def poly_sub(cfg_par, x, y, deg):
'''
Continuum subtraction on spectrum through polynomial fitting
INPUT:
parameter file
x-axis of the spectrum
y-axis of the spectrum
degre of polynomial to fit
OUTPUT:
continuum subtracted y-axis of spectrum
'''
if cfg_par['abs_ex'].get('zunit') == 'm/s':
unit_z = u.m / u.s
else:
unit_z = u.Hz
step = (x[-1] - x[0]) / len(x)
wave_for_spec = WaveCoord(cdelt=step, crval=x[0], cunit=unit_z)
spe = Spectrum(wave=wave_for_spec, data=y)
cont = spe.poly_spec(deg)
cont_sub = y - cont.data
return cont_sub
def test_spectrum_methods(spec_var, spec_novar):
"""Spectrum class: testing sum/mean/abs/sqrt methods"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, cunit=u.nm, shape=10)
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]),
wave=wave)
sum1 = spectrum1.sum()
assert_almost_equal(sum1[0], spectrum1.data.sum())
spectrum2 = spectrum1[1:-2]
sum1 = spectrum1.sum(lmin=spectrum1.wave.coord(1),
lmax=spectrum1.wave.coord(10 - 3),
unit=u.nm)
sum2 = spectrum2.sum()
assert_almost_equal(sum1, sum2)
mean1 = spectrum1.mean(lmin=spectrum1.wave.coord(1),
lmax=spectrum1.wave.coord(10 - 3),
unit=u.nm)
mean2 = spectrum2.mean()
assert_almost_equal(mean1, mean2)
spvar2 = spec_var.abs()
assert spvar2[23] == np.abs(spec_var[23])
spvar2 = spec_var.abs().sqrt()
assert spvar2[8] == np.sqrt(np.abs(spec_var[8]))
assert_almost_equal(spec_var.mean()[0], 11.526, 2)
assert_almost_equal(spec_novar.mean()[0], 11.101, 2)
spvarsum = spvar2 + 4 * spvar2 - 56 / spvar2
assert_almost_equal(spvarsum[10],
spvar2[10] + 4 * spvar2[10] - 56 / spvar2[10], 2)
assert_almost_equal(spec_var.get_step(), 0.630, 2)
assert_almost_equal(spec_var.get_start(), 4602.604, 2)
assert_almost_equal(spec_var.get_end(), 7184.289, 2)
assert_almost_equal(spec_var.get_range()[0], 4602.604, 2)
assert_almost_equal(spec_var.get_range()[1], 7184.289, 2)
def test_rebin(spec_var, spec_novar):
"""Spectrum class: testing rebin function"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, shape=10)
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]) * 2.3,
wave=wave)
unit = spectrum1.wave.unit
factor = 3
s = slice(0, factor * (spectrum1.shape[0] // factor)) # The rebinned slice
flux1 = spectrum1[s].sum()[0] * spectrum1[s].wave.get_step(unit=unit)
spectrum2 = spectrum1.rebin(factor, margin='left')
flux2 = spectrum2.sum()[0] * spectrum2.wave.get_step(unit=unit)
assert_almost_equal(flux1, flux2, 2)
unit = spec_novar.wave.unit
factor = 4
s = slice(0, factor * (spec_novar.shape[0] // factor))
flux1 = spec_novar[s].sum()[0] * spec_novar[s].wave.get_step(unit=unit)
spnovar2 = spec_novar.rebin(factor, margin='left')
flux2 = spnovar2.sum()[0] * spnovar2.wave.get_step(unit=unit)
assert_almost_equal(flux1, flux2, 2)
unit = spec_var.wave.unit
factor = 4
s = slice(0, factor * (spec_var.shape[0] // factor))
flux1 = spec_var[s].sum(weight=False)[0] * \
spec_var[s].wave.get_step(unit=unit)
spvar2 = spec_var.rebin(factor, margin='left')
flux2 = spvar2.sum(weight=False)[0] * spvar2.wave.get_step(unit=unit)
assert_almost_equal(flux1, flux2, 2)
def test_resample2():
"""Spectrum class: testing resampling function
with a spectrum of integers and resampling to a smaller pixel size"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, cunit=u.nm)
spectrum1 = Spectrum(data=np.array([0, 0, 1, 2, 3, 4, 5, 6, 7, 8, 9, 0]),
wave=wave)
flux1 = spectrum1.sum()[0] * spectrum1.wave.get_step()
spectrum2 = spectrum1.resample(0.3)
flux2 = spectrum2.sum()[0] * spectrum2.wave.get_step()
assert_almost_equal(flux1, flux2, 2)
def residual(p,
datacube=datacube,
pos=None,
specwidth=spectralpixel,
galcen=galcen,
galPA=galPA):
par = p.valuesdict()
incli = par['incli']
