def __init__(self, cube, wcs=None, mask=None, sigma=None, empty_channel=0,
keep_threshold_mask=True, distance=None, galaxy_props={}):
super(BubbleFinder, self).__init__()
if not isinstance(cube, SpectralCube):
if wcs is None:
raise TypeError("When cube is not a SpectralCube, wcs must be"
" given.")
cube = SpectralCube(cube, wcs)
if mask is not None:
cube = cube.with_mask(mask)
self.cube = cube
self.empty_channel = empty_channel
if sigma is None:
self.estimate_sigma()
else:
self.sigma = sigma
self.keep_threshold_mask = keep_threshold_mask
self._mask = None
self.distance = distance
self.galaxy_props = galaxy_props
def line_flux2(catalog, line_name='13co10',
asgn=datadir + 'COHRS_all_asgn.fits',
cubefile=datadir + 'GRS_13CO_all.fits'):
flux = Column(np.zeros(len(catalog)),name=line_name)
asgn = SpectralCube.read(asgn)
linefile = SpectralCube.read(cubefile)
previous_file=''
fill_data=None
previous_cube_file=''
for idx, obj in enumerate(catalog):
if obj['orig_file'] != previous_cube_file:
print "Pulling line subcube for {0}".format(obj['orig_file'])
subx1 = obj['orig_file'].split('_')[2]
subx2 = obj['orig_file'].split('_')[3]
subcube = linefile[:, :, int(subx1):int(subx2)]
fill_cube_data = (subcube.filled_data[:].value)
previous_cube_file = obj['orig_file']
outtuple = sparse_mask(obj, asgn,
previous_file=previous_file,
fill_data=fill_data)
previous_file, fill_data, zcld, ycld, xcld = outtuple
if len(xcld)>0:
flux[idx] = np.nansum(fill_cube_data[zcld, ycld, xcld])
catalog.add_column(flux)
return catalog
def load_and_reduce(filename, add_noise=False, rms_noise=0.001,
nsig=3):
'''
Load the cube in and derive the property arrays.
'''
if add_noise:
if rms_noise is None:
raise TypeError("Must specify value of rms noise.")
cube, hdr = getdata(filename, header=True)
from scipy.stats import norm
cube += norm.rvs(0.0, rms_noise, cube.shape)
sc = SpectralCube(data=cube, wcs=WCS(hdr))
mask = LazyMask(np.isfinite, sc)
sc = sc.with_mask(mask)
else:
sc = filename
reduc = Mask_and_Moments(sc, scale=rms_noise)
reduc.make_mask(mask=reduc.cube > nsig * reduc.scale)
reduc.make_moments()
reduc.make_moment_errors()
return reduc.to_dict()
def __init__(self, highres, lowres):
super(MultiResObs, self).__init__()
self.highres = SpectralCube.read(highres)
self.lowres = SpectralCube.read(lowres)
self.highres_convolved = None
self.lowres_convolved = None
self.lowbeam = self.lowres.beam
self.highbeam = self.highres.beam
self.combined_beam = self.lowbeam.convolve(self.highbeam)
def cubegen(ymin,ymax,xmin,xmax, deltaX=30):
"""Generates a subcube of the specified dimensions from the .fits files,
for 12CO and 13CO. Returns the subcubes for 12CO and 13CO, respectively.
Argument format: "(ymin,ymax, xmin,xmax.)"
^ These are the parameters of the desired subcubes."""
cube12 = SpectralCube.read("paws-30m-12co10-23as-cube.fits")
cube13 = SpectralCube.read("paws-30m-13co10-23as-cube.fits")
subcube12 = cube12[:,ymin:ymax,xmin:xmax]
subcube13 = cube13[:,ymin:ymax,xmin:xmax]
return subcube12,subcube13
def reduce_and_save(filename, add_noise=False, rms_noise=0.001,
output_path="", cube_output=None,
nsig=3, slicewise_noise=True):
'''
Load the cube in and derive the property arrays.
'''
if add_noise:
if rms_noise is None:
raise TypeError("Must specify value of rms noise.")
cube, hdr = getdata(filename, header=True)
# Optionally scale noise by 1/10th of the 98th percentile in the cube
if rms_noise == 'scaled':
rms_noise = 0.1*np.percentile(cube[np.isfinite(cube)], 98)
from scipy.stats import norm
if not slicewise_noise:
cube += norm.rvs(0.0, rms_noise, cube.shape)
else:
spec_shape = cube.shape[0]
slice_shape = cube.shape[1:]
for i in range(spec_shape):
cube[i, :, :] += norm.rvs(0.0, rms_noise, slice_shape)
sc = SpectralCube(data=cube, wcs=WCS(hdr))
mask = LazyMask(np.isfinite, sc)
sc = sc.with_mask(mask)
else:
sc = filename
reduc = Mask_and_Moments(sc, scale=rms_noise)
reduc.make_mask(mask=reduc.cube > nsig * reduc.scale)
reduc.make_moments()
reduc.make_moment_errors()
# Remove .fits from filename
save_name = filename.split("/")[-1][:-4]
reduc.to_fits(output_path+save_name)
# Save the noisy cube too
if add_noise:
if cube_output is None:
reduc.cube.hdu.writeto(output_path+save_name)
else:
reduc.cube.hdu.writeto(cube_output+save_name)
def warp_ellipse_to_circle(cube, a, b, pa, stop_if_huge=True):
'''
Warp a SpectralCube such that the given ellipse is a circle int the
warped frame.
Since you should **NOT** be doing this with a large cube, we're going
to assume that the given cube is a subcube centered in the middle of the
cube.
This requires a rotation, then scaling. The equivalent matrix is:
[b cos PA b sin PA]
[-a sin PA a cos PA ].
'''
if cube._is_huge:
if stop_if_huge:
raise Warning("The cube has the huge flag enabled. Disable "
"'stop_if_huge' if you would like to continue "
"anyways with the warp.")
else:
warn("The cube has the huge flag enabled. This may use a lot "
"of memory!")
# Let NaNs be 0
data = cube.with_fill_value(0.0).filled_data[:].value
warped_array = []
for i in range(cube.shape[0]):
warped_array.append(nd.zoom(nd.rotate(data[i], np.rad2deg(-pa)),
(1, a / b)))
warped_array = np.array(warped_array)
# We want to mask outside of the original bounds
mask = np.ones(data.shape[1:])
warp_mask = \
np.isclose(nd.zoom(nd.rotate(mask, np.rad2deg(-pa)),
(1, a / b)), 1)
# There's probably a clever way to transform the WCS, but all the
# solutions appear to need pyast/starlink. The output of the wrap should
# give a radius of b and the spectral dimension is unaffected.
# Also this is hidden and users won't be able to use this weird cube
# directly
warped_cube = SpectralCube(warped_array * cube.unit, cube.wcs)
warped_cube = warped_cube.with_mask(warp_mask)
return warped_cube
def test_qglue():
from spectral_cube import SpectralCube
cube = SpectralCube.read(os.path.join(DATA, 'cube_3d.fits'))
data = parse_data(cube, 'x')[0]
assert data.label == 'x'
data['STOKES I']
assert data.shape == (2, 3, 4)
def writeplanes(save_name='/mnt/work/erosolow/GRS_13CO_all.fits'):
spatial_template = fits.open('INTEG/COHRS_RELEASE1_FULL_INTEG.fit')
spectral_template = SpectralCube.read('reprojected.fits')
# Smoosh astrometry components together
spatial_header = spatial_template[0].header
spectral_header = spectral_template.header
new_header = spatial_header.copy()
new_header["NAXIS"] = 3
for keyword in ['NAXIS3', 'CRVAL3', 'CDELT3','CRPIX3','CUNIT3']:
new_header[keyword] = spectral_header[keyword]
new_header['BMAJ'] = 14./3600
new_header['BMIN'] = 14./3600
new_header['BPA'] = 0.00
if os.path.exists(save_name):
raise Exception("The file name {} already "
"exists".format(save_name))
# Open a file and start filling this with planes.
output_fits = fits.StreamingHDU(save_name, new_header)
# Again, set up a common vel axis and spin out
vel = np.linspace(-30, 160, 191)
for v in vel:
output_fits.write(fits.getdata(planesdir +
'GRSPLANE_{0}'.format(v) +
'.fits'))
output_fits.close()
def S2_drawM33(vmin=40,vmax=80, deltaX=40, deltaV=6, deltadeltaX=10, deltadeltaV=1): """Activates S2_draw with each of the .py file's subcube selections, with the same args as S2_arrayM33. Argument format: "(vmin=40,vmax=80, deltaX=40, deltaV=6, deltadeltaX=10, deltadeltaV=1). These MUST match the args/kwargs used in S2_arrayM33!""" galaxyname = 'M33' filename = 'm33.co21_iram_CLEANED' cube = SpectralCube.read(filename+".fits") pixelwidthDEG = cube.header['CDELT2'] # The width of each pixel, in degrees. distancePC = 840000.0 # The distance to the galaxy that M51's .fits file deals with, in parsecs. (???) Is this number accurate, though? pixelwidthPC = pixelwidthDEG*np.pi/180.0*distancePC # The width of each pixel, in pc. ymin = np.array([350,600,650,525,300,250]) # These are the minimum "y" values of the regions that we're dealing with. ymax = np.array([550,800,850,725,500,450]) # These are the corresponding maximum "y" values of these regions. xmin = np.array([500,100,400,288,200,550]) # These are the corresponding minimum "x" values of these regions. xmax = np.array([700,300,600,488,400,750]) # These are the corresponding maximum "x" values of these regions. (Example: The first region has ymin=350, ymax=550, xmin=500, xmax=700.) sets = np.ravel(ymin.shape)[0] # This is the number of regions that we're dealing with. for i in range(0,sets): S2_draw(vmin,vmax,ymin[i],ymax[i],xmin[i],xmax[i],deltaX,deltaV,deltadeltaX,deltadeltaV,filename,galaxyname)
def moments(cube_fits, line_values, line_names, moment, save_file=False):
"""
cube: str
The datacube in fits format to open
line_values: list of floats
The wavelengths of the lines. !!! In general: if moment=0 the required wavelenth should be air, if moment=1 it should be vacuum !!!
line_names: list of str
The identifier of the lines
moment: 0 or 1
save_file: bool, optional
Set to True if the result is to be saved as a fits file. Default is False.
example:
moment = moments('cube.fits', [4861.33, 6562.8], ['Hb', 'Ha'], moment=0)
"""
print line_values, line_names
cube=SpectralCube.read(cube_fits)
for line,stri in zip(line_values,line_names):
if moment==0:
mom = cube.spectral_slab((line-3)*u.AA, (line+3)*u.AA).sum(axis=0)
if save_file==True:
mom.hdu.writeto(str(stri)+'_moment0.fits',clobber=True)
if moment==1:
mom = cube.with_spectral_unit(u.km/u.s, rest_value=line*u.AA,velocity_convention='optical').spectral_slab(-300*u.km/u.s,300*u.km/u.s).moment1()
if save_file==True:
mom.hdu.writeto(str(stri)+'_moment1.fits',clobber=True)
return mom
def FirstLook_Cepheus():
print("Now NH3(1,1)")
a_rms = [ 0, 135, 290, 405, 505, 665]
b_rms = [ 70, 245, 350, 455, 625, 740]
index_rms=first_look.create_index( a_rms, b_rms)
index_peak=np.arange(350,410)
file_in='Cepheus/Cepheus_NH3_11.fits'
# 1st order polynomial
file_out=file_in.replace('.fits','_base1.fits')
file_new=first_look.baseline( file_in, file_out, index_clean=index_rms, polyorder=1)
first_look.peak_rms( file_new, index_rms=index_rms, index_peak=index_peak)
print("Now NH3(2,2)")
linelist = ['NH3_22','NH3_33','C2S','HC5N','HC7N_21_20','HC7N_22_21']
vsys = -3.8*u.km/u.s
throw = 2.0*u.km/u.s
for line in linelist:
file_in = 'Cepheus/Cepheus_{0}.fits'.format(line)
s = SpectralCube.read(file_in)
s = s.with_spectral_unit(u.km/u.s,velocity_convention='radio')
a_rms = [s.closest_spectral_channel(vsys+3*throw),
s.closest_spectral_channel(vsys-throw)]
b_rms = [s.closest_spectral_channel(vsys+throw),
s.closest_spectral_channel(vsys-3*throw)]
index_peak = np.arange(s.closest_spectral_channel(vsys+3*u.km/u.s),
s.closest_spectral_channel(vsys-3*u.km/u.s))
index_rms=first_look.create_index( a_rms, b_rms)
file_out=file_in.replace('.fits','_base1.fits')
file_new=first_look.baseline( file_in, file_out,
index_clean=index_rms, polyorder=1)
first_look.peak_rms( file_new, index_rms=index_rms,
index_peak=index_peak)
def cube_w11(region='IC348'):
if region == 'IC348':
OneOneFile = 'IC348mm/IC348mm-11_cvel_clean_rob05.fits'
TwoTwoFile = 'IC348mm/IC348mm-11_cvel_clean_rob05.fits'
vmin=7.4
vmax=10.0
elif region == 'IRAS03282':
OneOneFile = 'IRAS03282/IRAS03282-11_cvel_clean_rob05.fits'
TwoTwoFile = 'IRAS03282/IRAS03282-11_cvel_clean_rob05.fits'
vmin=6.0
vmax=8.5
elif region == 'L1451mm':
OneOneFile = 'L1451mm/L1451MM-11_cvel_clean_rob05.fits'
TwoTwoFile = 'L1451mm/L1451MM-11_cvel_clean_rob05.fits'
vmin=3.2
vmax=4.9
cube = SpectralCube.read(OneOneFile)
vcube = cube.with_spectral_unit(u.km/u.s, rest_value=freq11, velocity_convention='radio')
slab = vcube.spectral_slab( vmax*u.km/u.s, vmin*u.km/u.s)
w11=slab.moment( order=0, axis=0)
#beam = Beam.from_fits_header(fits.getheader(OneOneFile))
# Next line is to solve bug in spectralcube:
# it should be something like this in line 2234 of spectral_cube.py:
# ```
# if axis == 0 and self._meta['beam'] is not None:
# meta = { blabla, 'beam':self._meta['beam']}
# else:
# meta = { blabla}
w11._meta['beam'] = slab.beam
w11.write(OneOneFile.replace('.fits','_w11.fits'), overwrite=True)
def select_cloud(idxarray, cloudcat):
for idx in idxarray:
entry = cloudcat[idx]
asgn = SpectralCube.read(cohrsdir+'FINALASGNS/'+
entry['orig_file']+
'_fasgn.fits')
data = SpectralCube.read(cohrsdir+'DATA/'+
entry['orig_file']+
'.fits')
mask = (asgn == entry['_idx'] *
u.dimensionless_unscaled)
cube = data.with_mask(mask)
cube = cube.minimal_subcube()
cube.write('cohrscld_{0}'.format(entry['_idx'])+'.fits',
overwrite=True)
def write_skycoord_table(data, cube_ref, **kwargs):
"""
Writes out a text file with flattened coordinates of the cube
stacked with input array data. Additional arguments are passed
to astropy's text writing function.
