def addPhasePerAntenna(self,phase,antennaId,dataType="DATA"):
"Add a phase (degree) per antennaId. Careful with the order !"
tb.open(self.visName,nomodify=False)
ant1 = tb.getcol("ANTENNA1")
ant2 = tb.getcol("ANTENNA2")
data = tb.getcol(dataType)
phase = DEGREE2RAD*phase
print "Phase rotation: %f"%(phase)
nDim = data.shape
for i in range(nDim[0]):
for j in range(nDim[1]):
for k in range(nDim[2]):
antenna1 = ant1[k]
antenna2 = ant2[k]
if antenna1 == antennaId:
value = data[i][j][k]
real = value.real
image = value.imag
cosRot = math.cos(phase)
sinRot = math.sin(phase)
xRot = cosRot*real-sinRot*image
yRot = sinRot*real+sinRot*image
data[i][j][k] = complex(xRot,yRot)
# print "Amplitude:%f"%(math.sqrt(xRot*xRot+yRot*yRot))
if antenna2 == antennaId:
value = data[i][j][k]
real = value.real
image = value.imag
cosRot = math.cos(-phase)
sinRot = math.sin(-phase)
xRot = cosRot*real-sinRot*image
yRot = sinRot*real+sinRot*image
data[i][j][k] = complex(xRot,yRot)
# print "Amplitude:%f"%(math.sqrt(xRot*xRot+yRot*yRot))
tb.putcol(dataType,data)
tb.close()
def goodenough_field_solutions(tablename,
minsnr=5,
maxphasenoise=np.pi / 4.,
pols=[0]):
"""
After an initial self-calibration run, determine which fields have good
enough solutions. This only inspects the *phase* component of the
solutions.
Parameters
----------
tablename : str
The name of the calibration table (e.g., phase.cal)
minsnr : float
The minimum *average* signal to noise ratio for a given field
maxphasenoise : float
The maximum average phase noise permissible for a given field in
radians
pols : list
The list of polarizations to include in the heuristics
Returns
-------
An array of field IDs. This will need to be converted to a list of strings
for use in CASA tasks
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
fields = tb.getcol('FIELD_ID')
snr = tb.getcol('SNR')
tb.close()
all_angles = []
all_snrs = []
ufields = np.unique(fields)
for field in ufields:
sel = fields == field
angles = np.angle(solns[:, :, sel])
all_angles.append(angles)
all_snrs.append(snr[:, :, sel])
all_angles = np.array(all_angles)
all_snrs = np.array(all_snrs)
# not sure what 2nd column of these is...
# first is mean across pols, then mean across all data points
good_enough = (
(all_snrs[:, pols, 0, :].mean(axis=1).mean(axis=1) > minsnr) &
(all_angles[:, pols, 0, :].std(axis=2).mean(axis=1) < maxphasenoise))
return ufields[good_enough]
def pixelmask2cleanmask(imagename='',
maskname='mask0',
maskimage='',
usemasked=False):
"""
convert pixel(T/F) mask (in a CASA image) to a mask image (1/0)
used for clean
imagename - input imagename that contain a mask to be used
maskname - mask name in the image (default: mask0)
maskimage - output mask image name
usemasked - if True use masked region as a valid region
"""
ia.open(imagename)
masks = ia.maskhandler('get')
ia.close()
inmaskname = ''
if type(masks) != list:
masks = [masks]
for msk in masks:
if maskname == msk:
inmaskname = msk
break
if inmaskname == '':
raise Exception, "mask %s does not exist. Available masks are: %s" % (
maskname, masks)
tb.open(imagename + '/' + maskname)
dat0 = tb.getcol('PagedArray')
tb.close()
#os.system('cp -r %s %s' % (imagename, maskimage))
shutil.copytree(imagename, maskimage)
ia.open(maskimage)
# to unset mask
ia.maskhandler('set', [''])
# make all valid
if (usemasked):
ia.set(1)
else:
ia.set(0)
ia.close()
#
tb.open(maskimage, nomodify=False)
imd = tb.getcol('map')
# maybe shape check here
#by default use True part of bool mask
masked = 1
if (usemasked): masked = 0
imd[dat0] = masked
tb.putcol('map', imd)
tb.close()
def goodenough_field_solutions(tablename, minsnr=5, maxphasenoise=np.pi/4.,
pols=[0]):
"""
After an initial self-calibration run, determine which fields have good
enough solutions. This only inspects the *phase* component of the
solutions.
Parameters
----------
tablename : str
The name of the calibration table (e.g., phase.cal)
minsnr : float
The minimum *average* signal to noise ratio for a given field
maxphasenoise : float
The maximum average phase noise permissible for a given field in
radians
pols : list
The list of polarizations to include in the heuristics
Returns
-------
An array of field IDs. This will need to be converted to a list of strings
for use in CASA tasks
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
fields = tb.getcol('FIELD_ID')
snr = tb.getcol('SNR')
tb.close()
all_angles = []
all_snrs = []
ufields = np.unique(fields)
for field in ufields:
sel = fields==field
angles = np.angle(solns[:,:,sel])
all_angles.append(angles)
all_snrs.append(snr[:,:,sel])
all_angles = np.array(all_angles)
all_snrs = np.array(all_snrs)
# not sure what 2nd column of these is...
# first is mean across pols, then mean across all data points
good_enough = ((all_snrs[:,pols,0,:].mean(axis=1).mean(axis=1) > minsnr) &
(all_angles[:,pols,0,:].std(axis=2).mean(axis=1) < maxphasenoise))
return ufields[good_enough]
def pixelmask2cleanmask(imagename='',maskname='mask0',maskimage='',usemasked=False):
"""
convert pixel(T/F) mask (in a CASA image) to a mask image (1/0)
used for clean
imagename - input imagename that contain a mask to be used
maskname - mask name in the image (default: mask0)
maskimage - output mask image name
usemasked - if True use masked region as a valid region
"""
ia.open(imagename)
masks=ia.maskhandler('get')
ia.close()
inmaskname=''
if type(masks)!=list:
masks=[masks]
for msk in masks:
if maskname == msk:
inmaskname=msk
break
if inmaskname=='':
raise Exception, "mask %s does not exist. Available masks are: %s" % (maskname,masks)
tb.open(imagename+'/'+maskname)
dat0=tb.getcol('PagedArray')
tb.close()
#os.system('cp -r %s %s' % (imagename, maskimage))
shutil.copytree(imagename,maskimage)
ia.open(maskimage)
# to unset mask
ia.maskhandler('set',[''])
# make all valid
if (usemasked):
ia.set(1)
else:
ia.set(0)
ia.close()
#
tb.open(maskimage,nomodify=False)
imd=tb.getcol('map')
# maybe shape check here
#by default use True part of bool mask
masked=1
if (usemasked): masked=0
imd[dat0]=masked
tb.putcol('map',imd)
tb.close()
def goodenough_field_solutions(tablename,
minsnr=5,
maxphasenoise=np.pi / 4.,
pols=[0]):
"""
After an initial self-calibration run, determine which fields have good
enough solutions. This only inspects the *phase* component of the
solutions.
