def __init__(self,
model="kpno",
extinction=None,
spectral_axis=None,
cache=True,
show_progress=False,
**kwargs):
if extinction is not None:
if not isinstance(extinction, u.Quantity):
warnings.warn(
"Input extinction is not a Quanitity. Assuming it is given in magnitudes...",
AstropyUserWarning)
extinction = u.Magnitude(
extinction, u.MagUnit(u.dimensionless_unscaled)).to(
u.dimensionless_unscaled
) # Spectrum1D wants this to be linear
if isinstance(
extinction,
(u.LogUnit, u.Magnitude)) or extinction.unit == u.mag:
# if in log or magnitudes, recast into Magnitude with dimensionless physical units
extinction = u.Magnitude(extinction.value,
u.MagUnit(
u.dimensionless_unscaled)).to(
u.dimensionless_unscaled)
if extinction.unit != u.dimensionless_unscaled:
# if we're given something linear that's not dimensionless_unscaled,
# it's an error
msg = "Input extinction must have unscaled dimensionless units."
raise ValueError(msg)
if extinction is None and spectral_axis is None:
if model not in SUPPORTED_EXTINCTION_MODELS:
msg = (f"Requested extinction model, {model}, not in list "
f"of available models: {SUPPORTED_EXTINCTION_MODELS}")
raise ValueError(msg)
model_file = os.path.join("extinction", f"{model}extinct.dat")
model_path = get_reference_file_path(path=model_file,
cache=cache,
show_progress=show_progress)
t = Table.read(model_path,
format="ascii",
names=['wavelength', 'extinction'])
# the specreduce_data models all provide wavelengths in angstroms
spectral_axis = t['wavelength'].data * u.angstrom
# the specreduce_data models all provide extinction in magnitudes at an airmass of 1
extinction = u.Magnitude(t['extinction'].data,
u.MagUnit(u.dimensionless_unscaled)).to(
u.dimensionless_unscaled)
if spectral_axis is None:
msg = "Missing spectral axis for input extinction data."
raise ValueError(msg)
super(AtmosphericExtinction,
self).__init__(flux=extinction,
spectral_axis=spectral_axis,
unit=u.dimensionless_unscaled,
**kwargs)
def test_str(self):
"""Do some spot checks that str, repr, etc. work as expected."""
lu1 = u.mag(u.Jy)
assert str(lu1) == 'mag(Jy)'
assert repr(lu1) == 'Unit("mag(Jy)")'
assert lu1.to_string('generic') == 'mag(Jy)'
with pytest.raises(ValueError):
lu1.to_string('fits')
with pytest.raises(ValueError):
lu1.to_string(format='cds')
lu2 = u.dex()
assert str(lu2) == 'dex'
assert repr(lu2) == 'Unit("dex(1)")'
assert lu2.to_string() == 'dex(1)'
lu3 = u.MagUnit(u.Jy, function_unit=2 * u.mag)
assert str(lu3) == '2 mag(Jy)'
assert repr(lu3) == 'MagUnit("Jy", unit="2 mag")'
assert lu3.to_string() == '2 mag(Jy)'
lu4 = u.mag(u.ct)
assert lu4.to_string('generic') == 'mag(ct)'
assert lu4.to_string('latex') == ('$\\mathrm{mag}$$\\mathrm{\\left( '
'\\mathrm{ct} \\right)}$')
assert lu4._repr_latex_() == lu4.to_string('latex')
def test_custom_mag_model():
"""
Test creation of custom model from Quantity arrays
"""
wave = np.linspace(0.3, 2.0, 50)
extinction = u.Magnitude(1. / wave, u.MagUnit(u.dimensionless_unscaled))
ext = AtmosphericExtinction(extinction=extinction, spectral_axis=wave * u.um)
assert(len(ext.extinction_mag) > 0)
assert(len(ext.transmission) > 0)
def test_littleh():
H0_70 = 70*u.km/u.s/u.Mpc
h70dist = 70 * u.Mpc/u.littleh
assert_quantity_allclose(h70dist.to(u.Mpc, u.with_H0(H0_70)), 100*u.Mpc)
# make sure using the default cosmology works
cosmodist = cosmology.default_cosmology.get().H0.value * u.Mpc/u.littleh
assert_quantity_allclose(cosmodist.to(u.Mpc, u.with_H0()), 100*u.Mpc)
# Now try a luminosity scaling
h1lum = .49 * u.Lsun * u.littleh**-2
assert_quantity_allclose(h1lum.to(u.Lsun, u.with_H0(H0_70)), 1*u.Lsun)