TODO: add a useful `names` keyword?
See astropy.io.ascii.write docstring for more info.
Parameters
----------
data : array-like structure of the same xy-grid as cube_ref.
cube_ref : a cube file to get the coordinate grid from.
"""
from astropy.table import Table
from astropy.io import ascii
from spectral_cube import SpectralCube
cube = SpectralCube.read(cube_ref)
flat_coords = [cube.spatial_coordinate_map[i].flatten() for i in [1,0]]
# TODO: finish this up for multiple components
#n_repeat = np.prod(np.array(data).shape)%np.prod(cube.shape[1:])+1
table = Table(np.vstack(flat_coords +
[np.array(xy_slice).flatten() for xy_slice in data]).T)
ascii.write(table, **kwargs)
def subcubes_from_ds9(cube, region_file='../nro_maps/SouthShells.reg', pad_factor=1., shape='exact'):
"""
Extracts subcubes using the ds9 region file.
Parameters
----------
cube : SpectralCube, str
The cube to be chopped. Must be type spectral_cube.SpectralCube or str filename.
region_file : str
Path to a ds9 region file.
pad_factor : float, optional
Expand the subcube around the region by this factor.
shape : {'square', 'exact'}
The shape of the subcube returned. 'square' returns the
smallest square subcube that contains the region.
'exact' returns only the pixels contained within the region.
Returns
-------
subcubes: list of SpectralCube of SpectralCube
"""
from spectral_cube import SpectralCube
import pyregion
try:
#If cube is a str filename, read a SpectralCube.
cube = SpectralCube.read(cube)
except ValueError:
pass
if shape == 'square':
import astropy.units as u
subcube_list = []
region_list = pyregion.open(region_file)
for region in region_list:
half_width = region.coord_list[2] * pad_factor * u.deg
ra_center = region.coord_list[0] * u.deg
dec_center = region.coord_list[1] * u.deg
ra_range = [ra_center - half_width, ra_center + half_width]
dec_range = [dec_center - half_width, dec_center + half_width]
#print(ra_range, dec_range)
subcube_list.append(cube.subcube(ra_range[1], ra_range[0], dec_range[0], dec_range[1]))
if shape == 'exact':
region_list = pyregion.open(region_file)
subcube_list = []
for region in region_list:
if pad_factor != 1.:
new_string = '{};{}({},{},{}")'.format(region.coord_format, region.name,
region.coord_list[0], region.coord_list[1],
region.coord_list[2]*3600.*pad_factor)
region = pyregion.parse(new_string)[0]
subcube_list.append(cube.subcube_from_ds9region(pyregion.ShapeList([region])))
if len(subcube_list) == 1:
return subcube_list[0]
else:
return subcube_list
def summary_plot(filelist):
for thisfile in filelist:
s = SpectralCube.read(thisfile)
outfile = thisfile.replace('.fits','_summary.png')
mom0 = s.moment0()
f = aplpy.FITSFigure(mom0.hdu)
f.show_colorscale()
f.show_colorbar()
f.save(outfile)
def cubegen(vmin,vmax,ymin,ymax,xmin,xmax, filename = "paws_norot", drawmap = False, mapname="3Dcube"):
"""
Returns a subcube of the specified dimensions from the .fits file.
Also displays the subcube as it appears on the galaxy map if drawmap=True.
Parameters:
-----------
vmin,...,xmax : int
Parameters used in relevant xi map.
WARNING: Selecting too large of a vmax-vmin will hugely increase
processing time in later calculations.
filename : str
Name of the .paws data file.
"paws_norot" for M51, "m33.co21_iram_CLEANED" for M33.
drawmap : bool
Enables or disables drawing the subcube Tmax map.
galaxyname : str
Name of the galaxy.
'M51' for M51, 'M33' for M33.
mapname : str
Name of the saved image of the subcube's Tmax map, if
drawmap==True.
Returns:
-----------
subcube : spectral cube (?)
The data inside the selected subcube.
"""
cube = SpectralCube.read(filename+".fits")
data = cube.filled_data[:] # Pulls "cube"'s information (position, spectral info (?)) into a 3D Numpy array.
yshape = data.shape[1]/2.0
xshape = data.shape[2]/2.0
pixelwidthDEG = cube.header['CDELT2'] # The width of each pixel, in degrees.
if (filename =='m33.co21_iram_CLEANED') or (filename =='m33.co21_iram_CLEANED_smooth') or (filename =='m33.co21_iram_CLEANED_blank'): # Checks if the galaxy's Header file contains its distance.
distancePC = 840000.0 # The distance to the galaxy that M33's .fits file deals with, in parsecs. ONLY works on the CLEANED file!
else:
distancePC = cube.header['DIST'] # The distance to the galaxy that M51's .fits file deals with, in parsecs. (???) Is this number accurate, though?
pixelwidthPC = pixelwidthDEG*np.pi/180.0*distancePC # The width of each pixel, in pc.
subcube = cube[vmin:vmax,ymin:ymax,xmin:xmax]
if drawmap == True:
plt.figure(1)
plt.imshow(np.nanmax(data[vmin:vmax,ymin:ymax,xmin:xmax].value,axis=0), extent=[(xmin-xshape)*pixelwidthPC,(xmax-xshape)*pixelwidthPC, \
(ymin-yshape)*pixelwidthPC,(ymax-yshape)*pixelwidthPC], origin='lower')
fig = matplotlib.pyplot.gcf()
#fig.set_size_inches(5, 5) # Enlarges the image so as to prevent squishing.
plt.xlabel('Distance from Centre in x-direction (pc)')
plt.ylabel('Distance from Centre in y-direction (pc)')
plt.savefig('galaxy_'+mapname+'.png')
plt.clf() # Clears the image after saving.
return subcube
def FirstLook_NGC1333():
print("Now NH3(1,1)")
a_rms = [ 0, 158, 315, 428, 530, 693, 751]
b_rms = [ 60, 230, 327, 438, 604, 735, 760]
index_rms=first_look.create_index( a_rms, b_rms)
index_peak=np.arange(326,430)
file_in='NGC1333/NGC1333_NH3_11.fits'
# 1st order polynomial
file_out=file_in.replace('.fits','_base1.fits')
file_new=first_look.baseline( file_in, file_out, index_clean=index_rms, polyorder=1)
first_look.peak_rms( file_new, index_rms=index_rms, index_peak=index_peak)
print("Now NH3(2,2)")
a_rms = [ 0, 190, 360, 600]
b_rms = [70, 300, 470, 640]
index_rms=first_look.create_index( a_rms, b_rms)
index_peak=np.arange(380,520)
# file_in='NGC1333/NGC1333_NH3_22.fits'
# # 1st order polynomial
# file_out=file_in.replace('.fits','_base1.fits')
# file_new=first_look.baseline( file_in, file_out, index_clean=index_rms, polyorder=1)
# first_look.peak_rms( file_new, index_rms=index_rms, index_peak=index_peak)
## 2nd order polynomial
#file_out=file_in.replace('.fits','_base2.fits')
#file_new=first_look.baseline( file_in, file_out, index_clean=index_rms, polyorder=2)
#first_look.peak_rms( file_new, index_rms=index_rms, index_peak=index_peak)
#
# print("Now NH3(3,3)")
# a_rms = [ 10, 190, 420]
# b_rms = [70, 360, 500]
# index_rms=first_look.create_index( a_rms, b_rms)
# index_peak=np.arange(410,540)
# file_in='NGC1333/NGC1333_NH3_33.fits'
# 1st order polynomial
# file_out=file_in.replace('.fits','_base1.fits')
# file_new=first_look.baseline( file_in, file_out, index_clean=index_rms, polyorder=1)
# first_look.peak_rms( file_new, index_rms=index_rms, index_peak=index_peak)
linelist = ['NH3_22','NH3_33','C2S','HC5N','HC7N_21_20','HC7N_22_21']
vsys = 8.5*u.km/u.s
throw = 8*u.km/u.s
for line in linelist:
file_in = 'NGC1333/NGC1333_{0}.fits'.format(line)
s = SpectralCube.read(file_in)
s = s.with_spectral_unit(u.km/u.s,velocity_convention='radio')
a_rms = [s.closest_spectral_channel(vsys+2*throw),
s.closest_spectral_channel(vsys-throw)]
b_rms = [s.closest_spectral_channel(vsys+throw),
s.closest_spectral_channel(vsys-2*throw)]
index_peak = np.arange(s.closest_spectral_channel(vsys+3*u.km/u.s),
s.closest_spectral_channel(vsys-3*u.km/u.s))
index_rms=first_look.create_index( a_rms, b_rms)
file_out=file_in.replace('.fits','_base1.fits')
file_new=first_look.baseline( file_in, file_out,
index_clean=index_rms, polyorder=1)
first_look.peak_rms( file_new, index_rms=index_rms,
index_peak=index_peak)
def dendropix(fileprefix='SgrB2_b3_12M.HC3N'):
cube = SpectralCube.read(dpath('{0}.image.pbcor.contsub.fits'.format(fileprefix))).minimal_subcube()
noise = cube.spectral_slab(-200*u.km/u.s, -100*u.km/u.s).std(axis=0)
keep_mask = cube.max(axis=0) > noise
tblfile = tpath('{0}.dendrotable.ecsv'.format(fileprefix))
if os.path.exists(tblfile):
table = Table.read(tblfile, format='ascii.ecsv')
else:
table = Table([Column(name='xpix'),
Column(name='ypix'),
Column(name='zpix'),
Column(name='lon'),
Column(name='lat'),
Column(name='velo'),
Column(name='peakval'),])
xpyp_done = set(zip(table['xpix'], table['ypix']))
all_keepers = zip(*np.where(keep_mask))
xpyp = [x for x in all_keepers if x not in xpyp_done]
print(len(xpyp), len(all_keepers), len(xpyp_done))
if len(xpyp_done) > 0:
assert len(xpyp) < len(all_keepers)
for ii,(ypix,xpix) in enumerate(ProgressBar(xpyp)):
data = cube[:,ypix,xpix].value
error = noise[ypix,xpix].value
# alternative:
#error = stats.sigma_clipped_stats(data)[2]
D = astrodendro.Dendrogram.compute(data, min_value=0,
min_delta=2*error, min_npix=7,
is_independent=astrodendro.pruning.min_peak(5*error))
if not D.leaves:
table.add_row([xpix,ypix,]+[np.nan]*5)
del D
continue
#peaks = [S.get_peak()[0][0] for S in D]
#peak_vals = [S.get_peak()[1] for S in D]
#peaks = [cube.spectral_axis[S.get_peak()[0][0]].to(u.km/u.s).value for S in D]
for S in D:
(peak_pix,),peak_val = S.get_peak()
velo,lat,lon = cube.world[peak_pix, ypix, xpix]
table.add_row([xpix,ypix,peak_pix,lon,lat,velo,peak_val])
if ii % 100 == 0:
table.write(tblfile, format='ascii.ecsv')
del D
del S
del data
def __init__(self, cube, scale=None, spatial_norm=None,
spectral_norm=None, beam=None, method="MAD"):
"""
Construct a new Noise object.