Parameters
----------
tablename : str
The name of the calibration table (e.g., phase.cal)
minsnr : float
The minimum *average* signal to noise ratio for a given field
maxphasenoise : float
The maximum average phase noise permissible for a given field in
radians
pols : list
The list of polarizations to include in the heuristics
Returns
-------
An array of field IDs. This will need to be converted to a list of strings
for use in CASA tasks
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
fields = tb.getcol('FIELD_ID')
snr = tb.getcol('SNR')
tb.close()
okfields = []
not_ok_fields = []
ufields = np.unique(fields)
for field in ufields:
sel = fields == field
angles = np.angle(solns[:, :, sel])
field_ok = (angles.std() < maxphasenoise) & (snr[:, :, sel].mean() >
minsnr)
if field_ok:
okfields.append(field)
else:
not_ok_fields.append(field)
return okfields, not_ok_fields
def getobstimes(caltable):
"""
Converts observation times from measurement set to a format that can be read by plotcal
"""
tb.open(caltable + "/OBSERVATION")
start, end = tb.getcol("TIME_RANGE")
outputtimes = []
for i in range(len(start)):
starttime = qa.quantity(start[i], 's')
convertedstarttime = str(qa.time(starttime, form='ymd')[0])
endtime = qa.quantity(end[i], 's')
convertedendtime = str(qa.time(endtime, form='ymd')[0])
outputtimes.append(convertedstarttime + '~' + convertedendtime)
return outputtimes
def goodenough_field_solutions(tablename, minsnr=5, maxphasenoise=np.pi/4.,
pols=[0]):
"""
After an initial self-calibration run, determine which fields have good
enough solutions. This only inspects the *phase* component of the
solutions.
Parameters
----------
tablename : str
The name of the calibration table (e.g., phase.cal)
minsnr : float
The minimum *average* signal to noise ratio for a given field
maxphasenoise : float
The maximum average phase noise permissible for a given field in
radians
pols : list
The list of polarizations to include in the heuristics
Returns
-------
An array of field IDs. This will need to be converted to a list of strings
for use in CASA tasks
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
fields = tb.getcol('FIELD_ID')
snr = tb.getcol('SNR')
tb.close()
okfields=[]
not_ok_fields = []
ufields = np.unique(fields)
for field in ufields:
sel = fields==field
angles = np.angle(solns[:,:,sel])
field_ok = (angles.std() < maxphasenoise) & (snr[:,:,sel].mean() > minsnr)
if field_ok:
okfields.append(field)
else:
not_ok_fields.append(field)
return okfields, not_ok_fields
def __readUVW(self):
"""Read the UVW data from the MS. Works fine for a simulation (simdata).
To Be Checked for a real obs. with different targets."""
ms.open(self.vis)
uvw=ms.getdata(['amplitude','u','v','w'])
ms.done()
tb.open(self.vis)
self.f=tb.getcol('FLAG_ROW')
self.ff=tb.getcol('FLAG')
tb.done()
self.u=uvw['u']
self.v=uvw['v']
self.w=uvw['w']
self.amp=uvw['amplitude']
def parseflux(self, gainfile):
"""Takes CASA cal table and scales self.gain to it per spw,pol
"""
tb.open(gainfile)
mjd = tb.getcol('TIME')/(24*3600) # mjd days, as for telcal
spw = tb.getcol('SPECTRAL_WINDOW_ID')
antnum = tb.getcol('ANTENNA1')
gain = tb.getcol('CPARAM') # dimensions of (npol, 1?, ntimes*nants)
flagged = tb.getcol('FLAG')
tb.close()
nants = len(n.unique(antnum))
nspw = len(n.unique(spw))
spwlist = n.unique(spw)
npol = len(gain)
# merge times less than 2s
nsol = 0
newmjd = [n.unique(mjd)[0]]
for i in range(1, len(n.unique(mjd))):
if 24*3600*(n.unique(mjd)[i] - n.unique(mjd)[i-1]) < 2.:
print 'Flux solution at %.5f closer than 1s to previous. Skipping.' % (n.unique(mjd)[i])
continue
else:
newmjd.append(n.unique(mjd)[i])
uniquemjd = n.array(newmjd)
nsol = len(uniquemjd)
print 'Parsed flux table solutions for %d solutions, %d ants, %d spw, and %d pols' % (nsol, nants, nspw, npol)
flux = n.zeros( (nsol, nants, nspw, npol), dtype='complex' )
flags = n.zeros( (nsol, nants, nspw, npol), dtype='complex' )
for sol in range(nsol):
for ant in range(nants):
for spw in range(nspw):
for pol in range(npol):
flux[sol, ant, spw, pol] = gain[pol,0,spw*nsol*nants+sol*nants+ant]
flags[sol, ant, spw, pol] = flagged[pol,0,spw*nsol*nants+sol*nants+ant]
flux = n.ma.masked_array(flux, flags)
ampref = n.abs(flux).mean(axis=1)
scale = ampref/n.abs(self.gain).mean(axis=1)
self.gain = self.gain * scale[:,None,:,:]
def bandpass_normalize(bandpass_table, bandpass_table_inv):
shutil.copytree(bandpass_table, bandpass_table_inv)
tb.open(bandpass_table_inv, nomodify=False)
gain = tb.getcol('CPARAM')
gain_norm = gain
#for each antenna and for each channel of the bandpass I divide out by the modulo of the complex number
for i in range(0, gain.shape[2]):
for j in range(0, gain.shape[1]):
a = gain[0, j, i]
#if the real part of the antenna gain is set to 1 it means that that antenna a/o channel is flag, so don't bother looking at it
if a.real != 1:
gain_norm[0, j, i] = gain_norm[0, j, i] / abs(gain_norm[0, j, i])
gain_norm[1, j, i] = gain_norm[1, j, i] / abs(gain_norm[1, j, i])
# print abs(gain_norm[i,j,0]),abs(gain[i,j,0]),i,j
# put back the normalized bandpass
tb.putcol('CPARAM', gain_norm)
tb.close()
tb.done()
def flag_extreme_amplitudes(tablename, maxpctchange=50, pols=[0], channels=[0]):
"""
Flag out all gain amplitudes with >``maxpctchange``% change (e.g., for the
default 50%, flag everything outside the range 0.5 < G < 1.5). This is a
*very simple* cut, but it cannot be easily applied with existing tools
since it is cutting on the value of the amplitude correction, not on any
particular normal data selection type. It is still highly advisable to
plot the amp vs snr or similar diagnostics after running this to make sure
you understand what's going on. For example, after I ran this on a data
set, I discovered that one antenna had high gain corrections even in the
high SNR regime, which probably indicates a problem with that antenna.