# And the trickiest one: magnitudes. Using H0=10 here for the round numbers
H0_10 = 10*u.km/u.s/u.Mpc
# assume the "true" magnitude M = 12.
# Then M - 5*log_10(h) = M + 5 = 17
withlittlehmag = 17 * (u.mag - u.MagUnit(u.littleh**2))
assert_quantity_allclose(withlittlehmag.to(u.mag, u.with_H0(H0_10)), 12*u.mag)
@pytest.mark.parametrize(
'strings, unit',
[
(["m s", "m*s", "m.s"], u.m * u.s),
(["m/s", "m*s**-1", "m /s", "m / s", "m/ s"], u.m / u.s),
(["m**2", "m2", "m**(2)", "m**+2", "m+2", "m^(+2)"], u.m**2),
(["m**-3", "m-3", "m^(-3)", "/m3"], u.m**-3),
(["m**(1.5)", "m(3/2)", "m**(3/2)", "m^(3/2)"], u.m**1.5),
(["2.54 cm"], u.Unit(u.cm * 2.54)),
(["10+8m"], u.Unit(u.m * 1e8)),
# This is the VOUnits documentation, but doesn't seem to follow the
# unity grammar (["3.45 10**(-4)Jy"], 3.45 * 1e-4 * u.Jy)
(["sqrt(m)"], u.m**0.5),
(["dB(mW)", "dB (mW)"], u.DecibelUnit(u.mW)),
(["mag"], u.mag),
(["mag(ct/s)"], u.MagUnit(u.ct / u.s)),
(["dex"], u.dex),
(["dex(cm s**-2)", "dex(cm/s2)"], u.DexUnit(u.cm / u.s**2))
])
def test_unit_grammar(strings, unit):
for s in strings:
print(s)
unit2 = u_format.Generic.parse(s)
assert unit2 == unit
@pytest.mark.parametrize(
'string', ['sin( /pixel /s)', 'mag(mag)', 'dB(dB(mW))', 'dex()'])
def test_unit_grammar_fail(string):
with pytest.raises(ValueError):
print(string)
>>> import sbpy.units
>>> sbpy.units.enable() # doctest: +SKIP
"""
__all__ = ['spectral_density_vega', 'enable', 'VEGA', 'VEGAmag', 'JM', 'JMmag']
from warnings import warn
import numpy as np
import astropy.units as u
from astropy.utils.exceptions import AstropyWarning
from ..spectroscopy.vega import Vega
VEGA = u.def_unit(['VEGA', 'VEGAflux'], doc='Spectral flux density of Vega.')
VEGAmag = u.MagUnit(VEGA)
VEGAmag.__doc__ = "Vega-based magnitude: Vega is 0 mag at all wavelengths"
JM = u.def_unit(['JM', 'JMflux'],
represents=VEGA * 10**(0.4 * 0.03),
doc=('Johnson-Morgan magnitude system flux density '
'zeropoint (Johnson et al. 1966; Bessell & Murphy '
'2012).'))
