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« prev ^ index » next coverage.py v7.10.4, created at 2025-08-21 07:43 +0000
1##################### generated by xml-casa (v2) from tsdimaging.xml ################
2##################### 713609c253d369e84269a826601df774 ##############################
3from __future__ import absolute_import
4import numpy
5from casatools.typecheck import CasaValidator as _val_ctor
6_pc = _val_ctor( )
7from casatools.coercetype import coerce as _coerce
8from casatools.errors import create_error_string
9from .private.task_tsdimaging import tsdimaging as _tsdimaging_t
10from casatasks.private.task_logging import start_log as _start_log
11from casatasks.private.task_logging import end_log as _end_log
12from casatasks.private.task_logging import except_log as _except_log
14class _tsdimaging:
15 """
16 tsdimaging ---- SD task: imaging for total power and spectral data
19 Task sdimaging creates an image from input single-dish data sets.
20 The input can be either total power and spectral data.
22 The coordinate of output image is defined by four axes, i.e., two
23 spatial axes, frequency and polarization axes.n
24 By default, spatial coordinate of image is defined so that the all
25 pointing directions in POINTING tables of input data sets are covered
26 with the cell size, 1/3 of FWHM of primary beam of antennas in the
27 first MS. Therefore, it is often easiest to leave spatial definitions
28 at the default values. It is also possible to define spatial axes of
29 the image by specifying the image center direction (phasecenter),
30 number of image pixel (imsize) and size of the pixel (cell).n
31 The frequency coordinate of image is defined by three parameters,
32 the number of channels (nchan), the channel id/frequency/velocity of
33 the first channel (start), and channel width (width).There are three
34 modes available to define unit of start and width, i.e., 'channel' (use
35 channel indices), 'frequency' (use frequency unit, e.g., 'GHz'),
36 and 'velocity' (use velocity unit, e.g., 'km/s'). By default, nchan,
37 start, and width are defined so that all selected spectral windows are
38 covered with the channel width equal to separation of first two
39 channels selected.n
40 Finally, polarizations of image is defined by stokes parameter or
41 polarization. For example, stokes='XXYY' produces an image cube with
42 each plane contains the image of one of the polarizations, while
43 stokes='I' produces a 'total intensity' or Stokes I image.
44 The stokes parameter has a special option, 'pseudoI'. The option is
45 introduced to support imaging of partially flagged correlations.
46 Main difference between 'I' and 'pseudoI' is that the former only takes
47 into account the data whose correlations are all valid (this is the
48 Stokes I in the strict sense) while the latter accumulates partially
49 flagged data in addition. Note that the 'pseudoI' option is compatible
50 with 'I' for sdimaging task.
52 The task also supports various grid function (convolution kernel) to
53 weight spectra as well as an option to remove the most extreme minimum
54 and maximum (unweighted) values prior to computing the gridded pixel
55 values. See description below for details of gridfunction available.
59 --------- parameter descriptions ---------------------------------------------
61 infiles a list of names of input SD Measurementsets (only MS is allowed for this task)
62 outfile prefix of output images (.image, .weight)
63 overwrite overwrite the output file if already exists [True, False]
64 field select data by field IDs and names, e.g. \'3C2*\' (\'\'=all)
65 spw select data by IF IDs (spectral windows), e.g. \'3,5,7\' (\'\'=all)
66 antenna select data by antenna names or IDs, e.g, \'PM03\' (\'\' = all antennas)
67 scan select data by scan numbers, e.g. \'21~23\' (\'\'=all)
68 intent select data by observational intent, e.g. \'*ON_SOURCE*\' (\'\'=all)
69 timerange select data by range of time, e.g. 20:15:00~20:16:00 (\'\'=all)
70 outframe velocity frame of output image (''=current frame or LSRK for multiple-MS inputs)
71 mode spectral gridding type [\'channel\', \'frequency\', \'velocity\']
72 nchan number of channels (planes) in output image (-1=all)
73 start start of output spectral dimension, e.g. \'0\', \'110GHz\', \'-20km/s\'
74 width width of output spectral channels
75 veltype velocity definition
76 specmode Spectral definition mode (cube, cubedata, cubesource)
77 interpolation Spectral interpolation ["nearest", "linear", "cubic"]
78 Interpolation rules to use when binning data channels onto image channels and evaluating visibility values at the centers of image channels.