Parameters
----------
maxpctchange : float
The maximum percent change permitted in an amplitude
pols : list
The list of polarizations to include in the heuristics
channels : list
The list of channels to include in the heuristics
Returns
-------
None
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
snr = tb.getcol('SNR')
# true flag = flagged out, bad data
flags = tb.getcol('FLAG')
tb.close()
amp = np.abs(solns)
maxfrac = maxpctchange / 100.
bad = ((amp[pols, channels] > (1+maxfrac)) |
(amp[pols, channels] < (1-maxfrac)))
bad_snr = snr[pols, channels, :][bad]
print("Found {0} bad amplitudes with mean snr={1}".format(bad.sum(), bad_snr.mean()))
print("Total flags in tb.flag: {0}".format(flags.sum()))
flags[pols, channels, :] = bad | flags[pols, channels, :]
assert all(flags[pols, channels, :][bad]), "Failed to modify array"
tb.open(tablename, nomodify=False)
tb.putcol(columnname='FLAG', value=flags)
tb.flush()
tb.close()
tb.open(tablename, nomodify=True)
flags = tb.getcol('FLAG')
print("Total flags in tb.flag after: {0}".format(flags.sum()))
assert all(flags[pols, channels, :][bad]), "Failed to modify table"
tb.close()
def LSRKvel_to_chan(msfile, field, spw, restfreq, LSRKvelocity):
"""
Identifies the channel(s) corresponding to input LSRK velocities.
Useful for choosing which channels to split out or flag if a line is expected to be present
Parameters:
msfile: Name of measurement set (string)
spw: Spectral window number (int)
restfreq: Rest frequency in Hz (float)
LSRKvelocity: input velocity in LSRK frame in km/s (float or array of floats)
Returns:
Channel number most closely corresponding to input LSRK velocity
"""
tb.open(msfile + "/SPECTRAL_WINDOW")
chanfreqs = tb.getcol("CHAN_FREQ", startrow=0, nrow=1)
tb.close()
tb.open(msfile + "/FIELD")
fieldnames = tb.getcol("NAME")
tb.close()
nchan = len(chanfreqs)
ms.open(msfile)
lsrkfreqs = ms.cvelfreqs(spwids=[spw],
fieldids=np.where(fieldnames == field)[0][0],
mode='channel',
nchan=nchan,
start=0,
outframe='LSRK')
chanvelocities = (
restfreq - lsrkfreqs
) / restfreq * cc / 1.e3 #converted to LSRK velocities in km/s
if type(LSRKvelocity) == np.ndarray:
outchans = np.zeros_like(LSRKvelocity)
for i in range(len(LSRKvelocity)):
outchans[i] = np.argmin(np.abs(chanvelocities - LSRKvelocity[i]))
return outchans
else:
return np.argmin(np.abs(chanvelocities - LSRKvelocity))
def parsegain(self, gainfile):
"""Takes .g1 CASA cal table and places values in numpy arrays.
"""
tb.open(gainfile)
mjd = tb.getcol('TIME')/(24*3600) # mjd days, as for telcal
spw = tb.getcol('SPECTRAL_WINDOW_ID')
antnum = tb.getcol('ANTENNA1')
gain = tb.getcol('CPARAM') # dimensions of (npol, 1?, ntimes*nants)
snr = tb.getcol('SNR')
flagged = tb.getcol('FLAG')
tb.close()
# # need to find parent data MS to get some metadata
# mslist = glob.glob(gainfile[:-3] + '*.ms')
# try:
# msfile = mslist[0]
# print 'Found parent data MS %s' % msfile
# except IndexError:
# print 'Could not find parent data MS for metadata...'
# tb.open(msfile + '/ANTENNA')
# antname = tb.getcol('NAME') # one name per ant
# tb.close()
# tb.open(msfile + '/SPECTRAL_WINDOW')
# reffreq = 1e-6*(tb.getcol('REF_FREQUENCY')+tb.getcol('TOTAL_BANDWIDTH')/2) # similar to telcal "skyfreq"
# specname = tb.getcol('NAME')
# tb.close()
# tb.open(msfile + '/SOURCE')
# source = [name for name in tb.getcol('NAME') if 'J' in name][0] # should return single cal name **hack**
# tb.close()
# nsol = len(gain[0,0])
# ifid0R = specname[0][7] + '-' + specname[0][8] # one value
# ifid0L = specname[0][9] + '-' + specname[0][10] # one value
# ifid1R = specname[1][7] + '-' + specname[1][8] # one value
# ifid1L = specname[1][9] + '-' + specname[1][10] # one value
# # paste R,L end to end, so first loop over time, then spw, then pol
# mjd = n.concatenate( (time, time), axis=0)
# ifid = [ifid0R]*(nsol/2) + [ifid1R]*(nsol/2) + [ifid0L]*(nsol/2) + [ifid1L]*(nsol/2) # first quarter is spw0,pol0, then spw1,pol0, ...