Parameters
----------
method : {'MAD','STD'}
Chooses method for estimating noise variance either 'MAD'
for median absolute deviation and 'STD' for standard
deviation. Default: 'MAD'
"""
if isinstance(cube,SpectralCube):
self.cube = cube
elif isinstance(cube, str):
self.cube = SpectralCube.read(cube)
else:
warnings.warn("Noise currently requires a SpectralCube instance.")
self.spatial_footprint = np.any(self.cube.get_mask_array(), axis=0)
if beam is None:
try:
self.beam = cube.beam
except AttributeError:
warnings.warn("cube object has no associated beam. All beam "
"operations are disabled.")
self.beam = None
self.astropy_beam_flag = False
else:
if isinstance(beam, Beam):
self.astropy_beam_flag = False
elif isinstance(beam, Kernel2D):
self.astropy_beam_flag = True
else:
warnings.warn("beam must be a radio_beam Beam object or an "
"astropy Kernel2D object. All beam operations "
"are disabled.")
self.beam = beam
# Default to a normal distribution
self.distribution = ss.norm
# SUGGESTION: calculate on initialization?
# Fit the data
if scale is None:
self.calculate_scale(method=method) # [1] is the std. of a Gaussian
self.spatial_norm = np.ones((self.cube.shape[1], self.cube.shape[2]))
self.spectral_norm = np.ones((self.cube.shape[0]))
# Compute the scale_cube
self.get_scale_cube()
def plot_overview(cube='../nro_maps/12CO_20161002_FOREST-BEARS_spheroidal_xyb_grid7.5_0.099kms.fits',
region_file='../nro_maps/SouthShells.reg', mode='peak', plotname='12co_peak_shells.png',
interactive=False, show_shells=False):
"""
Show full image with all shells.
Parameters
----------
cube : str, optional
Description
region_file : str, optional
Description
mode : str, optional
Description
plotname : str, optional
Description
interactive : bool, optional
Description
show_shells : bool, optional
Description
"""
try:
cube = SpectralCube.read(cube)
except ValueError:
pass
if mode == "peak":
image = cube.max(axis=0)
fig = plt.figure()
wcs = WCS(image.header)
ax = WCSAxes(fig, [0.1,0.1,0.8,0.8], wcs=wcs)
fig.add_axes(ax)
imgplot = plt.imshow(image.data, cmap=cm.gray, origin='lower', interpolation='none',
vmin=0., vmax=100)
cb = plt.colorbar()
cb.set_label(r'K [T$_{MB}$]')
plt.title(r"$^{12}$CO Peak")
if show_shells:
r = pyregion.open(region_file).as_imagecoord(image.header)
patch_list, artist_list = r.get_mpl_patches_texts()
for p in patch_list:
ax.add_patch(p)
for t in artist_list:
ax.add_artist(t)
pass
if interactive:
plt.show()
else:
plt.savefig(plotname)
def line_flux(catalog,
asgn=datadir + 'COHRS_all_asgn.fits'):
thco10 = Column(np.zeros(len(catalog)), name='13co10')
thco32 = Column(np.zeros(len(catalog)), name='13co32')
c18o32 = Column(np.zeros(len(catalog)), name='c18o32')
twco32 = Column(np.zeros(len(catalog)), name='12co32')
asgn = SpectralCube.read(asgn)
previous_file=''
fill_data=None
previous_file=''
for idx, obj in enumerate(ProgressBar(catalog)):
outtuple = sparse_mask(obj, asgn,
previous_file=previous_file,
fill_data=fill_data)
if obj['orig_file'] != previous_file:
print "Pulling img tiles for {0}".format(obj['orig_file'])
subx1 = obj['orig_file'].split('_')[2]
subx2 = obj['orig_file'].split('_')[3]
co32cube = (SpectralCube.read(
'./COHRS_tiles/COHRS_{0}_{1}.fits'.format(
subx1, subx2))).filled_data[:].value
thco32cube = (SpectralCube.read(
'./CHIPS_13CO_tiles/CHIMPS_13CO_{0}_{1}.fits'.format(
subx1, subx2))).filled_data[:].value
c18o32cube = (SpectralCube.read(
'./CHIPS_C18O_tiles/CHIMPS_C18O_{0}_{1}.fits'.format(
subx1, subx2))).filled_data[:].value
grscube = (SpectralCube.read(
'./GRS_tiles/GRS_13CO_{0}_{1}.fits'.format(
subx1, subx2))).filled_data[:].value
previous_file, fill_data, z, y, x = outtuple
thco10[idx] = np.nansum(grscube[z, y, x])
thco32[idx] = np.nansum(thco32cube[z, y, x])
c18o32[idx] = np.nansum(c18o32cube[z, y, x])
twco32[idx] = np.nansum(co32cube[z, y, x])
catalog.add_columns([thco10, thco32, c18o32, twco32])
return catalog
def to_spectral_cube(data, header):
'''
Convert the output from input_data into a SpectralCube.
'''
if not HAS_SC:
raise ValueError("spectral-cube needs to be installed.")
hdu = fits.PrimaryHDU(data, header)
return SpectralCube.read(hdu)
def cubegen(ymin,ymax,xmin,xmax, deltaX=30):
"""Generates a subcube of the specified dimensions from the specified
.fits file.
Argument format: "(ymin,ymax, xmin,xmax.)"
^ These are the parameters of the desired subcube."""
cube = SpectralCube.read("paws-30m-12co10-23as-cube.fits")
subcube = cube[:,ymin:ymax,xmin:xmax]
return subcube
def load_and_reduce(filename, add_noise=False, rms_noise=0.001,
nsig=3, slicewise_noise=True):
'''
Load the cube in and derive the property arrays.
'''
if add_noise:
if rms_noise is None:
raise TypeError("Must specify value of rms noise.")
cube, hdr = getdata(filename, header=True)
# Optionally scale noise by 1/10th of the 98th percentile in the cube
if rms_noise == 'scaled':
rms_noise = 0.1*np.percentile(cube[np.isfinite(cube)], 98)
from scipy.stats import norm
if not slicewise_noise:
cube += norm.rvs(0.0, rms_noise, cube.shape)
else:
spec_shape = cube.shape[0]
slice_shape = cube.shape[1:]
for i in range(spec_shape):
cube[i, :, :] += norm.rvs(0.0, rms_noise, slice_shape)
sc = SpectralCube(data=cube, wcs=WCS(hdr))
mask = LazyMask(np.isfinite, sc)
sc = sc.with_mask(mask)
else:
sc = filename
reduc = Mask_and_Moments(sc, scale=rms_noise)
reduc.make_mask(mask=reduc.cube > nsig * reduc.scale)
reduc.make_moments()
reduc.make_moment_errors()
return reduc.to_dict()
def __init__(self, cube, beam=None, mask=None, method="MAD", compute=True):
# Initialize cube object
self.cube = SpectralCube.read(cube)
if mask is not None:
_check_mask(mask)
self.mask = mask
if beam is not None:
_check_beam(mask)
# Initialize noise object
self.noise = Noise(self.cube, beam=beam, method=method)
def binning(f_nam, bin_width=500, thisbin=0):
"""A function creating brightness bins of pixels, and eventualy a map, in the given spectral cube"""
cube = SpectralCube.read(f_nam)
cube = cube.with_spectral_unit(u.km/u.s,velocity_convention='radio')
Tmax = cube.apply_numpy_function(np.nanmax,axis=0) # array of the maximum values in the spectra of each pixel
baddata = nd.morphology.binary_dilation(np.isnan(Tmax),np.ones((25,25)))
Tmax[baddata]=0.0
Tmax[np.isfinite(Tmax)]
bin_arr = np.sort(Tmax[np.isfinite(Tmax)])
bin_arr2 = bin_arr[:: - bin_width] # this creates an array of the bin margins, in which every bin has a width of "bin_width"
np.digitize(Tmax,bin_arr2)
bins = np.digitize(Tmax,bin_arr2)
y, x = np.where(bins==thisbin)
return y, x
def SampleWithConvolution(file, positions, beam=defaultBeam,
order=1, **kwargs):
s = SpectralCube.read(file)
spaxis = s.spectral_axis.value
spaxis.shape += (1,)
spaxis_ones = np.ones_like(spaxis)
s2 = s.convolve_to(beam)
ravals = spaxis_ones * positions.ra.value
decvals = spaxis_ones * positions.dec.value
vvals = spaxis * np.ones_like(positions.ra.value)
x, y, v = s.wcs.all_world2pix(ravals, decvals, vvals, 0)
output = map_coordinates(s2.filled_data[:], [v, y, x],
order=order, **kwargs)
# import pdb; pdb.set_trace()
return output
def deblend_cube(region='OrionA',vmin=0.,vmax=20.):
tex = fits.getdata('{0}/parameterMaps/{0}_Tex_DR1_rebase3_flag.fits'.format(region))
mom0 = fits.getdata('{0}/{0}_NH3_11_DR1_rebase3_mom0_QA_trim.fits'.format(region))
vlsr = fits.getdata('{0}/parameterMaps/{0}_Vlsr_DR1_rebase3_flag.fits'.format(region))
sigv = fits.getdata('{0}/parameterMaps/{0}_Sigma_DR1_rebase3_flag.fits'.format(region))
nnh3 = fits.getdata('{0}/parameterMaps/{0}_N_NH3_DR1_rebase3_flag.fits'.format(region))
cube = SpectralCube.read('{0}/{0}_NH3_11_DR1_rebase3_trim.fits'.format(region))
cube = cube.with_spectral_unit(u.km/u.s,velocity_convention='radio')
tpeak = mom0/(np.sqrt(2*np.pi)*sigv)
vlsr[vlsr==0]=np.nan
sigv[sigv==0]=np.nan
deblend = np.zeros(cube.shape)
hdr = cube.wcs.to_header()
spaxis = cube.spectral_axis.value
for plane in np.arange(deblend.shape[0]):
deblend[plane,:,:] = tpeak*np.exp(-(spaxis[plane]-vlsr)**2/(2*sigv**2))
newcube = SpectralCube(deblend,cube.wcs,header=hdr)
slab = newcube.spectral_slab(vmin*u.km/u.s,vmax*u.km/u.s)
slab.write('{0}/{0}_singlecomp.fits'.format(region),overwrite=True)
]
cubes = {}
mx = {}
m1 = {}
for region in ("N", "M"):
for spw in (0, 1, 2, 3):
for band in (3, 6):
#for line in freqs:
for line in maser_lines:
fn = 'full_SgrB2{0}_spw{1}_lines_cutout{0}_medsub.fits'.format(
region, spw)
fn = 'sgr_b2m.{0}.spw{1}.B{2}.lines.clarkclean1000.robust0.5.image.pbcor.medsub.fits'.format(
region, spw, band)
cube = SpectralCube.read(paths.eFpath(fn))
freq = freqs[line]
if cube.spectral_extrema[0] < freq < cube.spectral_extrema[1]:
subcube = (cube.with_spectral_unit(
u.km / u.s,
velocity_convention='radio',
rest_value=freq).spectral_slab(55 * u.km / u.s,
110 * u.km / u.s))
try:
subcube = subcube.to(u.K)
except Exception as ex:
print("Failed: {0}".format(ex))
if 'OBJECT' in subcube.meta:
subcube.meta['OBJECT'] = subcube.meta['OBJECT'] + line
else:
subcube.meta['OBJECT'] = "{0}_{1}".format(region, line)
# Save table of parameters
co_param_df = DataFrame(co_fit_vals, index=parnames_hwhm)
co_param_df.to_latex(alltables_path("co_gaussian_totalprof_fits_hwhm_38arcsec.tex"))
co_param_df.to_csv(iram_co21_14B088_data_path("smooth_2beam/tables/co_gaussian_totalprof_fits_hwhm_38arcsec.csv",
no_check=True))
hi_param_df = DataFrame(hi_fit_vals, index=parnames_hwhm)
hi_param_df.to_latex(alltables_path("hi_gaussian_totalprof_fits_hwhm_38arcsec.tex"))
hi_param_df.to_csv(fourteenB_HI_data_wGBT_path("smooth_2beam/tables/hi_gaussian_totalprof_fits_hwhm_38arcsec.csv",
no_check=True))
# Same for the radial bins.
# Load in radial profiles
total_spectrum_hi_radial_cent = SpectralCube.read(hi_stackpath("centroid_stacked_radial_{}.fits".format(wstring)))
total_spectrum_hi_radial_peakvel = SpectralCube.read(hi_stackpath("peakvel_stacked_radial_{}.fits".format(wstring)))
total_spectrum_co_radial_cent = SpectralCube.read(co_stackpath("centroid_stacked_radial_{}.fits".format(wstring)))
total_spectrum_co_radial_peakvel = SpectralCube.read(co_stackpath("peakvel_stacked_radial_{}.fits".format(wstring)))
labels = ["centsub", "peaksub"]
# Make the bin edges
# Convert these into kpc
inneredge = np.arange(0, max_radius.value, dr.value) / 1000.