79 Note :
80 - "linear" and "cubic" interpolation requires data points on both sides of each image frequency. Errors are therefore possible at edge channels, or near flagged data channels. When image channel width is much larger than the data channel width there is nothing much to be gained using linear or cubic thus not worth the extra computation involved.
81 - If there are significant differences in the observation dates of the input MSes, "nearest" interpolation may cause some problems with frequency channel matching.
82 pointingcolumn pointing data column to use
83 convertfirst Specify whether the direction of the specified pointing column must be converted to image"s reference frame prior to being interpolated at data-taking time, and when. "never": interpolate against the pointing column, then convert. "always": interpolate against the beforehand converted pointing column. "auto": if there are less pointings than selected data rows convert first, else interpolate first
84 projection map projection type
85 imsize x and y image size in pixels, e.g., [64,64]. Single value: same for both spatial axes ([] = number of pixels to cover whole pointings in MSes)
86 cell x and y cell size, (e.g., [\'8arcsec\',\'8arcsec\']. default unit arcmin. ('' = 1/3 of FWHM of primary beam)
87 phasecenter image center direction: position or field index or ephemeris source info, e.g., \'J2000 17:30:15.0 -25.30.00.0\', \'MARS\'. (\'\' = the center of pointing directions in MSes)
88 stokes stokes parameters or polarization types to image, e.g. \'I\', \'XX\'
89 gridfunction gridding function for imaging (see description in help)
90 convsupport convolution support for gridding
91 truncate truncation radius for gridding
92 gwidth HWHM for gaussian
93 jwidth c-parameter for jinc function
94 clipminmax Clip minimum and maximum value from each pixel. Note the benefit of clipping is lost when the number of integrations contributing to each gridded pixel is small, or where the incidence of spurious datapoints is approximately or greater than the number of beams (in area) encompassed by expected image.
95 minweight Minimum weight ratio to the median of weight used in weight correction and weight beased masking
96 brightnessunit Overwrite the brightness unit in image (\'\' = respect the unit in MS) [\'K\' or \'Jy/beam\'].
97 If no unit is provided, the task examines unit keywords ('UNIT' and 'QuantumUnits' in turn) of data columns.
98 Order of the examination is 'CORRECTED_DATA' - 'FLOAT_DATA' - 'DATA'. The order also represents the priority.
99 When unit string is found, it will be used as brightness unit.
100 restfreq rest frequency to assign to image, e.g., \'114.5GHz\'. When the default value \'\' is used, the task currently internally uses REST_FREQUENCY of SOURCE table or mean frequency of given spectral window as a default value.
101 [1;42mRETURNS[1;m void
103 --------- examples -----------------------------------------------------------
106 Keyword arguments:
107 infiles -- a list of names of input SD Measurementsets
108 example: 'm100.PM01.ms'
109 ['m100.PM01.ms','m100.PM03.ms']; multiple MSes
110 outfile -- prefix of output images
111 Currently, four images are created by the task:
112 .image -- target image
113 .weight -- weight image
114 .sumwt -- sumwt image
115 .psf -- psf image (equivalent to weight image)
116 .sumwt and .psf are kind of useless so far. image products
117 will be improved later.