# skyfreq = n.concatenate( (reffreq[0]*n.ones(nsol/2), reffreq[1]*n.ones(nsol/2), reffreq[0]*n.ones(nsol/2), reffreq[1]*n.ones(nsol/2)), axis=0)
# gain = n.concatenate( (gain[0,0],gain[1,0]), axis=0)
# amp = n.abs(gain)
# phase = n.degrees(n.angle(gain))
# source = [source]*nsol*2
# flagged = n.concatenate( (flag[0,0],flag[1,0]), axis=0)
nants = len(n.unique(antnum))
nspw = len(n.unique(spw))
self.spwlist = n.unique(spw)
npol = len(gain)
# merge times less than 2s
nsol = 0
newmjd = [n.unique(mjd)[0]]
for i in range(1, len(n.unique(mjd))):
if 24*3600*(n.unique(mjd)[i] - n.unique(mjd)[i-1]) < 2.:
print 'Gain solution at %.5f closer than 2s to previous. Skipping.' % (n.unique(mjd)[i])
continue
else:
newmjd.append(n.unique(mjd)[i])
self.uniquemjd = n.array(newmjd)
nsol = len(self.uniquemjd)
print 'Parsed gain table solutions for %d solutions, %d ants, %d spw, and %d pols' % (nsol, nants, nspw, npol)
print 'Unique solution times', self.uniquemjd
self.gain = n.zeros( (nsol, nants, nspw, npol), dtype='complex' )
flags = n.zeros( (nsol, nants, nspw, npol), dtype='complex' )
for sol in range(nsol):
for ant in range(nants):
for spw in range(nspw):
for pol in range(npol):
self.gain[sol, ant, spw, pol] = gain[pol,0,spw*nsol*nants+sol*nants+ant]
flags[sol, ant, spw, pol] = flagged[pol,0,spw*nsol*nants+sol*nants+ant]
self.gain = n.ma.masked_array(self.gain, flags)
# gain = n.concatenate( (n.concatenate( (gain[0,0,:nants*nsol].reshape(nsol,nants,1,1), gain[1,0,:nants*nsol].reshape(nsol,nants,1,1)), axis=3), n.concatenate( (gain[0,0,nants*nsol:].reshape(nsol,nants,1,1), gain[1,0,nants*nsol:].reshape(nsol,nants,1,1)), axis=3)), axis=2)
# flagged = n.concatenate( (n.concatenate( (flagged[0,0,:nants*nsol].reshape(nsol,nants,1,1), flagged[1,0,:nants*nsol].reshape(nsol,nants,1,1)), axis=3), n.concatenate( (flagged[0,0,nants*nsol:].reshape(nsol,nants,1,1), flagged[1,0,nants*nsol:].reshape(nsol,nants,1,1)), axis=3)), axis=2)
# self.gain = n.ma.masked_array(gain, flagged == True)
self.mjd = n.array(mjd); self.antnum = antnum
def ms2ripples(vis,
savepath,
timebinsec,
Nsam=None,
timebin=False,
overwrite=True,
verbose=True,
debug=False):
import astropy.constants as c
if timebin:
print("Performing time binning, by {:}s:".format(timebinsec))
prefix = vis.replace('.ms', '_timebin' + '{:}s.ms'.format(timebinsec))
prefix = os.path.basename(prefix)
timebinVis = os.path.join(savepath, prefix)
if overwrite:
rmtables(timebinVis)
default(split2)
split2(vis=vis,
timebin=str(timebinsec) + 's',
outputvis=timebinVis,
datacolumn='data',
keepflags=False)
if overwrite:
plotms(vis=timebinVis,
xaxis='uvdist',
yaxis='amp',
coloraxis='spw')
if debug and not os.path.exists(
timebinVis[:timebinVis.find('.ms')] + '.image'):
clean(vis=timebinVis,
imagename=timebinVis[:timebinVis.find('.ms')],
spw='',
mode='mfs',
nchan=-1,
imsize=800,
cell='0.0300arcsec',
niter=0,
interactive=False,
stokes='I')
oldvis = vis
vis = timebinVis
else:
raw_input(
"No time binning...proceed with caution. Press Enter to continue.")
# check that the MS has only 1 science target
tb.open(timebinVis + '/FIELD')
src = tb.getcell('NAME')
print("Source in {}: {}\n").format(timebinVis, src)
tb.close()
ms.open(timebinVis)
spwInfo = ms.getspectralwindowinfo()
nchan = spwInfo["0"]["NumChan"]
npol = spwInfo["0"]["NumCorr"]
ms.close()
tb.open(oldvis)
_dataShape = tb.getcol('DATA').shape
tb.close()
tb.open(timebinVis)
# tb.colnames
data = tb.getcol('DATA')
uvw = tb.getcol('UVW')
uvwShape = uvw.shape
nvis = len(uvw[1, :]) # before dropping flagged data
flagRow = tb.getcol('FLAG_ROW')
assert (flagRow == True).any() == False
data_desc_id = tb.getcol("DATA_DESC_ID")
sigma = tb.getcol('SIGMA')
# weight = tb.getcol('WEIGHT')
weight = 1. / sigma**2
# del sigma
if Nsam is not None:
from ripples_utils import pick_highSNR
idx = pick_highSNR(weight, Nsam, plothist=verbose)
uvw = uvw[:, idx]
with open(os.path.join(savepath, 'u.bin'), 'wb') as f:
f.write(uvw[0, :])
with open(os.path.join(savepath, 'v.bin'), 'wb') as f:
f.write(uvw[1, :])
if debug:
print uvw[0, :].max()
print uvw[0, :].min()
print uvw[1, :].max()
print uvw[1, :].min()
print uvw.dtype # float64
# del uvw
ant1 = tb.getcol('ANTENNA1')
ant2 = tb.getcol('ANTENNA2')
assert len(ant1) == nvis
assert len(ant2) == nvis
tb.done()
if Nsam is not None:
ant1 = ant1[idx]
ant2 = ant2[idx]
assert len(ant1) == len(uvw[0, :])
with open(os.path.join(savepath, 'ant1.bin'), 'wb') as f:
ant1 = np.asarray(ant1, dtype=np.float_)
# print ant1.dtype
f.write(ant1)
with open(os.path.join(savepath, 'ant2.bin'), 'wb') as f:
ant2 = np.asarray(ant2, dtype=np.float_)
f.write(ant2)
# ant1.tofile(os.path.join(savepath, 'ant1.bin'))
if debug:
print ant1.max()
print ant1.min()
print ant2.max()
print ant2.min()
xx = np.fromfile(os.path.join(savepath, 'ant1.bin'))
if Nsam is None:
assert len(xx) == nvis
else:
assert len(xx) == len(idx)
assert (xx == ant1).all()
xx = np.fromfile(os.path.join(savepath, 'ant2.bin'))
if Nsam is None:
assert len(xx) == nvis
else:
assert len(xx) == len(idx)
assert (xx == ant2).all()
# del ant1, ant2
if verbose:
print("Number of coorelation: ", npol)
print("data shape", data.shape)
print("data shape before time binning", _dataShape)
print("uvw shape", uvwShape)
print("weight shpae", weight.shape) # (npol, nvis)
tb.open(vis + '/SPECTRAL_WINDOW')
SPWFreqs = np.squeeze(tb.getcol("CHAN_FREQ"))
tb.done()
freq_per_vis = np.array([SPWFreqs[fff] for fff in data_desc_id])
# freqs = np.mean(SPWFreqs)
assert len(freq_per_vis) == nvis
if Nsam is not None:
freq_per_vis = freq_per_vis[idx]
with open(os.path.join(savepath, 'frequencies.bin'), 'wb') as f:
f.write(freq_per_vis)
del data_desc_id, SPWFreqs
if Nsam is not None:
data = data[:, :, idx]
weight = weight[:, idx]
if debug:
# randomly sample 1000 to image
from ripples_utils import calc_img_from_vis
_idx = np.random.choice(len(weight[0, :]), size=3000)
if npol == 2:
if data.shape[1] == 1:
# expand the channel axis for weight
__weight = weight[:, np.newaxis, :]
_data = np.average(data, weights=__weight, axis=0)
_weight = np.average(weight, axis=0) # npol, nvis
print _weight.shape
print _data.shape
_real = _data[0, _idx].real # nchan, nvis
_imag = _data[0, _idx].imag
visOut = np.array(zip(_real, _imag)).flatten()
_weight = _weight[_idx]
__weight_factor = len(_idx) / np.sum(_weight * _real**2 +
_weight * _imag**2)
print __weight_factor
_weight *= __weight_factor
test_img = calc_img_from_vis(uvw[0, _idx],
uvw[1, _idx],
_weight,
visOut,
freq_per_vis[_idx],
800,
pixsize=0.01)
import pdb
pdb.set_trace()
if npol == 1:
real = data.real
imag = data.imag
elif npol == 2:
print "Real and Imag shape before averaging two hands (npol, nchan, nvis): ", data.real.shape
if data.shape[1] == 1:
# expand the channel axis for weight
weight = weight[:, np.newaxis, :]
else:
print weight.shape
print("We shouldn't have to enter this condition.")
import pdb
pdb.set_trace()
# average the two hands
data = np.average(data, weights=weight, axis=0)
# print data.shape (nchan, nvis)
weight = np.average(weight, axis=0)
print weight.shape # should be (nchan, nvis)
real = data.real
imag = data.imag
del data
print "Shape after averaging two hands: ", real.shape
elif npol > 2:
raise NotImplementedError("more than 2 hands..")
