def ok(self):
"""
Checks for silly parameter values. Runnning this before chisq could
save time and disaster
"""
return self.vcheck('q', 0.001, 100.) and self.vcheck('iangle', 0., 90.) and \
self.vcheck('r1',0.,1.) and \
(float(self['r2'][0]) <= 0. or self.vcheck('r2',0.,1-roche.xl1(float(self['q'][0])))) and \
self.vcheck('cphi3',0.,0.25) and self.vcheck('cphi4',float(self['cphi3'][0]),0.25) and \
self.vcheck('t1',0.,1.e6) and self.vcheck('t2',-1.e6,1.e6) and \
self.vcheck('ldc1_1',-20.,20.) and self.vcheck('ldc1_2',-20.,20.) and \
self.vcheck('ldc1_3',-20.,20.) and self.vcheck('ldc1_4',-20.,20.) and \
self.vcheck('ldc2_1',-20.,20.) and self.vcheck('ldc2_2',-20.,20.) and \
self.vcheck('ldc2_3',-20.,20.) and self.vcheck('ldc2_3',-20.,20.) and \
self.vcheck('period',0.,100.) and self.vcheck('gravity_dark1',0.,1.) and \
self.vcheck('gravity_dark2',0.,1.) and \
(self['add_disc'][0] == '0' or \
((float(self['rdisc1'][0]) <= 0. or self.vcheck('rdisc1',float(self['r1'][0]),1.0)) \
and (float(self['rdisc2'][0]) <= 0. or \
self.vcheck('rdisc2',float(self['rdisc1'][0]),1.)) and \
self.vcheck('temp_disc',0.,1.e6) and self.vcheck('texp_disc',-10.,10.))) and \
(self['add_spot'][0] == '0' or \
(self.vcheck('radius_spot',0.,0.85*roche.xl1(float(self['q'][0]))) and \
self.vcheck('length_spot',0.,10.) and \
self.vcheck('expon_spot',0.,30.) and self.vcheck('temp_spot',0.,1.e6) and \
self.vcheck('cfrac_spot',0.,1.) and self.vcheck('epow_spot',0.,10.)))
def ln_prior(pars):
lnp = 0.0
# mass ratio - be loose (B12 says about 0.15)
prior = Prior("uniform", 0.02, 0.3)
lnp += prior.ln_prob(pars[0])
# r1_a (B12)
prior = Prior("gaussPos", 0.0213, 0.0015)
lnp += prior.ln_prob(pars[1])
# limb darkening
prior = Prior("gaussPos", 0.32, 0.03)
lnp += prior.ln_prob(pars[2])
# size of donor (B12)
prior = Prior("gaussPos", 0.113, 0.02)
# is donor bigger than roche lobe?
if pars[0] <= 0 or pars[3] > 1.0 - roche.xl1(pars[0]):
lnp += -np.inf
else:
lnp += prior.ln_prob(pars[3])
# inclination (B12)
prior = Prior("gaussPos", 85.9, 1.0)
if pars[4] >= 90.0:
lnp += -np.inf
else:
lnp += prior.ln_prob(pars[4])
# wd flux
prior = Prior("uniform", 0.01, 0.05)
lnp += prior.ln_prob(pars[5])
# donor flux
prior = Prior("uniform", 0.00, 0.01)
lnp += prior.ln_prob(pars[6])
# phase offset
prior = Prior("uniform", -0.01, 0.01)
lnp += prior.ln_prob(pars[7])
return lnp
def solve(input_data,baseDir):
q,dphi,rw,twd,p = input_data
# Kepler's law gives a quantity related to wd mass and separation, a
# scaled_mass = a**3/M_wd. I call this the scaled mass.
scaled_mass = const.G * (1+q) * p**2 / 4.0 / np.pi**2
# convert white dwarf radius to units of separation, rw/a
xl1_a = roche.xl1(q)
rw_a = rw*xl1_a
solved = True
try:
# try wood models
mw = find_wdmass(twd,scaled_mass,rw_a,baseDir,model='wood')
except:
# try panei models (usually for masses above 1 Msun)
try:
mw = find_wdmass(twd,scaled_mass,rw_a,baseDir,model='panei')
except:
# try hamada models (for masses less than 0.4 or more than 1.2 Msun)
try:
mw=find_wdmass(twd,scaled_mass,rw_a,baseDir,model='hamada')
except:
solved = False
# do nothing if none of the models yielded a solution
# otherwise,
if solved:
# donor star mass
mr = mw*q
# from this wd mass and scaled mass, find a
a3 = scaled_mass*mw
a = a3**(1./3.)
