def ma_with_oversmpling(Time,
per,
Tmid,
p,
a,
i,
linLimb,
quadLimb,
orbit="circular",
ld="quad",
b=0,
ReBin_N=1,
ReBin_dt=0,
ToPlot=False):
# Added ReBin_N, ReBin_dt to allow for finite integration time calculation by re-binning. These are the PyAstronomy parameters for the number of subsamples and the duration of the original samples
if ReBin_N > 1 and ReBin_dt > 0:
MA_Rebin = fuf.turnIntoRebin(ft.MandelAgolLC)
ma = MA_Rebin()
ma.setRebinArray_Ndt(Time, ReBin_N, ReBin_dt)
else:
ma = ft.MandelAgolLC()
ma.pars._Params__params = {
"orbit": orbit,
"ld": ld,
"per": per,
"i": i,
"a": a,
"p": p,
"linLimb": linLimb,
"quadLimb": quadLimb,
"b": b,
"T0": Tmid
}
model = ma.evaluate(Time)
if ToPlot:
plt.plot((Time - Tmid + per / 2) % per - per / 2, model, '.')
plt.xlabel("Time since T_mid [d]")
#plt.show()
return model
The analytical light curve is stored in the property `lightcurve`.
"""
# Translate the given parameters into an orbit and, finally,
# into a projected, normalized distance (z-parameter)
if self._orbit == "circular":
self._calcZList(time - self["T0"])
else:
# The orbit is keplerian
self._calcZList(time)
# Use occultquad Fortran library to compute flux decrease
df = numpy.zeros(len(time))
if len(self._intrans) > 0:
if self._ld == "quad":
# Use occultquad Fortran library to compute flux decrease
result = occultquad.occultquad(self._zlist[self._intrans], self["linLimb"], self["quadLimb"],
self["p"], len(self._intrans))
else:
result = occultnl.occultnl(self["p"], self["a1"], self["a2"], self["a3"],
self["a4"], self._zlist[self._intrans])
df[self._intrans] = (1.0 - result[0])
self.lightcurve = (1. - df) * 1. / \
(1. + self["b"]) + self["b"] / (1.0 + self["b"])
return self.lightcurve
MandelAgolLC_Rebin = fuf.turnIntoRebin(MandelAgolLC)
# 'W' parameters corresponding to notation in Pal '08
w = 6. - 2. * self["linLimb"] - self["quadLimb"]
w0 = (6. - 6. * self["linLimb"] - 12. * self["quadLimb"]) / w
w1 = (6. * self["linLimb"] + 12. * self["quadLimb"]) / w
w2 = 6. * self["quadLimb"] / w
# Initialize flux decrease array
df = numpy.zeros(len(time))
# Get a list of 'cases' (according to Pal '08). Depends on radius ratio and 'z'-parameter along the orbit
ca = self._selectCases()
# Loop through in-transit points in z-list,
# and calculate the light curve at each point in z (->time)
for i in self._intrans:
# Calculate the coefficients to be substituted into the Pal '08 equation
c = self._returnCoeff(ca[i].step, self._zlist[i])
# Substitute the coefficients and get 'flux decrease'
if ca[i].step != 12:
# Calculate flux decrease only if there is an occultation
if not self.useBoost:
df[i] = w0 * c[0] + w2 * c[5] + w1 * (c[1] + c[2] * mpmath.ellipk(
c[6]**2) + c[3] * mpmath.ellipe(c[6]**2) + c[4] * mpmath.ellippi(c[7], c[6]**2))
else:
df[i] = w0 * c[0] + w2 * c[5] + w1 * (c[1] + c[2] * self.ell.ell1(
c[6]) + c[3] * self.ell.ell2(c[6]) + c[4] * self.ell.ell3(c[7], c[6]))
self.lightcurve = (1. - df) * 1. / \
(1. + self["b"]) + self["b"] / (1.0 + self["b"])
return self.lightcurve
PalLC_Rebin = fuf.turnIntoRebin(PalLC)
(1.0 - self["gamma"]**2 - self["epsilon"]*(1./3. - self["gamma"]**2*(1.0-self.W1(rho[indi]))))
indi = numpy.where(numpy.logical_and( \
numpy.logical_and(rho >= 1.-self["gamma"], rho < 1.0+self["gamma"]), dphase < 0.25))[0]
z0 = self.z0(etap, indi)
y[indi] = (Xp[indi]*self["Omega"]*sin(self["Is"])*( \
(1.0-self["epsilon"]) * (-z0[indi]*zeta[indi] + self["gamma"]**2*acos(zeta[indi]/self["gamma"])) + \
(self["epsilon"]/(1.0+etap[indi]))*self.W4(x0[indi], zeta[indi], xc[indi], etap[indi]))) / \
(pi*(1.-1.0/3.0*self["epsilon"]) - (1.0-self["epsilon"]) * (asin(z0[indi])-(1.+etap[indi])*z0[indi] + \
self["gamma"]**2*acos(zeta[indi]/self["gamma"])) - self["epsilon"]*self.W3(x0[indi], zeta[indi], xc[indi], etap[indi]))
return y
RmcL_Rebin = turnIntoRebin(RmcL)
class RmcL_Hirano(OneDFit):
def __init__(self):
"""
This class implements analytical expressions for the Rossiter-McLaughlin \
effect for the case when the anomalous radial velocity is obtained by \
cross-correlation with a stellar spectrum, according to *Hirano et. al 2010*.