col_denst = par['col_dens']
h = par['height']
bes = par['dop_param']
v_max = par['vel_max']
h_vt = par['h_v']
csize = par['csize']
r_0t = par['r_0']
print(par)
h_v = 10**h_vt
col_dens = 10**col_denst
r_0 = 10**r_0t
coord_sky = datacube.wcs.pix2sky([int(pos[0]), int(pos[1])], unit=u.deg)
dec = coord_sky[0][0]
ra = coord_sky[0][1]
c1 = SkyCoord(ra * u.degree, dec * u.degree, frame='icrs')
flux = datacube[:, int(pos[0]), int(pos[1])]
abso = flux.data[specwidth[0]:specwidth[1] + 1]
sigma = np.sqrt(flux.var[specwidth[0]:specwidth[1] + 1])
scale = 7.28 # z=0.73379 # plat scale (kpc/") for Planck
c1 = SkyCoord(ra * u.degree, dec * u.degree, frame='icrs')
#D = scale * galcen.separation(c1).arcsec
#pa = galcen.position_angle(c1).to(u.deg)
#alpha = galPA - pa.value
alpha = csu.get_alpha(c1, galcen, galPA)
D = csu.get_impactparam(c1, galcen, scale)
lam2 = np.arange(4825.12, 4886.37 + 1.5, 0.1)
wave1 = WaveCoord(cdelt=0.1, crval=4825.12, cunit=u.angstrom)
model = Disco(h, incli, Rcore=0.1)
spec = model.averagelos(D, alpha, lam2, 100, 12, z, csize, col_dens, bes,
r_0, v_max, h_v, 0)
spe = Spectrum(wave=wave1, data=spec)
rspe = spe.resample(1.25)
fluxmodel = rspe.data
absomodel = fluxmodel[specwidth[0]:specwidth[1] + 1]
#ymodelt = np.concatenate((ymodel[0][14:36],ymodel[1][16:36],ymodel[2][16:36]))
rest = ((abso - absomodel) / sigma)**2
dif = abso - absomodel
return (fluxmodel, rest, datacube[:, int(pos[0]),
int(pos[1])].data, sigma, dif)
def __init__(self, source=None, **kwargs) :
"""Initialisation of the opening of spectra
"""
self.verbose = kwargs.pop('verbose', False)
# Arguments for the plots
self.title = kwargs.pop('title', "Spectrum")
self.add_sky_lines = kwargs.pop("add_sky_lines", False)
if self.add_sky_lines :
self.color_sky = kwargs.pop("color_sky", "red")
self.linestyle_sky = kwargs.pop("linestyle_sky", "--")
self.alpha_sky = kwargs.pop("alpha_sky", 0.3)
if source is not None:
self.__dict__.update(source.__dict__)
else :
Spectrum.__init__(self, **kwargs)
def load_spectra(filename):
spectra = OrderedDict()
with fits.open(filename) as hdul:
for i in range(1, len(hdul), 2):
spec_id = int(hdul[i].name[4:])
spectra[spec_id] = Spectrum(hdulist=hdul, ext=(i, i + 1))
return spectra
def test_get_Spectrum(spec_var):
"""Spectrum class: testing getters"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, cunit=u.nm)
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]) * 2.3,
wave=wave)
a = spectrum1[1:7]
assert a.shape[0] == 6
a = spectrum1.subspec(1.2, 15.6, unit=u.nm)
assert a.shape[0] == 6
unit = spec_var.wave.unit
spvarcut = spec_var.subspec(5560, 5590, unit=unit)
assert spvarcut.shape[0] == 48
assert_almost_equal(spvarcut.get_start(unit=unit), 5560.25, 2)
assert_almost_equal(spvarcut.get_end(unit=unit), 5589.89, 2)
assert_almost_equal(spvarcut.get_step(unit=unit), 0.63, 2)
def get_sky_spectrum(filename) :
"""Read sky spectrum from MUSE data reduction
"""
sky = pyfits.getdata(filename)
crval = sky['lambda'][0]
cdelt = sky['lambda'][1] - crval
wavein = WaveCoord(cdelt=cdelt, crval=crval, cunit= units.angstrom)
spec = Spectrum(wave=wavein, data=sky['data'], var=sky['stat'])
return spec
def getsp(self):
"""
Get estimated spectra as a dict (with the HST ids as keys) of mpdaf Spectra
"""
cat = {}
for k, key in enumerate(self.listHST_ID):
cat[key] = Spectrum(data=self.sources[k],
var=self.varSources[k],
wave=self.src.spectra['MUSE_TOT'].wave)
return cat
def test_arithmetric():
"""Spectrum class: testing arithmetic functions"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, cunit=u.nm)
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]),
wave=wave)
spectrum2 = spectrum1 > 6 # [-,-,-,-,-,-,-,7,8,9]
