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casa
$Rev:20696$
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casa
$Rev:20696$
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00001 # 00002 # This file was generated using xslt from its XML file 00003 # 00004 # Copyright 2008, Associated Universities Inc., Washington DC 00005 # 00006 import sys 00007 import os 00008 from casac import * 00009 import string 00010 import time 00011 import inspect 00012 import gc 00013 import numpy 00014 from odict import odict 00015 from task_setjy import setjy 00016 from task_setjy import casalog 00017 00018 class setjy_pg_: 00019 __name__ = "setjy" 00020 00021 def __init__(self) : 00022 self.__bases__ = (setjy_pg_,) 00023 self.__doc__ = self.__call__.__doc__ 00024 00025 00026 def __call__(self, vis=None, field=None, spw=None, selectdata=None, timerange=None, scan=None, observation=None, modimage=None, listmodels=None, scalebychan=None, fluxdensity=None, spix=None, reffreq=None, standard=None, useephemdir=None, usescratch=None, async=None): 00027 00028 """Fills the model column with the visibilities of a calibrator 00029 00030 The task sets the model visibility amp and phase of a specified source 00031 (generally a calibrator). The simplest way is to enter the flux density 00032 (I,Q,U,V) explicitly, but this is valid only for a point source. 00033 00034 For an extended source, the clean model (image.model) can be 00035 specified and the model visibilities associated with this clean 00036 model is placed in the visibility model column. 00037 00038 Models are available for 3C48, 3C138, 3C286 between 1.4 and 43 GHz. 00039 3C147 is available above 4 GHz. These models are scaled to the precise 00040 frequency of the data. Only I models are presently available. 00041 00042 The location of the models is system dependent: At the AOC and CV, the 00043 models are in the directory::/usr/lib/casapy/data/nrao/VLA/CalModels or 00044 /usr/lib64/casapy/data/nrao/VLA/CalModels (depending on whether 32 or 64 00045 bit CASA was installed on the machine being used). In general (using 00046 Python), the stock models should be in 00047 casa['dirs']['data'] + '/nrao/VLA/CalModels' 00048 setjy also looks for models in the current directory before trying 00049 casa['dirs']['data'] + '/nrao/VLA/CalModels'. 00050 00051 setjy need only be run on the calibrator sources with a known flux 00052 density and/or model. 00053 00054 00055 Solar System Objects are supported via the 'Butler-JPL-Horizons 2012' 00056 standard. This uses new brightness temperature models and a new flux 00057 calculation code that replace the 'Butler-JPL-Horizons 2010' standard. 00058 The older 'Butler-JPL-Horizons 2010' standard is still available 00059 for comparison. Users may want to use predictcomp task to see the differeces. 00060 Currently they are modeled as uniform temperature disks based 00061 on their ephemerides at the time of observation (note that this may 00062 oversimply objects, in particular asteroids). The object name is 00063 obtained from the 'field' parameter. Recognized objects are listed 00064 below, under 'standard'. 00065 00066 Note that fluxdensity, modimage, and standard interact in a possibly 00067 confusing way! Generally, if fluxdensity[0] (Stokes I) is <= 0, it 00068 will be ignored. If it is < 0, standard (which has a default) will 00069 be used to calculate flux density as a function of frequency, even if 00070 modimage is specified. If is is exactly 0 and modimage is given, the 00071 brightness of the model image will be used as is. If fluxdensity([0]) 00072 is > 0, it will be used. The latter two options come at the price of 00073 disabling frequency scaling, i.e. the same fluxdensity will be used for 00074 all frequencies. 