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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 casac 00010 import string 00011 import time 00012 import inspect 00013 import gc 00014 import numpy 00015 from odict import odict 00016 from taskmanager import tm 00017 from task_setjy import setjy 00018 class setjy_cli_: 00019 __name__ = "setjy" 00020 __async__ = {} 00021 rkey = None 00022 i_am_a_casapy_task = None 00023 # The existence of the i_am_a_casapy_task attribute allows help() 00024 # (and other) to treat casapy tasks as a special case. 00025 00026 def __init__(self) : 00027 self.__bases__ = (setjy_cli_,) 00028 self.__doc__ = self.__call__.__doc__ 00029 00030 self.parameters={'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} 00031 00032 00033 def result(self, key=None): 00034 #### here we will scan the task-ids in __async__ 00035 #### and add any that have completed... 00036 if key is not None and self.__async__.has_key(key) and self.__async__[key] is not None: 00037 ret = tm.retrieve(self.__async__[key]) 00038 if ret['state'] == "done" : 00039 self.__async__[key] = None 00040 elif ret['state'] == 'crashed' : 00041 self.__async__[key] = None 00042 return ret 00043 return None 00044 00045 00046 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): 00047 00048 """Fills the model column with the visibilities of a calibrator 00049 00050 The task sets the model visibility amp and phase of a specified source 00051 (generally a calibrator). The simplest way is to enter the flux density 00052 (I,Q,U,V) explicitly, but this is valid only for a point source. 00053 00054 For an extended source, the clean model (image.model) can be 00055 specified and the model visibilities associated with this clean 00056 model is placed in the visibility model column. 00057 00058 Models are available for 3C48, 3C138, 3C286 between 1.4 and 43 GHz. 00059 3C147 is available above 4 GHz. These models are scaled to the precise 00060 frequency of the data. Only I models are presently available. 00061 00062 The location of the models is system dependent: At the AOC and CV, the 00063 models are in the directory::/usr/lib/casapy/data/nrao/VLA/CalModels or 00064 /usr/lib64/casapy/data/nrao/VLA/CalModels (depending on whether 32 or 64 00065 bit CASA was installed on the machine being used). In general (using 00066 Python), the stock models should be in 00067 casa['dirs']['data'] + '/nrao/VLA/CalModels' 00068 setjy also looks for models in the current directory before trying 00069 casa['dirs']['data'] + '/nrao/VLA/CalModels'. 00070 00071 setjy need only be run on the calibrator sources with a known flux 00072 density and/or model. 00073 00074 00075 Solar System Objects are supported via the 'Butler-JPL-Horizons 2012' 00076 standard. This uses new brightness temperature models and a new flux 00077 calculation code that replace the 'Butler-JPL-Horizons 2010' standard. 00078 The older 'Butler-JPL-Horizons 2010' standard is still available 00079 for comparison. Users may want to use predictcomp task to see the differeces. 00080 Currently they are modeled as uniform temperature disks based 00081 on their ephemerides at the time of observation (note that this may 00082 oversimply objects, in particular asteroids). The object name is 00083 obtained from the 'field' parameter. Recognized objects are listed 00084 below, under 'standard'. 00085 00086 Note that fluxdensity, modimage, and standard interact in a possibly 00087 confusing way! Generally, if fluxdensity[0] (Stokes I) is <= 0, it 00088 will be ignored. If it is < 0, standard (which has a default) will 00089 be used to calculate flux density as a function of frequency, even if 00090 modimage is specified. If is is exactly 0 and modimage is given, the 00091 brightness of the model image will be used as is. If fluxdensity([0]) 00092 is > 0, it will be used. The latter two options come at the price of 00093 disabling frequency scaling, i.e. the same fluxdensity will be used for 00094 all frequencies. 