# +
spectrum3 = spectrum1 + spectrum2
assert spectrum3.data.data[3] == 3
assert spectrum3.data.data[8] == 16
spectrum3 = 4.2 + spectrum1
assert spectrum3.data.data[3] == 3 + 4.2
# -
spectrum3 = spectrum1 - spectrum2
assert spectrum3.data.data[3] == 3
assert spectrum3.data.data[8] == 0
spectrum3 = spectrum1 - 4.2
assert spectrum3.data.data[8] == 8 - 4.2
# *
spectrum3 = spectrum1 * spectrum2
assert spectrum3.data.data[8] == 64
spectrum3 = 4.2 * spectrum1
assert spectrum3.data.data[9] == 9 * 4.2
# /
spectrum3 = spectrum1 / spectrum2
# divide functions that have a validity domain returns the masked constant
# whenever the input is masked or falls outside the validity domain.
assert spectrum3.data.data[8] == 1
spectrum3 = 1.0 / (4.2 / spectrum1)
assert spectrum3.data.data[5] == 5 / 4.2
# with cube
wcs = WCS()
cube1 = Cube(data=np.ones(shape=(10, 6, 5)), wave=wave, wcs=wcs)
cube2 = spectrum1 + cube1
sp1data = spectrum1.data[:, np.newaxis, np.newaxis]
assert_array_almost_equal(cube2.data, sp1data + cube1.data)
cube2 = spectrum1 - cube1
assert_array_almost_equal(cube2.data, sp1data - cube1.data)
cube2 = spectrum1 * cube1
assert_array_almost_equal(cube2.data, sp1data * cube1.data)
cube2 = spectrum1 / cube1
assert_array_almost_equal(cube2.data, sp1data / cube1.data)
# spectrum * image
data = np.ones(shape=(6, 5)) * 2
image1 = Image(data=data, wcs=wcs)
cube2 = spectrum1 * image1
assert_array_almost_equal(cube2.data,
sp1data * image1.data[np.newaxis, :, :])
def get_sky_spectrum(specname):
"""Read sky spectrum from MUSE data reduction
"""
if not os.path.isfile(specname):
upipe.print_error("{0} not found".format(specname))
return None
sky = pyfits.getdata(specname)
crval = sky['lambda'][0]
cdelt = sky['lambda'][1] - crval
wavein = WaveCoord(cdelt=cdelt, crval=crval, cunit=u.angstrom)
spec = Spectrum(wave=wavein, data=sky['data'], var=sky['stat'])
return spec
def run(self, orig, grid_dxy=0, spectrum_size_fwhm=6):
self.Cat2, line_est, line_var = estimation_line(
orig.Cat1,
orig.cube_raw,
orig.var,
orig.PSF,
orig.wfields,
orig.wcs,
orig.wave,
size_grid=grid_dxy,
criteria='flux',
order_dct=30,
horiz_psf=1,
horiz=5,
)
_format_cat(self.Cat2)
self._loginfo('Save the updated catalog in self.Cat2 (%d lines)',
len(self.Cat2))
# Radius for spectrum trimming
radius = np.ceil(np.array(orig.FWHM_profiles) * spectrum_size_fwhm / 2)
radius = radius.astype(int)
self.spectra = OrderedDict()
for row, data, vari in zip(self.Cat2, line_est, line_var):
profile, z, num_line = row['profile', 'z', 'num_line']
z_min = z - radius[profile]
z_max = z + radius[profile]
if len(data) > 1: # RB test for bug in GridAnalysis
sp = Spectrum(data=data,
var=vari,
wave=orig.wave,
mask=np.ma.nomask,
copy=False)
self.spectra[num_line] = sp.subspec(z_min, z_max, unit=None)
self._loginfo('Save estimated spectrum of each line in self.spectra')
def to_mpdaf(self, row=1, scale=True):
"""
Creates a mpdaf.obj.Spectrum object from FADO 1D files.
The spectrum can be specified as a row or as a name.
Allowed names are the following
1: 'Observed' spectrum de-redshifted and rebinned'
2: 'Error'
3: 'Mask'
4: 'Best'
5: 'Average' of individual solutions
6: 'Median'
7: 'Stdev'
8: 'Stellar' using best fit'
9: 'Nebular' using best fit'
10: 'AGN' using best fit'
11: 'M/L'
12: 'LSF' Line spread function
The best-fits for individual solution can only be specified as a number 13-XX
see self.max_rows
Parameters
----------
row: str, int
Allowed names: 'observed', 'error', 'mask', 'best', 'average', 'median', 'stdev', 'stellar', 'nebular'
'agn', 'm/l', 'lsf'
The row number where the spectra is extracted, default=1 (0 in python notation)
scale: bool, whether to scale the spectra or not, default True
Returns
-------
a mpdaf.obj.Spectrum object
"""
try:
from mpdaf.obj import Spectrum, WaveCoord
except ImportError as e:
print(e, "MPDAF not installed, cannot continue")
raise
sp = self.spectrum(row, scale)
wave_coord = WaveCoord(cdelt=self.header["CDELT1"],
crval=self.header["CRVAL1"],
cunit=self.fado_load.wave_unit)
sp_mpdaf = Spectrum(wave=wave_coord, data=sp.flux)
return sp_mpdaf
def read(self):
"""Read sky continuum spectrum from MUSE data reduction
"""
if not os.path.isfile(self.filename):
upipe.print_error("{0} not found".format(self.filename))
crval = 0.0
data = np.zeros(0)
cdelt = 1.0
else:
sky = pyfits.getdata(self.filename)
crval = sky['lambda'][0]
cdelt = sky['lambda'][1] - crval
data = sky['flux']
wavein = WaveCoord(cdelt=cdelt, crval=crval, cunit=u.angstrom)
self.spec = Spectrum(wave=wavein, data=data)
def test_mag():
"""Spectrum class: testing magnitude computations."""
Vega = Spectrum(get_data_file('obj', 'Vega.fits'))
Vega.unit = u.Unit('2E-17 erg / (Angstrom cm2 s)')
Vega.wave.wcs.wcs.cunit[0] = u.angstrom
assert_almost_equal(Vega.abmag_filter_name('V')[0], 0, 1)
mag = Vega.abmag_filter_name('Ic')[0]
assert mag > 0.4 and mag < 0.5
mag = Vega.abmag_band(22500, 2500)[0]
assert mag > 1.9 and mag < 2.0
def test_write(tmpdir):
"""Spectrum class: testing write."""