a = a.to(units.R_sun)
# inc
inc = roche.findi(q,dphi)
sini = np.sin(np.radians(inc))
# radial velocities
kw = (2.0*np.pi*sini*q*a/(1+q)/p).to(units.km/units.s)
kr = kw/q
#secondary radius
#use from Warner 1995 (eggleton)
#radius of sphere with same volume as Roche Lobe...
r2 = 0.49*a*q**(2.0/3.0)
r2 /= 0.6 * q**(2.0/3.0) + np.log(1.0+q**(1.0/3.0))
# need to be a little careful here for different versions of astropy
data = (q,mw,rw_a*a,mr,r2,a,kw,kr,inc)
if not quantitySupport:
data = [getval(datum) for datum in data]
return data
else:
return None
def ok(self):
"""
Checks for silly parameter values. Runnning this before chisq could
save time and disaster.
"""
return (
self.vcheck('q', 0.001, 100.) and self.vcheck('iangle', 0., 90.)
and self.vcheck('r1', 0., 1.)
and (float(self['r2'][0]) <= 0.
or self.vcheck('r2', 0., 1 - roche.xl1(float(self['q'][0]))))
and self.vcheck('cphi3', 0., 0.25)
and self.vcheck('cphi4', float(self['cphi3'][0]), 0.25)
and self.vcheck('t1', 0., 1.e6) and self.vcheck('t2', -1.e6, 1.e6)
and self.vcheck('ldc1_1', -50., 50.)
and self.vcheck('ldc1_2', -50., 50.)
and self.vcheck('ldc1_3', -50., 50.)
and self.vcheck('ldc1_4', -50., 50.)
and self.vcheck('ldc2_1', -50., 50.)
and self.vcheck('ldc2_2', -50., 50.)
and self.vcheck('ldc2_3', -50., 50.)
and self.vcheck('ldc2_3', -50., 50.)
and self.vcheck('period', 0., 100.)
and self.vcheck('gravity_dark1', 0., 5.)
and self.vcheck('gravity_dark2', 0., 5.) and
(self['add_disc'][0] == '0' or
((float(self['rdisc1'][0]) <= 0.
or self.vcheck('rdisc1', float(self['r1'][0]), 1.0)) and
(float(self['rdisc2'][0]) <= 0.
or self.vcheck('rdisc2', float(self['rdisc1'][0]), 1.))
and self.vcheck('temp_disc', 0., 1.e6)
and self.vcheck('texp_disc', -10., 10.))) and
(self['add_spot'][0] == '0' or
(self.vcheck('radius_spot', 0., 0.85 * roche.xl1(
float(self['q'][0]))) and self.vcheck('length_spot', 0., 10.)
and self.vcheck('expon_spot', 0., 30.) and self.vcheck(
'temp_spot', 0., 1.e6) and self.vcheck('cfrac_spot', 0., 1.)
and self.vcheck('epow_spot', 0., 10.))))
def solve(input_data, baseDir):
q, dphi, rw, twd, p = input_data
# Kepler's law gives a quantity related to wd mass and separation, a
# scaled_mass = a**3/M_wd. I call this the scaled mass.
scaled_mass = const.G * (1 + q) * p**2 / 4.0 / np.pi**2
# convert white dwarf radius to units of separation, rw/a
xl1_a = roche.xl1(q)
rw_a = rw * xl1_a
solved = True
try:
# try wood models
mw = find_wdmass(twd, scaled_mass, rw_a, baseDir, model='wood')
except:
# try panei models (usually for masses above 1 Msun)
try:
mw = find_wdmass(twd, scaled_mass, rw_a, baseDir, model='panei')
except:
# try hamada models (for masses less than 0.4 or more than 1.2 Msun)
try:
mw = find_wdmass(twd,
scaled_mass,
rw_a,
baseDir,
model='hamada')
except:
solved = False
# do nothing if none of the models yielded a solution
# otherwise,
if solved:
# donor star mass
mr = mw * q
# from this wd mass and scaled mass, find a
a3 = scaled_mass * mw
a = a3**(1. / 3.)
a = a.to(units.R_sun)
# inc
inc = roche.findi(q, dphi)
sini = np.sin(np.radians(inc))
# radial velocities
kw = (2.0 * np.pi * sini * q * a / (1 + q) / p).to(units.km / units.s)
kr = kw / q
#secondary radius
#use from Warner 1995 (eggleton)
#radius of sphere with same volume as Roche Lobe...
r2 = 0.49 * a * q**(2.0 / 3.0)
r2 /= 0.6 * q**(2.0 / 3.0) + np.log(1.0 + q**(1.0 / 3.0))
# need to be a little careful here for different versions of astropy
data = (q, mw, rw_a * a, mr, r2, a, kw, kr, inc)
if not quantitySupport:
data = [getval(datum) for datum in data]
return data
else:
return None
def ln_prior(self,verbose=False):
"""Returns the natural log of the prior probability of this model.