00095 00096 Keyword arguments: 00097 vis -- Name of input visibility file 00098 default: none. example: vis='ngc5921.ms' 00099 field -- Select field using field id(s) or field name(s). 00100 default: ''=all fields, but run setjy one field at a time. 00101 [run listobs to obtain the list id's or names of calibrators] 00102 If field is a non-negative integer, it is assumed to be a field 00103 index. Otherwise, it is taken to be a field name (case sensitive 00104 - it must match the name as listed by listobs). 00105 field='0~2'; field ids 0,1,2 00106 field='0,4,5~7'; field ids 0,4,5,6,7 00107 field='3C286,3C295'; field named 3C286 and 3C295 00108 field = '3,4C*'; field id 3, all names starting with 4C 00109 spw -- Spectral window selection string. 00110 default: '' = all spectral windows 00111 Note that setjy only selects by spectral window, and ignores 00112 channel selections. Fine-grained control could be achieved using 00113 (and possibly constructing) a cube for modimage. 00114 00115 selectdata -- Other parameters for selecting part(s) of the MS 00116 to operate on. 00117 (Currently all time-oriented and most likely only of 00118 interest when using a Solar System object as a calibrator.) 00119 default: False 00120 00121 >>> selectdata=True expandable parameters 00122 See help par.selectdata for more on these. 00123 00124 timerange -- Select data based on time range: 00125 default: '' (all); examples, 00126 timerange = 'YYYY/MM/DD/hh:mm:ss~YYYY/MM/DD/hh:mm:ss' 00127 Note: if YYYY/MM/DD is missing date defaults to first 00128 day in data set 00129 timerange='09:14:0~09:54:0' picks 40 min on first day 00130 timerange='25:00:00~27:30:00' picks 1 hr to 3 hr 00131 30min on NEXT day 00132 timerange='09:44:00' pick data within one integration 00133 of time 00134 timerange='>10:24:00' data after this time 00135 For multiple MS input, a list of timerange strings can be 00136 used: 00137 timerange=['09:14:0~09:54:0','>10:24:00'] 00138 timerange='09:14:0~09:54:0''; apply the same timerange for 00139 all input MSes 00140 scan -- Scan number range. 00141 default: '' (all) 00142 example: scan='1~5' 00143 For multiple MS input, a list of scan strings can be used: 00144 scan=['0~100','10~200'] 00145 scan='0~100; scan ids 0-100 for all input MSes 00146 Check 'go listobs' to insure the scan numbers are in order. 00147 observation -- Observation ID range. 00148 default: '' (all) 00149 example: observation='1~5' 00150 00151 00152 modimage -- Model image (I only) for setting the model visibilities. 00153 modimage can be a cube, and its channels do not have to exactly 00154 match those of vis. It is recommended to use modimage for 00155 sources that are resolved by the observation, but the 00156 Butler-JPL-Horizons standard supplies a basic model of what 00157 several Solar System objects look like. default: '': do not use 00158 a model image. 00159 00160 Each field must be done separately when using a model image. The 00161 flux density of the image will be scaled from the frequency in 00162 the model to that actually used (ignoring fluxdensity), unless 00163 fluxdensity >= 0 (or fluxdensity[0] >= 0). If 00164 fluxdensity([0]) is 0.0, the image's flux density will be used. 00165 If fluxdensity([0]) > 0.0, it will be used (and spix and 00166 reffreq if modimage is not a cube). Since the spectral index 00167 usually varies with direction, applying a single spectral index 00168 to a 2D modimage is typically not as good as using a cube. 00169 00170 Both the amplitude and phase are calculated. At the AOC or CV, 00171 the models are located in casa['dirs']['data'] 00172 + '/nrao/VLA/CalModels/', e.g. 00173 /usr/lib/casapy/data/nrao/VLA/CalModels/3C286_L.im 00174 lib64 00175 00176 If modimage does not start with '/', setjy will look for a match 00177 in '.', './CalModels', and any CalModels directories within 00178 the casa['dirs']['data'] tree (excluding certain branches). 