testfile = str(tmpdir.join('spec.fits'))
sp = Spectrum(data=np.arange(10), wave=WaveCoord(cunit=u.nm))
sp.write(testfile)
with fits.open(testfile) as hdu:
assert_array_equal(hdu[1].data.shape, sp.shape)
hdr = hdu[1].header
assert hdr['EXTNAME'] == 'DATA'
assert hdr['NAXIS'] == 1
assert u.Unit(hdr['CUNIT1']) == u.nm
assert hdr['NAXIS1'] == sp.shape[0]
# Same with Angstrom
sp = Spectrum(data=np.arange(10), wave=WaveCoord(cunit=u.angstrom))
sp.write(testfile)
with fits.open(testfile) as hdu:
assert u.Unit(hdu[1].header['CUNIT1']) == u.angstrom
def test_gauss_fit(capsys, cont):
"""Spectrum class: testing Gaussian fit"""
contval = cont or 0
wave = WaveCoord(crpix=1, cdelt=0.3, crval=400, cunit=u.nm)
spem = Spectrum(data=np.zeros(600) + contval, wave=wave)
spem.add_gaussian(5000, 1200, 20, unit=u.angstrom)
setup_logging()
gauss = spem.gauss_fit(lmin=(4500, 4800),
lmax=(5200, 6000),
lpeak=5000,
cont=cont,
unit=u.angstrom)
gauss.print_param()
out, err = capsys.readouterr()
assert '[INFO] Gaussian center = 5000 ' in err
assert_almost_equal(gauss.lpeak, 5000, 2)
assert_almost_equal(gauss.flux, 1200, 2)
assert_almost_equal(gauss.fwhm, 20, 2)
assert_allclose(spem.fwhm(gauss.lpeak, cont=contval), 20, atol=0.2)
ra = coord_sky[0][1]
scale = 7.28 # z=0.73379 # plat scale (kpc/") for Planck
c1 = SkyCoord(ra * u.degree, dec * u.degree, frame='icrs')
alpha = csu.get_alpha(c1, galcen, galPA)
D = csu.get_impactparam(c1, galcen, scale)
flux = datacube[:, i, j]
abso = flux.data[specwidth[0]:specwidth[1] + 1]
sigma = np.sqrt(flux.var[specwidth[0]:specwidth[1] + 1])
lam2 = np.arange(4825.12, 4886.37 + 1.5, 0.1)
wave1 = WaveCoord(cdelt=0.1, crval=4825.12, cunit=u.angstrom)
model = Disco(h, incli, Rcore=0.1)
spec = model.averagelos(D, alpha, lam2, 100, 12, z, csize,
col_dens, bes, r_0, v_max, h_v, 0)
spe = Spectrum(wave=wave1, data=spec)
rspe = spe.resample(1.25)
fluxmodel = rspe.data
absomodel = fluxmodel[specwidth[0]:specwidth[1] + 1]
#ymodelt = np.concatenate((ymodel[0][14:36],ymodel[1][16:36],ymodel[2][16:36]))
dif = np.sum(((abso - absomodel) / sigma)**2)
ima.data[i, j] = dif
ima.mask[i, j] = False
else:
ima.data[i, j] = 0
ima.mask[i, j] = True
ima.plot(colorbar='v')
plt.show()
def spec_var():
return Spectrum(get_data_file('obj', 'Spectrum_Variance.fits'), ext=[0, 1])
def spec_novar():
return Spectrum(get_data_file('obj', 'Spectrum_Novariance.fits'))
def __init__(self):
self.img = None
self.cube = None
self.spec = None
if os.path.exists(SKYREF):
self.sky = Spectrum(SKYREF)
self.sky.data /= self.sky.data.max()
else:
print('Sky file missing')
self.sky = None
pg.mkQApp()
self.win = win = QtGui.QWidget()
win.setWindowTitle('MUSE Cube Viewer')
# layout = QtGui.QGridLayout()
layout = QtGui.QVBoxLayout()
layout.setContentsMargins(0, 0, 0, 0)
win.setLayout(layout)
self.splitter = QtGui.QSplitter()
self.splitter.setOrientation(QtCore.Qt.Horizontal)
layout.addWidget(self.splitter)
self.tree = ParameterTree(showHeader=False)
self.splitter.addWidget(self.tree)
self.params = Parameter.create(name='params',
type='group',
children=PARAMS)
self.tree.setParameters(self.params, showTop=False)
self.tree.setWindowTitle('pyqtgraph example: Parameter Tree')
self.connect(('Median filter', ), self.update_spec_plot)
self.connect(('Sky', ), self.update_spec_plot)
self.connect(('Spectrum', 'Lambda Max'), self.show_image)
self.connect(('Spectrum', 'Lambda Min'), self.show_image)
self.connect(('Spectrum', 'Line color'), self.update_spec_plot)
self.connect(('Spectrum', 'Selection color'), self.update_spec_plot)
self.connect(('Spectrum', 'Show Zoom'), self.add_zoom_window)
self.win_inner = win = pg.GraphicsLayoutWidget()
self.splitter2 = QtGui.QSplitter()
self.splitter2.setOrientation(QtCore.Qt.Vertical)
self.splitter.addWidget(self.win_inner)
# self.img_label = win.addLabel('Hello !', justify='right')
# A plot area (ViewBox + axes) for displaying the white-light image
win.nextRow()
self.white_plot = win.addPlot(title='White-light Image')
self.white_plot.setAspectLocked(lock=True, ratio=1)
self.white_item = pg.ImageItem()
self.white_plot.addItem(self.white_item)
# A plot area (ViewBox + axes) for displaying the image
win.nextColumn()
self.img_plot = win.addPlot(title='Band Image')
self.img_plot.setAspectLocked(lock=True, ratio=1)
self.img_item = pg.ImageItem()
self.img_plot.addItem(self.img_item)
# pg.SignalProxy(self.img_plot.scene().sigMouseMoved, rateLimit=60,
# slot=self.on_mouse_moved)
# Contrast/color control
self.hist = hist = pg.HistogramLUTItem()
hist.setImageItem(self.img_item)
win.addItem(hist)
# self.specplot = win.addPlot(row=2, col=0, colspan=2)
win.nextRow()
self.specplot = win.addPlot(title='Spectrum', colspan=3)
self.zoomplot = None
self.zoomplot_visible = False
# self.lbdareg = region = pg.LinearRegionItem(movable=False)
# self.specplot.addItem(region)
# region.setZValue(10)
self.zoomreg = region = pg.LinearRegionItem()
region.setZValue(10)
self.specplot.addItem(self.zoomreg, ignoreBounds=True)
region.sigRegionChanged.connect(self.update_zoom_spec_from_region)
p = self.params
lmin = p['Spectrum', 'Lambda Min']
lmax = p['Spectrum', 'Lambda Max']
region.setRegion([lmin, lmax])
self.win.resize(1000, 800)
self.win.show()
def test_integrate():
"""Spectrum class: testing integration"""
wave = WaveCoord(crpix=2.0, cdelt=3.0, crval=0.5, cunit=u.nm)
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]),
wave=wave,
unit=u.Unit('ct/Angstrom'))