JMmag = u.MagUnit(JM)
JMmag.__doc__ = ("Johnson-Morgan magnitude system: Vega is 0.03 mag at "
"all wavelengths (Johnson et al. 1966; Bessell & Murphy "
"2012).")
def enable():
need to import the module::
>>> import astropy.units as u
>>> import etc.units
>>> u.Unit('mag(VEGA)')
Unit("mag(VEGA)")
"""
import numpy as np
import astropy.units as u
VEGA = u.def_unit(['VEGA', 'VEGAflux'],
doc='Spectral flux density of Vega.')
VEGAmag = u.MagUnit(VEGA)
VEGAmag.__doc__ = "Vega-based magnitude: Vega is 0 mag at all wavelengths"
u.add_enabled_units(VEGA)
def spectral_density(wfb):
"""Flux density equivalencies, extended for Vega-based magnitude systems.
This uses the default Vega spectrum that comes for 4MOST in the
Instrument Control Repository (ICR).
Vega is assumed to have an apparent magnitude of 0 in the
``VEGAmag`` system.
See https://github.com/astropy/astropy/issues/10821 for a
def overplot_spectroscopic(res,
drp_logcube,
drpall_row,
mass_ax,
ml_ax,
f_ax,
pca_system,
res_wcs,
cmlr,
mlb='i'):
'''
overplot cumulative spectroscopic masses, log M/L, cumulative fluxes
'''
# synthetic photometry of IFU data in rest frame
ebvgal = drpall_row['ebvgal']
r_v = 3.1
dustcorr = 10.**(0.4 * extinction.fitzpatrick99(
drp_logcube['WAVE'].data, a_v=r_v * ebvgal, r_v=r_v))[:, None, None]
ifu_s2p = spectrophot.Spec2Phot(
lam=drp_logcube['WAVE'].data / (1. + drpall_row['nsa_z']),
flam=1.0e-17 * drp_logcube['FLUX'].data * (1. + drpall_row['nsa_z']) *
dustcorr)
res_flux = (ifu_s2p.ABmags['sdss2010-{}'.format(mlb)] * u.ABmag).to(m.Mgy)
# map sky coordinates to number of effective radii from center
pos_to_nRe = RotatedParaboloid(ctr=np.array(
[drpall_row['objra'], drpall_row['objdec']]),
phi=drpall_row['nsa_elpetro_phi'] * u.deg,
axis_ratio=drpall_row['nsa_elpetro_ba'],
Re=drpall_row['nsa_elpetro_th50_r'] / 3600.)
badpdf = res.badPDF()
ml_mask = np.logical_or(res.mask, badpdf)
# WCS from results file determines where elliptical projection is sampled
#res_wcs = wcs.WCS(res['SNRMED'].header)
res_II, res_JJ = np.meshgrid(
*[np.linspace(0., s - 1., s) for s in res['SNRMED'].shape],
indexing='ij')
res_AA, res_DD = res_wcs.wcs_pix2world(res_JJ, res_II, 1)
# sample Re at spaxel centers
res_Re = pos_to_nRe(np.column_stack([res_AA.flatten(),
res_DD.flatten()
])).reshape(res_AA.shape)
nRe_to_plot = np.linspace(0., res_Re[~ml_mask].max(), 50.)