outeredge = (inneredge + dr.to(u.kpc).value)
# How do the model parameters change with radius?
import glob
import radio_beam
import regions
fname = '/ufrc/adamginsburg/d.jeff/imaging_results/SgrB2DS_field1_spw2_cube_medsub.image.fits' #glob.glob('/ufrc/adamginsburg/d.jeff/imaging_results/*.fits')
z = 0.0002333587
#chem= input('Molecule?: ')
#chem=(' '+chem+' ')
linelist = input(
'Linelist? (Lovas, SLAIM, JPL, CDMS, ToyoMA, OSU, Recomb, Lisa, RFI): ')
speciesdata = {}
imgnames = ['spw2']
#'/ufrc/adamginsburg/d.jeff/imaging_results/SgrB2DS_field1_spw1_cube_medsub.image.fits'#'/ufrc/adamginsburg/d.jeff/imaging_results/SgrB2DS_field1_spw0_cube.image.fits'
cube = sc.read(fname)
header = fits.getheader(fname)
freqs = cube.spectral_axis
freq_max = freqs[0] * (1 + z) #215*u.GHz
freq_min = freqs[(len(freqs) - 1)] * (1 + z) #235*u.GHz
linewidth = 0.5 * 0.0097 * u.GHz
'''Generate methanol table for contaminant search'''
methanol_table = utils.minimize_table(
Splatalogue.query_lines(freq_min,
freq_max,
chemical_name=' CH3OH ',
energy_max=1840,
energy_type='eu_k',
line_lists=[linelist],
return wcs, data_masked
def cut_2d(data, position, size, wcs):
cut = Cutout2D(data=data, position=position, size=size, wcs=wcs)
data_cut = cut.data
wcs_cut = cut.wcs
return wcs_cut, data_cut
############################################################
### 12CO 1-0 cube processing. ###
name = imageDir + '12CO10/NGC5258_12CO10_combine_contsub_uvrange_pbcor.fits'
imagecube = SpectralCube.read(name)
common_beam = imagecube.beams.common_beam(tolerance=1e-5)
# Imcube = imagecube.convolve_to(common_beam)
smooth_beam = radio_beam.Beam(major=2.186 * u.arcsec,
minor=1.896 * u.arcsec,
pa=-87.6 * u.deg)
Imcube = imagecube.convolve_to(smooth_beam)
## create rms cube
rmscube = cube.calc_noise_in_cube(Imcube,
spatial_average_nbeam=1.0,
spectral_average_nchan=2)
## find the signal of the cube.
outcube = cube.find_signal_in_cube(Imcube,
rmscube,
j += 1
xi = i
xf = csize
subcubes.append('mwisp_' + str(j).zfill(2) + '_' + str(xi) + '_' + str(xf))
np.save(path + 'SUBCUBES/subfiles.npy', subcubes)
#%&%&%&%&%&%&%&%&%&%&%&%&%&%
# Slicing
#%&%&%&%&%&%&%&%&%&%&%&%&%&%
if do_slicing:
fcube = SpectralCube.read(mpath + full_cube_name + '.fits')
subfiles = np.load(path + 'SUBCUBES/subfiles.npy')
print("Slicing...")
#for j,subfile in enumerate(subfiles):
for j in range(len(subfiles)):
subfile = subfiles[j]
print(subfile)
xi = int(subfile.split('_')[2])
xf = int(subfile.split('_')[3])
scube = fcube[:, :, xi:xf]
def load_casa_image(filename,
skipdata=False,
skipvalid=False,
skipcs=False,
**kwargs):
"""
Load a cube (into memory?) from a CASA image. By default it will transpose
the cube into a 'python' order and drop degenerate axes. These options can
be suppressed. The object holds the coordsys object from the image in
memory.
"""
try:
from taskinit import ia
except ImportError:
raise ImportError(
"Could not import CASA (casac) and therefore cannot read CASA .image files"
)
# use the ia tool to get the file contents
ia.open(filename)
# read in the data
if not skipdata:
data = ia.getchunk()
# CASA stores validity of data as a mask
if not skipvalid:
valid = ia.getchunk(getmask=True)
# transpose is dealt with within the cube object
# read in coordinate system object
casa_cs = ia.coordsys()
wcs = wcs_casa2astropy(casa_cs)
# don't need this yet
# stokes = get_casa_axis(temp_cs, wanttype="Stokes", skipdeg=False,)
# if stokes == None:
# order = np.arange(self.data.ndim)
# else:
# order = []
# for ax in np.arange(self.data.ndim+1):
# if ax == stokes:
# continue
# order.append(ax)
# self.casa_cs = ia.coordsys(order)
# This should work, but coordsys.reorder() has a bug
# on the error checking. JIRA filed. Until then the
# axes will be reversed from the original.
# if transpose == True:
# new_order = np.arange(self.data.ndim)
# new_order = new_order[-1*np.arange(self.data.ndim)-1]
# print new_order
# self.casa_cs.reorder(new_order)
# close the ia tool
ia.close()
meta = {'filename': filename}
mask = BooleanArrayMask(wcs, np.logical_not(valid))
cube = SpectralCube(data, wcs, mask, meta=meta)
return cube
from __future__ import print_function
# TODO: put this in a package
execfile("/Users/adam/repos/w51evlareductionscripts/singledish_combine/singledish_combine.py")
from spectral_cube import SpectralCube
pairs = [
('CH3CN', 'CH3CN54_hires_lmv.fits', 'SgrB2_a_03_7M.CH3CN_5-4_3.image.pbcor.fits', 91.98705*1e9), #91971465000.0),
('H41a', 'H41a_lmv.fits', 'SgrB2_a_03_7M.H41a.image.pbcor.fits', 92034434000.0),
]
for species,iram,aca,restfrq in pairs:
print(species)
iramcube = SpectralCube.read(iram)
acacube = SpectralCube.read(aca)
mc = iramcube.with_spectral_unit(u.km/u.s, rest_value=restfrq*u.Hz,
velocity_convention='radio')
acac = acacube.with_spectral_unit(u.km/u.s, rest_value=restfrq*u.Hz,
velocity_convention='radio')
h1 = acacube.header
jyk = (1*u.Jy).to(u.K, u.brightness_temperature(h1['BMAJ']*u.deg *
h1['BMIN']*u.deg * 2 *
np.pi, h1['RESTFRQ']*u.Hz))
combcube,f2 = fourier_combine_cubes(acac, mc, highresscalefactor=jyk.value,
lowresfwhm=0.30*u.arcmin,
return_regridded_cube2=True)
f2.writeto("Regridded_"+iram, clobber=True)
f1 = fits.open(aca)
from astropy.io import fits
from spectral_cube import SpectralCube
from astropy import coordinates, units as u
centerN = coordinates.SkyCoord('17:47:19.877',
'-28:22:18.39',
frame='fk5',
unit=(u.hour, u.deg))
centerM = coordinates.SkyCoord('17:47:20.166',
'-28:23:04.68',
frame='fk5',
unit=(u.hour, u.deg))
for spw in (0, 1, 3, 2):
print("Extracting spw{0} M".format(spw))
cube = SpectralCube.read('full_SgrB2M_spw{0}_lines.fits'.format(spw))
center_M = centerM.transform_to(getattr(coordinates, cube.wcs.wcs.radesys))
cx, cy = map(
int,
cube.wcs.celestial.wcs_world2pix(centerM.ra.deg, centerM.dec.deg, 0))
cutout_M = cube[:, cy - 250:cy + 250, cx - 250:cx + 250]
cutout_M.write("full_SgrB2M_spw{0}_lines_cutoutM.fits".format(spw),
overwrite=True)
print("Extracting spw{0} N".format(spw))
cube = SpectralCube.read('full_SgrB2N_spw{0}_lines.fits'.format(spw))
center_N = centerN.transform_to(getattr(coordinates, cube.wcs.wcs.radesys))
cx, cy = map(
int,
cube.wcs.celestial.wcs_world2pix(centerN.ra.deg, centerN.dec.deg, 0))
cutout_N = cube[:, cy - 300:cy + 300, cx - 300:cx + 300]
0.04,
#0.05,
0.06,
#0.08,
0.10,
#0.15,
0.20,
#0.30,
0.40,
],
colors=['w'] * 12,
layer='alma_cont_hires')
F.save(paths.fpath("NACO_green_outflows_aplpy_CONTours_hires.png"))
F.save(paths.fpath("NACO_green_outflows_aplpy_CONTours_hires.pdf"))
h77a = SpectralCube.read(paths.vpath('data/W51north_H77_Outflow_cutout.fits'))
h77a_outflow = h77a.spectral_slab(-16 * u.km / u.s,
-60 * u.km / u.s).sum(axis=0)
h77a_green = paths.dpath('W51_H77a_LacyJetOutflow_Sum.fits')
h77a_outflow.hdu.writeto(h77a_green, clobber=True)
F.show_contour(h77a_green,
levels=[0.0075, 0.015, 0.030],
colors=['b'] * 6,
layer='h77a_outflow')
F.save(paths.fpath("NACO_green_outflows_aplpy_CONTours_hires_h77acontour.png"))
F.save(paths.fpath("NACO_green_outflows_aplpy_CONTours_hires_h77acontour.pdf"))
F.hide_layer('h77a_outflow')
F.hide_layer('alma_cont_hires')
from astropy import units as u
import paths
from constants import distance
from astropy import convolution
import radio_beam
#p303 = paths.dpath('w51_H2CO_303_202_contsub.image.pbcor.fits')
#p321 = paths.dpath('w51_H2CO_321_220_contsub.image.pbcor.fits')
p303 = paths.dpath('merge/W51_b6_7M_12M.H2CO303_202.regrid_medsub.fits')
p321 = paths.dpath('merge/W51_b6_7M_12M.H2CO321_220.regrid_medsub.fits')
p322 = paths.dpath('merge/W51_b6_7M_12M.H2CO322_221.regrid_medsub.fits')
beam_size_goal = 0.4*u.arcsec # change to 0.7 if using natural
if os.path.exists(p303) and os.path.exists(p321) and os.path.exists(p322):
cube303 = SpectralCube.read(p303)
cube321 = SpectralCube.read(p321)
cube322 = SpectralCube.read(p322)
else:
p303_ = paths.dpath('merge/W51_b6_7M_12M.H2CO303_202.image.pbcor.fits')
p321_ = paths.dpath('merge/W51_b6_7M_12M.H2CO321_220.image.pbcor.fits')
p322_ = paths.dpath('merge/W51_b6_7M_12M.H2CO322_221.image.pbcor.fits')
cube303 = SpectralCube.read(p303_).with_spectral_unit(u.km/u.s,
velocity_convention='radio').spectral_slab(25*u.km/u.s, 90*u.km/u.s)
min_slices = cube303.subcube_slices_from_mask(cube303.mask, spatial_only=True)
cube321 = SpectralCube.read(p321_).with_spectral_unit(u.km/u.s,
velocity_convention='radio').spectral_slab(25*u.km/u.s, 90*u.km/u.s)
cube322 = SpectralCube.read(p322_).with_spectral_unit(u.km/u.s,
velocity_convention='radio').spectral_slab(25*u.km/u.s, 90*u.km/u.s)
):
for field in "G353.41 G008.67 G337.92 W51-E W43-MM3 G328.25 G351.77 W43-MM1 G010.62 W51-IRS2 G012.80 G333.60 W43-MM2 G327.29 G338.93".split(
):
for spw in (0, 1, 2, 3, 4, 5, 6, 7):
filename = ftemplate.format(
spw=spw,
field=field,
band=band,
array=array,
suffix=suffix,
robust=robust,
)
if os.path.exists(filename):
cube = SpectralCube.read(filename, use_dask=True)
else:
log.exception("File {0} does not exist".format(filename))
if os.path.exists(filename[:-5]):
log.exception("But {0} does!!!!".format(filename[:-5]))
continue
for operation in ('mean', 'max', 'median'):
out_fn = f'spectra/{field}_{array}_{band}_spw{spw}_robust{robust}{suffix}.{operation}spec.fits'
if overwrite or not os.path.exists(out_fn):
spec = getattr(cube, operation)(axis=(1, 2))
#spec = cube.apply_numpy_function(getattr(np, 'nan'+operation),
# axis=(1,2),
# progressbar=True,
# projection=True,
# how='slice',
def _parse_hdu(app, hdulist, file_name=None):
if file_name is None:
if hasattr(hdulist, 'file_name'):
file_name = hdulist.file_name
file_name = file_name or "Unknown HDU object"