# Integrate the whole spectrum, by not specifying starting or ending
# wavelengths. This should be the sum of the pixel values multiplied
# by cdelt in angstroms (because the flux units are per angstrom).
result, err = spectrum1.integrate()
expected = spectrum1.get_step(unit=u.angstrom) * spectrum1.sum()[0]
assert_almost_equal(result.value, expected)
assert result.unit == u.ct
assert np.isinf(err)
# The result should not change if we change the wavelength units of
# the wavelength limits to nanometers.
result = spectrum1.integrate(unit=u.nm)[0]
expected = spectrum1.get_step(unit=u.angstrom) * spectrum1.sum()[0]
assert_almost_equal(result.value, expected)
assert result.unit == u.ct
# new spectrum with variance
spectrum1 = Spectrum(data=np.array([0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9]),
var=np.ones(10),
wave=wave,
unit=u.Unit('ct/Angstrom'))
# Integrate over a wavelength range 3.5 to 6.5 nm. The WCS
# conversion equation from wavelength to pixel index is,
#
# index = crpix-1 + (lambda-crval)/cdelt
# index = 1 + (lambda - 0.5) / 3.0
#
# So wavelengths 3.5 and 6.5nm, correspond to pixel indexes
# of 2.0 and 3.0. These are the centers of pixels 2 and 3.
# Thus the integration should be the value of pixel 2 times
# half of cdelt, plus the value of pixel 3 times half of cdelt.
# This comes to 2*3.0/2 + 3*3.0/2 = 7.5 ct/Angstrom*nm, which
# should be rescaled to 75 ct, since nm/Angstrom is 10.0.
result, err = spectrum1.integrate(lmin=3.5, lmax=6.5, unit=u.nm)
assert_almost_equal(result.value, 75)
assert result.unit == u.ct
datasum, var = spectrum1.sum(lmin=3.5, lmax=6.5, unit=u.nm)
assert_almost_equal(result.value, datasum * 15)
assert_almost_equal(err.value, var * 15)
# Do the same test, but specify the wavelength limits in angstroms.
# The result should be the same as before.
result = spectrum1.integrate(lmin=35.0, lmax=65.0, unit=u.angstrom)[0]
assert_almost_equal(result.value, 75)
assert result.unit == u.ct
assert_almost_equal(result.value, datasum * 15)
assert_almost_equal(err.value, var * 15)
# Do the same experiment yet again, but this time after changing
# the flux units of the spectrum to simple counts, without any per
# wavelength units. Since there are no wavelength units in the
# flux units, the result should not be rescaled from the native
# value of 7.5, and because we specified a wavelength range in
# angstroms, the resulting units should be counts * nm.
spectrum1.unit = u.ct
result = spectrum1.integrate(lmin=3.5, lmax=6.5, unit=u.nm)[0]
assert_almost_equal(result.value, 7.5)
assert result.unit == u.ct * u.nm
wavep = 4855
for i in range(datacube.shape[1]):
for j in range(datacube.shape[2]):
spe = datacube[:, i, j]
var = spe.var
sigma = np.sqrt(var)
#arrays
flux = spe.data
sigma = sigma.data
wave = spe.wave.coord()
#vel = (wave/(wave0*(1+zabs))-1)*299792.458
#mask pixels for continuum definition
p1 = np.int(spe.wave.pixel(wavep - 60 * 1.25))
p2 = np.int(spe.wave.pixel(wavep - 30 * 1.25))
p3 = np.int(spe.wave.pixel(wavep + 30 * 1.25))
p4 = np.int(spe.wave.pixel(wavep + 100 * 1.25))
flux1 = flux[np.r_[p1:p2, p3:p4]]
wave1 = wave[np.r_[p1:p2, p3:p4]]
#continuum
z = np.polyfit(wave1, flux1, 2)
p = np.poly1d(z)
cont = p(wave)
nflux = flux / cont
stdev = sigma / cont #for displaying
#mpdaf normalized continuum
wave_aux = WaveCoord(cdelt=1.25, crval=wave[0], cunit=u.angstrom)
nspe = Spectrum(wave=wave_aux, data=nflux, var=(stdev**2))
norcube[:, i, j] = nspe
#co[:] = sp-ai
def test_resample():
"""Spectrum class: Test resampling"""
# Choose the dimensions of the spectrum, choosing a large number that is
# *not* a convenient power of 2.
oldshape = 4000
# Choose the wavelength pixel size and the default wavelength units.
oldstep = 1.0
oldunit = u.angstrom
# Create the wavelength axis coordinates.
wave = WaveCoord(crpix=2.0,
cdelt=oldstep,
crval=0.5,
cunit=oldunit,
shape=oldshape)
# Specify the desired increase in pixel size, and the resulting pixel size.
factor = 6.5
newstep = ((factor * oldstep) * oldunit).to(u.nm).value
# Specify the wavelength at which the peak of the resampled spectrum should
# be expected.
expected_peak_wave = 3000.0
# Create the array in which the test spectrum will be composed.
data = np.zeros(oldshape)
# Get the wavelength coordinates of each pixel in the spectrum.
w = wave.coord()