# mass, log M/L
badpdf = res.badPDF()
ml_mask = np.logical_or.reduce((res.mask, badpdf))
interior_mask = np.logical_or.reduce(
(badpdf,
(m.mask_from_maskbits(drp_logcube['MASK'].data, [3]).sum(axis=0) > 0),
(m.mask_from_maskbits(drp_logcube['MASK'].data, [2]).sum(axis=0) >
0)))
logml = infer_masked(res.param_dist_med(extname='ML{}'.format(mlb)),
ml_mask, interior_mask)
ml = 10.**logml * m.m_to_l_unit
res_MAG = res_flux.to(u.ABmag) - cosmo.distmod(drpall_row['nsa_zdist'])
mlb_sollum = 10.**(-0.4 * (res_MAG - spectrophot.absmag_sun_band[mlb] * u.ABmag)).value * \
m.bandpass_sol_l_unit
spectro_mass = (ml * mlb_sollum).to(u.Msun)
# sum mass within some number of Re
mass_within_nRe = np.array(
[sum_within_nRe(spectro_mass, res_Re, n) for n in nRe_to_plot])
mass_ax.plot(nRe_to_plot, mass_within_nRe, c='C1')
# plot mass to light versus Re
ml_sc = ml_ax.scatter(res_Re[~ml_mask],
logml[~ml_mask],
c='C1',
edgecolor='None',
s=.5)
res_Re_m = np.ma.array(res_Re, mask=ml_mask)
# find ring method log M/L
outer_ring = np.logical_and((res_Re_m <= res_Re_m.max()),
(res_Re_m >= res_Re_m.max() - .5))
outer_logml_ring = np.median(logml[~ml_mask * outer_ring])
ml_ax.scatter(x=[np.median(res_Re_m[~ml_mask * outer_ring])],
y=[outer_logml_ring],
marker='x',
c='C1')
# find CMLR log M/L
nsa_MAG = (np.array(drpall_row['nsa_elpetro_absmag'][2:]) * \
(u.ABmag - u.MagUnit(u.littleh**2))).to(u.ABmag, u.with_H0(cosmo.H0))
nsa_mag = (nsa_MAG + cosmo.distmod(drpall_row['nsa_zdist']))
nsa_flux = nsa_mag.to(m.Mgy)
ifu_mag = np.array(
[ifu_s2p.ABmags['sdss2010-{}'.format(b_)] for b_ in 'ugriz']) * u.ABmag
ifu_mag[~np.isfinite(ifu_mag)] = 40. * u.ABmag
ifu_flux = ifu_mag.to(m.Mgy)
flux_deficit = nsa_flux - ifu_flux.sum(axis=(1, 2))
logml_missingflux_cmlr = cmlr(2.5 *
np.log10(flux_deficit[1] / flux_deficit[2]))
ml_ax.scatter(x=[np.median(res_Re_m[~ml_mask * outer_ring])],
y=[logml_missingflux_cmlr],
marker='s',
c='C1',
edgecolor='k')