00075 00076 Keyword arguments: 00077 vis -- Name of input visibility file 00078 default: none. example: vis='ngc5921.ms' 00079 field -- Select field using field id(s) or field name(s). 00080 default: ''=all fields, but run setjy one field at a time. 00081 [run listobs to obtain the list id's or names of calibrators] 00082 If field is a non-negative integer, it is assumed to be a field 00083 index. Otherwise, it is taken to be a field name (case sensitive 00084 - it must match the name as listed by listobs). 00085 field='0~2'; field ids 0,1,2 00086 field='0,4,5~7'; field ids 0,4,5,6,7 00087 field='3C286,3C295'; field named 3C286 and 3C295 00088 field = '3,4C*'; field id 3, all names starting with 4C 00089 spw -- Spectral window selection string. 00090 default: '' = all spectral windows 00091 Note that setjy only selects by spectral window, and ignores 00092 channel selections. Fine-grained control could be achieved using 00093 (and possibly constructing) a cube for modimage. 00094 00095 selectdata -- Other parameters for selecting part(s) of the MS 00096 to operate on. 00097 (Currently all time-oriented and most likely only of 00098 interest when using a Solar System object as a calibrator.) 00099 default: False 00100 00101 >>> selectdata=True expandable parameters 00102 See help par.selectdata for more on these. 00103 00104 timerange -- Select data based on time range: 00105 default: '' (all); examples, 00106 timerange = 'YYYY/MM/DD/hh:mm:ss~YYYY/MM/DD/hh:mm:ss' 00107 Note: if YYYY/MM/DD is missing date defaults to first 00108 day in data set 00109 timerange='09:14:0~09:54:0' picks 40 min on first day 00110 timerange='25:00:00~27:30:00' picks 1 hr to 3 hr 00111 30min on NEXT day 00112 timerange='09:44:00' pick data within one integration 00113 of time 00114 timerange='>10:24:00' data after this time 00115 For multiple MS input, a list of timerange strings can be 00116 used: 00117 timerange=['09:14:0~09:54:0','>10:24:00'] 00118 timerange='09:14:0~09:54:0''; apply the same timerange for 00119 all input MSes 00120 scan -- Scan number range. 00121 default: '' (all) 00122 example: scan='1~5' 00123 For multiple MS input, a list of scan strings can be used: 00124 scan=['0~100','10~200'] 00125 scan='0~100; scan ids 0-100 for all input MSes 00126 Check 'go listobs' to insure the scan numbers are in order. 00127 observation -- Observation ID range. 00128 default: '' (all) 00129 example: observation='1~5' 00130 00131 00132 modimage -- Model image (I only) for setting the model visibilities. 00133 modimage can be a cube, and its channels do not have to exactly 00134 match those of vis. It is recommended to use modimage for 00135 sources that are resolved by the observation, but the 00136 Butler-JPL-Horizons standard supplies a basic model of what 00137 several Solar System objects look like. default: '': do not use 00138 a model image. 00139 00140 Each field must be done separately when using a model image. The 00141 flux density of the image will be scaled from the frequency in 00142 the model to that actually used (ignoring fluxdensity), unless 00143 fluxdensity >= 0 (or fluxdensity[0] >= 0). If 00144 fluxdensity([0]) is 0.0, the image's flux density will be used. 00145 If fluxdensity([0]) > 0.0, it will be used (and spix and 00146 reffreq if modimage is not a cube). Since the spectral index 00147 usually varies with direction, applying a single spectral index 00148 to a 2D modimage is typically not as good as using a cube. 00149 00150 Both the amplitude and phase are calculated. At the AOC or CV, 00151 the models are located in casa['dirs']['data'] 00152 + '/nrao/VLA/CalModels/', e.g. 00153 /usr/lib/casapy/data/nrao/VLA/CalModels/3C286_L.im 00154 lib64 00155 00156 If modimage does not start with '/', setjy will look for a match 00157 in '.', './CalModels', and any CalModels directories within 00158 the casa['dirs']['data'] tree (excluding certain branches). 