def test_hashable():
lu1 = u.dB(u.mW)
lu2 = u.dB(u.m)
lu3 = u.dB(u.mW)
assert hash(lu1) != hash(lu2)
assert hash(lu1) == hash(lu3)
luset = {lu1, lu2, lu3}
assert len(luset) == 2
def test_hashable():
lu1 = u.dB(u.mW)
lu2 = u.dB(u.m)
lu3 = u.dB(u.mW)
assert hash(lu1) != hash(lu2)
assert hash(lu1) == hash(lu3)
luset = {lu1, lu2, lu3}
assert len(luset) == 2
mixin_cols = {
'tm':
tm,
'dt':
TimeDelta([1, 2] * u.day),
'sc':
sc,
'scc':
scc,
'scd':
SkyCoord([1, 2], [3, 4], [5, 6],
unit='deg,deg,m',
frame='fk4',
obstime=['J1990.5', 'J1991.5']),
'x': [1, 2] * u.m,
'qdb': [10, 20] * u.dB(u.mW),
'qdex': [4.5, 5.5] * u.dex(u.cm / u.s**2),
'qmag': [21, 22] * u.ABmag,
'lat':
Latitude([1, 2] * u.deg),
'lon':
Longitude([1, 2] * u.deg, wrap_angle=180. * u.deg),
'ang':
Angle([1, 2] * u.deg),
'el2':
el2,
}
time_attrs = ['value', 'shape', 'format', 'scale', 'location']
compare_attrs = {
'c1': ['data'],
't_a_from_powerflux_nu',
'powerflux_nu_from_t_a',
'free_space_loss',
'Erx_unit',
'R0',
'MU0',
'EPS0',
'C',
'KB',
'efield_equivalency',
] + UNITS
# define some useful dB-Scales
# dimless = apu.Unit(1)
dimless = apu.dimensionless_unscaled
dB = dBi = dBc = apu.dB(dimless)
dB_W = apu.dB(apu.W)
dB_W_Hz = apu.dB(apu.W / apu.Hz)
dB_W_m2 = apu.dB(apu.W / apu.m**2)
dB_W_m2_Hz = apu.dB(apu.W / apu.Hz / apu.m**2)
dB_Jy_Hz = apu.dB(apu.Jy * apu.Hz)
dBm = dB_mW = apu.dB(apu.mW)
dBm_MHz = dB_mW_MHz = apu.dB(apu.mW / apu.MHz)
dB_uV_m = apu.dB(apu.uV**2 / apu.m**2)
dB_1_m = apu.dB(1. / apu.m) # for antenna factor
# Astropy.unit equivalency between linear and logscale field strength
# this is necessary, because the dB_uV_m is from E ** 2 (dB scale is power)
# one can make use of the equivalency in the .to() function, e.g.:
# Erx_unit.to(cnv.dB_uV_m, equivalencies=efield_equivalency)
# this conflicts with apu.logarithmic():
'powerflux_from_efield', 'efield_from_powerflux',
'ptx_from_efield', 'efield_from_ptx',
'powerflux_from_ptx', 'ptx_from_powerflux',
'prx_from_powerflux', 'powerflux_from_prx',
'prx_from_ptx', 'ptx_from_prx',
't_a_from_prx_nu', 'prx_nu_from_t_a',
't_a_from_powerflux_nu', 'powerflux_nu_from_t_a',
'free_space_loss',
'Erx_unit', 'R0', 'efield_equivalency',
] + UNITS
# define some useful dB-Scales
# dimless = apu.Unit(1)
dimless = apu.dimensionless_unscaled
dB = dBi = dBc = apu.dB(dimless)
dB_W = apu.dB(apu.W)
dB_W_Hz = apu.dB(apu.W / apu.Hz)
dB_W_m2 = apu.dB(apu.W / apu.m ** 2)
dB_W_m2_Hz = apu.dB(apu.W / apu.Hz / apu.m ** 2)
dB_Jy_Hz = apu.dB(apu.Jy * apu.Hz)
dBm = dB_mW = apu.dB(apu.mW)
dBm_MHz = dB_mW_MHz = apu.dB(apu.mW / apu.MHz)
dB_uV_m = apu.dB(apu.uV ** 2 / apu.m ** 2)
dB_1_m = apu.dB(1. / apu.m) # for antenna factor
# Astropy.unit equivalency between linear and logscale field strength
# this is necessary, because the dB_uV_m is from E ** 2 (dB scale is power)
# one can make use of the equivalency in the .to() function, e.g.:
# Erx_unit.to(cnv.dB_uV_m, equivalencies=efield_equivalency)
# this conflicts with apu.logarithmic():
def get_scaling(self):
return float(
self._interface.query("DISP:WIND:SUBW:TRAC:Y:SCAL:RLEV?")) * u.dB(
u.mW)
