUP
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  [IMAGER_\]PIPELINE SETUP

  SETUP         Basic setup, composed of the 4 following sub-steps:
.nf
    FIND          Locate the UV tables
    SELECT        Select the Wide bands vs Narrow bands
    EXPLORE       Explore imaging parameters
    SCAN          Explore covered spectral lines
.fi
    This is Step 2, NEXT step is CHECK
    
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2 FIND
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  [IMAGER_\]PIPELINE FIND
    
    Finds the UV tables in the directory tree and scan their properties for further use

    This is Step 2.1, NEXT step is SELECT

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2 SELECT
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  [IMAGER_\]PIPELINE SELECT
    
    Select the UV tables to be processed according to the Filter (all%filter) and identify
the Wide bands and Narrow bands
  
    This is Step 2.2, NEXT step is EXPLORE 
    
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2 EXPLORE
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  [IMAGER_\]PIPELINE EXPLORE
    
    Explore data size and suggest to adjust some Imaging parameters to save space
or optimize imaging (in particular, set MAP__ROBUST when spatical dynamic range
is large).
  
    This is Step 2.3, NEXT step is SCAN.
    
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2 SCAN
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  [IMAGER_\]PIPELINE SCAN

    Scan the currently selected UV tables (from All%FIlter) to find 
out which spectral lines from the current catalog are covered by the 
available spectral setups. The identified lines are stored in a new
local catalog, named

  local-coverage.lin

Lines may appear several times in this catalog, as the UV tables
may have redundant spectral coverage.  A trimmed version, ordered
by increasing frequency, is also created in

  sorted-coverage.lin

It can be re-used after edition as a local catalog. Both catalogs are 
in an Astro CSV (Comma Separated Value) format and are easily editable
(e.g. to suppress spectral lines too close to each other, 
in particular for hyperfine component groups). 

    This is Step 2.4, NEXT step is ChECK.

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2 CHECK
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  [IMAGER_\]PIPELINE CHECK
    
    Check whether the continuum is strong enough to require and allow self-calibration.
  
    This is Step 3, NEXT step is COMPUTE (or its alias SELF)

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2 COMPUTE
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  [IMAGER_\]PIPELINE COMPUTE    or    [IMAGER_\]PIPELINE SELF
  
    Compute the Self-calibration solution from the Wide bands UV tables
    
    This is Step 4, NEXT step is COLLECT
    
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2 SELF
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  [IMAGER_\]PIPELINE COMPUTE    or    [IMAGER_\]PIPELINE SELF
  
    Compute the Self-calibration solution from the Wide bands UV tables
    
    This is Step 4, NEXT step is COLLECT
    
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2 COLLECT
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  [IMAGER_\]PIPELINE COLLECT
  
    Improve self-calibration solution by interpolating correction delays between different
wide bands.  This can increase S/N of self-calibration on weaker sources, but may degrade 
solutions with very high S/N per band on strong sources.

    This is Step 5, NEXT step is APPLY

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2 APPLY
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  [IMAGER_\]PIPELINE APPLY
  
    Apply self-calibration solution derived previously to all Wide and Narrow band UV tables.
The selected solution is from the Wide band that is closest in Frequency, using the DELAY
mode for the solution.
  
    This is Step 6, NEXT step is TIME
    
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2 TIME
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  [IMAGER_\]PIPELINE TIME
  
    Time average the self-calibrated UV tables to save space and further time processing
    
    This is Step 7, NEXT step is TABLES 
    
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2 TABLES
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  [IMAGER_\]PIPELINE TABLES
  
    Extract UV tables around each spectral line available in the CATALOG and covered by the
frequency setup. Continuum emission is (empirically) separated from Line emission using
the UV__PREVIEW, UV__BASELINE / UV__FILTER mechanism.

  This step is only needed when direct image analysis in the UV plane is required.
    