00159 00160 Note that modimage should be deconvolved, i.e. a set of clean 00161 components instead of an image that has been convolved with a 00162 clean beam. 00163 00164 listmodels -- If True, do nothing but list candidates for modimage 00165 (for extragalactic calibrators) that are present on the system. It looks for *.im* *.mod* in ., 00166 CalModels, and CalModels directories in the casa['dirs']['data'] 00167 tree. It does not check whether they are appropriate for the MS! 00168 If standard='Butler-JPL-Horizons 2012', Tb models (frequency-depended 00169 brightness temperature models) for Solar System objects used in the 00170 standard. For standard='Butler-JPL-Horizons 2010', the recognized 00171 Solar System objects are listed. 00172 00173 scalebychan -- This determines whether the fluxdensity set in the model is 00174 calculated on a per channel basis. If False then it only one 00175 fluxdensity value is calculated per spw. (Either way, all channels 00176 in spw are modified.) It is effectively True if fluxdensity[0] > 00177 0.0. 00178 default: True 00179 00180 fluxdensity -- Specified flux density [I,Q,U,V] in Jy 00181 default: -1, uses [1,0,0,0] flux density for unrecognized sources, 00182 and standard flux densities for ones recognized by 'standard', 00183 including 3C286, 3C48, 3C147, and several planets, moons, and 00184 asteroids. setjy will try to use standard if fluxdensity is not 00185 positive. 00186 00187 Only one flux density can be specified at a time. The phases are 00188 set to zero. 00189 example fluxdensity=-1 will use standard for recognized 00190 calibrators (like 3C286, 3C147 and 3C48, depending on 00191 standard) and insert 1.0 for selected fields with 00192 unrecognized sources. 00193 example field = '1'; fluxdensity=[3.2,0,0,0] wil put in 00194 a flux density of I=3.2 for field='1' 00195 00196 At present (June 2000), this is the only method to insert a 00197 polarized flux density model. 00198 example: fluxdensity=[2.63,0.21,-0.33,0.02] 00199 will put in I,Q,U,V flux densities of 2.63,0.21,-0.33, 00200 and 0.02, respectively, in the model column. 00201 00202 spix -- Spectral index for fluxdensity: 00203 S = fluxdensity * (freq/reffreq)**spix 00204 Default: 0 (no effect) 00205 Only used if fluxdensity is being used. 00206 N.B.: If fluxdensity is positive, and spix is nonzero, then reffreq 00207 must be set too! (See below) 00208 00209 It is applied in the same way to all polarizations, and does 00210 not account for Faraday rotation or depolarization. 00211 00212 reffreq -- The reference frequency for spix, given with units. 00213 Default: '1GHz'; this is only here to prevent division by 0! 00214 N.B.: If the flux density is being scaled by spectral index, 00215 then reffreq must be set to whatever reference frequency is 00216 correct for the given fluxdensity and spix. It cannot be 00217 determined from vis. On the other hand, if spix is 0, then any 00218 positive frequency can be used (and ignored). 00219 00220 Examples: '86.0GHz', '4.65e9Hz' 00221 00222 standard -- Flux density standard, used if fluxdensity[0] < 0.0 00223 default: 'Perley-Butler 2010'; example: standard='Baars' 00224 Options: 'Baars','Perley 90','Perley-Taylor 95', 00225 'Perley-Taylor 99', 'Perley-Butler 2010', 'Perley-Butler 2013', 00226 'Butler-JPL-Horizons 2010', and 'Butler-JPL-Horizons 2012'. 