def Compute_dNdf(input, output, h): # Meat of the code we are computing
'''
Compute d4N/(dz dM dq df) for a given df bin
This formula is made to work with the joblib python package
@param input: An array of appropriate parameters, see first few lines of this formula which unpacks the input array
@param output: An empty array which gets filled by this formula
@param h: The index for which df bin to fill in the output array
'''
alpha = input[0][h] # gravitational wave frequency specific to a bin
Redshifts = input[1]
logGalMass = input[2]
MassRatios = input[3]
dz = input[4]
dMass = input[5]
dq = input[6]
Dist = input[7]
Vc_interp = input[8] # comoving volume to use for interpolation
z_interp = input[9] # redshift to use for interpolation
dist4interp = input[10] # proper distance to use for interpolation
dVdz_interp = interp.interp1d(z_interp, Vc_interp) # Does 1-dimensional interpolation to find the slope
dist_interp = interp.interp1d(z_interp, dist4interp)
RandState = np.random.RandomState()
dNdt_ET = 1e-100 # initialize number of early type memory events
dNdt_LT = 1e-100 # initialize numer of late type memory events
epsilon = RandState.normal(0, 0.36, (2, len(Redshifts), len(logGalMass), len(MassRatios)))
for ii in xrange(len(Redshifts)):
z = Redshifts[ii]
frac = ABBSutils.KeenanPairFraction(z)
dV = ABBSinit.CoMoveVolume(z)
dVcdz = ABBSinit.Vdz(z)
dtrdt = 1/(1+z)
dist = Dist[ii]
for jj in xrange(len(logGalMass)):
logM1 = logGalMass[jj]
M1 = 10**logM1
dM = dMass[jj]
PhiET = ABBSutils.CANDELS_ZFOURGE_MF(logM1, z, 'early')
PhiLT = ABBSutils.CANDELS_ZFOURGE_MF(logM1, z, 'late')
for kk in xrange(len(MassRatios)):
q = MassRatios[kk]
dfrac = -frac / (q * np.log(0.4)) # from Sesana 2013 - [ dfrac/d(log q) = constant from Xu 2012 ]
tau = (1.264e16) * (M1 * 1.75e-11)**(-0.3) * (1 + (z/8)) # from Lotz 2011 - units of secs
d3nET = (PhiET * dfrac * dtrdt * dVcdz / tau) # Differential Number of Early-Type Galaxy Mergers
d3nLT = (PhiLT * dfrac * dtrdt * dVcdz / tau) # Differential Number of Late-Type Galaxy Mergers
# McET, MtotET, MqET = ABBSinit.MChirpEarlyType_NoScatter(M1, q, 8.46, 1.05)
# McLT, MtotLT, MqLT = ABBSinit.MChirpLateType_NoScatter(M1, q, 8.46, 1.05)
ep_ET = epsilon[0, ii, jj, kk]
McET, MtotET, MqET = ABBS.init.MChirpEarlyType(M1, q, 8.46, 1.05, ep_ET)
ep_LT = epsilon[1, ii, jj, kk]
McLT, MtotLT, MqLT = ABBSinit.MChirpLateType(M1, q, 8.46, 1.05, ep_LT)
# # Calculate Memory Signal #
tauET = ABBSinit.Tau_GW_alpha(alpha, MtotET, McET) #. Convert f to output of Kepler's third law (use alpha for semi-major axis)
tauLT = ABBSinit.Tau_GW_alpha(alpha, MtotLT, McLT) #. Convert f to output of Kepler's third law
z_coalET = ABBSinit.z_coal(z, tauET)
z_coalLT = ABBSinit.z_coal(z, tauLT)
#print tauET, z_coalET
muET = MtotET * (MqET / (1 + MqET))
muLT = MtotLT * (MqLT / (1 + MqLT))
i_ET = np.arcsin(RandState.uniform())
i_LT = np.arcsin(RandState.uniform())
dist_mem_ET = dist_interp(z_coalET) * 1e6
dist_mem_LT = dist_interp(z_coalLT) * 1e6
h_mem_ET = ABBSinit.h_mem_plus(i_ET, muET, dist_mem_ET, z_coalET)
h_mem_LT = ABBSinit.h_mem_plus(i_LT, muLT, dist_mem_LT, z_coalLT)
dVcdzET_mem = dVdz_interp(z_coalET)
dVcdzLT_mem = dVdz_interp(z_coalLT)
dzdt_ET_mem = ABBSinit.tdz(z_coalET)**(-1)
dzdt_LT_mem = ABBSinit.tdz(z_coalLT)**(-1)
dtdz_merger = ABBSinit.tdz(z)
#. In order to find the number of memory events occuring during some observation time, we need to first
#. convert the rate of events from that measured in the binary's rest frame to that measured on Earth.