# rescale weight
# uvmcmcfit way
if Nsam is None:
_factor = nvis / np.sum(weight * real**2 + weight * imag**2)
else:
_factor = len(idx) / np.sum(weight * real**2 + weight * imag**2)
_sigmas = (weight**-0.5) * _factor
if verbose:
print "simple rescale, factor of: ", _factor
print _sigmas.min(), _sigmas.max(), _sigmas.std()
print "New sigma in [mjy/beam]", (_sigmas**-2).sum()**-0.5 * 1.e3
del _sigmas
# Yashar way
# first grouping the visibilities into bins that probe the same signal
# take differences btw visibilities that null the sky
# then, we simply assume that the variance in the subtracted visibilities is equal to twice the noise variance
plotms(timebinVis, xaxis='V', yaxis='U', coloraxis='baseline')
scaling = []
for a1 in np.unique(ant1):
for a2 in np.unique(ant2):
if a1 < a2:
baselineX = (ant1 == a1) & (ant2 == a2)
if debug:
print a1, a2
print ant1, ant2
print ""
print a1 in ant1
print a2 in ant2
print ""
print np.where(a1 == ant1)
print np.where(a2 == ant2)
print np.where((ant1 == a1) & (ant2 == a2) == True)
if baselineX.any(
) == True: # important line! if we are picking a subset of points with nsam since we may miss some baselines.
if nchan == 1:
print real.shape
reals = real[0, baselineX]
imags = imag[0, baselineX]
sigs = weight[0, baselineX]**-0.5
else:
raise NotImplementedError(
"Not implemented for MS files with more than 1 channel per spw..."
)
# randomly split points into "two sets"
# subtract from "two set"
# subtract from neighboring
diffrs = reals - np.roll(reals, -1)
diffis = imags - np.roll(imags, -1)
std = np.mean([diffrs.std(), diffis.std()])
if debug:
print diffrs.min(), diffis.min()
print diffrs.max(), diffis.max()
print diffrs.std(), diffis.std()
print std / sigs.mean() / np.sqrt(2)
scaling.append(std / sigs.mean() / np.sqrt(2))
del ant1, ant2
sigma = weight**-0.5
scaling = np.asarray(scaling).mean()
sigma *= scaling
print 'Scaling factor: ', scaling
print 'Sigma after scaling [mJy/beam]: ', ((sigma**-2).sum())**-0.5 * 1E+3
# real_1, imag_1, real_2, imag_2, etc
visOut = np.array(zip(real, imag)).flatten()
if Nsam is None:
assert len(visOut) == int(nvis * 2)
weight = sigma**-2
weight = np.array(zip(
weight,
weight)).flatten() # TODO: want to make sure this works for nchan > 1
assert len(weight) == len(visOut)
if Nsam is not None:
assert len(visOut) == Nsam * 2
if Nsam is not None:
assert len(weight) == Nsam * 2
with open(os.path.join(savepath, 'vis_chan_0.bin'), 'wb') as f:
f.write(visOut)
with open(os.path.join(savepath, 'sigma_squared_inv.bin'), 'wb') as f:
f.write(weight)
if Nsam is None:
blah = np.zeros((nvis))
else:
blah = np.zeros((len(idx)))
with open(os.path.join(savepath, 'chan.bin'), 'wb') as f:
f.write(blah)
if debug:
# image the SAVED visibilities
uu = np.fromfile(os.path.join(savepath, 'u.bin'), 'wb')
vv = np.fromfile(os.path.join(savepath, 'v.bin'), 'wb')
weight = np.fromfile(os.path.join(savepath, 'sigma_squared_inv.bin'),
'wb')
visout = np.fromfile(os.path.join(savepath, 'vis_chan_0.bin'), 'wb')
calc_img_from_vis(uu, vv, weight, visOut, 1000, pixsize=0.05)
return None
#
if first_pass == 1:
#
# specific PAPER options
#
#cmd = 'rm -rf '+filename
#os.system(cmd)
#cmd = 'python /home/gianni/Python_code/swap_column.py /home/gianni/PAPER/psa32/data/Original/'+filename+' '+filename
#os.system(cmd)
#ft(vis=filename,model='First_model/2455819.50285.model',usescratch=True)
#
cmd = 'rm -rf ' + filename
os.system(cmd)
cmd = 'cp -r /home/gianni/PAPER/psa32/data/Original/'+ filename + ' ' + filename
os.system(cmd)
tb.open(filename,nomodify=False)
data = tb.getcol('DATA')
tb.putcol('CORRECTED_DATA',data) # the CORRECTED_DATA column is initialized to DATA
tb.close()
tb.done()
#
tflagdata(vis=filename,mode='manual',spw='0:167~202',action='apply',datacolumn='DATA')
flagdata(vis=filename,mode='clip',clipminmax=[0,300],correlation='ABS_XY,YX',action='apply',datacolumn='DATA')
flagdata(vis=filename,mode='clip',clipminmax=[0,1000],correlation='ABS_XX,YY',action='apply',datacolumn='DATA')
#
out_fits = lst+'.fits'
out_fits_res = lst+'_residual.fits'
out_fits_model = lst+'_model.fits'
#
cmd = 'rm -rf '+ lst + '.image ' + lst + '.model ' + lst + '.residual ' + lst + '.flux' + lst + '.psf'
os.system(cmd)
def fill_flagged_soln(caltable='', doplot=False):
"""
This is to replace the gaincal solution of flagged/failed solutions by the nearest valid
one.
If you do not do that and applycal blindly with the table your data gets
flagged between calibration runs that have a bad/flagged solution at one edge.
Can be pretty bad when you calibrate every hour or more
(when you are betting on self-cal) of observation (e.g L-band of the EVLA)..one can
lose the whole hour of good data without realizing !