00227 All but the last two are for extragalactic calibrators, 00228 and the final two are for Solar System objects. 00229 00230 Extragalactic calibrators: 00231 Following source names and their common aliases are recognized. 00232 The last column shows which standards support for each source. 00233 Note that the task does not do exact matching of the name and 00234 it recognizes as long as the field name contains the string 00235 listed below (e.g. 'PKS 1934-638' works). 00236 ----------------------------------------------------------- 00237 3C Name B1950 Name J2000 Name Alt. J2000 Name standards* 00238 3C48 0134+329 0137+331 J0137+3309 1,3,4,5,6 00239 3C123 0433+295 0437+296 J0437+2940 2 00240 3C138 0518+165 0521+166 J0521+1638 1,3,4,5,6 00241 3C147 0538+498 0542+498 J0542+4951 1,3,4,5,6 00242 3C196 0809+483 0813+482 J0813+4813 1,2 00243 3C286 1328+307 1331+305 J1331+3030 1,2,3,4,5,6 00244 3C295 1409+524 1411+522 J1411+5212 1,2,3,4,5,6 00245 - 1934-638 - J1939-6342 1,3,4,5,6 00246 ----------------------------------------------------------- 00247 * supported in: 1 - Perley-Butler 2010, 2 - Perley-Butler 2013, 00248 3 - Perley-Taylor 99, 4 - Perley-Taylor 95, 5 - Perley 90, 6 - Baars 00249 00250 Solar system objects: 00251 The 'Butler-JPL-Horizons 2012' standard is recommended over 00252 'Butler-JPL-Horizons 2010' as the former uses updated models. 00253 Recognized Solar System objects (for 'Butler-JPL-Horizons 2012') are: 00254 00255 00256 Planets: Venus, Mars, Jupiter, Uranus, Neptune 00257 00258 Moons: Jupiter: Io, Europa, Ganymede, Callisto 00259 Saturn: Titan 00260 00261 Asteroids: Ceres, Pallas**, Vesta**, Juno** 00262 00263 * Venus: model for ~300MHz to 350GHz, no atmospheric lines (CO,H2O,HDO, etc) 00264 * Mars: tabulated as a function of time and frequency (30 - 1000GHz) based on 00265 Rudy el tal (1988), no atmopheric lines (CO, H20, H2O2, HDO, etc) 00266 * Jupiter: model for 30-1020GHz, does not include synchrotron emission 00267 * Uranus: model for 60-1800GHz, contains no rings or synchrotron. 00268 * Neptune: model for 2-2000GHz, the broad CO absorption line 00269 is included, but contains no rings or syncrotron. 00270 * Titan: model for 53.3-1024.1GHz, include many spectral lines 00271 00272 ** not recommended (The temperature is not yet adjusted for 00273 varying distance from the Sun. The model data can be scaled 00274 after running setjy, but it is an involved process.) 00275 00276 The 'field' parameter must match the case of the field name(s) 00277 in vis (as shown by listobs). 00278 00279 Flux density calculation with Solar System objects depends on 00280 ephemerides. The setjy task looks for the data in 00281 00282 os.getenv('CASAPATH').split()[0] + '/data/ephemerides/JPL-Horizons'. 00283 00284 If no ephemeris for the right object at the right time is 00285 present, the calculation will fail. Ask the helpdesk to make an 00286 ephemeris. The very adventurous and well versed in python can 00287 try it using CASA's recipes.ephemerides package: 00288 import recipes.ephemerides as eph 00289 help eph 00290 00291 CASA comes with ephemerides for several more objects, but they 00292 are intended for use with me.framecomet(), and are not (yet) 00293 suitable flux density calibrators. It is up to the observer to 00294 pick a good flux density calibrator (bright, spherical and 00295 featureless, on a circular orbit, in the right part of the sky, 00296 and not too resolved). Even some of the objects listed above 00297 may prove to require more sophisticated flux density models than 00298 are currently implemented in CASA. For many objects running 00299 casalog.filter('INFO1') before running setjy will send more 00300 information to the logger. The cookbook also has an appendix 00301 with descriptions of the models used by setjy (both 00302 extragalactic and Solar System). 