#
ml_missingflux_cmlr = 10.**logml_missingflux_cmlr * m.m_to_l_unit
ml_missingflux_ring = 10.**outer_logml_ring * m.m_to_l_unit
missing_mlb_MAG = flux_deficit[3].to(u.ABmag) - cosmo.distmod(
drpall_row['nsa_zdist'])
missing_mlb_sollum = 10.**(-0.4 * (missing_mlb_MAG - spectrophot.absmag_sun_band[mlb] * u.ABmag)).value * \
m.bandpass_sol_l_unit
missing_mass_cmlr = (ml_missingflux_cmlr * missing_mlb_sollum).to(u.Msun)
missing_mass_ring = (ml_missingflux_ring * missing_mlb_sollum).to(u.Msun)
mass_ax.scatter(x=res_Re.max() - .1,
y=mass_within_nRe[-1] * u.Msun + missing_mass_cmlr,
marker='s',
c='C1',
edgecolor='k',
zorder=3,
label='+AC(CMLR)')
mass_ax.scatter(x=res_Re.max(),
y=mass_within_nRe[-1] * u.Msun + missing_mass_ring,
marker='x',
c='C1',
edgecolor='k',
zorder=3,
label='+AC(RING)')
mass_ax.legend(loc='best', prop={'size': 'x-small'})
summed_flux = np.array([
sum_within_nRe(arr=res_flux, Re_a=res_Re, nRe=n) for n in nRe_to_plot
])
f_ax.plot(nRe_to_plot, summed_flux, label='IFU', c='C1')
f_ax.scatter(x=res_Re.max() + .1,
y=summed_flux[-1] * m.Mgy + flux_deficit[3],
marker='o',
c='C1',
edgecolor='k',
zorder=3)
def make_stellarmass_aperture_plot(preimaging,
dap_maps,
drp_logcube,
cmlr,
drpall_row,
mlb='i',
cb1='g',
cb2='r'):
'''
make aperture plot of included mass (from CMLR and preimaging) versus radius (from DAP)
preimaging: MaNGA_PreImage object
dap_maps: FITS HDUList with DAP MAPS outputs
'''
ebvgal = drpall_row['ebvgal']
# WCS from DAP determines sampling for Re grid, and where k-correction map is sampled
dap_wcs = wcs.WCS(dap_maps['SPX_SNR'].header)
dap_AA, dap_DD = dap_wcs.wcs_pix2world(
*np.meshgrid(*[
np.linspace(0., s - 1., s) for s in dap_maps['SPX_SNR'].data.shape
]), 1)
# map sky coordinates to number of effective radii from center
pos_to_nRe = RotatedParaboloid(ctr=np.array(
[drpall_row['objra'], drpall_row['objdec']]),
phi=drpall_row['nsa_elpetro_phi'] * u.deg,
axis_ratio=drpall_row['nsa_elpetro_ba'],
Re=drpall_row['nsa_elpetro_th50_r'] / 3600.)