.. note::
The intrinsic line profile and the rotation kernel are both \
approximated by Gaussians, while the planet is assumed to be \
'sufficiently small enough'.
def sanity_Overbinning(self):
# Import numpy and matplotlib
from numpy import arange, sqrt, exp, pi, random, ones
import matplotlib.pylab as plt
# ... and now the funcFit package
from PyAstronomy import funcFit as fuf
# Creating a Gaussian with some noise
# Choose some parameters...
gPar = {"A":-5.0, "sig":10.0, "mu":10.0, "off":1.0, "lin":0.0}
# Calculate profile
x = arange(20)/20.0 * 100.0 - 50.0
y = gPar["off"] + gPar["A"] / sqrt(2*pi*gPar["sig"]**2) \
* exp(-(x-gPar["mu"])**2/(2*gPar["sig"]**2))
# Add some noise
y += random.normal(0.0, 0.01, x.size)
# Let us see what we have done...
plt.plot(x, y, 'bp')
# First, we create a "GaussFit1d_Rebin" class object (note that the
# class object has still to be instantiated, the name is arbitrary).
GaussFit1d_Rebin = fuf.turnIntoRebin(fuf.GaussFit1d)
# Do the instantiation and specify how the overbinning should be
# carried out.
gf = GaussFit1d_Rebin()
gf.setRebinArray_Ndt(x, 10, x[1]-x[0])
# See what parameters are available
print "List of available parameters: ", gf.availableParameters()
# Set guess values for the parameters
gf["A"] = -10.0
gf["sig"] = 15.77
gf["off"] = 0.87
gf["mu"] = 7.5
# Let us see whether the assignment worked
print "Parameters and guess values: "
print " A : ", gf["A"]
print " sig : ", gf["sig"]
print " off : ", gf["off"]
print " mu : ", gf["mu"]
print ""
# Now some of the strengths of funcFit are demonstrated; namely, the
# ability to consider some parameters as free and others as fixed.
# By default, all parameters of the GaussFit1d are frozen.
# Show values and names of frozen parameters
print "Names and values if FROZEN parameters: ", gf.frozenParameters()
# Which parameters shall be variable during the fit?
# 'Thaw' those (the order is irrelevant)
gf.thaw(["A", "sig", "off", "mu"])
# Let us assume that we know that the amplitude is negative, i.e.,
# no lower boundary (None) and 0.0 as upper limit.
gf.setRestriction({"A":[None,0.0]})
# Now start the fit
gf.fit(x, y, yerr=ones(x.size)*0.01)
# Write the result to the screen and plot the best fit model
gf.parameterSummary()
# Plot the final best-fit model
plt.plot(x, gf.model, 'rp--')
# Show the overbinned (=unbinned) model, indicate by color
# which point are averaged to obtain a point in the binned
# model.
for k, v in gf.rebinIdent.iteritems():
c = "y"
if k % 2 == 0: c = "k"
plt.plot(gf.rebinTimes[v], gf.unbinnedModel[v], c+'.')
w1 = (6. * self["linLimb"] + 12. * self["quadLimb"]) / w
w2 = 6. * self["quadLimb"] / w
# Initialize flux decrease array
df = numpy.zeros(len(time))
# Get a list of 'cases' (according to Pal '08). Depends on radius ratio and 'z'-parameter along the orbit
ca = self._selectCases()
# Loop through in-transit points in z-list,
# and calculate the light curve at each point in z (->time)
for i in self._intrans:
# Calculate the coefficients to be substituted into the Pal '08 equation
c = self._returnCoeff(ca[i].step, self._zlist[i])
# Substitute the coefficients and get 'flux decrease'
if ca[i].step != 12:
# Calculate flux decrease only if there is an occultation
if not self.useBoost:
df[i] = w0 * c[0] + w2 * c[5] + w1 * (
c[1] + c[2] * mpmath.ellipk(c[6]**2) +
c[3] * mpmath.ellipe(c[6]**2) +
c[4] * mpmath.ellippi(c[7], c[6]**2))
else:
df[i] = w0 * c[0] + w2 * c[5] + w1 * (
c[1] + c[2] * self.ell.ell1(c[6]) + c[3] *
self.ell.ell2(c[6]) + c[4] * self.ell.ell3(c[7], c[6]))
self.lightcurve = (1. - df) * 1. / \
(1. + self["b"]) + self["b"] / (1.0 + self["b"])
return self.lightcurve
PalLC_Rebin = fuf.turnIntoRebin(PalLC)
time : array
An array of time points at which the light curve
shall be calculated.
.. note:: time = 0 -> Planet is exactly in the line of sight (phase = 0).
Returns
-------
Model : array
The analytical light curve is stored in the property `lightcurve`.
"""
# Translate the given parameters into an orbit and, finally,
# into a projected, normalized distance (z-parameter)
self._calcZList(time - self["T0"])
# Use occultquad Fortran library to compute flux decrease
result = occultnl.occultnl(self["p"],self["a1"],self["a2"],self["a3"], \
self["a4"],self._zlist[self._intrans])
df = numpy.zeros(len(time))
df[self._intrans] = (1.0 - result[0])
self.lightcurve = (1. - df) * 1. / (1. + self["b"]) + self["b"] / (
1.0 + self["b"])
return self.lightcurve
MandelAgolNLLC_Rebin = fuf.turnIntoRebin(MandelAgolNLLC)