# Add the following list gaussians to the spectrum, where each
# gaussian is specified as: (amplitude, sigma_in_pixels,
# center_wavelength). Given that narrow gaussians are reduced in
# amplitude by resampling more than wide gaussians, we arrange
# that the peak gaussian before and after correctly resampling are
# different.
gaussians = [
(0.5, 12.0, 800.0),
(0.7, 5.0, 1200.0),
(0.4, 700.0, 1600.0),
(1.5, 2.6, 1980.0), # Peak before resampling
(1.2, 2.6, 2000.0),
(1.3, 15.0, expected_peak_wave), # Peak if resampled correctly
(1.0, 2.0, 3200.0)
]
for amp, sigma, center in gaussians:
sigma *= oldstep
data += amp * np.exp(-0.5 * ((center - w) / sigma)**2)
# Fill the variance array with a simple window function.
var = np.hamming(oldshape)
# Add gaussian random noise to the spectrum, but leave 3 output
# pixel widths zero at each end of the spectrum so that the PSF of
# the output grid doesn't spread flux from the edges off the edge
# of the output grid. It takes about 3 pixel widths for the gaussian
# PSF to drop to about 0.01 of its peak.
margin = np.ceil(3 * factor).astype(int)
data[margin:-margin] += np.random.normal(scale=0.1,
size=data.shape - 2 * margin)
# Install the spectral data in a Spectrum container.
oldsp = Spectrum(data=data, var=var, wave=wave)
# Mask a few pixels.
masked_slice = slice(900, 910)
oldsp.mask[masked_slice] = True
# Create a down-sampled version of the input spectrum.
newsp = oldsp.resample(newstep, unit=u.nm)
# Check that the integral flux in the resampled spectrum matches that of
# the original spectrum.
expected_flux = oldsp.sum(weight=False)[0] * oldsp.wave.get_step(
unit=oldunit)
actual_flux = newsp.sum(weight=False)[0] * newsp.wave.get_step(
unit=oldunit)
assert_allclose(actual_flux, expected_flux, 1e-2)
# Do the same test, but with fluxes weighted by the inverse of the variances.
expected_flux = oldsp.sum(weight=True)[0] * oldsp.wave.get_step(
unit=oldunit)
actual_flux = newsp.sum(weight=True)[0] * newsp.wave.get_step(unit=oldunit)
assert_allclose(actual_flux, expected_flux, 1e-2)
# Check that the peak of the resampled spectrum is at the wavelength
# where the strongest gaussian was centered in the input spectrum.
assert_allclose(np.argmax(newsp.data),
newsp.wave.pixel(expected_peak_wave, nearest=True))
# Now upsample the downsampled spectrum to the original pixel size.
# This won't recover the same spectrum, since higher spatial frequencies
# are lost when downsampling, but the total flux should be about the
# same, and the peak should be at the same wavelength as the peak in
# original spectrum within one pixel width of the downsampled spectrum.
newsp2 = newsp.resample(oldstep, unit=oldunit)
# Check that the doubly resampled spectrum has the same integrated flux
# as the original.
expected_flux = oldsp.sum(weight=False)[0] * oldsp.wave.get_step(
unit=oldunit)
actual_flux = newsp2.sum(weight=False)[0] * newsp2.wave.get_step(
unit=oldunit)
assert_allclose(actual_flux, expected_flux, 1e-2)
# Check that the peak of the up-sampled spectrum is at the wavelength
# of the peak of the down-sampled spectrum to within the pixel resolution
# of the downsampled spectrum.
assert_allclose(
newsp.wave.pixel(newsp2.wave.coord(np.argmax(newsp2.data)),
nearest=True),
newsp.wave.pixel(expected_peak_wave, nearest=True))
# Check that pixels that were masked in the input spectrum are still
# masked in the final spectrum.
np.testing.assert_equal(newsp2.mask[masked_slice],
oldsp.mask[masked_slice])
def create_source(
source_id,
source_table,
source_lines,
origin_params,
cube_cor_filename,
cube_std_filename,
mask_filename,
skymask_filename,
spectra_fits_filename,
segmaps,
version,
source_ts,
profile_fwhm,
*,
author="",
nb_fwhm=2,
expmap_filename=None,
save_to=None,
):
"""Create a MPDAF source.
This function create a MPDAF source object for the ORIGIN source.
Parameters
----------
source_id : int
Identifier for the source in the source and line tables.
source_table : astropy.table.Table
Catalogue of sources like the Cat3_sources one.
source_lines : astropy.table.Table
Catalogue of lines like the Cat3_lines one.
origin_params : dict
Dictionary of the parameters for the ORIGIN run.
cube_cor_filename : str
Name of the file containing the correlation cube of the ORIGIN run.
cube_std_filename : str
Name of the file containing the std cube of the ORIGIN run.
mask_filenam e: str
Name of the file containing the mask of the source.
skymask_filename : str
Name of the file containing the sky mask of the source.
spectra_fits_filename : str
Name of the FITS file containing the spectra of the lines.
segmaps : dict(str: str)
Dictionnary associating to a segmap type the associated FITS file name.
version : str
Version number stored in the source.
source_ts : str
Time stamp for when the source was created.
profile_fwhm : list of int
List of line profile FWHM in pixel. The index in the list is the
profile number.
author : str
Name of the author.
nb_fwhm : float
Factor multiplying the FWHM of the line to compute the width of the
narrow band image.
expmap_filename : str
Name of the file containing the exposure map. If not None, a cut-out
of the exposure map will be added to the source file.
save_to : str
If not None, the source will be saved to the given file.
Returns
-------
mpdaf.sdetect.Source or None
If save_to is used, the function returns None.