00179 00180 Note that modimage should be deconvolved, i.e. a set of clean 00181 components instead of an image that has been convolved with a 00182 clean beam. 00183 00184 listmodels -- If True, do nothing but list candidates for modimage 00185 (for extragalactic calibrators) that are present on the system. It looks for *.im* *.mod* in ., 00186 CalModels, and CalModels directories in the casa['dirs']['data'] 00187 tree. It does not check whether they are appropriate for the MS! 00188 If standard='Butler-JPL-Horizons 2012', Tb models (frequency-depended 00189 brightness temperature models) for Solar System objects used in the 00190 standard. For standard='Butler-JPL-Horizons 2010', the recognized 00191 Solar System objects are listed. 00192 00193 scalebychan -- This determines whether the fluxdensity set in the model is 00194 calculated on a per channel basis. If False then it only one 00195 fluxdensity value is calculated per spw. (Either way, all channels 00196 in spw are modified.) It is effectively True if fluxdensity[0] > 00197 0.0. 00198 default: True 00199 00200 fluxdensity -- Specified flux density [I,Q,U,V] in Jy 00201 default: -1, uses [1,0,0,0] flux density for unrecognized sources, 00202 and standard flux densities for ones recognized by 'standard', 00203 including 3C286, 3C48, 3C147, and several planets, moons, and 00204 asteroids. setjy will try to use standard if fluxdensity is not 00205 positive. 00206 00207 Only one flux density can be specified at a time. The phases are 00208 set to zero. 00209 example fluxdensity=-1 will use standard for recognized 00210 calibrators (like 3C286, 3C147 and 3C48, depending on 00211 standard) and insert 1.0 for selected fields with 00212 unrecognized sources. 00213 example field = '1'; fluxdensity=[3.2,0,0,0] wil put in 00214 a flux density of I=3.2 for field='1' 00215 00216 At present (June 2000), this is the only method to insert a 00217 polarized flux density model. 00218 example: fluxdensity=[2.63,0.21,-0.33,0.02] 00219 will put in I,Q,U,V flux densities of 2.63,0.21,-0.33, 00220 and 0.02, respectively, in the model column. 00221 00222 spix -- Spectral index for fluxdensity: 00223 S = fluxdensity * (freq/reffreq)**spix 00224 Default: 0 (no effect) 00225 Only used if fluxdensity is being used. 00226 N.B.: If fluxdensity is positive, and spix is nonzero, then reffreq 00227 must be set too! (See below) 00228 00229 It is applied in the same way to all polarizations, and does 00230 not account for Faraday rotation or depolarization. 00231 00232 reffreq -- The reference frequency for spix, given with units. 00233 Default: '1GHz'; this is only here to prevent division by 0! 00234 N.B.: If the flux density is being scaled by spectral index, 00235 then reffreq must be set to whatever reference frequency is 00236 correct for the given fluxdensity and spix. It cannot be 00237 determined from vis. On the other hand, if spix is 0, then any 00238 positive frequency can be used (and ignored). 00239 00240 Examples: '86.0GHz', '4.65e9Hz' 00241 00242 standard -- Flux density standard, used if fluxdensity[0] < 0.0 00243 default: 'Perley-Butler 2010'; example: standard='Baars' 00244 Options: 'Baars','Perley 90','Perley-Taylor 95', 00245 'Perley-Taylor 99', 'Perley-Butler 2010', 'Perley-Butler 2013', 00246 'Butler-JPL-Horizons 2010', and 'Butler-JPL-Horizons 2012'. 00247 All but the last two are for extragalactic calibrators, 00248 and the final two are for Solar System objects. 00249 00250 Extragalactic calibrators: 00251 Following source names and their common aliases are recognized. 00252 The last column shows which standards support for each source. 00253 Note that the task does not do exact matching of the name and 00254 it recognizes as long as the field name contains the string 00255 listed below (e.g. 'PKS 1934-638' works). 