# WCS may only exist in a single extension (in this case, just the flux
# flux extension), so first find and store then wcs information.
wcs = None
for hdu in hdulist:
if hdu.data is None or not hdu.is_image:
continue
try:
sc = SpectralCube.read(hdu, format='fits')
except (ValueError, FITSReadError):
continue
else:
wcs = sc.wcs
# Now loop through and attempt to parse the fits extensions as spectral
# cube object. If the wcs fails to parse in any case, use the wcs
# information we scraped above.
for hdu in hdulist:
data_label = f"{file_name}[{hdu.name}]"
if hdu.data is None or not hdu.is_image:
continue
# This is supposed to fail on attempting to load anything that
# isn't cube-shaped. But it's not terribly reliable
try:
sc = SpectralCube.read(hdu, format='fits')
except (ValueError, OSError):
# This will fail if the parsing of the wcs does not provide
# proper celestial axes
try:
hdu.header.update(wcs.to_header())
sc = SpectralCube.read(hdu)
except (ValueError, AttributeError) as e:
logging.warn(e)
continue
except FITSReadError as e:
logging.warn(e)
continue
app.add_data(sc, data_label)
# If the data type is some kind of integer, assume it's the mask/dq
if hdu.data.dtype in (np.int, np.uint, np.uint32) or \
any(x in hdu.name.lower() for x in EXT_TYPES['mask']):
app.add_data_to_viewer('mask-viewer', data_label)
if 'errtype' in [x.lower() for x in hdu.header.keys()] or \
any(x in hdu.name.lower() for x in EXT_TYPES['uncert']):
app.add_data_to_viewer('uncert-viewer', data_label)
if any(x in hdu.name.lower() for x in EXT_TYPES['flux']):
app.add_data_to_viewer('flux-viewer', data_label)
app.add_data_to_viewer('spectrum-viewer', data_label)
def flux_hist(finaliter_prefix_b3,
finaliter_prefix_b6,
basepath='/home/adam/work/alma-imf/reduction/',
las=None):
image_b3 = SpectralCube.read(f'{finaliter_prefix_b3}.image.tt0.fits',
use_dask=False,
format='fits').minimal_subcube()
image_b6 = SpectralCube.read(f'{finaliter_prefix_b6}.image.tt0.fits',
use_dask=False,
format='fits').minimal_subcube()
image_b3 = image_b3 * u.beam / image_b3.beam.sr
image_b6 = image_b6 * u.beam / image_b6.beam.sr
fieldname = os.path.basename(finaliter_prefix_b6).split("_")[0]
if las:
smb3 = image_b3[0].convolve_to(radio_beam.Beam(las), allow_huge=True)
image_b3 = image_b3 - smb3
smb6 = image_b6[0].convolve_to(radio_beam.Beam(las), allow_huge=True)
image_b6 = image_b6 - smb6
noise_region_b3 = regions.read_ds9(
f"{basepath}/reduction/noise_estimation_regions/{fieldname}_B3_noise_sampling.reg"
)
noise_region_b6 = regions.read_ds9(
f"{basepath}/reduction/noise_estimation_regions/{fieldname}_B6_noise_sampling.reg"
)
noiseim_b3 = image_b3.subcube_from_regions(noise_region_b3)[0]
noiseim_b6 = image_b6.subcube_from_regions(noise_region_b6)[0]
b3_std = stats.mad_std(noiseim_b3, ignore_nan=True)
b6_std = stats.mad_std(noiseim_b6, ignore_nan=True)
print(fieldname, b3_std, b6_std)
fig = pl.figure(2, figsize=(12, 7))
fig.clf()
ax = pl.subplot(1, 2, 1)
b3data = image_b3[0].value
bins_b3 = np.linspace(np.nanmin(b3data), np.nanmax(b3data), 100)
bins_b3b = np.linspace(np.nanmin(b3data), np.nanmax(b3data), 10000)
H, L, P = ax.hist(b3data[np.isfinite(b3data)], bins=bins_b3, density=False)
#ax.hist(noiseim_b3.value.ravel(), bins=bins_b3)
ax.set_yscale('log')
ax.set_ylim(0.5, ax.get_ylim()[1])
ax.plot(bins_b3b,
H.max() * np.exp(-bins_b3b**2 / (2 * b3_std.value**2)), 'k')
ax.set_xlabel("$S_{3mm}$ [Jy/sr]")
ax.set_ylabel("Number of Pixels")
axin = fig.add_axes([0.25, 0.6, 0.20, 0.25])
bins = np.linspace(-5 * b3_std.value, 5 * b3_std.value, 100)
H, L, P = axin.hist(b3data[(b3data < 5 * b3_std.value)
& (b3data > -5 * b3_std.value)],
bins=bins,
density=False)
#axin.hist(noiseim_b3.value.ravel(), bins=bins)
gauss = H.max() * np.exp(-bins**2 / (2 * b3_std.value**2))
axin.plot(bins, gauss, 'k')
axin.set_xticklabels([])
axin.set_yticks(axin.get_yticks()[1:])
axin2 = fig.add_axes([0.25, 0.5, 0.2, 0.1])
loc = (L[1:] + L[:-1]) / 2
axin2.plot(loc,
H - H.max() * np.exp(-loc**2 / (2 * b3_std.value**2)),
drawstyle='steps',
color='k')
axin2.set_xlim(axin.get_xlim())
ax = pl.subplot(1, 2, 2)
b6data = image_b6[0].value
bins_b6 = np.linspace(np.nanmin(b6data), np.nanmax(b6data), 100)
bins_b6b = np.linspace(np.nanmin(b6data), np.nanmax(b6data), 10000)
H, L, P = ax.hist(b6data[np.isfinite(b6data)], bins=bins_b6, density=False)
ax.plot(bins_b6b,
H.max() * np.exp(-bins_b6b**2 / (2 * b6_std.value**2)), 'k')
#ax.hist(noiseim_b6.value.ravel(), bins=bins_b6)
ax.set_ylim(0.5, ax.get_ylim()[1])
ax.set_yscale('log')
ax.yaxis.set_label_position("right")
ax.yaxis.tick_right()
ax.set_xlabel("$S_{1mm}$ [Jy/sr]")
ax.set_ylabel("Number of Pixels")
axin = fig.add_axes([0.65, 0.6, 0.20, 0.25])
bins = np.linspace(-5 * b6_std.value, 5 * b6_std.value, 100)
H, L, P = axin.hist(b6data[(b6data < 5 * b6_std.value)
& (b6data > -5 * b6_std.value)],
bins=bins,
density=False)
#axin.hist(noiseim_b6.value.ravel(), bins=bins)
axin.plot(bins, H.max() * np.exp(-bins**2 / (2 * b6_std.value**2)), 'k')
axin.set_xticklabels([])
axin.set_yticks(axin.get_yticks()[1:])
axin2 = fig.add_axes([0.65, 0.5, 0.2, 0.1])
loc = (L[1:] + L[:-1]) / 2
axin2.plot(loc,
H - H.max() * np.exp(-loc**2 / (2 * b6_std.value**2)),
drawstyle='steps',
color='k')
axin2.set_xlim(axin.get_xlim())
def subtract_components(cube_name,
remove_params_name,
output_name,
chunk_size=20000):
'''
Subtract Gaussian components given in remove_params_name
'''
with fits.open(remove_params_name) as params_hdu:
params_array = params_hdu[0].data
# Create huge fits
ncomp_array = np.isfinite(params_array).sum(0) // 3
cube = SpectralCube.read(cube_name)
assert cube.shape[1:] == params_array.shape[1:]
# yposn, xposn = np.where(ncomp_array > 0)
yposn, xposn = np.indices(cube.shape[1:])
vels = cube.spectral_axis.to(u.m / u.s)
vels_val = vels.value
yshape, xshape = ncomp_array.shape
basename = os.path.basename(cube_name)
# Create the output cube.
from cube_analysis.io_utils import create_huge_fits
create_huge_fits(output_name, cube.header, fill_nan=True)
del cube
# evaluate and subtract all components
hdu = fits.open(output_name, mode='update')
cube_hdu = fits.open(cube_name, mode='denywrite')
for i, (y, x) in tqdm(enumerate(zip(yposn.ravel(),
xposn.ravel())),
ascii=True,
desc=f"Model eval. for: {basename[:15]}",
total=yposn.size):
# Reload cube to release memory
if i % chunk_size == 0:
hdu.flush()
hdu.close()
del hdu
hdu = fits.open(output_name, mode='update')
cube_hdu.close()
del cube_hdu
cube_hdu = fits.open(cube_name, mode='denywrite')
# No components = no change
if ncomp_array[y, x] == 0:
hdu[0].data[:, y, x] = cube_hdu[0].data[:, y, x]
continue
pars = params_array[:, y, x][np.isfinite(params_array[:, y, x])]
hdu[0].data[:, y, x] = cube_hdu[0].data[:, y, x] - \
multigaussian_nolmfit(vels_val, pars)
hdu.flush()
hdu.close()
del hdu
cube_hdu.close()
del cube_hdu
fifteenA_HI_BCtaper_04kms_data_wEBHIS_path("braun09_subcubes") + "/*.fits")
fifteenAtapercubes.sort()
noise_val = 2.8 * u.K # K
# Change to data directory
os.chdir(
fifteenA_HI_BCtaper_04kms_data_wEBHIS_path("braun09_subcubes",
no_check=True))
for i, subcube_name in enumerate(fifteenAtapercubes[::-1]):
subcube_filename = os.path.split(subcube_name)[-1][:-5]
subcube = SpectralCube.read(subcube_name)
# Smooth to 25"
# new_beam = Beam(25 * u.arcsec)
new_beam = subcube.beams.common_beam()
subcube = subcube.convolve_to(new_beam)
# Downsample the spectral resolution to 2.3 km/s
chan_width = np.diff(subcube.spectral_axis)[0]
# target = 2.3 * u.km / u.s
# target = chan_width * 2
# spec_kern = Gaussian1DKernel(np.sqrt((target / 2.)**2 - chan_width**2).value)
# subcube = subcube.spectral_smooth(spec_kern, verbose=True,
# num_cores=4)
# New spectral axis
m0fn = dpath("moments/{0}_medsub_moment0.fits".format(fname))
m1fn = dpath("moments/{0}_medsub_moment1.fits".format(fname))
m2fn = dpath("moments/{0}_medsub_moment2.fits".format(fname))
madstdfn = dpath("moments/{0}_medsub_madstd.fits".format(fname))
maxfn = dpath("moments/{0}_medsub_max.fits".format(fname))
argmaxfn = dpath("moments/{0}_medsub_argmax.fits".format(fname))
if os.path.exists(m0fn) and os.path.exists(madstdfn):
m0 = load_projection(m0fn)
m1 = load_projection(m1fn)
m2 = load_projection(m2fn)
pmax = load_projection(maxfn)
madstd = load_projection(madstdfn)
# argmaxfn = dpath("moments/{0}_medsub_argmax.fits".format(fname))
else:
cube = SpectralCube.read(dpath(fn)).minimal_subcube()
vcube = cube.with_spectral_unit(u.km / u.s,
velocity_convention='radio')
vcube.beam_threshold = 100
pct = 50
for key in cont_percentiles:
if key in fname:
pct = cont_percentiles[key]
contmasked_cube = vcube.with_mask(
((vcube.spectral_axis < 35 * u.km / u.s)
| (vcube.spectral_axis > 80 * u.km / u.s))[:, None, None])
med = contmasked_cube.percentile(pct, axis=0)
vcube = vcube.spectral_slab(50 * u.km / u.s, 65 * u.km / u.s)
def make_comparison_image(filename1, filename2, title1='bsens', title2='cleanest', writediff=False, allow_reproj=False, nticks=12,
asinh_scaling_factor=10, scalebarlength=15, diff_suffix='.preselfcal-diff'):
#fh_pre = fits.open()
#fh_post = fits.open()
cube_pre = SpectralCube.read(filename1, format='fits' if 'fits' in filename1 else 'casa_image').with_spectral_unit(u.GHz)
cube_post = SpectralCube.read(filename2, format='fits' if 'fits' in filename2 else 'casa_image').with_spectral_unit(u.GHz)
if 'pbcor' in filename1:
assert 'pbcor' in filename2
if 'pbcor' in filename2:
assert 'pbcor' in filename1
if allow_reproj:
if cube_pre.shape != cube_post.shape or (cube_post.wcs != cube_pre.wcs and cube_post.wcs.wcs != cube_pre.wcs.wcs):
cube_post = cube_post.reproject(cube_pre.header)
cube_pre = cube_pre.with_mask(cube_pre != 0*cube_pre.unit)
cube_post = cube_post.with_mask(cube_post != 0*cube_post.unit)
slices = cube_pre.subcube_slices_from_mask(cube_pre.mask & cube_post.mask,
spatial_only=True)[1:]
# make the cubes match the data; needed for later WCS cutouts
cube_pre = cube_pre[:, slices[0], slices[1]]
cube_post = cube_post[:, slices[0], slices[1]]
#cube_pre = cube_pre.minimal_subcube()
#cube_post = cube_post.minimal_subcube()
data_pre = cube_pre[0].value * 1e3
data_post = cube_post[0].value * 1e3
#data_pre[np.abs(data_pre) < 1e-7] = np.nan
#data_post[np.abs(data_post) < 1e-7] = np.nan
try:
diff = (data_post - data_pre)
except Exception as ex:
print(filename1, filename2, cube_pre.shape, cube_post.shape)
raise ex
ww = cube_post.wcs
pixscale = wcs.utils.proj_plane_pixel_area(ww)*u.deg**2
try:
beam = cube_post.beam
ppbeam = (beam.sr / pixscale).decompose()
assert ppbeam.unit.is_equivalent(u.dimensionless_unscaled)
ppbeam = ppbeam.value
except NoBeamError:
beam = np.nan*u.sr
ppbeam = np.nan
if writediff:
fits.PrimaryHDU(data=diff,
header=cube_post.header).writeto(filename2.split(".fits")[0]
+ diff_suffix + ".fits",
overwrite=True)
fig = pl.figure(1, figsize=(14,6))
fig.clf()
if fig.get_figheight() != 6:
fig.set_figheight(6)
if fig.get_figwidth() != 14:
fig.set_figwidth(14)
data_pre_display = np.arcsinh(data_pre*asinh_scaling_factor)
data_post_display = np.arcsinh(data_post*asinh_scaling_factor)
diff_display = np.arcsinh(diff*asinh_scaling_factor)
minv = np.nanpercentile(data_pre_display, 0.05)
maxv = np.nanpercentile(data_pre_display, 99.5)