00303 00304 >>> standard="Butler-JPL-Horizons 2012" expandable parameter 00305 00306 useephemdir -- If True: use the direction from the ephemeris table for 00307 the solar system object. 00308 default: False -use the direction information in the MS(i.e. Field table) 00309 00310 usescratch -- If False: 'virtual' model is created. The model is saved in the header 00311 and model visibilities are evaluated when calculating calibration or plotting in plotms. 00312 If True: the model visibility will be evaluated and saved on disk in the MODEL_DATA 00313 column. This will increase your ms in size by a factor of 1.5 (w.r.t. the case where 00314 you only have the DATA and the CORRECTED_DATA column). Use True if you need to interact 00315 with the MODEL_DATA in python, say. 00316 00317 *By running usescratch=T, it will remove the existing virtual model from previous runs. 00318 usescratch=F will not remove the existing MODEL_DATA but in subsequent process 00319 the virtual model with matching field and spw combination will be used if it exists 00320 regardless of the presence of the MODEL_DATA column. 00321 00322 default: False 00323 00324 00325 """ 00326 a=inspect.stack() 00327 stacklevel=0 00328 for k in range(len(a)): 00329 if (string.find(a[k][1], 'ipython console') > 0) or (string.find(a[k][1], '<string>') >= 0): 00330 stacklevel=k 00331 break 00332 myf=sys._getframe(stacklevel).f_globals 00333 myf['__last_task'] = 'setjy' 00334 myf['taskname'] = 'setjy' 00335 ### 00336 myf['update_params'](func=myf['taskname'],printtext=False) 00337 ### 00338 ### 00339 #Handle globals or user over-ride of arguments 00340 # 00341 function_signature_defaults=dict(zip(self.__call__.func_code.co_varnames,self.__call__.func_defaults)) 00342 useLocalDefaults = False 00343 00344 for item in function_signature_defaults.iteritems(): 00345 key,val = item 00346 keyVal = eval(key) 00347 if (keyVal == None): 00348 #user hasn't set it - use global/default 00349 pass 00350 else: 00351 #user has set it - use over-ride 00352 if (key != 'self') : 00353 useLocalDefaults = True 00354 #myf[key]=keyVal 00355 00356 myparams = {} 00357 if useLocalDefaults : 00358 for item in function_signature_defaults.iteritems(): 00359 key,val = item 00360 keyVal = eval(key) 00361 exec('myparams[key] = keyVal') 00362 if (keyVal == None): 00363 exec('myparams[key] = '+ key + ' = self.itsdefault(key)') 00364 keyVal = eval(key) 00365 if(type(keyVal) == dict) : 00366 exec('myparams[key] = ' + key + ' = keyVal[len(keyVal)-1][\'value\']') 00367 00368 else : 00369 uselessvariable = None 00370 myparams['vis'] = vis = myf['vis'] 00371 myparams['field'] = field = myf['field'] 00372 myparams['spw'] = spw = myf['spw'] 00373 myparams['selectdata'] = selectdata = myf['selectdata'] 00374 myparams['timerange'] = timerange = myf['timerange'] 00375 myparams['scan'] = scan = myf['scan'] 00376 myparams['observation'] = observation = myf['observation'] 00377 myparams['modimage'] = modimage = myf['modimage'] 00378 myparams['listmodels'] = listmodels = myf['listmodels'] 00379 myparams['scalebychan'] = scalebychan = myf['scalebychan'] 00380 myparams['fluxdensity'] = fluxdensity = myf['fluxdensity'] 00381 myparams['spix'] = spix = myf['spix'] 00382 myparams['reffreq'] = reffreq = myf['reffreq'] 00383 myparams['standard'] = standard = myf['standard'] 00384 myparams['useephemdir'] = useephemdir = myf['useephemdir'] 00385 