00256 ----------------------------------------------------------- 00257 3C Name B1950 Name J2000 Name Alt. J2000 Name standards* 00258 3C48 0134+329 0137+331 J0137+3309 1,3,4,5,6 00259 3C123 0433+295 0437+296 J0437+2940 2 00260 3C138 0518+165 0521+166 J0521+1638 1,3,4,5,6 00261 3C147 0538+498 0542+498 J0542+4951 1,3,4,5,6 00262 3C196 0809+483 0813+482 J0813+4813 1,2 00263 3C286 1328+307 1331+305 J1331+3030 1,2,3,4,5,6 00264 3C295 1409+524 1411+522 J1411+5212 1,2,3,4,5,6 00265 - 1934-638 - J1939-6342 1,3,4,5,6 00266 ----------------------------------------------------------- 00267 * supported in: 1 - Perley-Butler 2010, 2 - Perley-Butler 2013, 00268 3 - Perley-Taylor 99, 4 - Perley-Taylor 95, 5 - Perley 90, 6 - Baars 00269 00270 Solar system objects: 00271 The 'Butler-JPL-Horizons 2012' standard is recommended over 00272 'Butler-JPL-Horizons 2010' as the former uses updated models. 00273 Recognized Solar System objects (for 'Butler-JPL-Horizons 2012') are: 00274 00275 00276 Planets: Venus, Mars, Jupiter, Uranus, Neptune 00277 00278 Moons: Jupiter: Io, Europa, Ganymede, Callisto 00279 Saturn: Titan 00280 00281 Asteroids: Ceres, Pallas**, Vesta**, Juno** 00282 00283 * Venus: model for ~300MHz to 350GHz, no atmospheric lines (CO,H2O,HDO, etc) 00284 * Mars: tabulated as a function of time and frequency (30 - 1000GHz) based on 00285 Rudy el tal (1988), no atmopheric lines (CO, H20, H2O2, HDO, etc) 00286 * Jupiter: model for 30-1020GHz, does not include synchrotron emission 00287 * Uranus: model for 60-1800GHz, contains no rings or synchrotron. 00288 * Neptune: model for 2-2000GHz, the broad CO absorption line 00289 is included, but contains no rings or syncrotron. 00290 * Titan: model for 53.3-1024.1GHz, include many spectral lines 00291 00292 ** not recommended (The temperature is not yet adjusted for 00293 varying distance from the Sun. The model data can be scaled 00294 after running setjy, but it is an involved process.) 00295 00296 The 'field' parameter must match the case of the field name(s) 00297 in vis (as shown by listobs). 00298 00299 Flux density calculation with Solar System objects depends on 00300 ephemerides. The setjy task looks for the data in 00301 00302 os.getenv('CASAPATH').split()[0] + '/data/ephemerides/JPL-Horizons'. 00303 00304 If no ephemeris for the right object at the right time is 00305 present, the calculation will fail. Ask the helpdesk to make an 00306 ephemeris. The very adventurous and well versed in python can 00307 try it using CASA's recipes.ephemerides package: 00308 import recipes.ephemerides as eph 00309 help eph 00310 00311 CASA comes with ephemerides for several more objects, but they 00312 are intended for use with me.framecomet(), and are not (yet) 00313 suitable flux density calibrators. It is up to the observer to 00314 pick a good flux density calibrator (bright, spherical and 00315 featureless, on a circular orbit, in the right part of the sky, 00316 and not too resolved). Even some of the objects listed above 00317 may prove to require more sophisticated flux density models than 00318 are currently implemented in CASA. For many objects running 00319 casalog.filter('INFO1') before running setjy will send more 00320 information to the logger. The cookbook also has an appendix 00321 with descriptions of the models used by setjy (both 00322 extragalactic and Solar System). 00323 00324 >>> standard="Butler-JPL-Horizons 2012" expandable parameter 00325 00326 useephemdir -- If True: use the direction from the ephemeris table for 00327 the solar system object. 00328 default: False -use the direction information in the MS(i.e. Field table) 00329 00330 usescratch -- If False: 'virtual' model is created. The model is saved in the header 00331 and model visibilities are evaluated when calculating calibration or plotting in plotms. 00332 If True: the model visibility will be evaluated and saved on disk in the MODEL_DATA 00333 column. This will increase your ms in size by a factor of 1.5 (w.r.t. the case where 00334 you only have the DATA and the CORRECTED_DATA column). Use True if you need to interact 00335 with the MODEL_DATA in python, say. 00336 00337 *By running usescratch=T, it will remove the existing virtual model from previous runs. 00338 usescratch=F will not remove the existing MODEL_DATA but in subsequent process 00339 the virtual model with matching field and spw combination will be used if it exists 00340 regardless of the presence of the MODEL_DATA column. 