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casa
$Rev:20696$
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casa
$Rev:20696$
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Public Member Functions | |
| def | __init__ |
| def | __call__ |
Private Attributes | |
| __bases__ | |
| __doc__ | |
Static Private Attributes | |
| string | __name__ |
Definition at line 18 of file sdtpimaging_pg.py.
| def sdtpimaging_pg.sdtpimaging_pg_.__init__ | ( | self | ) |
Definition at line 21 of file sdtpimaging_pg.py.
| def sdtpimaging_pg.sdtpimaging_pg_.__call__ | ( | self, | |
infile = None, |
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calmode = None, |
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masklist = None, |
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blpoly = None, |
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backup = None, |
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flaglist = None, |
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antenna = None, |
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spw = None, |
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stokes = None, |
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createimage = None, |
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outfile = None, |
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imsize = None, |
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cell = None, |
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phasecenter = None, |
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ephemsrcname = None, |
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pointingcolumn = None, |
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gridfunction = None, |
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plotlevel = None, |
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async = None |
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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 26 of file sdtpimaging_pg.py.
References publish_summary.quantity, and vla_uvfits_line_sf.verify.
sdtpimaging_pg.sdtpimaging_pg_.__bases__ [private] |
Definition at line 22 of file sdtpimaging_pg.py.
sdtpimaging_pg.sdtpimaging_pg_.__doc__ [private] |
Definition at line 23 of file sdtpimaging_pg.py.
string sdtpimaging_pg.sdtpimaging_pg_.__name__ [static, private] |
Definition at line 19 of file sdtpimaging_pg.py.
1.8.0