"""
tb.open(caltable, nomodify=False)
flg=tb.getcol('FLAG')
sol=tb.getcol('SOLUTION_OK')
ant=tb.getcol('ANTENNA1')
gain=tb.getcol('GAIN')
t=tb.getcol('TIME')
dd=tb.getcol('CAL_DESC_ID')
maxant=np.max(ant)
maxdd=np.max(dd)
npol=len(gain[:,0,0])
nchan=len(gain[0,:,0])
k=1
if(doplot):
pl.ion()
pl.figure(1)
pl.plot(t[(ant==k)], sol[0,0,(ant==k)], 'b+')
pl.plot(t[(ant==k)], flg[0,0,(ant==k)], 'r+')
pl.twinx()
pl.plot(t[(ant==k)], abs(gain[0,0,(ant==k)]), 'go')
print 'maxant', maxant
numflag=0.0
for k in range(maxant+1):
for j in range (maxdd+1):
subflg=flg[:,:,(ant==k) & (dd==j)]
subt=t[(ant==k) & (dd==j)]
subsol=sol[:,:,(ant==k) & (dd==j)]
subgain=gain[:,:,(ant==k) & (dd==j)]
#print 'subgain', subgain.shape
for kk in range(1, len(subt)):
for chan in range(nchan):
for pol in range(npol):
if(subflg[pol,chan,kk] and not subflg[pol,chan,kk-1]):
numflag += 1.0
subflg[pol,chan,kk]=False
subsol[pol, chan, kk]=True
subgain[pol,chan,kk]=subgain[pol,chan,kk-1]
if(subflg[pol,chan,kk-1] and not subflg[pol,chan,kk]):
numflag += 1.0
subflg[pol,chan,kk-1]=False
subsol[pol, chan, kk-1]=True
subgain[pol,chan,kk-1]=subgain[pol,chan,kk]
flg[:,:,(ant==k) & (dd==j)]=subflg
sol[:,:,(ant==k) & (dd==j)]=subsol
gain[:,:,(ant==k) & (dd==j)]=subgain
print 'numflag', numflag
if(doplot):
pl.figure(2)
k=1
#pl.clf()
pl.plot(t[(ant==k)], sol[0,0,(ant==k)], 'b+')
pl.plot(t[(ant==k)], flg[0,0,(ant==k)], 'r+')
pl.twinx()
pl.plot(t[(ant==k)], abs(gain[0,0,(ant==k)]), 'go')
pl.title('antenna='+str(k))
###
tb.putcol('FLAG', flg)
tb.putcol('SOLUTION_OK', sol)
tb.putcol('GAIN', gain)
tb.done()
def flag_extreme_amplitudes(tablename,
maxpctchange=50,
pols=[0],
channels=[0]):
"""
Flag out all gain amplitudes with >``maxpctchange``% change (e.g., for the
default 50%, flag everything outside the range 0.5 < G < 1.5). This is a
*very simple* cut, but it cannot be easily applied with existing tools
since it is cutting on the value of the amplitude correction, not on any
particular normal data selection type. It is still highly advisable to
plot the amp vs snr or similar diagnostics after running this to make sure
you understand what's going on. For example, after I ran this on a data
set, I discovered that one antenna had high gain corrections even in the
high SNR regime, which probably indicates a problem with that antenna.
Parameters
----------
maxpctchange : float
The maximum percent change permitted in an amplitude
pols : list
The list of polarizations to include in the heuristics
channels : list
The list of channels to include in the heuristics
Returns
-------
None
"""
tb.open(tablename)
solns = tb.getcol('CPARAM')
snr = tb.getcol('SNR')
# true flag = flagged out, bad data
flags = tb.getcol('FLAG')
tb.close()
amp = np.abs(solns)
maxfrac = maxpctchange / 100.
bad = ((amp[pols, channels] > (1 + maxfrac)) | (amp[pols, channels] <
(1 - maxfrac)))
bad_snr = snr[pols, channels, :][bad]
print("Found {0} bad amplitudes with mean snr={1}".format(
bad.sum(), bad_snr.mean()))
print("Total flags in tb.flag: {0}".format(flags.sum()))
flags[pols, channels, :] = bad | flags[pols, channels, :]
assert all(flags[pols, channels, :][bad]), "Failed to modify array"
tb.open(tablename, nomodify=False)
tb.putcol(columnname='FLAG', value=flags)
tb.flush()
tb.close()
tb.open(tablename, nomodify=True)
flags = tb.getcol('FLAG')
print("Total flags in tb.flag after: {0}".format(flags.sum()))
assert all(flags[pols, channels, :][bad]), "Failed to modify table"
tb.close()
def make_primary_beams(image_name,lst,stokes_choice,beam_filename):
#
# define the frequencies of the simulated beams
#
freq_beams = np.zeros(11)
freq_beams[0] = 100e6
for j in range(1,11):
freq_beams[j] = freq_beams[j - 1] + 10e6
#
# read the input cube
#
tb.open(image_name)
q_cube = tb.getcol('map')
tb.close()
# ra = np.ndarray(shape=(image.shape[0],image.shape[1]),dtype=float)
# dec = np.ndarray(shape=(image.shape[0],image.shape[1]),dtype=float)
ia.open(image_name)
summary = ia.summary() # read the image summary
cube_shape = summary['shape'] # read the image shape: RA, DEC, Stokes, Freq
ra = np.ndarray(shape=(cube_shape[0],cube_shape[1]),dtype=float)
dec = np.ndarray(shape=(cube_shape[0],cube_shape[1]),dtype=float)
nchan = cube_shape[3] # number of channels in the cube
start_freq = summary['refval'][3] # start frequencies in Hz
df = summary['incr'][3] # frequency increment in Hz
#
# ra and dec will contain the RA and DEC corresponding to the pixel values in the image
#
#
for j in range(0,cube_shape[0]):
for k in range(0,cube_shape[1]):
a=ia.toworld([j,k,0,0]) # a dictionary is returned with the world coordinates of that pixel
b=a['numeric'] # the array is extracted from the dictionary a
ra[j,k] = b[0] # save the RA for pixel j,k
dec[j,k] = b[1] # save the DEC for pixel j,k
# print ra[j,k] * 12/np.pi,dec[j,k] * 180/np.pi,j,k
#
print 'RA and DEC calculated'
ia.close()
#
#
#
# read the beams
#
fekoX=fmt.FEKO('/home/gianni/PAPER/beams/fitBeam/data/PAPER_FF_X.ffe')
fekoY=fmt.FEKO('/home/gianni/PAPER/beams/fitBeam/data/PAPER_FF_Y.ffe')
feko_xpol=fekoX.fields[0]
feko_ypol=fekoY.fields[0]
phi=feko_xpol.phi*np.pi/180. # phi is the azimuth
theta=feko_xpol.theta*np.pi/180. # theta is the zenith angle
theta = np.pi/2 - theta # pyephem wants the elevation rather than the zenith angle