00341 00342 default: False 00343 00344 00345 """ 00346 if not hasattr(self, "__globals__") or self.__globals__ == None : 00347 self.__globals__=sys._getframe(len(inspect.stack())-1).f_globals 00348 #casac = self.__globals__['casac'] 00349 casalog = self.__globals__['casalog'] 00350 #casalog = casac.casac.logsink() 00351 self.__globals__['__last_task'] = 'setjy' 00352 self.__globals__['taskname'] = 'setjy' 00353 ### 00354 self.__globals__['update_params'](func=self.__globals__['taskname'],printtext=False,ipython_globals=self.__globals__) 00355 ### 00356 ### 00357 #Handle globals or user over-ride of arguments 00358 # 00359 function_signature_defaults=dict(zip(self.__call__.func_code.co_varnames,self.__call__.func_defaults)) 00360 useLocalDefaults = False 00361 00362 for item in function_signature_defaults.iteritems(): 00363 key,val = item 00364 keyVal = eval(key) 00365 if (keyVal == None): 00366 #user hasn't set it - use global/default 00367 pass 00368 else: 00369 #user has set it - use over-ride 00370 if (key != 'self') : 00371 useLocalDefaults = True 00372 00373 myparams = {} 00374 if useLocalDefaults : 00375 for item in function_signature_defaults.iteritems(): 00376 key,val = item 00377 keyVal = eval(key) 00378 exec('myparams[key] = keyVal') 00379 self.parameters[key] = keyVal 00380 if (keyVal == None): 00381 exec('myparams[key] = '+ key + ' = self.itsdefault(key)') 00382 keyVal = eval(key) 00383 if(type(keyVal) == dict) : 00384 if len(keyVal) > 0 : 00385 exec('myparams[key] = ' + key + ' = keyVal[len(keyVal)-1][\'value\']') 00386 else : 00387 exec('myparams[key] = ' + key + ' = {}') 00388 00389 else : 00390 async = self.parameters['async'] 00391 myparams['vis'] = vis = self.parameters['vis'] 00392 myparams['field'] = field = self.parameters['field'] 00393 myparams['spw'] = spw = self.parameters['spw'] 00394 myparams['selectdata'] = selectdata = self.parameters['selectdata'] 00395 myparams['timerange'] = timerange = self.parameters['timerange'] 00396 myparams['scan'] = scan = self.parameters['scan'] 00397 myparams['observation'] = observation = self.parameters['observation'] 00398 myparams['modimage'] = modimage = self.parameters['modimage'] 00399 myparams['listmodels'] = listmodels = self.parameters['listmodels'] 00400 myparams['scalebychan'] = scalebychan = self.parameters['scalebychan'] 00401 myparams['fluxdensity'] = fluxdensity = self.parameters['fluxdensity'] 00402 myparams['spix'] = spix = self.parameters['spix'] 00403 myparams['reffreq'] = reffreq = self.parameters['reffreq'] 00404 myparams['standard'] = standard = self.parameters['standard'] 00405 myparams['useephemdir'] = useephemdir = self.parameters['useephemdir'] 00406 myparams['usescratch'] = usescratch = self.parameters['usescratch'] 00407 00408 00409 result = None 00410 00411 # 00412 # The following is work around to avoid a bug with current python translation 00413 # 00414 mytmp = {} 00415 00416 mytmp['vis'] = vis 00417 mytmp['field'] = field 00418 mytmp['spw'] = spw 00419 mytmp['selectdata'] = selectdata 00420 mytmp['timerange'] = timerange 00421 mytmp['scan'] = scan 00422 mytmp['observation'] = observation 00423 mytmp['modimage'] = modimage 00424 mytmp['listmodels'] = listmodels 00425 mytmp['scalebychan'] = scalebychan 00426 mytmp['fluxdensity'] = fluxdensity 00427 mytmp['spix'] = spix 00428 mytmp['reffreq'] = reffreq 00429 mytmp['standard'] = standard 00430 mytmp['useephemdir'] = useephemdir 00431 mytmp['usescratch'] = usescratch 00432 pathname='file:///'+os.environ.get('CASAPATH').split()[0]+'/share/xml/' 00433 trec = casac.casac.utils().torecord(pathname+'setjy.xml') 00434 00435 casalog.origin('setjy') 00436 try : 00437 #if not trec.has_key('setjy') or not casac.casac.utils().verify(mytmp, trec['setjy']) : 00438 #return False 00439 00440 casac.casac.utils().verify(mytmp, trec['setjy'], True) 00441 scriptstr=[''] 00442 saveinputs = self.