myparams['usescratch'] = usescratch = myf['usescratch'] 00386 00387 00388 result = None 00389 00390 # 00391 # The following is work around to avoid a bug with current python translation 00392 # 00393 mytmp = {} 00394 00395 mytmp['vis'] = vis 00396 mytmp['field'] = field 00397 mytmp['spw'] = spw 00398 mytmp['selectdata'] = selectdata 00399 mytmp['timerange'] = timerange 00400 mytmp['scan'] = scan 00401 mytmp['observation'] = observation 00402 mytmp['modimage'] = modimage 00403 mytmp['listmodels'] = listmodels 00404 mytmp['scalebychan'] = scalebychan 00405 mytmp['fluxdensity'] = fluxdensity 00406 mytmp['spix'] = spix 00407 mytmp['reffreq'] = reffreq 00408 mytmp['standard'] = standard 00409 mytmp['useephemdir'] = useephemdir 00410 mytmp['usescratch'] = usescratch 00411 pathname='file:///'+os.environ.get('CASAPATH').split()[0]+'/share/xml/' 00412 trec = casac.utils().torecord(pathname+'setjy.xml') 00413 00414 casalog.origin('setjy') 00415 if not trec.has_key('setjy') or not casac.utils().verify(mytmp, trec['setjy']) : 00416 return False 00417 00418 00419 try : 00420 casalog.post('') 00421 casalog.post('##########################################') 00422 casalog.post('##### Begin Task: setjy #####') 00423 casalog.post('') 00424 result = setjy(vis, field, spw, selectdata, timerange, scan, observation, modimage, listmodels, scalebychan, fluxdensity, spix, reffreq, standard, useephemdir, usescratch) 00425 casalog.post('') 00426 casalog.post('##### End Task: setjy #####') 00427 casalog.post('##########################################') 00428 00429 00430 # saveinputs for individule engine has no use 00431 # saveinputs should alos be removed from casa_in_py.py 00432 # 00433 # 00434 # saveinputs = myf['saveinputs'] 00435 # saveinputs('setjy', 'setjy.last', myparams) 00436 # 00437 # 00438 except Exception, instance: 00439 #print '**** Error **** ',instance 00440 pass 00441 00442 gc.collect() 00443 return result 00444 # 00445 # 00446 ## 00447 # def paramgui(self, useGlobals=True): 00448 # """ 00449 # Opens a parameter GUI for this task. If useGlobals is true, then any relevant global parameter settings are used. 00450 # """ 00451 # import paramgui 00452 # 00453 # a=inspect.stack() 00454 # stacklevel=0 00455 # for k in range(len(a)): 00456 # if (string.find(a[k][1], 'ipython console') > 0) or (string.find(a[k][1], '<string>') >= 0): 00457 # stacklevel=k 00458 # break 00459 # myf = sys._getframe(stacklevel).f_globals 00460 # 00461 # if useGlobals: 00462 # paramgui.setGlobals(myf) 00463 # else: 00464 # paramgui.setGlobals({}) 00465 # 00466 # paramgui.runTask('setjy', myf['_ip']) 00467 # paramgui.setGlobals({}) 00468 # 00469 # 00470 # 00471 # 00472 def defaults(self, param=None): 00473 a=inspect.stack() 00474 stacklevel=0 00475 for k in range(len(a)): 00476 if (string.find(a[k][1], 'ipython console') > 0) or (string.find(a[k][1], '<string>') >= 0): 00477 stacklevel=k 00478 break 00479 myf=sys._getframe(stacklevel).f_globals 00480 a = odict() 00481 a['vis'] = '' 00482 a['field'] = '' 00483 a['spw'] = '' 00484 a['selectdata'] = False 00485 a['modimage'] = '' 00486 a['listmodels'] = False 00487 a['scalebychan'] = True 00488 a['fluxdensity'] = -1 00489 a['standard'] = 'Perley-Butler 2010' 00490 a['usescratch'] = False 00491 00492 a['async']=False 00493 a['selectdata'] = { 00494 0:{'value':False}, 00495 1:odict([{'value':True}, {'timerange':''}, {'scan':''}, {'observation':''}])} 00496 a['fluxdensity'] = { 00497 0:odict([{'notvalue':-1}, {'spix':0}, {'reffreq':'1GHz'}])} 00498 a['standard'] = { 00499 0:{'value':'Perley-Butler 2010'}, 00500 1:{'value':'Perley-Butler 2013'}, 00501 2:{'value':'Perley-Taylor 99'}, 00502 