118 default: ''
119 example: 'mySDimage.im'
120 overwrite -- overwrite the output file if already exists
121 options: (bool) True,False
122 default: False (do NOT overwrite)
123 example: if True, existing file will be overwritten
124 field -- select data by field IDs and names
125 If field string is a non-negative integer, it is assumed to
126 be a field index otherwise, it is assumed to be a
127 field name
128 default: '' (use all fields)
129 example: field='3C2*' (all names starting with 3C2)
130 field='0,4,5~7' (field IDs 0,4,5,6,7)
131 field='0,3C273' (field ID 3 or filed named 3C273)
132 For multiple MS input, a list of field strings can be used:
133 field = ['0~2','0~4'] (field ids 0-2 for the first MS and 0-4
134 for the second)
135 field = '0~2' (field ids 0-2 for all input MSes)
136 this selection is in addition to the other selections to data
137 spw -- select data by spectral window IDs/channels
138 NOTE: channels de-selected here will contain all zeros if
139 selected by the parameter mode subparameters.
140 default: '' (use all IFs and channels)
141 example: spw='3,5,7' (IF IDs 3,5,7; all channels)
142 spw='<2' (IF IDs less than 2, i.e., 0,1; all channels)
143 spw='30~45GHz' (IF IDs with the center frequencies in range 30-45GHz; all channels)
144 spw='0:5~61' (IF ID 0; channels 5 to 61; all channels)
145 spw='3:10~20;50~60' (select multiple channel ranges within IF ID 3)
146 spw='3:10~20,4:0~30' (select different channel ranges for IF IDs 3 and 4)
147 spw='1~4;6:15~48' (for channels 15 through 48 for IF IDs 1,2,3,4 and 6)
148 For multiple MS input, a list of spw strings can be used:
149 spw=['0','0~3'] (spw ids 0 for the first MS and 0-3 for the second)
150 spw='0~3' (spw ids 0-3 for all input MSes)
151 this selection is in addition to the other selections to data
152 antenna -- select data by antenna names or IDs
153 If antenna string is a non-negative integer, it is
154 assumed to be an antenna index, otherwise, it is
155 considered an antenna name.
156 default: '' (all baselines, i.e. all antenna in case of auto data)
157 example: antenna='PM03'
158 For multiple MS input, a list of antenna strings can be used:
159 antenna=['5','6'] (antenna id5 for the first MS and 6 for the second)
160 antenna='5' (antenna index 5 for all input MSes)
161 this selection is in addition to the other selections to data
162 scan -- select data by scan numbers
163 default: '' (use all scans)
164 example: scan='21~23' (scan IDs 21,22,23)
165 For multiple MS input, a list of scan strings can be used:
166 scan=['0~100','10~200'] (scan ids 0-100 for the first MS
167 and 10-200 for the second)
168 scan='0~100 (scan ids 0-100 for all input MSes)
169 this selection is in addition to the other selections to data
170 intent -- select data by observational intent, also referred to as 'scan intent'
171 default: 'OBSERVE_TARGET#ON_SOURCE' (ALMA ON-source intent)
172 example: intent='' (use all scan intents)
173 intent='*ON_SOURCE*' (any valid scan-intent expression accepted by the MSSelection module can be specified)
174 For multiple MS input, a list of scan-intent expressions can be used:
175 intent=['ON_SOURCE','CALIBRATE_BANDPASS'] (scan intent ON_SOURCE for the first MS
176 and CALIBRATE_BANDPASS for the second)
177 this selection is in addition to the other selections to data
178 mode -- spectral gridding type
179 options: 'channel', 'velocity', 'frequency'
180 default: 'channel'
181 >>> mode expandable parameters
182 nchan -- Total number of channels in the output image.
183 default: -1; Automatically selects enough channels to cover
184 data selected by 'spw' consistent with 'start' and 'width'.
185 It is often easiest to leave nchan at the default value.
186 example: nchan=100
187 start -- First channel, velocity, or frequency.
188 For mode='channel'; This selects the channel index number
189 from the MS (0 based) that you want to correspond to the
190 first channel of the output cube. The output cube will be
191 in frequency space with the first channel having the
192 frequency of the MS channel selected by start. start=0
193 refers to the first channel in the first selected spw, even
194 if that channel is de-selected in the spw parameter.