if maxv > np.arcsinh(1000):
maxv = np.arcsinh(1000)
if np.abs(minv) > maxv:
minv = -maxv
norm = visualization.simple_norm(data=diff_display.squeeze(), stretch='linear',
#min_percent=0.05, max_percent=99.995,)
min_cut=minv, max_cut=maxv)
#cm = pl.matplotlib.cm.gray
#cm.set_bad('white', 0)
cm = pl.matplotlib.cm.viridis
ax1 = pl.subplot(1,3,1)
ax2 = pl.subplot(1,3,2)
ax3 = pl.subplot(1,3,3)
for ax in (ax1,ax2,ax3):
ax.cla()
ax1.imshow(data_pre_display, norm=norm, origin='lower', interpolation='nearest', cmap=cm)
ax1.set_title(title1)
# scalebar
ww = cube_pre.wcs.celestial
cd = (ww.pixel_scale_matrix[1,1] * 3600)
blc = np.array(diff.shape)*0.1
ax1.add_patch(matplotlib.patches.Rectangle([blc[1]*0.8, blc[0]*0.9],
width=scalebarlength/cd*1.4,
height=blc[0]*0.6,
edgecolor='k', facecolor='w',
alpha=0.5))
ax1.plot([blc[1], blc[1]+scalebarlength/cd], [blc[0], blc[0]], color='k')
tx = ax1.annotate(f'{scalebarlength}"', (blc[1]+scalebarlength/2/cd, blc[0]*1.1))
tx.set_horizontalalignment('center')
ax2.imshow(data_post_display, norm=norm, origin='lower', interpolation='nearest', cmap=cm)
ax2.set_title(title2)
im = ax3.imshow(diff_display.squeeze(), norm=norm, origin='lower', interpolation='nearest', cmap=cm)
ax3.set_title(f"{title2} - {title1}")
for ax in (ax1,ax2,ax3):
ax.set_xticks([])
ax.set_yticks([])
pl.subplots_adjust(wspace=0.0)
cbax = fig.add_axes([0.91,0.18,0.03,0.64])
cb = fig.colorbar(cax=cbax, mappable=im)
cb.set_label("S$_\\nu$ [mJy/beam]")
mn,mx = cb.get_ticks().min(), cb.get_ticks().max()
ticklocs = np.concatenate([np.linspace(-norm.vmax, 0, nticks//2)[:-1], np.linspace(0, norm.vmax, nticks//2)])
ticks = np.sinh(ticklocs)
cb.update_normal(im)
cb.set_ticks(ticks)
ticklocs = cb.get_ticks()
ticklabels = [f"{np.sinh(x/asinh_scaling_factor):0.2f}" for x in ticklocs]
cb.set_ticklabels(ticklabels)
meta = parse_fn(filename1)
reg = get_noise_region(meta['region'], meta['band'])
if reg is not None:
reglist = regions.read_ds9(reg)
composite_region = reduce(operator.or_, reglist)
if hasattr(composite_region, 'to_mask'):
msk = composite_region.to_mask()
else:
preg = composite_region.to_pixel(cube_pre.wcs.celestial)
msk = preg.to_mask()
cutout_pixels_pre = msk.cutout(data_pre, fill_value=np.nan)[msk.data.astype('bool')]
mad_sample_pre = mad_std(cutout_pixels_pre, ignore_nan=True)
std_sample_pre = np.nanstd(cutout_pixels_pre)
if hasattr(composite_region, 'to_mask'):
msk = composite_region.to_mask()
else:
preg = composite_region.to_pixel(cube_post.wcs.celestial)
msk = preg.to_mask()
cutout_pixels_post = msk.cutout(data_post, fill_value=np.nan)[msk.data.astype('bool')]
mad_sample_post = mad_std(cutout_pixels_post, ignore_nan=True)
std_sample_post = np.nanstd(cutout_pixels_post)
if np.any(np.isnan(mad_sample_pre)):
log.warning("mad_sample_pre contains some NaN values")
if np.any(np.isnan(mad_sample_post)):
log.warning("mad_sample_post contains some NaN values")
if len(cutout_pixels_post) != len(cutout_pixels_pre):
log.warning(f"cutout pixels are different size in pre vs post ({filename1} : {filename2})")
if (cube_pre.wcs.celestial != cube_post.wcs.celestial) and (cube_pre.wcs.celestial.wcs != cube_post.wcs.celestial.wcs):
# wcs comparisons stopped working sometime in 2019-2020 - wcs.wcs comparisons appear to work?
log.warning(f"post and pre have different celestial WCSes ({filename1} : {filename2})")
if not np.isfinite(mad_sample_pre):
raise ValueError
mad_pre = mad_std(data_pre, ignore_nan=True)
mad_post = mad_std(data_post, ignore_nan=True)
mad_diff = mad_std(diff, ignore_nan=True)
diffmask = np.abs(diff) > 3*mad_diff
history = cube_post.header['HISTORY']
hasamp = any("'calmode': 'ap'" in x for x in history) or any("'calmode': 'a'" in x for x in history)
diffstats = {'mean': np.nanmean(diff),
'max': np.nanmax(diff),
'shape': diff.shape[0],
'ppbeam': ppbeam,
'sum': np.nansum(diff),
'masksum': diff[diffmask].sum(),
'min': np.nanmin(diff),
'median': np.nanmedian(diff),
'mad': mad_diff,
'dr_pre': np.nanmax(data_pre) / mad_std(data_pre, ignore_nan=True),
'dr_post': np.nanmax(data_post) / mad_std(data_post, ignore_nan=True),
'min_pre': np.nanmin(data_pre),
'min_post': np.nanmin(data_post),
'max_pre': np.nanmax(data_pre),
'max_post': np.nanmax(data_post),
'sum_pre': np.nansum(data_pre),
'sum_post': np.nansum(data_post),
'masksum_pre': (data_pre[data_pre > mad_pre*3]).sum(),
'masksum_post': (data_post[data_post > mad_post*3]).sum(),
'mad_pre': mad_pre,
'mad_post': mad_post,
'mad_sample_pre': np.nan,
'mad_sample_post': np.nan,
'std_sample_pre': np.nan,
'std_sample_post': np.nan,
'has_amp': hasamp,
}
if reg is not None:
diffstats.update({
'mad_sample_pre': mad_sample_pre,
'mad_sample_post': mad_sample_post,
'std_sample_pre': std_sample_pre,
'std_sample_post': std_sample_post,
})
return ax1, ax2, ax3, fig, diffstats
mywcs.wcs.ctype = ["RA---TAN", "DEC--TAN", 'VELO']
mywcs.wcs.cunit = ['deg', 'deg', 'm/s']
# Create a synthetic X-dimension in km/s
xarr = np.linspace(50, 70, 41) # km/s
# Define a line width, which will vary across our image
# It will increase from 1 km/s to 4 km/s over the X-direction (RA)
sigma = np.outer(np.linspace(1, 1.5, 2), np.ones(4)).T
# Define a line center, which will vary in the opposite direction,
# along increasing Y-direction (declination)
centroid = np.outer(np.ones(2), np.linspace(58, 62, 4)).T
data = np.exp(-(np.tile(xarr, (2, 4, 1)).T - centroid)**2 / (2. * sigma**2))
cube = SpectralCube(data=data, wcs=mywcs)
# Sanity checks: do the moments accurately recover the inputs?
assert (np.abs(cube.moment1().to(u.km / u.s).value - centroid).max()) < 1e-5
assert (np.abs(cube.moment2().to(u.km**2 / u.s**2).value -
sigma**2).max()) < 1e-5
# Create a pyspeckit cube
pcube = pyspeckit.Cube(cube=cube)
# For convenience, convert the X-axis to km/s
# (WCSLIB automatically converts to m/s even if you give it km/s)
pcube.xarr.convert_to_unit(u.km / u.s)
# Set up the fitter by doing a preliminary fit
pcube.specfit(fittype='gaussian', guesses='moments')
import pylab as pl
pl.close('all')
apertures = ((1, 2, 3, 4) * u.pc / (8.4 * u.kpc)).to
velo = 62.5 * u.km / u.s
species_names = list(restfreqs.keys())
frequencies = u.Quantity([restfreqs[key] for key in species_names], unit=u.GHz)
for fn in glob.glob(paths.Fpath('tp/tp_concat*fits')):
basefn = os.path.basename(fn)
outf = paths.Fpath('tp/avgspectra/avg_{0}'.format(basefn))
if not os.path.exists(outf):
cube = SpectralCube.read(fn)
cube.allow_huge_operations = True
mad = cube.mad_std(axis=0)
sum = (cube * mad).sum(axis=(1, 2))
mean = sum / np.nansum(mad)
mean.write(paths.Fpath(
'tp/avgspectra/weighted_avg_{0}'.format(basefn)),
overwrite=True)
mn = cube.mean(axis=(1, 2))
mn.write(outf, overwrite=True)
for fn in glob.glob(paths.Fpath('tp/tp_concat*fits')):
basefn = os.path.basename(fn)
#spw = pyspeckit.Spectrum('avspec/weighted_avg_{0}'.format(fn))
sp = pyspeckit.Spectrum(paths.Fpath(
'tp/avgspectra/avg_{0}'.format(basefn)))
def make_comparison_image(filename1,
filename2,
title1='bsens',
title2='cleanest',
writediff=False,
allow_reproj=False):
#fh_pre = fits.open()
#fh_post = fits.open()
cube_pre = SpectralCube.read(filename1,
format='fits' if 'fits' in filename1 else
'casa_image').with_spectral_unit(u.GHz)
cube_post = SpectralCube.read(filename2,
format='fits' if 'fits' in filename2 else
'casa_image').with_spectral_unit(u.GHz)
if 'pbcor' in filename1:
assert 'pbcor' in filename2
if 'pbcor' in filename2:
assert 'pbcor' in filename1
if allow_reproj:
if cube_pre.shape != cube_post.shape or (
cube_post.wcs != cube_pre.wcs
and cube_post.wcs.wcs != cube_pre.wcs.wcs):
cube_post = cube_post.reproject(cube_pre.header)
cube_pre = cube_pre.with_mask(cube_pre != 0 * cube_pre.unit)
cube_post = cube_post.with_mask(cube_post != 0 * cube_post.unit)
slices = cube_pre.subcube_slices_from_mask(cube_pre.mask & cube_post.mask,
spatial_only=True)[1:]
# make the cubes match the data; needed for later WCS cutouts
cube_pre = cube_pre[:, slices[0], slices[1]]
cube_post = cube_post[:, slices[0], slices[1]]
#cube_pre = cube_pre.minimal_subcube()
#cube_post = cube_post.minimal_subcube()
data_pre = cube_pre[0].value
data_post = cube_post[0].value
data_pre[np.abs(data_pre) < 1e-7] = np.nan
data_post[np.abs(data_post) < 1e-7] = np.nan
try:
diff = (data_post - data_pre)
except Exception as ex:
print(filename1, filename2, cube_pre.shape, cube_post.shape)
raise ex
ww = cube_post.wcs
beam = cube_post.beam
pixscale = wcs.utils.proj_plane_pixel_area(ww) * u.deg**2
ppbeam = (beam.sr / pixscale).decompose()
assert ppbeam.unit.is_equivalent(u.dimensionless_unscaled)
ppbeam = ppbeam.value
if writediff:
fits.PrimaryHDU(data=diff, header=cube_post.header).writeto(
filename2.split(".fits")[0] + ".preselfcal-diff.fits",
overwrite=True)
fig = pl.figure(1, figsize=(14, 6))
fig.clf()
if fig.get_figheight() != 6:
fig.set_figheight(6)
if fig.get_figwidth() != 14:
fig.set_figwidth(14)
minv = np.nanpercentile(data_pre, 0.05)
maxv = np.nanpercentile(data_pre, 99.5)
if np.abs(minv) > maxv:
minv = -maxv
norm = visualization.simple_norm(
data=diff.squeeze(),
stretch='asinh',
#min_percent=0.05, max_percent=99.995,)
min_cut=minv,
max_cut=maxv)
if norm.vmax < 0.001:
norm.vmax = 0.001
cm = pl.matplotlib.cm.gray
cm.set_bad('white', 0)
ax1 = pl.subplot(1, 3, 1)
ax2 = pl.subplot(1, 3, 2)
ax3 = pl.subplot(1, 3, 3)
for ax in (ax1, ax2, ax3):
ax.cla()
ax1.imshow(data_pre,
norm=norm,
origin='lower',
interpolation='nearest',
cmap=cm)
ax1.set_title(title1)
ax2.imshow(data_post,
norm=norm,
origin='lower',
interpolation='nearest',
cmap=cm)
ax2.set_title(title2)
im = ax3.imshow(diff.squeeze(),
norm=norm,
origin='lower',
interpolation='nearest',
cmap=cm)
ax3.set_title(f"{title2} - {title1}")
for ax in (ax1, ax2, ax3):
ax.set_xticks([])
ax.set_yticks([])
pl.subplots_adjust(wspace=0.0)
cbax = fig.add_axes([0.91, 0.18, 0.03, 0.64])
fig.colorbar(cax=cbax, mappable=im)
meta = parse_fn(filename1)
reg = get_noise_region(meta['region'], meta['band'])
if reg is not None:
reglist = regions.read_ds9(reg)
composite_region = reduce(operator.or_, reglist)
if hasattr(composite_region, 'to_mask'):
msk = composite_region.to_mask()
else:
preg = composite_region.to_pixel(cube_pre.wcs.celestial)
msk = preg.to_mask()
cutout_pixels_pre = msk.cutout(
data_pre, fill_value=np.nan)[msk.data.astype('bool')]
mad_sample_pre = mad_std(cutout_pixels_pre, ignore_nan=True)
std_sample_pre = np.nanstd(cutout_pixels_pre)
if hasattr(composite_region, 'to_mask'):
msk = composite_region.to_mask()
else:
preg = composite_region.to_pixel(cube_post.wcs.celestial)
msk = preg.to_mask()
cutout_pixels_post = msk.cutout(
data_post, fill_value=np.nan)[msk.data.astype('bool')]
mad_sample_post = mad_std(cutout_pixels_post, ignore_nan=True)
std_sample_post = np.nanstd(cutout_pixels_post)
if np.any(np.isnan(mad_sample_pre)):
log.warning("mad_sample_pre contains some NaN values")
if np.any(np.isnan(mad_sample_post)):
log.warning("mad_sample_post contains some NaN values")
if len(cutout_pixels_post) != len(cutout_pixels_pre):
log.warning(
f"cutout pixels are different size in pre vs post ({filename1} : {filename2})"
)
if (cube_pre.wcs.celestial != cube_post.wcs.celestial) and (
cube_pre.wcs.celestial.wcs != cube_post.wcs.celestial.wcs):