3:{'value':'Baars'}, 00503 4:{'value':'Perley 90'}, 00504 5:{'value':'Perley-Taylor 95'}, 00505 6:odict([{'value':'Butler-JPL-Horizons 2012'}, {'useephemdir':False}]), 00506 7:{'value':'Butler-JPL-Horizons 2010'}} 00507 00508 ### This function sets the default values but also will return the list of 00509 ### parameters or the default value of a given parameter 00510 if(param == None): 00511 myf['__set_default_parameters'](a) 00512 elif(param == 'paramkeys'): 00513 return a.keys() 00514 else: 00515 if(a.has_key(param)): 00516 #if(type(a[param]) == dict) : 00517 # return a[param][len(a[param])-1]['value'] 00518 #else : 00519 return a[param] 00520 00521 00522 # 00523 # 00524 def check_params(self, param=None, value=None): 00525 a=inspect.stack() 00526 stacklevel=0 00527 for k in range(len(a)): 00528 if (string.find(a[k][1], 'ipython console') > 0) or (string.find(a[k][1], '<string>') >= 0): 00529 stacklevel=k 00530 break 00531 myf=sys._getframe(stacklevel).f_globals 00532 00533 # print 'param:', param, 'value:', value 00534 try : 00535 if str(type(value)) != "<type 'instance'>" : 00536 value0 = value 00537 value = myf['cu'].expandparam(param, value) 00538 matchtype = False 00539 if(type(value) == numpy.ndarray): 00540 if(type(value) == type(value0)): 00541 myf[param] = value.tolist() 00542 else: 00543 #print 'value:', value, 'value0:', value0 00544 #print 'type(value):', type(value), 'type(value0):', type(value0) 00545 myf[param] = value0 00546 if type(value0) != list : 00547 matchtype = True 00548 else : 00549 myf[param] = value 00550 value = myf['cu'].verifyparam({param:value}) 00551 if matchtype: 00552 value = False 00553 except Exception, instance: 00554 #ignore the exception and just return it unchecked 00555 myf[param] = value 00556 return value 00557 00558 # 00559 # 00560 def description(self, key='setjy', subkey=None): 00561 desc={'setjy': 'Fills the model column with the visibilities of a calibrator', 00562 'vis': 'Name of input visibility file', 00563 'field': 'Field name(s)', 00564 'spw': 'Spectral window identifier (list)', 00565 'selectdata': 'Other data selection parameters', 00566 'timerange': 'Time range to operate on', 00567 'scan': 'Scan number range', 00568 'observation': 'Observation ID range', 00569 'modimage': 'File location for field model', 00570 'listmodels': 'List the available modimages for VLA calibrators or Tb models for Solar System objects', 00571 'scalebychan': 'scale the flux density on a per channel basis or else on a per spw basis', 00572 'fluxdensity': 'Specified flux density [I,Q,U,V]; -1 will lookup values', 00573 'spix': 'Spectral index of fluxdensity', 00574 'reffreq': 'Reference frequency for spix', 00575 'standard': 'Flux density standard', 00576 'useephemdir': 'use directions in the ephemeris table', 00577 'usescratch': 'Will create if necessary and use the MODEL_DATA ', 00578 00579 'async': 'If true the taskname must be started using setjy(...)' 00580 } 00581 00582 # 00583 # Set subfields defaults if needed 00584 # 00585 00586 if(desc.has_key(key)) : 00587 return desc[key] 00588 00589 def itsdefault(self, paramname) : 00590 a = {} 00591 a['vis'] = '' 00592 a['field'] = '' 00593 a['spw'] = '' 00594 a['selectdata'] = False 00595 a['timerange'] = '' 00596 a['scan'] = '' 00597 a['observation'] = '' 00598 a['modimage'] = '' 00599 a['listmodels'] = False 00600 a['scalebychan'] = True 00601 a['fluxdensity'] = -1 00602 a['spix'] = 0.0 00603 a['reffreq'] = '1GHz' 00604 a['standard'] = 'Perley-Butler 2010' 00605 a['useephemdir'] = False 00606 a['usescratch'] = False 00607 00608 if a.has_key(paramname) : 00609 return a[paramname] 00610 setjy_pg = setjy_pg_()
1.8.0