195 Channels de-selected by the spw parameter will be filled with
196 zeros if included by the start parameter. For example,
197 spw=3~8:3~100 and start=2 will produce a cube that starts on
198 the third channel (recall 0 based) of spw index 3, and the
199 first channel will be blank.
200 default: '' (the first input channel of first input spw)
201 example: start=100 (mode='channel')
202 start='22.3GHz' (mode='frequency')
203 start='5.0km/s' (mode='velocity')
204 width -- Output channel width
205 For mode='channel', default=1; width>1 indicates channel averaging
206 example: width=4.
207 For mode= 'velocity' or 'frequency', default=''; width of
208 first input channel, or more precisely, the difference
209 in frequencies between the first two selected channels.
210 -- For example if channels 1 and 3 are selected with spw,
211 then the default width will be the difference between their
212 frequencies, and not the width of channel 1.
213 -- Similarly, if the selected data has uneven channel-spacing,
214 the default width will be picked from the first two selected
215 channels. In this case, please specify the desired width.
216 When specifying the width, one must give units
217 examples: width='1.0km/s', or width='24.2kHz'.
218 Setting width>0 gives channels of increasing frequency for
219 mode='frequency', and increasing velocity for mode='velocity'.
220 veltype -- Velocity definition
221 Options: 'radio','optical','true','relativistic'
222 default: 'radio'
223 specmode -- Spectral definition mode (cube, cubedata, cubesource)
224 default: 'cube'
225 Options: 'cube', 'cubedata', 'cubesource'
226 'cube' : Spectral line imaging with one or more channels
227 Parameters start, width,and nchan define the spectral
228 coordinate system and can be specified either in terms
229 of channel numbers, frequency or velocity in whatever
230 spectral frame is specified in 'outframe'.
231 All internal and output images are made with outframe as the
232 base spectral frame. However imaging code internally uses the fixed
233 spectral frame, LSRK for automatic internal software
234 Doppler tracking so that a spectral line observed over an
235 extended time range will line up appropriately.
236 Therefore the output images have additional spectral frame conversion
237 layer in LSRK on the top the base frame.
238 'cubedata' : Spectral line imaging with one or more channels
239 There is no internal software Doppler tracking so
240 a spectral line observed over an extended time range
241 may be smeared out in frequency. There is strictly
242 no valid spectral frame with which to label the output
243 images, but they will list the frame defined in the MS
244 'cubesource': Spectral line imaging while
245 tracking moving source (near field or solar system
246 objects). The velocity of the source is accounted
247 and the frequency reported is in the source frame.
248 As there is not SOURCE frame defined,
249 the frame reported will be REST (as it may not be
250 in the rest frame emission region may be
251 moving w.r.t the systemic velocity frame)
252 outframe -- velocity reference frame of output image
253 Options: '','LSRK','LSRD','BARY','GEO','TOPO','GALACTO',
254 'LGROUP','CMB'
255 default: ''; same as input data or 'LSRK' for multiple-MS inputs
256 example: frame='bary' for Barycentric frame
257 gridfunction -- gridding function for imaging
258 options: 'BOX' (Box-car), 'SF' (Spheroidal),
259 'PB' (Primary-beam), 'GAUSS' (Gaussian),
260 'GJINC' (Gaussian*Jinc)
261 default: 'BOX'
262 example: 'SF'
263 >>> gridfunction expandable parameter:
264 convsupport -- convolution support for 'SF'
265 default: -1 (use default for each gridfunction)
266 example: 3
267 truncate -- truncattion radius of convolution kernel.
268 effective only for 'GAUSS' and 'GJINC'.
269 default: '-1' (use default for each gridfunction)
270 example: 3, '20arcsec', '3pixel'
271 gwidth -- HWHM for gaussian. Effective only for
272 'GAUSS' and 'GJINC'.
273 default: '-1' (use default for each gridfunction)
274 example: 3, '20arcsec', '3pixel'
275 jwidth -- Width of jinc function. Effective only for
276 'GJINC'.