ra_beams = np.ndarray(shape=(phi.shape[0]),dtype=float) # array of RA corresponding to (phi,theta)
dec_beams = np.ndarray(shape=(phi.shape[0]),dtype=float) # array of DEC corresponding to (phi,theta)
#
# compute complex beams
#
gxx=feko_xpol.etheta*np.conj(feko_xpol.etheta)+feko_xpol.ephi*np.conj(feko_xpol.ephi)
#
# define an array that will contain all the simulated beams
#
beams = np.ndarray(shape=(gxx.shape[0],4,freq_beams.shape[0]),dtype=float)
#
# read all the beam models and save them in the beams array
#
for j in range(0,freq_beams.shape[0]):
feko_xpol = fekoX.fields[j] # these two lines give an error, I need to check with Griffin how to fix it
feko_ypol = fekoY.fields[j]
#
gxx = feko_xpol.etheta*np.conj(feko_xpol.etheta)+feko_xpol.ephi*np.conj(feko_xpol.ephi)
gyy = feko_ypol.etheta*np.conj(feko_ypol.etheta)+feko_ypol.ephi*np.conj(feko_ypol.ephi)
gxy = feko_xpol.etheta*np.conj(feko_ypol.etheta)+feko_xpol.ephi*np.conj(feko_ypol.ephi)
gyx = feko_ypol.etheta*np.conj(feko_xpol.etheta)+feko_ypol.ephi*np.conj(feko_xpol.ephi)
#
# make the stokes beams
#
beams[:,0,j] = (gxx+gyy).real
# beams[:,0,j] = beams[:,0,j] / np.max(beams[:,0,j]) # normalize the beams to be 1 at zenith
beams[:,1,j] = (gxx-gyy).real
beams[:,2,j] = (gxy+gyx).real
beams[:,3,j] = (gxy-gyx).imag
#
norm_beam = np.max(beams[:,0,5]) # beam peak at 150 MHz
beams[:,0,:] = beams[:,0,:] / norm_beam # normalize the beams to be 1 at zenith at 150 MHz
#
print norm_beam,np.max(beams[:,0,:])
print 'Beams read'
#
# bring the beam to RA,DEC coordinates
#
# Create an observer
#
paper = Observer()
#
# Set the observer at the Karoo
#
paper.lat, paper.long, paper.elevation = '-30:43:17', '21:25:40.08', 0.0
# j0 = ephem.julian_date(0) # invoked this way if import ephem
j0 = julian_date(0) # invoked this way if from ephem import *
# paper.date = float(lst)
paper.date = float(lst) - j0 + 5./60/24 # I think I need this. At http://stackoverflow.com/questions/8962426/convert-topocentric-coordinates-azimuth-elevation-to-equatorial-coordinates
# they seem to suggest that this is needed in order to get the right date and I seem to get the right
# RA if I include this. The factor 5./60/24 needs to be added as the lst reported in the filename refers to
# the beginning of the integration which is ~10 min long
for j in range(0,ra_beams.shape[0]):
a = paper.radec_of(phi[j],theta[j])
ra_beams[j] = a[0] # RA is in radians
dec_beams[j] = a[1] # DEC is in radians
#
#
# now interpolate the beams in frequency
#
interp_beam = np.ndarray(shape=(beams.shape[0],beams.shape[1],nchan),dtype=float)
cube_freq = start_freq
for chan in range(0,nchan):
a = np.max(q_cube[:,:,0,chan,0])
b = np.min(q_cube[:,:,0,chan,0])
if (a != 0 and b != 0): # if the image is not empty, then proceed
freq_dist = np.abs(cube_freq - freq_beams)
freq_dist_s = np.sort(freq_dist)
w = np.where(freq_dist == freq_dist_s[0])
if freq_dist_s[0] == 0:
#
# if the beam is simulated at the exact frequency channel, then do not interpolate
#
for j in range(0,4):
interp_beam[:,j,chan] = beams[:,j,w[0][0]]
#
# if they are not, perform a weighted average of the two closest beams in frequency. The weights are the inverse of the frequency distance squared
#
else:
w1 = np.where(freq_dist == freq_dist_s[1])
for j in range(0,4):
interp_beam[:,j,chan] = (beams[:,j,w[0][0]] * freq_dist_s[0]**(-2) + beams[:,j,w1[0][0]] * freq_dist_s[1]**(-2)) / (freq_dist_s[0]**(-2) + freq_dist_s[1]**(-2))
#
cube_freq = cube_freq + df
#
print 'Beams interpolated in frequency'
#
# now interpolate the beam at the observed RA,DEC
#
interp_beam_maps_q = np.ndarray(shape=(ra.shape[0],ra.shape[1],1,nchan,1),dtype=float)
#
for j in range(0,ra.shape[0]):
for k in range(0,ra.shape[1]):
#
# interpolating amongst the three closest points
#
# x = np.cos(ra[j,k])*np.cos(ra_beams)*np.cos(dec[j,k])*np.cos(dec_beams)
# y = np.sin(ra[j,k])*np.sin(ra_beams)*np.cos(dec[j,k])*np.cos(dec_beams)
# z = np.sin(dec[j,k])*np.sin(dec_beams)
# dist = np.sqrt(x**2 + y**2 + z**2)
#
dist = np.sqrt((ra[j,k] - ra_beams)**2 + (dec[j,k] - dec_beams)**2)
dist_s = np.sort(dist)
w0 = np.where(dist == dist_s[0])
w1 = np.where(dist == dist_s[1])
w2 = np.where(dist == dist_s[2])
#
interp_beam_maps_q[j,k,0,:,0] = interp_beam[w0[0][0],stokes_choice,:] / dist_s[0] + interp_beam[w1[0][0],stokes_choice,:] / dist_s[1] + interp_beam[w2[0][0],stokes_choice,:] / dist_s[2]
interp_beam_maps_q[j,k,0,:,0] = interp_beam_maps_q[j,k,0,:,0] / (dist_s[0]**(-1) + dist_s[1]**(-1) + dist_s[2]**(-1))
#
# nearest neighbour interpolation
#
# dist = np.sqrt((ra[j,k] - ra_beams)**2 + (dec[j,k] - dec_beams)**2)
# dist_s = np.sort(dist)
# w0 = np.where(dist == dist_s[0])
# interp_beam_maps_q[j,k,0,:,0] = interp_beam[w0[0][0],stokes_choice,:]
#
print 'Beams interpolated in angle'
#
# store the beams into an image
#
# beam_filename = image_name.strip('.image')
cmd = 'rm -rf ' + beam_filename + '.beams'
os.system(cmd)
cmd = 'cp -r ' + image_name + ' ' + beam_filename + '.beams'
os.system(cmd)
#
tb.open(beam_filename + '.beams',nomodify=False)
tb.putcol('map',interp_beam_maps_q)
tb.close()
tb.done()
ia.open(beam_filename + '.beams')
ia.tofits(beam_filename + '_beams.fits',overwrite=true)
ia.close()
def fill_flagged_soln(caltable='', doplot=False):
"""
This is to replace the gaincal solution of flagged/failed solutions by the nearest valid
one.