Certain parameters (dphi, rdisc, scale, az) need to be treated as special cases,
as the model contains more prior information than included in the parameter priors"""
# Use of the super function allows abstract class in model.py to be referenced
# Here the ln_prior function is referenced
retVal = super(LCModel,self).ln_prior()
# Remaining part of this function deals with special cases
# dphi
tol = 1.0e-6
try:
# Uses getParam function from model.py to get the objects of variable parameters
q = self.getParam('q')
dphi = self.getParam('dphi')
# maxphi is dphi when i = 90
maxphi = roche.findphi(q.currVal,90.0)
# dphi cannot be greater than (or within a certain tolerance of) maxphi
if dphi.currVal > maxphi-tol:
if verbose:
print('Combination of q and dphi is invalid')
retVal += -np.inf
except:
# We get here when roche.findphi raises error - usually invalid q
retVal += -np.inf
if verbose:
print('Combination of q and dphi is invalid')
# rdisc
try:
xl1 = roche.xl1(q.currVal) # xl1/a
maxrdisc = 0.46/xl1 # Maximum size disc can reach before precessing
# rdisc is unique to each eclipse, so have to use slightly different method to
# obtain its object, compared to q and dphi which are shared parameters
rdiscTemplate = 'rdisc_{0}'
for iecl in range(self.necl):
rdisc = self.getParam(rdiscTemplate.format(iecl))
# rdisc cannot be greater than maxrdisc
if rdisc.currVal > maxrdisc:
retVal += -np.inf
except:
# We get here when roche.findphi raises error - usually invalid q
if verbose:
print('Rdisc and q imply disc does not hit stream')
retVal += -np.inf
#BS scale
rwd = self.getParam('rwd')
minscale = rwd.currVal/3 # Minimum BS scale equal to 1/3 of rwd
maxscale = rwd.currVal*3 # Maximum BS scale equal to 3x rwd
scaleTemplate = 'scale_{0}'
for iecl in range(self.necl):
scale = self.getParam(scaleTemplate.format(iecl))
# BS scale must be within allowed range
if scale.currVal < minscale or scale.currVal > maxscale:
retVal += -np.inf
if verbose:
print('BS Scale is not between 1/3 and 3 times WD size')
#BS az
slope = 80.0
try:
# Find position of bright spot where it hits disc
azTemplate = 'az_{0}'
for iecl in range(self.necl):
rdisc = self.getParam(rdiscTemplate.format(iecl))
rd_a = rdisc.currVal*xl1 # rdisc/a
az = self.getParam(azTemplate.format(iecl))
# Does stream miss disc? (rdisc/a < 0.2 or rdisc/a > 0.65 )
# If yes, Tom's code will fail
# Calculate position of BS
x,y,vx,vy = roche.bspot(q.currVal,rd_a)
# Find tangent to disc at this point
alpha = np.degrees(np.arctan2(y,x))
# Alpha is between -90 and 90. If negative, spot lags disc (i.e. alpha > 90)
if alpha < 0: alpha = 90 - alpha
tangent = alpha + 90 # Disc tangent
# Calculate minimum and maximum az values using tangent and slope
minaz = max(0,tangent-slope)
maxaz = min(178,tangent+slope)
# BS az must be within allowed range
if az.currVal < minaz or az.currVal > maxaz:
retVal += -np.inf
except:
if verbose:
print('Stream does not hit disc, or az is outside 80 degree tolerance')
# We get here when roche.findphi raises error - usually invalid q
retVal += -np.inf
if complex:
# BS exponential parameters
# Total extent of bright spot is scale*(e1/e2)**(1/e2)
# Limit this to half an inner lagrangian distance
scaleTemplate = 'scale_{0}'
exp1Template = 'exp1_{0}'
exp2Template = 'exp2_{0}'
for iecl in range(self.necl):
sc = self.getParam(scaleTemplate.format(iecl))
e1 = self.getParam(exp1Template.format(iecl))
e2 = self.getParam(exp2Template.format(iecl))
if sc.currVal*(e1.currVal/e2.currVal)**(1.0/e2.currVal) > 0.5:
retVal += -np.inf
return retVal
from __future__ import print_function
import matplotlib.pyplot as plt
import numpy as np
from trm import roche
import sys
import lfit
import time
import os
phi = np.linspace(-0.15,0.2,1000,endpoint=False)
width = np.mean(np.diff(phi))*np.ones_like(phi)/2.