# wcs comparisons stopped working sometime in 2019-2020 - wcs.wcs comparisons appear to work?
log.warning(
f"post and pre have different celestial WCSes ({filename1} : {filename2})"
)
if not np.isfinite(mad_sample_pre):
raise ValueError
mad_pre = mad_std(data_pre, ignore_nan=True)
mad_post = mad_std(data_post, ignore_nan=True)
mad_diff = mad_std(diff, ignore_nan=True)
diffmask = np.abs(diff) > 3 * mad_diff
diffstats = {
'mean': np.nanmean(diff),
'max': np.nanmax(diff),
'shape': diff.shape[0],
'ppbeam': ppbeam,
'sum': np.nansum(diff),
'masksum': diff[diffmask].sum(),
'min': np.nanmin(diff),
'median': np.nanmedian(diff),
'mad': mad_diff,
'dr_pre': np.nanmax(data_pre) / mad_std(data_pre, ignore_nan=True),
'dr_post': np.nanmax(data_post) / mad_std(data_post, ignore_nan=True),
'min_pre': np.nanmin(data_pre),
'min_post': np.nanmin(data_post),
'max_pre': np.nanmax(data_pre),
'max_post': np.nanmax(data_post),
'sum_pre': np.nansum(data_pre),
'sum_post': np.nansum(data_post),
'masksum_pre': (data_pre[data_pre > mad_pre * 3]).sum(),
'masksum_post': (data_post[data_post > mad_post * 3]).sum(),
'mad_pre': mad_pre,
'mad_post': mad_post,
'mad_sample_pre': np.nan,
'mad_sample_post': np.nan,
'std_sample_pre': np.nan,
'std_sample_post': np.nan,
}
if reg is not None:
diffstats.update({
'mad_sample_pre': mad_sample_pre,
'mad_sample_post': mad_sample_post,
'std_sample_pre': std_sample_pre,
'std_sample_post': std_sample_post,
})
return ax1, ax2, ax3, fig, diffstats
plot.plot(x, y.value, drawstyle='steps')
plot.set_title(trans)
'''
print(f'ymin: {y.min()}')
print(f'yvaluemin: {y.value.min()}')
print(f'tempymin/ymin: {tempymin/y.value.min()}')
'''
def contamlines(plot, contamlinelist):
return
for i in range(len(files)):
print('Getting ready - ' + imgnames[i])
cube = sc.read(files[i])
header = fits.getheader(files[i])
freqs = cube.spectral_axis
freqflip = False
if freqs[0] > freqs[1]:
freqs = freqs[::-1]
freqflip = True
print('Corrected decreasing frequency axis')
else:
pass
freq_min = freqs[0] * (1 + z) #215*u.GHz
freq_max = freqs[(len(freqs) - 1)] * (1 + z) #235*u.GHz
assert freq_max > freq_min, 'Decreasing frequency axis'
import paths
files = [
'OrionSourceI_Unknown_1_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_2_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_3_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_4_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_5_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_8_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_9_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_Unknown_10_robust0.5maskedclarkclean10000_medsub_K.fits',
'OrionSourceI_U229.682_robust0.5maskedclarkclean10000_medsub_K.fits',
]
allbeamlist = [
SpectralCube.read(paths.dpath('cubes/' + fn)).beams.common_beam()
for fn in files
]
allbeams = radio_beam.Beams(major=u.Quantity([x.major for x in allbeamlist]),
minor=u.Quantity([x.minor for x in allbeamlist]),
pa=u.Quantity([x.pa for x in allbeamlist]))
refbeam = allbeams.common_beam()
refcube = SpectralCube.read(paths.dpath('cubes/' + files[0]))
refcube = refcube.convolve_to(refbeam)
stackcube = [refcube]
for cubefn in files[1:]:
reproj_cube = (SpectralCube.read(
paths.dpath('cubes/' +
import numpy as np
from paths import hpath, mpath, fpath
from astropy import log
from spectral_cube import SpectralCube, BooleanArrayMask
from masked_cubes import (cube303m, cube321m, cube303msm, cube321msm, cube303,
cube321, cube303sm, cube321sm, sncube, sncubesm)
for suffix in ("", "_smooth"):
outpath = 'TemperatureCube_DendrogramObjects{0}.fits'
tcube = SpectralCube.read(hpath(outpath.format(suffix)))
outpath_leaf = 'TemperatureCube_DendrogramObjects{0}_leaves.fits'
tcubeleaf = SpectralCube.read(hpath(outpath_leaf.format(suffix)))
integ = tcube.mean(axis=0)
integ.hdu.writeto(hpath(outpath.format(suffix)).replace(
".fits", "_integ.fits"),
clobber=True)
integleaf = tcubeleaf.mean(axis=0)
integleaf.hdu.writeto(hpath(outpath_leaf.format(suffix)).replace(
".fits", "_integ.fits"),
clobber=True)
hdu_template = integ.hdu
log.info("Writing Weighted Integrated TemperatureCube")
tcubed = tcube.filled_data[:].value
weight_cube = cube303sm if 'smooth' in suffix else cube303
weights = weight_cube.filled_data[:].value
weights[weights < 0] = 0
def deblend(para,
specCubeRef,
vmin=4.0,
vmax=11.0,
f_spcsamp=None,
tau_wgt=0.1,
n_cpu=None):
'''
Deblend hyperfine structures in a cube based on fitted models, i.e., reconstruct the fitted model with Gaussian
lines with optical depths accounted for (e.g., similar to CO (J = 0-1))
:param para: <ndarray>
The fitted parameters in the order of vel, width, tex, and tau for each velocity slab.
(Note: the size of the z axis for para must thus be in the multiple of 4)
:param specCubeRef: <SpectralCube.Cube>
The reference cube from which the deblended cube is constructed from
:param vmin: <float>
The lower veloicty limit on the deblended cube in the unit of km/s
:param vmax: <float>
The upper veloicty limit on the deblended cube in the unit of km/s
:param f_spcsamp: <int>
The scaling factor for the spectral sampling relative the reference cube
(e.g., f_spcsamp = 2 give you twice the spectral resolution)
:param tau_wgt:
The scaling factor for the input tau
(e.g., tau_wgt = 0.1 better represents the true optical depth of a NH3 (1,1) hyperfine group than the
"fitted tau")
:param n_cpu: <int>
The number of cpus to use. If None, defaults to all the cpus available minus one.
