def Dc2(z1,z2):
Dcz1 = (p15.comoving_distance(z1).value*p15.h)
Dcz2 = (p15.comoving_distance(z2).value*p15.h)
res = Dcz2-Dcz1+1e-8
return res
"""Dc2(z1,z2) returns comoving distance between two objects at different redshifts. It accepts z1
and z2 as input, which are redshifts of lens and source, respectively."""
"""Parameters
def convert_one_from_dir(file_name_base,ncc):
mp=7.43e9
zs = 1.0
file_dir = "./15x15/"
#file_name_base = "s97"
file_in_base = file_dir+file_name_base
zl_array = np.fromfile(file_in_base+"_redshift.bin",dtype = ">f")
zl = 0.5*(zl_array.max()+zl_array.min())
zD = cosmo.comoving_distance(zl)*cosmo.h
zB = cosmo.comoving_distance(zl_array.max())-cosmo.comoving_distance(zl_array.min())
x1 = np.fromfile(file_in_base+"_theta.bin",dtype = ">f")
npp=len(x1) # total mass = 1e9*2e5 M_sun/h
bsz = 15.0
if ((npp/500000.0)<2):
nsa = 1
else:
nsa = int(npp/500000.0)
#nsa = 1
xc1 = (x1.max()+x1.min())*0.5
x1 = x1[::nsa]-xc1
x2 = np.fromfile(file_in_base+"_phi.bin",dtype = ">f")
xc2 = (x2.max()+x2.min())*0.5
x2 = x2[::nsa]-xc2
x3 = (np.random.random_sample((len(x1)))-0.5)*zB/zD*mm.apr/3600
#print zB/zD*mm.apr/3600
#x3 = np.linspace(-0.5,0.5,len(x1))*100.0/zD*mm.apr/3600
#print nsa,len(x1),len(x2),len(x3)
if npp > 100:
sdens_angular = call_cic_sdens(x1,x2,bsz,ncc,len(x1))*mp/np.deg2rad(1.0)**2.0*npp/len(x1)
else:
sdens_angular = call_sph_sdens(x1,x2,x3,bsz,ncc,len(x1))*mp/np.deg2rad(1.0)**2.0*npp/len(x1)
#sdens_angular_normal = (sdens_angular-sdens_angular.mean())
sdens_angular_normal = sdens_angular
Dcl = (cosmo.comoving_distance(zl).value*cosmo.h)
Dcs = (cosmo.comoving_distance(zs).value*cosmo.h)
Dcls = Dcs-Dcl
kappa = 4.0*np.pi*mm.G/mm.vc**2*(1.0+zl)/Dcl*Dcls/Dcs*sdens_angular_normal
##----------------------------
#sdens_normal = sdens_angular_normal/mm.Da(zl)**2.0/mm.sigma_crit(zl,zs)
##----------------------------
#file_out ="./output_files/"+file_name_base+"_"+str(zl)+"_sdens_normal.bin"
#sdens_normal.astype(np.float32).tofile(file_out)
return kappa,zl
def projected_rho_mean(z1, z2):
# return the mean density of the unvierse integrated across redshifts
# z1 and z2, in comoving (M_sun/h)(Mpc/h)^-3
pc0 = cosmo.critical_density(0).to(units.Msun / units.Mpc**3).value
Om0 = cosmo.Om0
rho_mean_0 = Om0 * pc0
d1 = cosmo.comoving_distance(z1).value
d2 = cosmo.comoving_distance(z2).value
return rho_mean_0 * (d2 - d1) / cosmo.h
def _SFR_UV(self, z, fmag, nmag, rmag, f_flux):
''' calculate UV star formation rates based on Salim+(2007) Eq. 5, 7, 8.
:param z:
redshift
:param fmag:
FUV absolute magnitude
:param nmag:
NUV absolute magnitude
:param rmag:
r-band absolute magnitude
:param f_flux:
FUV flux in Janskies. See `_jansky` method for conversion
'''
from astropy.cosmology import WMAP7
fn = fmag - nmag
opt = nmag - rmag # N-r
#Luminosity Distance
dist = WMAP7.comoving_distance(z)
ldist = (1 + z) * dist.value
#calculating Attenuation 'atten'
atten = np.repeat(-999., len(fmag))
case1 = np.where((opt > 4.) & (fn < 0.95))
atten[case1] = 3.32 * fn[case1] + 0.22
case2 = np.where((opt > 4.) & (fn >= 0.95))
atten[case2] = 3.37
case3 = np.where((opt <= 4.) & (fn < 0.9))
atten[case3] = 2.99 * fn[case3] + 0.27
case4 = np.where((opt <= 4.) & (fn >= 0.9))
atten[case4] = 2.96
#if opt >= 4.0:
# if fn < 0.95:
# atten = 3.32*fn + 0.22
# else:
# atten = 3.37
#else:
# if fn < 0.90:
# atten = 2.99*fn +0.27
# else:
# atten = 2.96
lum = 4. * np.pi * (ldist**2.0) * (3.087**2.0) * (10**(
25.0 + (atten / 2.5))) * f_flux #Luminosity
sfr = 1.08 * (10**(-28.0)) * np.abs(lum)
return sfr
def UVsfr(z, fmag, nmag, rmag, f_flux):
''' Calculate UV star formation rates.