277 default: '-1' (use default for each gridfunction)
278 example: 3, '20arcsec', '3pixel'
279 imsize -- x and y image size in pixels, symmetric for single value
280 default: [] (=cover all pointings in MS)
281 example: imsize=200 (equivalent to [200,200])
282 cell -- x and y cell size. default unit arcmin
283 default: '' (= 1/3 of FWHM of primary beam)
284 example: cell=['0.2arcmin, 0.2arcmin']
285 cell='0.2arcmin' (equivalent to example above)
286 phasecenter -- image center: direction measure, field ID, or
287 ephemerides source information for moving source (solar system objects)
288 default: '' (= the center of pointing directions in
289 POINTING table of infiles)
290 example: phasecenter=6 (field ID)
291 phasecenter='J2000 13h44m00 -17d02m00'
292 phasecenter='AZEL -123d48m29 15d41m41'
293 phasecenter='MARS'
294 phasecenter='myComet_ephem.tab'
295 phasecenter='TRACKFIELD'
297 If the phasecenter is the name known major solar system object
298 ('MERCURY', 'VENUS', 'MARS', 'JUPITER', 'SATURN', 'URANUS',
299 'NEPTUNE', 'PLUTO', 'SUN', 'MOON') or is an ephemerides table
300 then that source is tracked and the background sources get smeared.
301 There is a special case, when phasecenter='TRACKFIELD', which
302 will use the ephemerides or polynomial phasecenter in the FIELD
303 table of the MS's as the source center to track.
305 When moving source correction is applied, the source is fixed to
306 the position at the beginning of on-source observations in the data.
307 Direction reference frame of output image refers phasecenter ('J2000'
308 if phasecenter is empty).
310 Caution: in case of specifying ephemeris table name, its name or path
311 must not start with known major solar system object listed
312 above (case-insensitive), otherwise, CASA will use its
313 internal ephemeris data for phasecenter instead. In such case
314 you need to add './' at the beginning so that the specified
315 table will be used. For example, if you wish to explicitly
316 specify ephemeris table attached to the input MS 'SunObs.ms',
317 set phasecenter like './SunObs.ms/FIELD/ephemtab_name.tab'.
319 projection -- map projection type. See Calabretta & Greisen (2002) for detail.
320 default: 'SIN'
321 options: 'SIN', 'CAR', 'TAN', 'SFL'
322 pointingcolumn -- pointing data column to use
323 option: 'direction', 'target', 'pointing_offset', 'source_offset', encoder'
324 default: 'direction'
325 restfreq -- specify rest frequency to use for output image
326 default: '' (refer input data)
327 example: 1.0e11, '100GHz'
328 stokes -- Stokes Planes to make
329 default='I'; example: stokes='XXYY';
330 options: 'I','Q','U','V','IV','QU','IQ','UV','IQUV','RR','LL','XX','YY','RRLL','XXYY','pseudoI'
331 Note : The 'pseudoI' option is a partial solution, allowing Stokes I imaging
332 when either of the parallel-hand correlations are unflagged.
334 minweight -- Minimum weight ratio to the median of weight used in
335 weight correction and weight based masking
336 default: 0.1
337 example: minweight = 0.
338 brightnessunit -- Overwrite the brightness unit in image ['K' or 'Jy/beam'].
339 If no unit is provided, the task examines unit keywords ('UNIT' and 'QuantumUnits' in turn) of data columns.
340 Order of the examination is 'CORRECTED_DATA' - 'FLOAT_DATA' - 'DATA'. The order also represents the priority.
341 When unit string is found, it will be used as brightness unit.
342 default: '' (use the unit in MS)
343 Options: '', 'K' (Kelvin), 'Jy/beam'
344 clipminmax -- Clip minimum and maximum value from each pixel.
345 Note the benefit of clipping is lost when the number of
346 integrations contributing to each gridded pixel is small,
347 or where the incidence of spurious datapoints is
348 approximately or greater than the number of beams (in area)
349 encompassed by expected image.