    This is Step 8, NEXT step is IMAGE

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2 IMAGE
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  [IMAGER_\]PIPELINE IMAGE
  
    Produce deconvolved images around each spectral line available in the CATALOG and covered by the
frequency setup. Continuum emission is (empirically) separated from Line emission using
the UV__PREVIEW, UV__BASELINE / UV__FILTER mechanism, and the continuum images are also produced.
  
    This step does not use the result of the PIPELINE TABLES step, but only the self-calibrated
UV tables produced by PIPELINE APPLY and PIPELINE TIME.

    This is Step 9, NEXT step is SHOW

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2 SHOW
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  [IMAGER_\]PIPELINE SHOW
  
    Show some plots about Self-calibration quality. More plots will be added
  later. The ultimate goal of PIPELINE SHOW is to produce a summary report.

    This is Step 10, NEXT step is SAVE

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2 SAVE
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  [IMAGER_\]PIPELINE SAVE
  
    Save PIPELINE input parameters into ./all-memory.ima, so that PIPELINE * will redo the whole 
processing with the these parameters. The script can be edited if any correction is required
(e.g. changing image size, robust parameter, etc...)

  An implicit SAVE is done after PIPELINE IMAGE
  
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2 SKY
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  [IMAGER_\]PIPELINE SKY

  Apply primary beam correction to the Clean images in the all%maps (default MAPS) directory
to produce the Sky brightness images (.lmv-sky).  This steps does nothing when processing
Mosaics, since Clean directly restores Sky brightness images for Mosaics.
		
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2 NEXT
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  [IMAGER_\]PIPELINE NEXT
  
    Run the next step of the Pipeline.
    
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2 LAST
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  [IMAGER_\]PIPELINE LAST
  
    Repeat the last executed step of the Pipeline (presumably after changing some control parameters)

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2 CONTINUUM
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  [IMAGER_\]PIPELINE CONTINUUM
  
  Merge all *+C.uvt tables from the TABLES directory into CONTINUUM/all+C.uvt in mode Continuum
  to produce an optimal sensitivity continuum data set. If PIPELINE SED has been used before,
  the fitted spectral index (sed%index) is used in the process.
  
  The resulting data set is imaged with current UV__MAP and CLEAN parameters, and saved
  as CONTINUUM/all+C.lmv-clean.
  
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2 SED
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  [IMAGER_\]PIPELINE SED  (or PIPELINE INDEX)
  
  Compute "Spectral Energy Distribution" from all continuum tables in TABLES, and fit flux and
  spectral index. Input parameters are stored in the sed% structure and can be found using PIPELINE SED ?
  
  
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2 Variables:
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  Apart from the usual imaging parameters, PIPELINE is controlled by a few variables.
.nf
  ALL%CATALOG   Spectral line catalog name (set by the CATALOG command)
  ALL%DROP[2]		Number of edge channels drop at each edge of windows
  ALL%FILTER    indicates the files to be processed
  ALL%MINFRES   (MHz) threshold in spectral resolution to separate continuum-only data from Lines
  ALL%RANGE[3]  gives the velocity range (Vmin and Vmax) and resolution (in km/s)
.fi
  
  In addition, the self-calibration step is controlled by ALL%PHASE__NITER, ALL%PHASE__TIMES,
ALL%AMPLI__NITER and ALL%AMPLI__TIMES that specify the number of Clean components and
integration times for Phase and Amplitude respectively
 
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2 ALL%CATALOG
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    Name of spectral line catalog. This is a Read-Only variable, defined using the CATALOG
command. See HELP CATALOG for details.
  
  If a line catalog is selected, the Pipeline scripts will produce one
image for each spectral line falling into the observed "high resolution"
spectral windows, over the specified velocity range ALL%RANGE.
  
  If no line catalog is selected, all channels of all "high resolution"
spectral windows will be imaged.  No velocity range is used in this case
but the spectral resolution can be modified by ALL%RANGE[3].
  