:return mcube: <SpectralCube.Cube>
The deblended cube
'''
# open the reference cube file
cube = specCubeRef
cube = cube.with_spectral_unit(u.km / u.s, velocity_convention='radio')
# trim the cube to the specified velocity range
cube = cube.spectral_slab(vmin * u.km / u.s, vmax * u.km / u.s)
# generate an empty SpectralCube to house the deblended cube
if f_spcsamp is None:
deblend = np.zeros(cube.shape)
hdr = cube.wcs.to_header()
wcs_new = cube.wcs
else:
deblend = np.zeros(
(cube.shape[0] * int(f_spcsamp), cube.shape[1], cube.shape[2]))
wcs_new = cube.wcs.deepcopy()
# adjust the spectral reference value
wcs_new.wcs.crpix[2] = wcs_new.wcs.crpix[2] * int(f_spcsamp)
# adjust the spaxel size
wcs_new.wcs.cdelt[2] = wcs_new.wcs.cdelt[2] / int(f_spcsamp)
hdr = wcs_new.to_header()
# retain the beam information
hdr['BMAJ'] = cube.header['BMAJ']
hdr['BMIN'] = cube.header['BMIN']
hdr['BPA'] = cube.header['BPA']
mcube = SpectralCube(deblend, wcs_new, header=hdr)
# convert back to an unit that the ammonia hf model can handle (i.e. Hz) without having to create a
# pyspeckit.spectrum.units.SpectroscopicAxis object (which runs rather slow for model building in comparison)
mcube = mcube.with_spectral_unit(u.Hz, velocity_convention='radio')
xarr = mcube.spectral_axis
yy, xx = np.indices(para.shape[1:])
# a pixel is valid as long as it has a single finite value
isvalid = np.any(np.isfinite(para), axis=0)
valid_pixels = zip(xx[isvalid], yy[isvalid])
def model_a_pixel(xy):
x, y = int(xy[0]), int(xy[1])
# nh3_vtau_singlemodel_deblended takes Hz as the spectral unit
models = [
nh3_deblended.nh3_vtau_singlemodel_deblended(xarr,
Tex=tex,
tau=tau * tau_wgt,
xoff_v=vel,
width=width)
for vel, width, tex, tau in zip(para[::4, y, x], para[1::4, y, x],
para[2::4, y, x], para[3::4, y, x])
]
mcube._data[:, y, x] = np.nansum(np.array(models), axis=0)
return ((x, y), mcube._data[:, y, x])
if n_cpu is None:
n_cpu = cpu_count() - 1
else:
n_cpu = 1
if n_cpu > 1:
print("------------------ deblending cube -----------------")
print("number of cpu used: {}".format(n_cpu))
sequence = [(x, y) for x, y in valid_pixels]
result = parallel_map(model_a_pixel, sequence, numcores=n_cpu)
merged_result = [
core_result for core_result in result if core_result is not None
]
for mr in merged_result:
((x, y), model) = mr
x = int(x)
y = int(y)
mcube._data[:, y, x] = model
else:
for xy in ProgressBar(list(valid_pixels)):
model_a_pixel(xy)
# convert back to km/s in units before saving
mcube = mcube.with_spectral_unit(u.km / u.s, velocity_convention='radio')
gc.collect()
print("--------------- deblending completed ---------------")
return mcube
#"SgrB2_b3_7M_12M_natural.H2CS322-221.image.pbcor.fits",
#"SgrB2_b3_7M_12M_natural.H41a.image.pbcor.fits",
#"SgrB2_b3_7M_12M_natural.HC3N.image.pbcor.fits",
#"SgrB2_b3_7M_12M_natural.HCN.image.pbcor.fits",
#"SgrB2_b3_7M_12M_natural.HCOp.image.pbcor.fits",
#"SgrB2_b3_7M_12M_natural.HNC.image.pbcor.fits",
):
suffix, species, robust = speciesre.search(interferometer_fn).groups()
outfilename = ('{species}{suffix}{robust}_TP_7m_12m_feather.fits'.format(
species=species, suffix=suffix, robust=robust))
medsubfn = ('{species}{suffix}{robust}_7m_12m_medsub.fits'.format(
species=species, suffix=suffix, robust=robust))
if not os.path.exists(medsubfn):
cube = (SpectralCube.read(dpath(interferometer_fn)).with_spectral_unit(
u.km / u.s, velocity_convention='radio'))
cube.beam_threshold = 100
# try to avoid contamination... won't work universally; need to examine
# individual cubes and have this as a parameter
#med = cube.spectral_slab(90*u.km/u.s, 160*u.km/u.s).median(axis=0).value
med = cube.spectral_slab(velocity_ranges[species][0] * u.km / u.s,
velocity_ranges[species][1] * u.km /
u.s).median(axis=0).value
cube.write(medsubfn, overwrite=True)
fh = fits.open(medsubfn, mode='update')
log.info("Median subtracting")
pb = ProgressBar(len(fh[0].data))
for ii, imslice in enumerate(fh[0].data):
fh[0].data[ii] = imslice - med
fh.flush()
pb.update()
'12CO2-1': {
'blue': [30, 50],
'red': [70, 95],
},
},
}
cutout_dict = {'LacyJet': 'north'}
for objname in vrange_dict:
for species in vrange_dict[objname]:
for shift in vrange_dict[objname][species]:
fn = paths.dpath(
'12m/cutouts/W51_b6_12M.{0}.image.pbcor_{1}cutout.fits'.format(
species, cutout_dict[objname]))
cube = SpectralCube.read(fn).with_spectral_unit(
u.km / u.s, velocity_convention='radio')
cube.beam_threshold = 1.0
med = cube.percentile(25, axis=0)
medsub = cube - med
vrange = vrange_dict[objname][species][shift]
slab = medsub.spectral_slab(*(vrange * u.km / u.s))
m0 = slab.moment0()
m0.write(
paths.dpath('12m/moments/{objname}_{species}_{shift}'
'{v1}_{v2}.fits'.format(
objname=objname,
species=species,
import pylab as pl
molecules = [
'CFp',
'CH3CN_5-4_3',
'H2CO615-616',
'H2CS',
'H2CS303-202',
'H2CS321-220',
'H41a',
'HC3N',
'HCN',
'HCOp',
'HNC',
]
cubes = {
mol: SpectralCube.read(
'SgrB2_a_03_7M.{0}.image.pbcor.fits'.format(mol)).with_spectral_unit(
u.km / u.s, velocity_convention='radio')
for mol in molecules
}
pcubes = {mol: pyspeckit.Cube(cube=cubes[mol]) for mol in molecules}
fig1 = pl.figure(1)
fig1.clf()
for pcube in pcubes.values():
pcube.plot_spectrum(101, 90, clear=False, figure=fig1)
def neighbourhood_fit_comparison(cube_name, params_name, chunk_size=80000,
diff_bic=10, err_map=None,
use_ncomp_check=True,
reverse_direction=False):
'''
Lazily account for spatial continuity by checking the fit
of each pixel relative to its neighbours.
If delta BIC < -10, will attempt to refit the pixel with that
neighbour's model.
If there is a difference in the number of components, will also
attempt to refit with a different number of components initialized
to the neighbour's fit.
This is done in serial. Which isn't ideal but accounts for other pixels
first being updated.
'''
with fits.open(params_name, memmap=False, mode='denywrite') as params_hdu:
params_array = params_hdu[0].data
uncerts_array = params_hdu[1].data
bic_array = params_hdu[2].data.squeeze()
ncomp_array = np.isfinite(params_array).sum(0) // 3
cube = SpectralCube.read(cube_name)
assert cube.shape[1:] == bic_array.shape
if err_map is not None:
if hasattr(err_map, 'value'):
err_map = err_map.value.copy()
assert err_map.shape == bic_array.shape
# Number of pixels with valid fits.
yposn, xposn = np.where(np.isfinite(bic_array) & (ncomp_array > 0))
if reverse_direction:
yposn = yposn[::-1]
xposn = xposn[::-1]
yshape, xshape = bic_array.shape
basename = os.path.basename(cube_name)
for i, (y, x) in tqdm(enumerate(zip(yposn, xposn)),
ascii=True,
desc=f"Rev. fit for: {basename[:15]}",
total=yposn.size):
err = None if err_map is None else err_map[y, x]
# Reload cube to release memory
if i % chunk_size == 0 and i != 0:
del cube
cube = SpectralCube.read(cube_name)
# Slice out 3x3 neighbourhood of y, x
ymin = max(0, y - 1)
ymax = min(yshape, y + 2)
xmin = max(0, x - 1)
xmax = min(xshape, x + 2)
bic_neighb = bic_array[ymin:ymax, xmin:xmax].copy()
ncomp_neighb = ncomp_array[ymin:ymax, xmin:xmax]
bic_neighb[ncomp_neighb == 0] = np.NaN
orig_posn = np.where(bic_neighb == bic_array[y, x])
orig_index = (orig_posn[0][0], orig_posn[1][0])
# If no valid neighbours, skip:
if np.isfinite(bic_neighb).sum() == 1:
continue
# Condition 1: delta BIC
if np.nanmax(bic_array[y, x] - bic_neighb) >= diff_bic:
argmin = np.unravel_index(np.nanargmin(bic_neighb), (3, 3))
yneighb = y + (argmin[0] - 1)
xneighb = x + (argmin[1] - 1)
# Refit
spec = cube[:, y, x]
init_params = params_array[:, yneighb, xneighb]
init_params = init_params[np.isfinite(init_params)]
# assert init_params.size > 0
out_new = \
refit_multigaussian(spec, init_params,
vels=None,
vcent=None,
err=err,
amp_const=None,
cent_const=None,
sigma_const=None,
discrete_fitter=False)
if bic_array[y, x] - out_new.bic >= diff_bic:
# Update the parameter array
params_array[:, y, x] = np.NaN
params_array[:len(out_new.params), y, x] = \
[val.value for val in out_new.params.values()]
uncerts_array[:, y, x] = np.NaN
uncerts_array[:len(out_new.params), y, x] = \
[val.stderr if val.stderr is not None else np.NaN
for val in out_new.params.values()]
bic_array[y, x] = out_new.bic
continue
# Condition 2: Change in # of components
elif ((ncomp_array[y, x] - ncomp_neighb) != 0).any():
if not use_ncomp_check:
continue
# We'll do this twice with the largest and smallest number of
# components.
# The lowest BIC fit will be kept.
spec = cube[:, y, x]
max_comp = ncomp_neighb.max()
min_bic = bic_neighb[ncomp_neighb == max_comp].min()
posn = np.where(bic_neighb == min_bic)
argmax = (posn[0][0], posn[1][0])
# Skip max if this is the original spectrum
if argmax == orig_index:
maxcomp_bic = bic_array[y, x]
else:
yneighb = y + (argmax[0] - 1)
xneighb = x + (argmax[1] - 1)
# Refit
init_params_max = params_array[:, yneighb, xneighb]
init_params_max = init_params_max[np.isfinite(init_params_max)]
assert init_params_max.size > 0
out_new_max = \
refit_multigaussian(spec, init_params_max,
vels=None,
vcent=None,
err=err,
amp_const=None,
cent_const=None,
sigma_const=None,
discrete_fitter=False)
maxcomp_bic = out_new_max.bic
min_comp = ncomp_neighb[ncomp_neighb > 0].min()
min_bic = bic_neighb[ncomp_neighb == min_comp].min()
posn = np.where(bic_neighb == min_bic)
argmin = (posn[0][0], posn[1][0])
# Skip max if this is the original spectrum
if argmin == orig_index:
mincomp_bic = bic_array[y, x]
else:
yneighb = y + (argmin[0] - 1)
xneighb = x + (argmin[1] - 1)
# Refit
init_params_min = params_array[:, yneighb, xneighb]
init_params_min = init_params_min[np.isfinite(init_params_min)]
assert init_params_min.size > 0
out_new_min = \
refit_multigaussian(spec, init_params_min,
vels=None,
vcent=None,
err=err,
amp_const=None,
cent_const=None,
sigma_const=None,
discrete_fitter=False)
mincomp_bic = out_new_min.bic
diff_maxcomp = (bic_array[y, x] - maxcomp_bic) >= diff_bic
diff_mincomp = (bic_array[y, x] - mincomp_bic) >= diff_bic
# Original fit is good.
if not diff_mincomp and not diff_maxcomp:
continue
# Both are better than original. Take best.
elif diff_mincomp and diff_maxcomp:
if maxcomp_bic < mincomp_bic:
out_new = out_new_max
else:
out_new = out_new_min
# Update to max component fit.
elif diff_maxcomp:
out_new = out_new_max
# Update to min component fit.
else:
out_new = out_new_min
# Update the parameter array
params_array[:, y, x] = np.NaN
params_array[:len(out_new.params), y, x] = \
[val.value for val in out_new.params.values()]
uncerts_array[:, y, x] = np.NaN
uncerts_array[:len(out_new.params), y, x] = \
[val.stderr if val.stderr is not None else np.NaN
for val in out_new.params.values()]
bic_array[y, x] = out_new.bic
# Otherwise no refit is needed.
else:
continue
del cube
cube = SpectralCube.read(cube_name)
# Grab the celestial header
spat_header = cube[0].header
del cube
# Return a combined HDU that can be written out.
params_hdu = fits.PrimaryHDU(params_array, spat_header.copy())
params_hdu.header['BUNIT'] = ("", "Gaussian fit parameters")
uncerts_hdu = fits.ImageHDU(uncerts_array, spat_header.copy())
uncerts_hdu.header['BUNIT'] = ("", "Gaussian fit uncertainty")
bics_hdu = fits.ImageHDU(bic_array, spat_header.copy())
bics_hdu.header['BUNIT'] = ("", "Gaussian fit BIC")
hdu_all = fits.HDUList([params_hdu, uncerts_hdu, bics_hdu])
del params_array
del uncerts_array
del bic_array
return hdu_all
cubemask=profileMask['mask'],
numcores=4,
sampling=1,
xarr=vels)
# Mask NaNs
contFluxesMasked = np.ma.masked_array(contFluxCube, mask=trueMask['mask'])
# Subtract the continuum from the spectra.
# Line profile range is not masked. NaNs are masked as TRUE.
contSubCube = trueMask['maskedData'] - contFluxCube
# --------------------------------------------- #
# Build the spectral cube using the contSubCube #
# --------------------------------------------- #
# NaNs and data to be ignored are FALSE.
specCube = SpectralCube(contSubCube, pacsWcs, mask=cubeMask, fill_value=1.)
# For convenience, convert the X-axis to km/s
# (WCSLIB automatically converts to m/s even if you give it km/s)
specCube = specCube.with_spectral_unit(u.km / u.s)
# --------------------------------------------- #
# Build the pySpecCube using the spectral cube. #
# --------------------------------------------- #
# NaN values are FALSE in the mask.
pyCube = pyspeckit.Cube(cube=specCube, maskmap=falseMask['mask'][0, :, :])
# -------------------------------- #
# Set up for line profile fitting. #
# -------------------------------- #
# Build the guesses array
import os
######## Input parameters here ########
image_filename = '/lustre/roberto/ALMA_IMF/lines/imaging_results/W43-MM2_B6_spw1_12M_sio.image'
mask_filename = '/lustre/roberto/ALMA_IMF/lines/imaging_results/W43-MM2_B6_spw1_12M_sio_multi_3sigma' # Don't include .mask
mask_threshold = 7.5 # In mJy
erosion_dilation = True
erosion_iter = 2
dilation_iter = 2
#######################################
print("Now masking the cube at sigma threshold")
# Use the code below to mask the cube at a certain sigma threshold
cube = SpectralCube.read(image_filename)
mask = cube > mask_threshold*u.mJy/u.beam
from casatools import image
ia = image()
print("Now computing boolmask")
boolmask = mask.include().compute()
print("Now getting coordinates from original image")
# Use the code below to output a mask file
ia.open(image_filename)
cs = ia.coordsys()
ia.close()
print("Now outputting the mask file")
ia.fromarray(outfile=mask_filename+'.mask', pixels=boolmask.astype('float')[:,None,:,:].T, csys=cs.torecord(), overwrite=True)
ia.close()