350 default: False
351 option: True, False
352 interpolation -- Spectral interpolation.
353 Interpolation rules to use when binning data channels onto image channels and
354 evaluating visibility values at the centers of image channels.
355 Note :
356 - 'linear' and 'cubic' interpolation requires data points on both sides of each image frequency.
357 Errors are therefore possible at edge channels, or near flagged data channels.
358 When image channel width is much larger than the data channel width there is nothing much to be gained
359 using linear or cubic thus not worth the extra computation involved.
360 - If there are significant differences in observing dates of input MSes, some problems merely occur
361 in frequency channel matching when 'nearest' interpolation.
362 option: 'linear', 'nearest', 'cubic'
363 default: 'linear'
365 -----------------
366 Gridding Kernel
367 -----------------
368 The parameter gridfunction sets gridding function (convolution kernel)
369 for imaging. Currently, the task supports 'BOX' (Box-car), 'SF' (Prolate
370 Spheroidal Wave Function), 'GAUSS' (Gaussian), 'GJINC' (Gaussian*Jinc),
371 where Jinc(x) = J_1(pi*x/c)/(pi*x/c) with a first order Bessel function
372 J_1, and 'PB' (Primary Beam). For 'PB', correct antenna informations
373 should be included in input file.
375 There are four subparameters for gridfunction: convsupport, truncate,
376 gwidth, and jwidth. The convsupport is an integer specifying cut-off
377 radius for 'SF' in units of pixel. By default (convsupport=-1),
378 the cut-off radius is set to 3 pixels. The truncate is a cut-off
379 radius for 'GAUSS' or 'GJINC'. It accepts integer, float, and
380 string values of numeric plus unit. Allowed units are angular
381 units such as 'deg', 'arcmin', 'arcsec', and 'pixel'. Default unit
382 is 'pixel' so that string without unit or numerical values (integer
383 or float) will be interpreted as radius in pixel. Default value
384 for truncate, which is used when negative radius is set, is 3*HWHM
385 for 'GAUSS' and radius at first null for 'GJINC'. The gwidth is
386 the HWHM of gaussian for 'GAUSS' and 'GJINC'. Default value is
387 sqrt(log(2)) pixel for 'GAUSS' and 2.52*sqrt(log(2)) pixel for
388 'GJINC'. The jwidth specifies width of the jinc function (parameter
389 'c' in the definition above). Default is 1.55 pixel. Both gwidth
390 jwidth allows integer, float, or string of numeric plus unit.
391 Default values for gwidth and jwidth are taken from Mangum et al.
392 (2007). Formula for 'GAUSS' and 'GJINC' are taken from Table 1 in
393 the paper, and are written as below using gwidth and jwidth:
395 GAUSS: exp[-log(2)*(|r|/gwidth)**2]
397 GJINC: J_1(pi*|r|/jwidth)/(pi*|r|/jwidth)
398 * exp[-log(2)*(|r|/gwidth)^2]
401 Reference: Mangum, et al. 2007, A&A, 474, 679-687
403 --------------------
404 Mask in Output Image
405 --------------------
406 The parameter minweight defines a threshold of weight values
407 to mask. The pixels in outfile whose weight is smaller than
408 minweight*median(weight) are masked out. The task also creates
409 a weight image with the name outfile.weight.