q = 0.1
inc = 85.9
xl1 = roche.xl1(q)
dphi = roche.findphi(q,inc)
rwd = 0.01
rdisc = 0.6
rexp = 0.2
az = 157.0
frac = 0.2
scale = 0.039
exp1 = 2.0
exp2 = 1.0
tilt = 120.0
yaw = 1.0
start = time.clock()
w = lfit.PyWhiteDwarf(rwd,0.4)
import numpy as np from trm import roche import sys import lfit import time import commands import os q = 0.1 inc = 86.9 phi = np.linspace(-0.5, 0.5, 1000) width = np.mean(np.diff(phi)) * np.ones_like(phi) / 2.0 xl1 = roche.xl1(q) dphi = roche.findphi(q, inc) rwd = 0.01 # r1_a w = lfit.PyWhiteDwarf(rwd / xl1, 0.4) rdisc = 0.6 rexp = 0.2 d = lfit.PyDisc(q, rwd / xl1, rdisc, rexp, 1000) az = 157.0 frac = 0.2 scale = 0.039 exp1 = 2.0 exp2 = 1.0 tilt = 120.0 yaw = 1.0
def ln_prior_base(pars):
lnp = 0.0
#Wd flux
prior = Prior('uniform',0.001,2)
lnp += prior.ln_prob(pars[0])
#Disc flux
prior = Prior('uniform',0.001,2)
lnp += prior.ln_prob(pars[1])
#BS flux
prior = Prior('uniform',0.001,2)
lnp += prior.ln_prob(pars[2])
#Donor flux
prior = Prior('uniform',0.0,2)
lnp += prior.ln_prob(pars[3])
#Mass ratio
prior = Prior('uniform',0.001,3.5)
lnp += prior.ln_prob(pars[4])
#Wd eclipse width, dphi
tol = 1.0e-6
try:
maxphi = roche.findphi(pars[4],90.0) #dphi when i is slightly less than 90
prior = Prior('uniform',0.001,maxphi-tol)
lnp += prior.ln_prob(pars[5])
except:
# we get here when roche.findphi raises error - usually invalid q
lnp += -np.inf
#Disc radius (XL1)
try:
xl1 = roche.xl1(pars[4]) # xl1/a
prior = Prior('uniform',0.25,0.46/xl1) # maximum size disc can be without precessing
lnp += prior.ln_prob(pars[6])
except:
# we get here when roche.findphi raises error - usually invalid q
lnp += -np.inf
#Limb darkening
prior = Prior('gauss',0.39,0.005)
lnp += prior.ln_prob(pars[7])
#Wd radius (XL1)
prior = Prior('uniform',0.0001,0.1)
lnp += prior.ln_prob(pars[8])
#BS scale (XL1)
rwd = pars[8]
prior = Prior('log_uniform',rwd/3.,rwd*3.)
lnp += prior.ln_prob(pars[9])
#BS az
slop=40.0
try:
# find position of bright spot where it hits disc
# will fail if q invalid
xl1 = roche.xl1(pars[4]) # xl1/a
rd_a = pars[6]*xl1
# Does stream miss disc? (disc/a < 0.2 or > 0.65 )
# if so, Tom's code will fail
x,y,vx,vy = roche.bspot(pars[4],rd_a)
# find tangent to disc at this point
alpha = np.degrees(np.arctan2(y,x))
# alpha is between -90 and 90. if negative spot lags disc ie alpha > 90
if alpha < 0: alpha = 90-alpha
tangent = alpha + 90 # disc tangent
prior = Prior('uniform',max(0,tangent-slop),min(178,tangent+slop))
lnp += prior.ln_prob(pars[10])
except:
lnp += -np.inf
#BS isotropic fraction
prior = Prior('uniform',0.001,0.9)
lnp += prior.ln_prob(pars[11])
#Disc exponent
prior = Prior('uniform',0.0001,2.5)
lnp += prior.ln_prob(pars[12])
#Phase offset
prior = Prior('uniform',-0.1,0.1)
lnp += prior.ln_prob(pars[13])
if len(pars) > 14:
#BS exp1
prior = Prior('uniform',0.01,4.0)
lnp += prior.ln_prob(pars[14])
#BS exp2
prior = Prior('uniform',0.9,3.0)
lnp += prior.ln_prob(pars[15])
#BS tilt angle
prior = Prior('uniform',0.0,165.0)
lnp += prior.ln_prob(pars[16])
#BS yaw angle
prior = Prior('uniform',-90,90.0)
lnp += prior.ln_prob(pars[17])
return lnp