If you do not do that and applycal blindly with the table your data gets
flagged between calibration runs that have a bad/flagged solution at one edge.
Can be pretty bad when you calibrate every hour or more
(when you are betting on self-cal) of observation (e.g L-band of the EVLA)..one can
lose the whole hour of good data without realizing !
"""
tb.open(caltable, nomodify=False)
flg = tb.getcol('FLAG')
sol = tb.getcol('SOLUTION_OK')
ant = tb.getcol('ANTENNA1')
gain = tb.getcol('GAIN')
t = tb.getcol('TIME')
dd = tb.getcol('CAL_DESC_ID')
maxant = np.max(ant)
maxdd = np.max(dd)
npol = len(gain[:, 0, 0])
nchan = len(gain[0, :, 0])
k = 1
if (doplot):
pl.ion()
pl.figure(1)
pl.plot(t[(ant == k)], sol[0, 0, (ant == k)], 'b+')
pl.plot(t[(ant == k)], flg[0, 0, (ant == k)], 'r+')
pl.twinx()
pl.plot(t[(ant == k)], abs(gain[0, 0, (ant == k)]), 'go')
print 'maxant', maxant
numflag = 0.0
for k in range(maxant + 1):
for j in range(maxdd + 1):
subflg = flg[:, :, (ant == k) & (dd == j)]
subt = t[(ant == k) & (dd == j)]
subsol = sol[:, :, (ant == k) & (dd == j)]
subgain = gain[:, :, (ant == k) & (dd == j)]
#print 'subgain', subgain.shape
for kk in range(1, len(subt)):
for chan in range(nchan):
for pol in range(npol):
if (subflg[pol, chan, kk]
and not subflg[pol, chan, kk - 1]):
numflag += 1.0
subflg[pol, chan, kk] = False
subsol[pol, chan, kk] = True
subgain[pol, chan, kk] = subgain[pol, chan, kk - 1]
if (subflg[pol, chan, kk - 1]
and not subflg[pol, chan, kk]):
numflag += 1.0
subflg[pol, chan, kk - 1] = False
subsol[pol, chan, kk - 1] = True
subgain[pol, chan, kk - 1] = subgain[pol, chan, kk]
flg[:, :, (ant == k) & (dd == j)] = subflg
sol[:, :, (ant == k) & (dd == j)] = subsol
gain[:, :, (ant == k) & (dd == j)] = subgain
print 'numflag', numflag
if (doplot):
pl.figure(2)
k = 1
#pl.clf()
pl.plot(t[(ant == k)], sol[0, 0, (ant == k)], 'b+')
pl.plot(t[(ant == k)], flg[0, 0, (ant == k)], 'r+')
pl.twinx()
pl.plot(t[(ant == k)], abs(gain[0, 0, (ant == k)]), 'go')
pl.title('antenna=' + str(k))
###
tb.putcol('FLAG', flg)
tb.putcol('SOLUTION_OK', sol)
tb.putcol('GAIN', gain)
tb.done()
def openBpolyFile(caltable, debug=False):
# mytb = au.createCasaTool(tbtool) # from analysisutilities by corder
tb.open(caltable)
desc = tb.getdesc()
if ('POLY_MODE' in desc):
polyMode = tb.getcol('POLY_MODE')
polyType = tb.getcol('POLY_TYPE')
scaleFactor = tb.getcol('SCALE_FACTOR')
antenna1 = tb.getcol('ANTENNA1')
times = tb.getcol('TIME')
cal_desc_id = tb.getcol('CAL_DESC_ID')
nRows = len(polyType)
for pType in polyType:
if (pType != 'CHEBYSHEV'):
print "I do not recognized polynomial type = %s" % (pType)
return
# Here we assume that all spws have been solved with the same mode
uniqueTimesBP = n.unique(tb.getcol('TIME'))
nUniqueTimesBP = len(uniqueTimesBP)
if (nUniqueTimesBP == 2):
print "Two BP sols found with times differing by %g seconds. Using first." % (uniqueTimesBP[1]-uniqueTimesBP[0])
nUniqueTimesBP = 1
uniqueTimesBP = uniqueTimesBP[0]
mystring = ''
nPolyAmp = tb.getcol('N_POLY_AMP')
nPolyPhase = tb.getcol('N_POLY_PHASE')
frequencyLimits = tb.getcol('VALID_DOMAIN')
increments = 0.001*(frequencyLimits[1,:]-frequencyLimits[0,:])
frequenciesGHz = []
for i in range(len(frequencyLimits[0])):
freqs = (1e-9)*n.arange(frequencyLimits[0,i],frequencyLimits[1,i],increments[i]) # **for some reason this is nch-1 long?**
frequenciesGHz.append(freqs)
polynomialAmplitude = []
polynomialPhase = []
for i in range(len(polyMode)):
polynomialAmplitude.append([1])
polynomialPhase.append([0])
if (polyMode[i] == 'A&P' or polyMode[i] == 'A'):
polynomialAmplitude[i] = tb.getcell('POLY_COEFF_AMP',i)[0][0][0]
if (polyMode[i] == 'A&P' or polyMode[i] == 'P'):
polynomialPhase[i] = tb.getcell('POLY_COEFF_PHASE',i)[0][0][0]
tb.close()
tb.open(caltable+'/CAL_DESC')
nSpws = len(tb.getcol('NUM_SPW'))
spws = tb.getcol('SPECTRAL_WINDOW_ID')
spwBP = []
for c in cal_desc_id:
spwBP.append(spws[0][c])
tb.close()
nPolarizations = len(polynomialAmplitude[0]) / nPolyAmp[0]
if (debug):
mystring += '%.3f, ' % (uniqueTimesBP/(24*3600))
print 'BP solution has unique time(s) %s and %d pols' % (mystring, nPolarizations)
# This value is overridden by the new function doPolarizations in ValueMapping.
# print "Inferring %d polarizations from size of polynomial array" % (nPolarizations)
return([polyMode, polyType, nPolyAmp, nPolyPhase, scaleFactor, nRows, nSpws, nUniqueTimesBP,
uniqueTimesBP, nPolarizations, frequencyLimits, increments, frequenciesGHz,
polynomialPhase, polynomialAmplitude, times, antenna1, cal_desc_id, spwBP])
else:
tb.close()
return([])
from casa import table as tb
obstablename="/home/trienko/HERA/software/casa-release-4.7.1-el7/data/geodetic/Observatories/"
tb.open(obstablename,nomodify=False)
paperi =(tb.getcol("Name")=="PAPER_SA").nonzero()[0]
tb.copyrows(obstablename,startrowin=paperi,startrowout=-1,nrow=1)
tb.putcell("Name",tb.nrows()-1,"HERA")
tb.close()