  "Low resolution" spectral windows will be used to produce continuum
only images. The distinction between "Low" and "High" resolution spectral
windows is made from variable ALL%MINFRES

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2 ALL%DROP
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	INTEGER ALL%DROP[2]

  This is an integer array giving the number of edge channels
ignored when reading a UV table. Edge channels may have different
weights than the other ones, especially for ALMA data because of the
off-line Doppler correction. 

Such low weights edge channels are automatically
dropped for Single fields, so you can use ALL%DROP = 0, 
but not yet for Mosaics, where ALL%DROP = 5 is more appropriate.

Larger values may be useful for SURVEY mode.

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2 ALL%FILTER
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    CHARACTER*256    ALL%FILTER
    
  File filter to be used to select the relevant UV tables.

  This filter MUST NOT contain the .uvt extension. The default filter
is *, but a specific file name can be given to process only one
UV table instead of all of them (or all tables for a given source for example).

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2 ALL%AMPLI__NITER
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    ALL%AMPLI__NITER is a size-variable integer array of rank 1. 
    
It indicates the number
of clean components for each iteration of Amplitude self-calibration.
The number of iterations is defined by its number of elements.
The size of this array can be changed using the LET /RESIZE option.
    
    0 means to select all Clean components.
    
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2 ALL%AMPLI__TIMES
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    ALL%AMPLI__TIMES is a size-variable real array of rank 1.
    
It indicates the 
integration time for each iteration of Phase self-calibration.
The number of iterations is defined by its number of elements.
The size of this array can be changed using the LET /RESIZE option.
    
    Typical values are 90 to 180 seconds for NOEMA, 60 seconds for ALMA.
Longer values can be used to adjust relative amplitude calibration for
observations made on different dates.

If Zero, no amplitude self-calibration is performed.
    
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2 ALL%COLLECT
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  Real ALL%COLLECT

Stability Threshold for flagging data after Self-Calibration. 

For Self-calibration solutions with more than
one iteration, the solution is flagged if the difference between the
last two iterations exceeds Threshold times the expected phase error
due to noise.

  The default is 0, a convention indicating to ignore this flagging step.

  When the noise level is appropriately estimated, a Threshold of 3
is a good value to suppress unstable solutions that reflect some
issues in the self-calibration model.


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2 ALL%COMBINE
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  Logical ALL%COMBINE
  
Indicates whether the COLLECT step (that derives an atmospheric delay
correction from the per-band phase correction) 
should be performed or not for the Self-Calibration in PIPELINE mode.

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2 ALL%ITIME

    Real ALL%ITIME
    
Integration time used for the TIME compression step. 0 means that 
IMAGER will derive the best time given the baseline lengths and 
field of view.

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2 ALL%MINFRES
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    REAL ALL%MINFRES
    
  Maximum frequency resolution under which a UV Table is considered
as a spectral line data. UV Tables with coarser spectral resolution
are treated as continuum only data: the line emission is filtered out,
and a pure continuum image is generated using bandwidth synthesis
in this case.
  
  
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2 ALL%PHASE__NITER

    ALL%PHASE__NITER is a size-variable integer array of rank 1.
    
It indicates the number
of clean components for each iteration of Phase self-calibration.
The number of iterations is defined by its number of elements.
The size of this array can be changed using the LET /RESIZE option.
    
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2 ALL%PHASE__TIMES

    ALL%PHASE__TIMES is a size-variable real array of rank 1.
    
It indicates the 
integration time for each iteration of Phase self-calibration.
The number of iterations is defined by its number of elements.
The size of this array can be changed using the LET /RESIZE option.
    
    Typical values are 45 seconds for NOEMA data, 6 to 24 sec for ALMA data.
    
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2 ALL%RANGE
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    REAL ALL%RANGE[3] 
    
  Velocity sampling around each spectral line (in km/s). ALL%RANGE[1:2] give
the Min and Max velocities ([0,0] indicates to take the whole coverage
of the sub-band).  
  