#. Multiply by one Earth year to find the number of events observed.
prefactor = (dfrac / tau) * dtdz_merger * dtrdt
#print PhiET, prefactor, dVcdzET_mem, dzdt_ET_mem, dq, dM, dz
dNdt_ET += PhiET * prefactor * dVcdzET_mem * dzdt_ET_mem * dq * dM * dz * (3.1e7)
dNdt_LT += PhiLT * prefactor * dVcdzLT_mem * dzdt_LT_mem * dq * dM * dz * (3.1e7)
print dNdt_ET, dNdt_LT
output[0,h] = dNdt_ET # output in 1/yr
output[1,h] = dNdt_LT
def Compute_dNdf(input, output, h):
'''
Compute d4N/(dz dM dq df) for a given df bin
This formula is made to work with the joblib python package
@param input: An array of appropriate parameters, see first few lines of this formula which unpacks the input array
@param output: An empty array which gets filled by this formula
@param h: The index for which df bin to fill in the output array
'''
f = input[0][h]
dfdlnf = f
Redshifts = input[1]
logGalMass = input[2]
MassRatios = input[3]
dz = input[4]
dMass = input[5]
dq = input[6]
dlnf = input[7][h]
Dist = input[8]
Vc_interp = input[9]
z_interp = input[10]
dist4interp = input[11]
dVdz_interp = interp.interp1d(z_interp, Vc_interp)
dist_interp = interp.interp1d(z_interp, dist4interp)
RandState = np.random.RandomState()
for ii in xrange(len(Redshifts)):
z = Redshifts[ii]
frac = ABBSutils.KeenanPairFraction(z)
dVcdz = ABBSinit.Vdz(z)
dtrdt = 1/(1+z)
dtdz = ABBSinit.tdz(z)
dist = Dist[ii]
for jj in xrange(len(logGalMass)):
logM1 = logGalMass[jj]
M1 = 10**logM1
dM = dMass[jj]
PhiET = ABBSutils.CANDELS_ZFOURGE_MF(logM1, z, 'early')
PhiLT = ABBSutils.CANDELS_ZFOURGE_MF(logM1, z, 'late')
for kk in xrange(len(MassRatios)):
q = MassRatios[kk]
dfrac = -frac / (q * np.log(0.4)) # from Sesana 2013 - [ dfrac/d(log q) = constant from Xu 2012 ]
tau = (1.264e16) * (M1 * 1.75e-11)**(-0.3) * (1 + (z/8)) # from Lotz 2011 - units of secs
d3nET = (PhiET * dfrac * dtrdt * dVcdz / tau) # Differential Number of Early-Type Galaxy Mergers
d3nLT = (PhiLT * dfrac * dtrdt * dVcdz / tau) # Differential Number of Late-Type Galaxy Mergers
McET, MtotET, MqET = ABBSinit.MChirpEarlyType_NoScatter(M1, q, 8.46, 1.05)
McLT, MtotLT, MqLT = ABBSinit.MChirpLateType_NoScatter(M1, q, 8.46, 1.05)
dtdfET = ABBSinit.tdf(z, McET, f)
dtdfLT = ABBSinit.tdf(z, McLT, f)
h_insp_ET = ABBSinit.RMSStrainFAST(z, McET, f, dist)
h_insp_LT = ABBSinit.RMSStrainFAST(z, McLT, f, dist)
d4NET_insp = d3nET * dtdfET * dfdlnf * dz * dM * dq * dlnf
d4NLT_insp = d3nLT * dtdfLT * dfdlnf * dz * dM * dq * dlnf
# Calculate Memory Signal #
# tau_GW_ET = ABBSinit.Tau_GW(z, McET, f)
# tau_GW_LT = ABBSinit.Tau_GW(z, McLT, f)
# z_coalET = ABBSinit.z_coal(z, tau_GW_ET)
# z_coalLT = ABBSinit.z_coal(z, tau_GW_LT)
muET = MtotET * (MqET / (1 + MqET)**2)
muLT = MtotLT * (MqLT / (1 + MqLT)**2)
i_ET = np.pi / 2. #np.arcsin(RandState.uniform())
i_LT = np.pi / 2. #np.arcsin(RandState.uniform())
# dist_mem_ET = dist_interp(z_coalET) * 1e6
# dist_mem_LT = dist_interp(z_coalLT) * 1e6
h_mem_ET = ABBSinit.h_mem_plus(i_ET, muET, dist * 1e6, z) # dist needs to be in parsec
h_mem_LT = ABBSinit.h_mem_plus(i_LT, muLT, dist * 1e6, z) # dist needs to be in parsec
# dVcdzET_mem = dVdz_interp(z_coalET)
# dVcdzLT_mem = dVdz_interp(z_coalLT)
# dzdt_ET_mem = ABBSinit.tdz(z_coalET)**(-1)
# dzdt_LT_mem = ABBSinit.tdz(z_coalLT)**(-1)
# d3nET_mem = (PhiET * dfrac * dtrdt * dtdz * dzdt_ET_mem * dVcdzET_mem / tau)
# d3nLT_mem = (PhiLT * dfrac * dtrdt * dtdz * dzdt_LT_mem * dVcdzLT_mem / tau)
d4NET_mem = d3nET * dz * dM * dq * dfdlnf
d4NLT_mem = d3nLT * dz * dM * dq * dfdlnf
output[0, h, ii, jj, kk] = d4NET_insp
output[1, h, ii, jj, kk] = d4NLT_insp
output[2, h, ii, jj, kk] = h_insp_ET**2
output[3, h, ii, jj, kk] = h_insp_LT**2
output[4, h, ii, jj, kk] = d4NET_mem
output[5, h, ii, jj, kk] = d4NLT_mem
output[6, h, ii, jj, kk] = (h_mem_ET / f)**2
output[7, h, ii, jj, kk] = (h_mem_LT / f)**2