# WCS from preimaging determines where elliptical projection is resampled
preimaging_wcs = wcs.WCS(preimaging['{} img'.format(mlb)].header)
preimaging_II, preimaging_JJ = np.meshgrid(
*[np.linspace(0., s - 1., s) for s in preimaging.img(mlb).shape],
indexing='ij')
preimaging_AA, preimaging_DD = preimaging_wcs.wcs_pix2world(
preimaging_JJ, preimaging_II, 1)
# evaluate Re interpolation on imaging RA/Dec grid
preimaging_Re = pos_to_nRe(
np.column_stack([preimaging_AA.flatten(),
preimaging_DD.flatten()
])).reshape(preimaging_AA.shape)
kcorr_cb1_interp, kcorr_cb2_interp, kcorr_mlb_interp = kcorr_spec_to_phot(
drp_logcube, dap_maps['SPX_MFLUX_IVAR'], drpall_row['nsa_z'], cb1, cb2,
mlb)
kcorr_cb1_phot = kcorr_cb1_interp(preimaging_AA.flatten(),
preimaging_DD.flatten()).reshape(
preimaging_AA.shape) * u.mag
kcorr_cb2_phot = kcorr_cb2_interp(preimaging_AA.flatten(),
preimaging_DD.flatten()).reshape(
preimaging_AA.shape) * u.mag
kcorr_color = kcorr_cb1_phot - kcorr_cb2_phot
kcorr_mlb_phot = kcorr_mlb_interp(preimaging_AA.flatten(),
preimaging_DD.flatten()).reshape(
preimaging_AA.shape) * u.mag
# evaluate CMLR given preimaging
ml_from_cmlr = 10.**cmlr(
color=preimaging.color(cb1, cb2, dustcorr=True, ebvgal=ebvgal) +
kcorr_color.value) * m.m_to_l_unit
img_mag = (preimaging.img(mlb) * 1.0e-9 * m.Mgy).to(
u.ABmag) + kcorr_mlb_phot
distmod = cosmo.distmod(drpall_row['nsa_zdist'])
img_MAG = img_mag - distmod
mlb_sollum = 10.**(-0.4 * (img_MAG - spectrophot.absmag_sun_band[mlb] * u.ABmag)).value * \
m.bandpass_sol_l_unit
mass_from_cmlr = (ml_from_cmlr * mlb_sollum).to(u.Msun)
nRe_to_plot = np.linspace(0., 0.9 * preimaging_Re.max(), 1000)
photomass_within_nRe = np.array([
sum_within_nRe(mass_from_cmlr, preimaging_Re, n) for n in nRe_to_plot
])
# solve for number of effective radii enclosing all of NSA flux
NSA_bands = 'FNugriz'
NSA_bands_ixs = dict(zip(NSA_bands, range(len(NSA_bands))))
NSA_MAG = drpall_row['nsa_elpetro_absmag'][NSA_bands_ixs[mlb]] * \
(u.ABmag - u.MagUnit(u.littleh**2))
NSA_kcorr_flux = (NSA_MAG.to(u.ABmag, u.with_H0(cosmo.H0)) + \
cosmo.distmod(drpall_row['nsa_zdist'])).to(m.Mgy)
fig, (ax1, ax2, ax3) = plt.subplots(nrows=3,
ncols=1,
figsize=(9, 7),
dpi=150,
sharex=True)
ax1.plot(nRe_to_plot, photomass_within_nRe, linewidth=1., color='C0')
ax1.set_yscale('log')
ax1.set_ylabel(r'$\frac{M_{< R}}{M_{\odot}}$', size='small')
ax2.scatter(preimaging_Re.flatten(),
np.log10(ml_from_cmlr.value.flatten()),
edgecolor='None',
s=.5,
c='C0')
ax2.set_ylabel(r'$\log \Upsilon^*_{{{}}}$'.format(mlb), size='small')
ax2.set_ylim([-2.5, 2.5])
summed_flux = np.array([
sum_within_nRe(arr=img_mag.to(m.Mgy), Re_a=preimaging_Re, nRe=n)
for n in nRe_to_plot
])
img_var = 1. / preimaging.img_ivar(mlb) * (1.0e-9 * m.Mgy)**2
quadsummed_fluxunc = np.sqrt(
np.array([
sum_within_nRe(arr=img_var, Re_a=preimaging_Re, nRe=n)
for n in nRe_to_plot
]))
ax3.plot(nRe_to_plot, summed_flux, label='K-Corr. Phot.', color='C0')
ax3.fill_between(nRe_to_plot,
summed_flux - quadsummed_fluxunc,
summed_flux + quadsummed_fluxunc,
alpha=0.5,
linewidth=0.25,
color='C0')
ax3.set_xlabel(r'$\frac{R}{R_e}$', size='small')
ax3.set_ylabel(r'$\frac{F_{<R}}{\rm Mgy}$', size='small')
ax3.set_yscale('log')
fig.suptitle(drpall_row['plateifu'])
return fig, ax1, ax2, ax3
class TestLogQuantityCreation:
@pytest.mark.parametrize('lq, lu',
zip(lq_subclasses + [u.LogQuantity],
lu_subclasses + [u.LogUnit]))
def test_logarithmic_quantities(self, lq, lu):
"""Check logarithmic quantities are all set up correctly"""
assert lq._unit_class == lu
assert type(lu()._quantity_class(1.)) is lq
@pytest.mark.parametrize('lq_cls, physical_unit',
itertools.product(lq_subclasses, pu_sample))
def test_subclass_creation(self, lq_cls, physical_unit):
"""Create LogQuantity subclass objects for some physical units,
and basic check on transformations"""
value = np.arange(1., 10.)