  ALL%RANGE[3] gives the desired spectral resolution (0 indicates to use the
spectral resolution of the sub-band).
  
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2 ALL%SPLIT
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    LOGICAL ALL%SPLIT
    
  Separate (Split) Line emission from Continuum emission in data Cubes or
extracted uv Tables, or keep Line+Continuum data together. This variable
is implicitely controlled by the selected MODE, but can be overidden
by the user.

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1 HOGBOM
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    [IMAGER_\]HOGBOM [First Last] [/FLUX [Min Max]]
  
  is a short cut for
.nf
      LET METHOD = HOGBOM
      CLEAN [First Last] [/FLUX [Min Max]]
.fi
      
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1 CLARK
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    [IMAGER_\]CLARK [First Last] [/FLUX [Min Max]]
    
  is a short cut for     
.nf
      LET METHOD = CLARK
      CLEAN [First Last] [/FLUX [Min Max]]
.fi
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1 GCLEAN
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    [IMAGER_\]GCLEAN [Gauss1 ... GaussN] [/FLUX [Min Max]] [/RESTART [File]]

  is a short cut for
.nf
      LET METHOD = GAUSS
      CLEAN [Gauss1 ... GaussN] [/FLUX [Min Max]] [/RESTART [File]]
.fi
      
    Where Gauss1 to GaussN are the size scales of the Gaussian components
in arcsecond. If no argument is given, these size scales are taken from
variable CLEAN__SCALES if not null, or derived from the Clean beam
size (0, 1 and 2 times the Clean beam size) otherwise.

Note that scale 0 (point source) is always the first scale, even if 
not specified as such. 

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1 MRC
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    [IMAGER_\]MRC [First Last] 

  is a short cut for     
.nf
      LET METHOD = MRC
      CLEAN [First Last] 
.fi
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1 MULTISCALE
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    [IMAGER_\]MULTISCALE [First Last] [/FLUX Min Max]

  is a short cut for
.nf
      LET METHOD = MULTI
      CLEAN [First Last] [/FLUX [Min Max]]
.fi
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1 SDI
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    [IMAGER_\]SDI [First Last] [/FLUX [Min Max]] 

  is a short cut for     
.nf
      LET METHOD = SDI
      CLEAN [First Last] [/FLUX [Min Max]]
.fi
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1 SIMULATE
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  [IMAGER_\]SIMULATE [?|Setup|Coverage|Model|Noise|Image|*]
  [/MODEL ModelFile  [Declination]] [/ARRAY Tele]
  [/CONFIGS List of Config] [/HOUR Hours per Config]
  [/NOISE Noise [BandWidth]

    Compute a UV coverage for the specified List of Configuration of the indicated
telescope Array, observing +/- Hours per configuration around the transit. Then
use the resulting UV table to simulate the observation of the sky brightness given in ModelFile.

    If the field of view of the ModelFile exceeds the primary beam of the array, an
appropriate Mosaic coverage is computed.

  Thermal noise can be added to the simulated visibilities.

  Actions are (in appropriate sequence order)
.nf
  SETUP     Setup the input parameters according to the specified options.
  COVERAGE  Compute Mosaic Pattern and UV coverage
  MODEL     Compute the noise-free simulated UV data
  NOISE     Add noise to the simulated UV data
  IMAGE     Perform the imaging using the noisy simulated UV data
  FIDELITY  Compute Image Fidelity
.fi
  In addition, the following arguments are recognized
.nf
  ?         List the input parameters
  *         Perform all actions in sequence.
.fi

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2 /MODEL
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  [IMAGER_\]SIMULATE /MODEL ModelFile [Declination]

  Specify the name of the (2D or 3D) model sky brightness. The declination is
taken from the ModelFile unless a new source Declination (in degree) is
specified.

  The ModelFile data units should be brightness (in K, or Jy/beam with a known
beam size, or Jy/pixel).