"""
logger = logging.getLogger(__name__)
# [0] is to get a Row not a table.
source_table = source_table.filled()
source_info = source_table[source_table["ID"] == source_id][0]
# The mask size is used for the cut-out size.
mask = Image(mask_filename)
mask_size = mask.shape[0]
data_cube = Cube(origin_params["cubename"], convert_float64=False)
origin = (
"ORIGIN",
origin_version,
os.path.basename(origin_params["cubename"]),
data_cube.primary_header.get("CUBE_V", ""),
)
source = Source.from_data(
source_info["ID"], source_info["ra"], source_info["dec"], origin
)
# Information about the source in the headers
source.header["SRC_V"] = version, "Source version"
source.header["SRC_TS"] = source_ts, "Timestamp of the source creation"
source.header["CAT3_TS"] = (
source_table.meta["CAT3_TS"],
"Timestamp of the catalog creation",
)
source.add_history("Source created with ORIGIN", author)
source.header["OR_X"] = source_info["x"], "x position in pixels"
source.header["OR_Y"] = source_info["y"], "y position in pixels"
source.header["OR_SEG"] = (
source_info["seg_label"],
"Label in the segmentation map",
)
source.header["OR_V"] = origin_version, "ORIGIN version"
source.header["OR_FLUX"] = source_info["flux"], "flux maximum in all lines"
source.header["OR_PMAX"] = (source_info["purity"], "maximum purity in all lines")
if not np.isnan(source_info["STD"]):
source.header["OR_STD"] = (source_info["STD"], "STD max value in all lines")
if not np.isnan(source_info["nsigSTD"]):
source.header["OR_nSTD"] = (
source_info["nsigSTD"],
"max of STD/std(STD) in all lines",
)
if not np.isnan(source_info["T_GLR"]):
source.header["OR_TGLR"] = (
source_info["T_GLR"],
"T_GLR max value in all lines",
)
if not np.isnan(source_info["nsigTGLR"]):
source.header["OR_nTGLR"] = (
source_info["nsigTGLR"],
"max of T_GLR/std(T_GLR) in all lines",
)
# source_header_keyword: (key_in_origin_param, description)
parameters_to_add = {
"OR_PROF": ("profiles", "OR input, spectral profiles"),
"OR_FSF": ("PSF", "OR input, FSF cube"),
"OR_THL%02d": ("threshold_list", "OR input threshold per area"),
"OR_NA": ("nbareas", "OR number of areas"),
"preprocessing": {"OR_DCT": ("dct_order", "OR input, DCT order")},
"areas": {
"OR_PFAA": ("pfa", "OR input, PFA used to create the area map"),
"OR_SIZA": ("maxsize", "OR input, maximum area size in pixels"),
"OR_MSIZA": ("minsize", "OR input, minimum area size in pixels"),
},
"compute_PCA_threshold": {"OR_PFAT": ("pfa_test", "OR input, PFA test")},
"compute_greedy_PCA": {
"OR_FBG": ("Noise_population", "OR input: fraction of spectra estimated"),
"OR_ITMAX": ("itermax", "OR input, maximum number of iterations"),
},
"compute_TGLR": {"OR_NG": ("size", "OR input, connectivity size")},
"detection": {
"OR_DXY": ("tol_spat", "OR input, spatial tolerance for merging (pix)"),
"OR_DZ": ("tol_spec", "OR input, spectral tolerance for merging (pix)"),
},
"compute_spectra": {"OR_NXZ": ("grid_dxy", "OR input, grid Nxy")},
}
def add_keyword(keyword, param, description, params):
if param == "threshold_list" and param in params:
for idx, threshold in enumerate(params["threshold_list"]):
source.header[keyword % idx] = (float("%0.2f" % threshold), description)
elif param in params:
if params[param] is None:
source.header[keyword] = "", description
else:
source.header[keyword] = params[param], description
else:
logger.debug("Parameter %s absent of the parameter list.", param)
for keyword, val in parameters_to_add.items():
if isinstance(val, dict) and keyword in origin_params:
for key, val2 in val.items():
add_keyword(key, *val2, origin_params[keyword]["params"])
else:
add_keyword(keyword, *val, origin_params)
source.header["COMP_CAT"] = (
source_info["comp"],
"1/0 (1=Pre-detected in STD, 0=detected in CORREL)",
)
if source.COMP_CAT:
threshold_keyword, purity_keyword = "threshold_std", "purity_std"
else:
threshold_keyword, purity_keyword = "threshold", "purity"
source.header["OR_TH"] = (
float("%0.2f" % origin_params[threshold_keyword]),
"OR input, threshold",
)
source.header["OR_PURI"] = (
float("%0.2f" % origin_params[purity_keyword]),
"OR input, purity",
)
# Mini-cubes
source.add_cube(
data_cube, "MUSE_CUBE", size=mask_size, unit_size=None, add_white=True
)
# Add FSF with the full cube, to have the same shape as fieldmap, then we
# can work directly with the subcube
has_fsf = True
try:
source.add_FSF(data_cube, fieldmap=origin_params["fieldmap"])
except:
logger.debug('No FSF information found in the cube')
has_fsf = False
data_cube = source.cubes["MUSE_CUBE"]
if source.COMP_CAT:
cube_ori = Cube(cube_std_filename, convert_float64=False)
source.add_cube(cube_ori, "ORI_SNCUBE", size=mask_size, unit_size=None)
cube_ori = source.cubes["ORI_SNCUBE"]
else:
cube_ori = Cube(cube_cor_filename, convert_float64=False)
source.add_cube(cube_ori, "ORI_CORREL", size=mask_size, unit_size=None)
cube_ori = source.cubes["ORI_CORREL"]
# Table of sources around the exported sources.
radius = mask_size / 2
x_min, x_max = source_info["x"] - radius, source_info["x"] + radius
y_min, y_max = source_info["y"] - radius, source_info["y"] + radius
nearby_sources = (
(source_table["x"] >= x_min)
& (source_table["x"] <= x_max)
& (source_table["y"] >= y_min)
& (source_table["y"] <= y_max)
)
source.tables["ORI_CAT"] = source_table["ID", "ra", "dec"][nearby_sources]
# Maps
# The white map was added when adding the MUSE cube.
source.images["ORI_MAXMAP"] = cube_ori.max(axis=0)