__globals__['saveinputs'] 00443 saveinputs('setjy', 'setjy.last', myparams, self.__globals__,scriptstr=scriptstr) 00444 if async : 00445 count = 0 00446 keybase = time.strftime("%y%m%d.%H%M%S") 00447 key = keybase + "_" + str(count) 00448 while self.__async__.has_key(key) : 00449 count += 1 00450 key = keybase + "_" + str(count) 00451 result = tm.execute('setjy', vis, field, spw, selectdata, timerange, scan, observation, modimage, listmodels, scalebychan, fluxdensity, spix, reffreq, standard, useephemdir, usescratch) 00452 print "Use: " 00453 print " tm.retrieve(return_value) # to retrieve the status" 00454 print 00455 self.rkey = key 00456 self.__async__[key] = result 00457 else : 00458 tname = 'setjy' 00459 spaces = ' '*(18-len(tname)) 00460 casalog.post('\n##########################################'+ 00461 '\n##### Begin Task: ' + tname + spaces + ' #####') 00462 casalog.post(scriptstr[1][1:]+'\n', 'INFO') 00463 result = setjy(vis, field, spw, selectdata, timerange, scan, observation, modimage, listmodels, scalebychan, fluxdensity, spix, reffreq, standard, useephemdir, usescratch) 00464 casalog.post('##### End Task: ' + tname + ' ' + spaces + ' #####'+ 00465 '\n##########################################') 00466 00467 except Exception, instance: 00468 if(self.__globals__.has_key('__rethrow_casa_exceptions') and self.__globals__['__rethrow_casa_exceptions']) : 00469 raise 00470 else : 00471 #print '**** Error **** ',instance 00472 tname = 'setjy' 00473 casalog.post('An error occurred running task '+tname+'.', 'ERROR') 00474 pass 00475 00476 gc.collect() 00477 return result 00478 # 00479 # 00480 # 00481 def paramgui(self, useGlobals=True, ipython_globals=None): 00482 """ 00483 Opens a parameter GUI for this task. If useGlobals is true, then any relevant global parameter settings are used. 00484 """ 00485 import paramgui 00486 if not hasattr(self, "__globals__") or self.__globals__ == None : 00487 self.__globals__=sys._getframe(len(inspect.stack())-1).f_globals 00488 00489 if useGlobals: 00490 if ipython_globals == None: 00491 myf=self.__globals__ 00492 else: 00493 myf=ipython_globals 00494 00495 paramgui.setGlobals(myf) 00496 else: 00497 paramgui.setGlobals({}) 00498 00499 paramgui.runTask('setjy', myf['_ip']) 00500 paramgui.setGlobals({}) 00501 00502 # 00503 # 00504 # 00505 def defaults(self, param=None, ipython_globals=None, paramvalue=None, subparam=None): 00506 if not hasattr(self, "__globals__") or self.__globals__ == None : 00507 self.__globals__=sys._getframe(len(inspect.stack())-1).f_globals 00508 if ipython_globals == None: 00509 myf=self.__globals__ 00510 else: 00511 myf=ipython_globals 00512 00513 a = odict() 00514 a['vis'] = '' 00515 a['field'] = '' 00516 a['spw'] = '' 00517 a['selectdata'] = False 00518 a['modimage'] = '' 00519 a['listmodels'] = False 00520 a['scalebychan'] = True 00521 a['fluxdensity'] = -1 00522 a['standard'] = 'Perley-Butler 2010' 00523 a['usescratch'] = False 00524 00525 a['async']=False 00526 a['selectdata'] = { 00527 0:{'value':False}, 00528 1:odict([{'value':True}, {'timerange':''}, {'scan':''}, {'observation':''}])} 00529 a['fluxdensity'] = { 00530 0:odict([{'notvalue':-1}, {'spix':0}, {'reffreq':'1GHz'}])} 00531 a['standard'] = { 00532 0:{'value':'Perley-Butler 2010'}, 00533 1:{'value':'Perley-Butler 2013'}, 00534 2:{'value':'Perley-Taylor 99'}, 00535 3:{'value':'Baars'}, 00536 4:{'value':'Perley 90'}, 00537 5:{'value':'Perley-Taylor 95'}, 00538 6:odict([{'value':'Butler-JPL-Horizons 2012'}, {'useephemdir':False}]), 00539 7:{'value':'Butler-JPL-Horizons 2010'}} 00540 00541 ### This function sets the default values but also will return the list of 00542 ### parameters or the default value of a given parameter 00543 if(param == None): 00544 myf['__set_default_parameters'](a) 00545 elif(param == 'paramkeys'): 