414 """
416 _info_group_ = """single dish"""
417 _info_desc_ = """SD task: imaging for total power and spectral data"""
419 def __call__( self, infiles=[ ], outfile='', overwrite=False, field='', spw='', antenna='', scan='', intent='OBSERVE_TARGET#ON_SOURCE', timerange='', outframe='', mode='channel', nchan=int(-1), start=int(0), width=int(1), veltype='radio', specmode='cube', interpolation='linear', pointingcolumn='direction', convertfirst='never', projection='SIN', imsize=[ ], cell='', phasecenter='', stokes='I', gridfunction='BOX', convsupport=int(-1), truncate=int(-1), gwidth=int(-1), jwidth=int(-1), clipminmax=False, minweight=float(0.1), brightnessunit='', restfreq='' ):
420 schema = {'infiles': {'type': 'cReqPathVec', 'coerce': [_coerce.to_list,_coerce.expand_pathvec]}, 'outfile': {'type': 'cStr', 'coerce': _coerce.to_str}, 'overwrite': {'type': 'cBool'}, 'field': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}]}, 'spw': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}]}, 'antenna': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}]}, 'scan': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}]}, 'intent': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}]}, 'timerange': {'type': 'cStr', 'coerce': _coerce.to_str}, 'outframe': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'LSRK', 'CMB', 'geo', 'bary', 'GALACTO', 'GEO', 'TOPO', 'LSRD', 'lsrk', 'topo', 'LGROUP', 'BARY', 'lsrd', 'cmb', 'galacto', 'lgroup', '' ]}, 'mode': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'channel', 'frequency', 'velocity' ]}, 'nchan': {'type': 'cInt'}, 'start': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cInt'}]}, 'width': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cInt'}]}, 'veltype': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'OPTICAL', 'RELATIVISTIC', 'radio', 'true', 'optical', 'RADIO', 'TRUE', 'relativistic' ]}, 'specmode': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'cube', 'cubedata', 'cubesource' ]}, 'interpolation': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'nearest', 'linear', 'cubic' ]}, 'pointingcolumn': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'TARGET', 'encoder', 'ENCODER', 'source_offset', 'pointing_offset', 'target', 'POINTING_OFFSET', 'DIRECTION', 'SOURCE_OFFSET', 'direction' ]}, 'convertfirst': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'never', 'auto', 'always' ]}, 'projection': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'sin', 'SIN', 'SFL', 'CAR', 'sfl', 'car', 'TAN', 'tan' ]}, 'imsize': {'anyof': [{'type': 'cIntVec', 'coerce': [_coerce.to_list,_coerce.to_intvec]}, {'type': 'cFloatVec', 'coerce': [_coerce.to_list,_coerce.to_floatvec]}]}, 'cell': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cStrVec', 'coerce': [_coerce.to_list,_coerce.to_strvec]}, {'type': 'cFloatVec', 'coerce': [_coerce.to_list,_coerce.to_floatvec]}]}, 'phasecenter': {'type': 'cVariant', 'coerce': [_coerce.to_variant]}, 'stokes': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'I', 'IQUV', 'UV', 'RRLL', 'IQ', 'V', 'pseudoI', 'QU', 'YY', 'RR', 'Q', 'U', 'IV', 'XX', 'XXYY', 'LL' ]}, 'gridfunction': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ 'GJINC', 'pb', 'sf', 'GAUSS', 'PB', 'SF', 'gauss', 'BOX', 'box', 'gjinc' ]}, 'convsupport': {'type': 'cInt'}, 'truncate': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cInt'}, {'type': 'cFloat', 'coerce': _coerce.to_float}]}, 'gwidth': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cInt'}, {'type': 'cFloat', 'coerce': _coerce.to_float}]}, 'jwidth': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cInt'}, {'type': 'cFloat', 'coerce': _coerce.to_float}]}, 'clipminmax': {'type': 'cBool'}, 'minweight': {'type': 'cFloat', 'coerce': _coerce.to_float, 'min': 0}, 'brightnessunit': {'type': 'cStr', 'coerce': _coerce.to_str, 'allowed': [ '', 'K', 'Jy/beam' ]}, 'restfreq': {'anyof': [{'type': 'cStr', 'coerce': _coerce.to_str}, {'type': 'cFloat', 'coerce': _coerce.to_float}]}}