log_q = lq_cls(value * physical_unit)
assert log_q.unit.physical_unit == physical_unit
assert log_q.unit.function_unit == log_q.unit._default_function_unit
assert_allclose(log_q.physical.value, value)
with pytest.raises(ValueError):
lq_cls(value, physical_unit)
@pytest.mark.parametrize(
'unit', (u.mag, u.mag(), u.mag(u.Jy), u.mag(u.m), u.Unit(
2 * u.mag), u.MagUnit('', 2. * u.mag), u.MagUnit(
u.Jy, -1 * u.mag), u.MagUnit(u.m, -2. * u.mag)))
def test_different_units(self, unit):
q = u.Magnitude(1.23, unit)
assert q.unit.function_unit == getattr(unit, 'function_unit', unit)
assert q.unit.physical_unit is getattr(unit, 'physical_unit',
u.dimensionless_unscaled)
@pytest.mark.parametrize('value, unit',
((1. * u.mag(u.Jy), None),
(1. * u.dex(u.Jy), None),
(1. * u.mag(u.W / u.m**2 / u.Hz), u.mag(u.Jy)),
(1. * u.dex(u.W / u.m**2 / u.Hz), u.mag(u.Jy))))
def test_function_values(self, value, unit):
lq = u.Magnitude(value, unit)
assert lq == value
assert lq.unit.function_unit == u.mag
assert lq.unit.physical_unit == getattr(unit, 'physical_unit',
value.unit.physical_unit)
@pytest.mark.parametrize(
'unit', (u.mag(), u.mag(u.Jy), u.mag(u.m), u.MagUnit('', 2. * u.mag),
u.MagUnit(u.Jy, -1 * u.mag), u.MagUnit(u.m, -2. * u.mag)))
def test_indirect_creation(self, unit):
q1 = 2.5 * unit
assert isinstance(q1, u.Magnitude)
assert q1.value == 2.5
assert q1.unit == unit
pv = 100. * unit.physical_unit
q2 = unit * pv
assert q2.unit == unit
assert q2.unit.physical_unit == pv.unit
assert q2.to_value(unit.physical_unit) == 100.
assert (q2._function_view / u.mag).to_value(1) == -5.
q3 = unit / 0.4
assert q3 == q1
def test_from_view(self):
# Cannot view a physical quantity as a function quantity, since the
# values would change.
q = [100., 1000.] * u.cm / u.s**2
with pytest.raises(TypeError):
q.view(u.Dex)
# But fine if we have the right magnitude.
q = [2., 3.] * u.dex
lq = q.view(u.Dex)
assert isinstance(lq, u.Dex)
assert lq.unit.physical_unit == u.dimensionless_unscaled
assert np.all(q == lq)
def test_using_quantity_class(self):
"""Check that we can use Quantity if we have subok=True"""
# following issue #5851
lu = u.dex(u.AA)
with pytest.raises(u.UnitTypeError):
u.Quantity(1., lu)
q = u.Quantity(1., lu, subok=True)
assert type(q) is lu._quantity_class
class TestLogUnitArithmetic:
def test_multiplication_division(self):
"""Check that multiplication/division with other units is only
possible when the physical unit is dimensionless, and that this
turns the unit into a normal one."""
lu1 = u.mag(u.Jy)
with pytest.raises(u.UnitsError):
lu1 * u.m
with pytest.raises(u.UnitsError):
u.m * lu1
with pytest.raises(u.UnitsError):
lu1 / lu1
for unit in (u.dimensionless_unscaled, u.m, u.mag, u.dex):
with pytest.raises(u.UnitsError):
lu1 / unit
lu2 = u.mag(u.dimensionless_unscaled)
with pytest.raises(u.UnitsError):
lu2 * lu1
with pytest.raises(u.UnitsError):
lu2 / lu1
# But dimensionless_unscaled can be cancelled.
assert lu2 / lu2 == u.dimensionless_unscaled
# With dimensionless, normal units are OK, but we return a plain unit.
tf = lu2 * u.m
tr = u.m * lu2
for t in (tf, tr):
assert not isinstance(t, type(lu2))
assert t == lu2.function_unit * u.m
with u.set_enabled_equivalencies(u.logarithmic()):
with pytest.raises(u.UnitsError):
t.to(lu2.physical_unit)
# Now we essentially have a LogUnit with a prefactor of 100,
# so should be equivalent again.
t = tf / u.cm
with u.set_enabled_equivalencies(u.logarithmic()):
assert t.is_equivalent(lu2.function_unit)
assert_allclose(
t.to(u.dimensionless_unscaled,
np.arange(3.) / 100.),
lu2.to(lu2.physical_unit, np.arange(3.)))