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2 /ARRAY
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  [IMAGER_\]SIMULATE /ARRAY Name

  Indicate which array is being used. Known arrays include ACA, ALMA, NOEMA, SMA
and VLA.
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2 /CONFIGS
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  [IMAGER_\]SIMULATE /CONFIGS List of Config

    Define the list of configurations used in the array. The configuration names
are array dependent as described below:
.nf
  ALMA   1 to 10
  ACA    I and NS
  NOEMA  A B C or D
  SMA    COM (compact), EXT (extended), SUB (sub-compact), VEX (very extended)
  VLA    A, AnB, B, BnC, C, CnD, D
.fi

    It is recommended to start by the longest baselines first for display reasons.
The configuration list appears in Sim%Config, a resizable character array.

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2 /HOUR
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  [IMAGER_\]SIMULATE /HOURS Hours per Config

    Define the span around transit in hours, one value per configuration, or if only
one value is given, the same span for all configurations.

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2 /NOISE
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  [IMAGER_\]SIMULATE /NOISE NoiseValue [BandWidth]

  Define the expected final point source noise (in Jy), for the Model channel spacing
or the specified BandWidth (in MHz) if present.  This noise level is used to rescale
weights accordingly, and generate appropriate scatter for the simulated data in the
SIMULATE NOISE step.

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2 Keywords:

SIMULATE has the following Action Keywords (in appropriate sequence order)
.nf
  SETUP     Setup the input parameters according to the specified options.
  COVERAGE  Compute Mosaic Pattern and UV coverage
  MODEL     Compute the noise-free simulated UV data
  NOISE     Add noise to the simulated UV data
  IMAGE     Perform the imaging using the noisy simulated UV data
  FIDELITY  Compute Image Fidelity
  SHOW      Show result
.fi
In addition, the following arguments are recognized
.nf
  ?         List the input parameters
  *         Perform all actions in sequence.
.fi

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2 COVERAGE
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  [IMAGER_\]SIMULATE COVERAGE 

  Compute Mosaic Pattern and UV coverage. The Mosaic pattern is
derived from the model image field-of-view, or the SIZE variable
if not 0. Fields are scanned in sequence, one per integration time.

  All specified configurations are used. 

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2 MODEL
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  [IMAGER_\]SIMULATE MODEL

  Compute the noise-free simulated UV data from the current UV coverage.
Primary beam is applied to the Model data set, according to the
Mosaic pointing centers.

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2 NOISE
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  [IMAGER_\]SIMULATE NOISE  [/NOISE Noise [BandWidth]]
  
  Add the "thermal" noise to the simulated UV data, according to the
specified final point source sensitivity.

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2 IMAGE 
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  [IMAGER_\]SIMULATE IMAGE 
  
  Perform the imaging using the noisy simulated UV data, using the
usual control parameters of UV__MAP and CLEAN.

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2 FIDELITY
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  [IMAGER_\]SIMULATE FIDELITY

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  *** under construction ***
  
  Compute Image Fidelity, which is defined as Model/abs(Obs-Model).
A median fidelity is also computed, and the Fidelity image displayed
from 0 to 3 times the median.

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2 SETUP
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  [IMAGER_\]SIMULATE SETUP 
  [/MODEL ModelFile  [Declination]] [/ARRAY Tele]
  [/CONFIGS List of Config] [/HOUR Hours per Config]
  [/NOISE Noise [BandWidth]]
  
  Setup all SIMULATE control variables according to the last (or current
if present) specified options. This completely re-initializes the modeling.
  
.ti -4
2 SHOW 
.ti +4
  [IMAGER_\]SIMULATE SHOW

  Display a visual summary of the Simulation. 4 panels contain 
the Smooth model, the Clean or Sky (if Mosaic) restored image,
the Difference and the Fidelity, respectively. An histogram
of the Fidelity is displayed at the right.
  

.ti -4
1 ENDOFHELP
    (Mandatory dummy entry) 
    