00546 return a.keys() 00547 else: 00548 if(paramvalue==None and subparam==None): 00549 if(a.has_key(param)): 00550 return a[param] 00551 else: 00552 return self.itsdefault(param) 00553 else: 00554 retval=a[param] 00555 if(type(a[param])==dict): 00556 for k in range(len(a[param])): 00557 valornotval='value' 00558 if(a[param][k].has_key('notvalue')): 00559 valornotval='notvalue' 00560 if((a[param][k][valornotval])==paramvalue): 00561 retval=a[param][k].copy() 00562 retval.pop(valornotval) 00563 if(subparam != None): 00564 if(retval.has_key(subparam)): 00565 retval=retval[subparam] 00566 else: 00567 retval=self.itsdefault(subparam) 00568 else: 00569 retval=self.itsdefault(subparam) 00570 return retval 00571 00572 00573 # 00574 # 00575 def check_params(self, param=None, value=None, ipython_globals=None): 00576 if ipython_globals == None: 00577 myf=self.__globals__ 00578 else: 00579 myf=ipython_globals 00580 # print 'param:', param, 'value:', value 00581 try : 00582 if str(type(value)) != "<type 'instance'>" : 00583 value0 = value 00584 value = myf['cu'].expandparam(param, value) 00585 matchtype = False 00586 if(type(value) == numpy.ndarray): 00587 if(type(value) == type(value0)): 00588 myf[param] = value.tolist() 00589 else: 00590 #print 'value:', value, 'value0:', value0 00591 #print 'type(value):', type(value), 'type(value0):', type(value0) 00592 myf[param] = value0 00593 if type(value0) != list : 00594 matchtype = True 00595 else : 00596 myf[param] = value 00597 value = myf['cu'].verifyparam({param:value}) 00598 if matchtype: 00599 value = False 00600 except Exception, instance: 00601 #ignore the exception and just return it unchecked 00602 myf[param] = value 00603 return value 00604 # 00605 # 00606 def description(self, key='setjy', subkey=None): 00607 desc={'setjy': 'Fills the model column with the visibilities of a calibrator', 00608 'vis': 'Name of input visibility file', 00609 'field': 'Field name(s)', 00610 'spw': 'Spectral window identifier (list)', 00611 'selectdata': 'Other data selection parameters', 00612 'timerange': 'Time range to operate on', 00613 'scan': 'Scan number range', 00614 'observation': 'Observation ID range', 00615 'modimage': 'File location for field model', 00616 'listmodels': 'List the available modimages for VLA calibrators or Tb models for Solar System objects', 00617 'scalebychan': 'scale the flux density on a per channel basis or else on a per spw basis', 00618 'fluxdensity': 'Specified flux density [I,Q,U,V]; -1 will lookup values', 00619 'spix': 'Spectral index of fluxdensity', 00620 'reffreq': 'Reference frequency for spix', 00621 'standard': 'Flux density standard', 00622 'useephemdir': 'use directions in the ephemeris table', 00623 'usescratch': 'Will create if necessary and use the MODEL_DATA ', 00624 00625 'async': 'If true the taskname must be started using setjy(...)' 00626 } 00627 00628 # 00629 # Set subfields defaults if needed 00630 # 00631 00632 if(desc.has_key(key)) : 00633 return desc[key] 00634 00635 def itsdefault(self, paramname) : 00636 a = {} 00637 a['vis'] = '' 00638 a['field'] = '' 00639 a['spw'] = '' 00640 a['selectdata'] = False 00641 a['timerange'] = '' 00642 a['scan'] = '' 00643 a['observation'] = '' 00644 a['modimage'] = '' 00645 a['listmodels'] = False 00646 a['scalebychan'] = True 00647 a['fluxdensity'] = -1 00648 a['spix'] = 0.0 00649 a['reffreq'] = '1GHz' 00650 a['standard'] = 'Perley-Butler 2010' 00651 a['useephemdir'] = False 00652 a['usescratch'] = False 00653 00654 #a = sys._getframe(len(inspect.stack())-1).f_globals 00655 00656 if self.parameters['selectdata'] == True: 00657 a['timerange'] = '' 00658 a['scan'] = '' 00659 a['observation'] = '' 00660 00661 if self.parameters['fluxdensity'] != -1: 00662 a['spix'] = 0 00663 a['reffreq'] = '1GHz' 00664 00665 if self.parameters['standard'] == 'Butler-JPL-Horizons 2012': 00666 a['useephemdir'] = False 00667 00668 if a.has_key(paramname) : 00669 return a[paramname] 00670 setjy_cli = setjy_cli_()
1.8.0