# If we effectively remove lu1, a normal unit should be returned.
t2 = tf / lu2
assert not isinstance(t2, type(lu2))
assert t2 == u.m
t3 = tf / lu2.function_unit
assert not isinstance(t3, type(lu2))
assert t3 == u.m
# For completeness, also ensure non-sensical operations fail
with pytest.raises(TypeError):
lu1 * object()
with pytest.raises(TypeError):
slice(None) * lu1
with pytest.raises(TypeError):
lu1 / []
with pytest.raises(TypeError):
1 / lu1
@pytest.mark.parametrize('power', (2, 0.5, 1, 0))
def test_raise_to_power(self, power):
"""Check that raising LogUnits to some power is only possible when the
physical unit is dimensionless, and that conversion is turned off when
the resulting logarithmic unit (such as mag**2) is incompatible."""
lu1 = u.mag(u.Jy)
if power == 0:
assert lu1**power == u.dimensionless_unscaled
elif power == 1:
assert lu1**power == lu1
else:
with pytest.raises(u.UnitsError):
lu1**power
# With dimensionless, though, it works, but returns a normal unit.
lu2 = u.mag(u.dimensionless_unscaled)
t = lu2**power
if power == 0:
assert t == u.dimensionless_unscaled
elif power == 1:
assert t == lu2
else:
assert not isinstance(t, type(lu2))
assert t == lu2.function_unit**power
# also check we roundtrip
t2 = t**(1. / power)
assert t2 == lu2.function_unit
with u.set_enabled_equivalencies(u.logarithmic()):
assert_allclose(t2.to(u.dimensionless_unscaled, np.arange(3.)),
lu2.to(lu2.physical_unit, np.arange(3.)))
@pytest.mark.parametrize('other', pu_sample)
def test_addition_subtraction_to_normal_units_fails(self, other):
lu1 = u.mag(u.Jy)
with pytest.raises(u.UnitsError):
lu1 + other
with pytest.raises(u.UnitsError):
lu1 - other
with pytest.raises(u.UnitsError):
other - lu1
def test_addition_subtraction_to_non_units_fails(self):
lu1 = u.mag(u.Jy)
with pytest.raises(TypeError):
lu1 + 1.
with pytest.raises(TypeError):
lu1 - [1., 2., 3.]
@pytest.mark.parametrize('other', (u.mag, u.mag(), u.mag(u.Jy), u.mag(
u.m), u.Unit(2 * u.mag), u.MagUnit('', 2. * u.mag)))
def test_addition_subtraction(self, other):
"""Check physical units are changed appropriately"""
lu1 = u.mag(u.Jy)
other_pu = getattr(other, 'physical_unit', u.dimensionless_unscaled)
lu_sf = lu1 + other
assert lu_sf.is_equivalent(lu1.physical_unit * other_pu)
lu_sr = other + lu1
assert lu_sr.is_equivalent(lu1.physical_unit * other_pu)
lu_df = lu1 - other
assert lu_df.is_equivalent(lu1.physical_unit / other_pu)
lu_dr = other - lu1
assert lu_dr.is_equivalent(other_pu / lu1.physical_unit)
def test_complicated_addition_subtraction(self):
"""for fun, a more complicated example of addition and subtraction"""
dm0 = u.Unit('DM', 1. / (4. * np.pi * (10. * u.pc)**2))
lu_dm = u.mag(dm0)
lu_absST = u.STmag - lu_dm
assert lu_absST.is_equivalent(u.erg / u.s / u.AA)
def test_neg_pos(self):
lu1 = u.mag(u.Jy)
neg_lu = -lu1
assert neg_lu != lu1
assert neg_lu.physical_unit == u.Jy**-1
assert -neg_lu == lu1
pos_lu = +lu1
assert pos_lu is not lu1
assert pos_lu == lu1
def nsa_absmags(self):
absmags = np.array([
nsa_absmag(self.drpall_row, band, kind='elpetro')
for band in self.bands
]) * (u.ABmag - u.MagUnit(u.littleh**2))
return absmags