421 doc = {'infiles': infiles, 'outfile': outfile, 'overwrite': overwrite, 'field': field, 'spw': spw, 'antenna': antenna, 'scan': scan, 'intent': intent, 'timerange': timerange, 'outframe': outframe, 'mode': mode, 'nchan': nchan, 'start': start, 'width': width, 'veltype': veltype, 'specmode': specmode, 'interpolation': interpolation, 'pointingcolumn': pointingcolumn, 'convertfirst': convertfirst, 'projection': projection, 'imsize': imsize, 'cell': cell, 'phasecenter': phasecenter, 'stokes': stokes, 'gridfunction': gridfunction, 'convsupport': convsupport, 'truncate': truncate, 'gwidth': gwidth, 'jwidth': jwidth, 'clipminmax': clipminmax, 'minweight': minweight, 'brightnessunit': brightnessunit, 'restfreq': restfreq}
422 assert _pc.validate(doc,schema), create_error_string(_pc.errors)
423 _logging_state_ = _start_log( 'tsdimaging', [ 'infiles=' + repr(_pc.document['infiles']), 'outfile=' + repr(_pc.document['outfile']), 'overwrite=' + repr(_pc.document['overwrite']), 'field=' + repr(_pc.document['field']), 'spw=' + repr(_pc.document['spw']), 'antenna=' + repr(_pc.document['antenna']), 'scan=' + repr(_pc.document['scan']), 'intent=' + repr(_pc.document['intent']), 'timerange=' + repr(_pc.document['timerange']), 'outframe=' + repr(_pc.document['outframe']), 'mode=' + repr(_pc.document['mode']), 'nchan=' + repr(_pc.document['nchan']), 'start=' + repr(_pc.document['start']), 'width=' + repr(_pc.document['width']), 'veltype=' + repr(_pc.document['veltype']), 'specmode=' + repr(_pc.document['specmode']), 'interpolation=' + repr(_pc.document['interpolation']), 'pointingcolumn=' + repr(_pc.document['pointingcolumn']), 'convertfirst=' + repr(_pc.document['convertfirst']), 'projection=' + repr(_pc.document['projection']), 'imsize=' + repr(_pc.document['imsize']), 'cell=' + repr(_pc.document['cell']), 'phasecenter=' + repr(_pc.document['phasecenter']), 'stokes=' + repr(_pc.document['stokes']), 'gridfunction=' + repr(_pc.document['gridfunction']), 'convsupport=' + repr(_pc.document['convsupport']), 'truncate=' + repr(_pc.document['truncate']), 'gwidth=' + repr(_pc.document['gwidth']), 'jwidth=' + repr(_pc.document['jwidth']), 'clipminmax=' + repr(_pc.document['clipminmax']), 'minweight=' + repr(_pc.document['minweight']), 'brightnessunit=' + repr(_pc.document['brightnessunit']), 'restfreq=' + repr(_pc.document['restfreq']) ] )
424 task_result = None
425 try:
426 task_result = _tsdimaging_t( _pc.document['infiles'], _pc.document['outfile'], _pc.document['overwrite'], _pc.document['field'], _pc.document['spw'], _pc.document['antenna'], _pc.document['scan'], _pc.document['intent'], _pc.document['timerange'], _pc.document['outframe'], _pc.document['mode'], _pc.document['nchan'], _pc.document['start'], _pc.document['width'], _pc.document['veltype'], _pc.document['specmode'], _pc.document['interpolation'], _pc.document['pointingcolumn'], _pc.document['convertfirst'], _pc.document['projection'], _pc.document['imsize'], _pc.document['cell'], _pc.document['phasecenter'], _pc.document['stokes'], _pc.document['gridfunction'], _pc.document['convsupport'], _pc.document['truncate'], _pc.document['gwidth'], _pc.document['jwidth'], _pc.document['clipminmax'], _pc.document['minweight'], _pc.document['brightnessunit'], _pc.document['restfreq'] )
427 except Exception as exc:
428 _except_log('tsdimaging', exc)
429 raise
430 finally:
431 task_result = _end_log( _logging_state_, 'tsdimaging', task_result )
432 return task_result
434tsdimaging = _tsdimaging( )