Functions
def	sdtpimaging
Function Documentation

def sdtpimaging.sdtpimaging	(	infile = `''`,
		calmode = `'none'`,
		masklist = `[]`,
		blpoly = `1`,
		backup = `True`,
		flaglist = `[]`,
		antenna = `''`,
		spw = `0`,
		stokes = `''`,
		createimage = `False`,
		outfile = `''`,
		imsize = `[256`,
		cell = `['1.0arcmin'`,
		arcmin,
		phasecenter = `''`,
		ephemsrcname = `''`,
		pointingcolumn = `'direction'`,
		gridfunction = `'BOX'`,
		plotlevel = `0`
	)
SD task: do a simple calibration and imaging for total power data 
  Keyword arguments:
infile -- name of input SD (MS) dataset
calmode -- calibration mode (currently only baseline subtraction)
        options: 'baseline','none'
        default: 'none'
        example: choose mode 'none' if you have
                 already calibrated and want to do
                 plotting nd/or imaging 
    >>> calmode='baseline' expandable parameters
       masklist -- mask in numbers of rows from each edge of each scan 
                   to be included for baseline fitting
         default: none
         example: [30,30] or [30] 
                  used first 30 rows and last 30 rows of each scan for 
                  the baseline 
       blpoly -- polynomial order for the baseline fit
         default: 1
       backup -- set True to create backup for input data
         default: True
flaglist -- list of scan numbers to flag (ranges can be accepted)  
        default: [] (use all scans)
        example: [[0,3],80]
                 flag the scan range [0,3] = [0,1,2,3] and scan 80 
antenna -- select data based on antenna name(s) or id(s) in string
        default: '' (use all antennas)
        example: '0,1', 'DV01'
        WARNING: currently baseline subtraction properly 
                 only one of the antennas.
spw -- spectral window id
        default: 0
        example: 1
stokes -- select data based on stokes or polarization type 
        default: '' (use all polarizations)
        example: 'XX'
createimage -- do imaging? 
        default: False 
    >>> createimage=True expandable parameters
       outfile -- output image name
         default: none
         example: 'mySDimage.im'
       imsize -- x and y image size in pixels, symmetric for single 
                 value
         default: [256,256]
         example: imsize=200 (equivalent to [200,200])
       cell -- x and y cell size. default unit arcmin
         default: '1.0arcmin'
         example: cell=['0.2arcmin, 0.2arcmin']
                  cell='0.2arcmin' (equivalent to example above)
       phasecenter -- image phase center: direction measure or fieldid 
         default: 0
         example: 'J2000 13h44m00 -17d02m00', 'AZEL -123d48m29 15d41m41'
       ephemsrcname -- ephemeris source name to proper shifting to 
                       center on the moving source for imaging
         default: ''
                  if the source name in the data matches one of the 
                  known solar objects by the system, this task 
                  automatically set the source name. 
         example: 'moon' 
       pointingcolumn -- pointing data column to use
         option: 'direction', 'target', 'pointing_offset', 
                 'source_offset', 'encoder' 
         default: 'direction'
       gridfunction -- gridding function for imaging
         options: 'BOX' (Box-car), 'SF' (Spheroidal), 
                  'PB' (Primary-beam), 'GAUSS' (Gaussian),
                  'GJINC' (Gaussian*Jinc)
         default: 'BOX'
         example: 'SF'
plotlevel -- control for plotting of results
        options: (int) 0=none, 1=some, 2=more, <0=hardcopy
        default: 0 (no plotting)
        example: plotlevel<0 as abs(plotlevel), e.g.
                 -1: hardcopy plot 
                     (will be named <infile>_scans.eps)
                  1: plot raw data, calibrated data 
                     (for calmode='baseline)
                     plot raw or if exist calibrated data 
                     (for calmode='none')
                  2: plot raw data, progressively display baseline 
                     fitting for each scan, and final calibrated data 
                     (for calmode='baseline')  


DESCRIPTION:

Task sdtpimaging performs data selection, calibration, and imaging for 
single-dish totalpower raster scan data.  This is a still experimental 
task made to work mostly for the data taken at the ALMA Testing 
Facility (ATF) or OSF. Currently, this task directly accesses the 
Measurement Set data only because of the data access efficiency. So it 
differs from other single-dish tasks that mostly operate on the ASAP 
scantable data format.  By setting calmode='none', one can run 
sdtpimaging to plot the data (raw or calibrated, if exists) and 
further imaging by setting createimage=True. 

The calibration available at this moment is just a simple baseline 
subtraction for each scan. The fitted regions set by masklist are the 
common for all the scans. Selection of the antennas can be made by 
setting antennaid(s) or antenna name(s) in string (e.g. '0', '0,1', 
'DV01',etc.). 

For baseline subtraction, it currently works properly for a single 
antenna selection. So a separate sdtpimaging task needs to be ran for 
each antenna. It currently assumes that the data has a single spw(=0) 
and fieldid(=0). By setting flaglist, one can set flag by scan numbers 
to be excluded from imaging. (Note: 'scan numbers' are determined from 
state id and related to SUB_SCAN column in STATE subtable and not to 
SCAN_NUMBER in MS.) By default, baseline subtraction stage overwrites 
(FLOAT_)DATA column of input data. You can keep original data by 
setting backup parameter to True. In this case, the task make a copy 
of input data specified by infile parameter. Name of backup file is 
<infile>.sdtpimaging.bak.<timestamp>.  

The selection of polarizations can be made by specifying the 
polarization name in stokes, such as 'XX' or 'YY' for linear 
polarizations. For example, with createimage=True, stokes='XXYY' will 
produces an image cube with each plane contains the image of one of
the polarizations while stokes='' or stokes='I' will produces a 'total 
intensity' or Stokes I image. 

Among the imaging sub-parameters, ephemsrcname is used to set the name 
of a moving source such as planets to produce a stationary image (can 
be omitted), and pointingcolumn is used to specify which pointing data 
column to use for imaging. Convolution kernel for imaging can be 
specified by using gridfunction. Available options are 'Box' (Box-car),
'SF' (Spheroidal), 'PB' (Primary-beam), 'GAUSS' (Gaussian), and 
'GJINC' (Gaussian*Jinc), where Jinc(x) = J_1(pi*x/c)/(pi*x/c) with a 
first order Bessel function J_1. Sub-parameters for convolution 
functions cannot be specified in this task. To costomize your 
convolution function, please do imaging using sdimaging task or 
imager tool.
Definition at line 13 of file sdtpimaging.py.
References publish_summary.quantity, task_sdtpimaging.sdtpimaging(), and vla_uvfits_line_sf.verify.
Functions

Function Documentation