# Using add_image, the image size is taken from the white map.
source.add_image(mask, "ORI_MASK_OBJ")
source.add_image(Image(skymask_filename), "ORI_MASK_SKY")
for segmap_type, segmap_filename in segmaps.items():
source.add_image(Image(segmap_filename), "ORI_SEGMAP_%s" % segmap_type)
if expmap_filename is not None:
source.add_image(Image(expmap_filename), "EXPMAP")
# Full source spectra
source.extract_spectra(
data_cube, obj_mask="ORI_MASK_OBJ", sky_mask="ORI_MASK_SKY", skysub=True
)
source.extract_spectra(
data_cube, obj_mask="ORI_MASK_OBJ", sky_mask="ORI_MASK_SKY", skysub=False
)
if source.COMP_CAT:
source.spectra["ORI_CORR"] = (
source.cubes["ORI_SNCUBE"] * source.images["ORI_MASK_OBJ"]
).mean(axis=(1, 2))
else:
source.spectra["ORI_CORR"] = (
source.cubes["ORI_CORREL"] * source.images["ORI_MASK_OBJ"]
).mean(axis=(1, 2))
# Add the FSF information to the source and use this information to compute
# the PSF weighted spectra.
if has_fsf:
try:
fsfmodel = source.get_FSF()
fwhm_fsf = fsfmodel.get_fwhm(data_cube.wave.coord())
beta_fsf = fsfmodel.get_beta(data_cube.wave.coord())
source.extract_spectra(
data_cube,
obj_mask="ORI_MASK_OBJ",
sky_mask="ORI_MASK_SKY",
skysub=True,
psf=fwhm_fsf,
beta=beta_fsf,
)
source.extract_spectra(
data_cube,
obj_mask="ORI_MASK_OBJ",
sky_mask="ORI_MASK_SKY",
skysub=False,
psf=fwhm_fsf,
beta=beta_fsf,
)
except:
# WIP to work with the new FSF model
has_fsf = False
# Per line data: the line table, the spectrum of each line, the narrow band
# map from the data and from the correlation cube.
# Content of the line table in the source
line_columns, line_units, line_fmt = zip(
*[
("NUM_LINE", None, None),
("RA_LINE", u.deg, ".2f"),
("DEC_LINE", u.deg, ".2f"),
("LBDA_OBS", u.Angstrom, ".2f"),
("FWHM", u.Angstrom, ".2f"),
("FLUX", u.erg / (u.s * u.cm ** 2), ".1f"),
("GLR", None, ".1f"),
("nGLR", None, ".1f"),
("PROF", None, None),
("PURITY", None, ".2f"),
]
)
# If the line is a complementary one, the GLR column is replace by STD
if source.COMP_CAT:
line_columns = list(line_columns)
line_columns[6] = "STD"
line_columns[7] = "nSTD"
# We put all the ORIGIN lines in an ORI_LINES tables but keep only the
# unique lines in the LINES tables.
source.add_table(source_lines, "ORI_LINES", select_in=None, col_dist=None)
# Table containing the information on the narrow band images.
nb_par_rows = []
hdulist = fits.open(spectra_fits_filename)
for line in source_lines[source_lines["merged_in"] == -9999]:
num_line, lbda_ori, prof = line[["num_line", "lbda", "profile"]]
fwhm_ori = profile_fwhm[prof] * data_cube.wave.get_step(unit=u.Angstrom)
if source.COMP_CAT:
glr_std = line["STD"]
nglr_std = line["nsigSTD"]
else:
glr_std = line["T_GLR"]
nglr_std = line["nsigTGLR"]
source.add_line(
cols=line_columns,
values=[
num_line,
line["ra"],
line["dec"],
lbda_ori,
fwhm_ori,
line["flux"],
glr_std,
nglr_std,
prof,
line["purity"],
],
units=line_units,
fmt=line_fmt,
desc=None,
)
if f"DATA{num_line}" in hdulist: # RB add test
source.spectra[f"ORI_SPEC_{num_line}"] = Spectrum(
hdulist=hdulist,
ext=(f"DATA{num_line}", f"STAT{num_line}"),
convert_float64=False,
)
source.add_narrow_band_image_lbdaobs(
data_cube,
f"NB_LINE_{num_line}",
lbda=lbda_ori,
width=nb_fwhm * fwhm_ori,
method="sum",
subtract_off=True,
margin=10.0,
fband=3.0,
)
nb_par_rows.append(
[f"NB_LINE_{num_line}", lbda_ori, nb_fwhm * fwhm_ori, 10.0, 3.0]
)
source.add_narrow_band_image_lbdaobs(
cube_ori,
f"ORI_CORR_{num_line}",
lbda=lbda_ori,
width=nb_fwhm * fwhm_ori,
method="max",
subtract_off=False,
)
# Compute the spectra weighted by the correlation map for the
# current line
tags = [f"ORI_CORR_{num_line}"]
source.extract_spectra(
data_cube,
obj_mask="ORI_MASK_OBJ",
sky_mask="ORI_MASK_SKY",
skysub=True,
tags_to_try=tags,
)
source.extract_spectra(
data_cube,
obj_mask="ORI_MASK_OBJ",
sky_mask="ORI_MASK_SKY",
skysub=False,
tags_to_try=tags,
)
# set REFSPEC to the spectrum weighted by the correlation map of the
# brightest line
num_max = source.lines["NUM_LINE"][np.argmax(source.lines["FLUX"])]
source.header["REFSPEC"] = f"ORI_CORR_{num_max}_SKYSUB"
hdulist.close()
nb_par = Table(
names=["LINE", "LBDA", "WIDTH", "MARGIN", "FBAND"],
dtype=["U20", float, float, float, float],
rows=nb_par_rows,
)
source.add_table(nb_par, "NB_PAR", select_in=None, col_dist=None)
if save_to is not None:
source.write(save_to)
else:
return source