Inputs: NSAID,z,F-band magnitude, N-band magnitude, r-band magnitude, F-band flux in Janskies
'''
fn = fmag - nmag
opt = nmag - rmag # N-r
#Luminosity Distance
dist = WMAP7.comoving_distance(z)
ldist = (1 + z) * dist
#calculating Attenuation 'atten'
atten = np.repeat(-999., len(fmag))
case1 = np.where((opt > 4.) & (fn < 0.95))
atten[case1] = 3.32 * fn[case1] + 0.22
case2 = np.where((opt > 4.) & (fn >= 0.95))
atten[case2] = 3.37
case3 = np.where((opt <= 4.) & (fn < 0.9))
atten[case3] = 2.99 * fn[case3] + 0.27
case4 = np.where((opt <= 4.) & (fn >= 0.9))
atten[case4] = 2.96
#if opt >= 4.0:
# if fn < 0.95:
# atten = 3.32*fn + 0.22
# else:
# atten = 3.37
#else:
# if fn < 0.90:
# atten = 2.99*fn +0.27
# else:
# atten = 2.96
lum = 4. * np.pi * (ldist**2.0) * (3.087**2.0) * (10**(
25.0 + (atten / 2.5))) * f_flux #Luminosity
sfr = 1.08 * (10**(-28.0)) * np.abs(lum)
return sfr
def uvsfr(id, z, fmag, nmag, rmag, f_flux):
fn = fmag - nmag
opt = nmag - rmag # N-r
#Luminosity Distance
dist = WMAP7.comoving_distance(z)
ldist = (1 + z) * dist
#calculating Attenuation 'a'
if opt >= 4.0:
if fn < 0.95:
a = 3.32 * float(fn) + 0.22
else:
a = 3.37
else:
if fn < 0.90:
a = 2.99 * float(fn) + 0.27
else:
a = 2.96
lum = 4 * 3.14159 * (ldist**2.0) * (3.087**2.0) * (10**(
25.0 + (a / 2.5))) * f_flux #Luminosity
sfr = 1.08 * (10**(-28.0)) * abs(lum)
return sfr
def dcomv(z):
return cosmo.comoving_distance(z).value * h #in Mpc/h
def Dc(z):
res = p15.comoving_distance(z).value * p15.h
return res
def __init__(self, snapnum, subhalos, mi, ci, RA_deg, DEC_deg, snapz,
galaxy_camera_posx, galaxy_camera_posy, galaxy_camera_posz,
centerz, galaxy_camera_velx, galaxy_camera_vely,
galaxy_camera_velz, cyl, gmag):
#fields=['SubhaloMass','SubhaloMassInMaxRad','SubhaloMassInRadType','SubhaloMassInMaxRadType','SubhaloPos','SubhaloSFR','SubhaloSFRinRad','SubhaloVel','SubhaloBHMass','SubhaloBHMdot','SubhaloStellarPhotometrics','SubhaloWindMass']
self.snapshot_number = snapnum + np.zeros_like(ci)
self.subhalo_index = subhalos['SubFindID'][mi[ci]]
self.RA_deg = RA_deg
self.DEC_deg = DEC_deg
self.snapz = snapz + np.zeros_like(RA_deg)
self.center_z = centerz + np.zeros_like(RA_deg)
self.cylinder_number = cyl + np.zeros_like(self.subhalo_index)
self.galaxy_comoving_x_mpc = galaxy_camera_posx[ci] / 1000.0
self.galaxy_comoving_y_mpc = galaxy_camera_posy[ci] / 1000.0
self.galaxy_comoving_z_mpc = galaxy_camera_posz[ci] / 1000.0
#self.galaxy_camera_posx = galaxy_camera_posx[ci]/1000.0
#self.galaxy_camera_posy = galaxy_camera_posy[ci]/1000.0
#self.galaxy_camera_posz = galaxy_camera_posz[ci]/1000.0
self.galaxy_camera_velx = galaxy_camera_velx[ci]
self.galaxy_camera_vely = galaxy_camera_vely[ci]
self.galaxy_camera_velz = galaxy_camera_velz[ci]
self.galaxy_peculiar_vr = 1.0 * self.galaxy_camera_velz
self.galaxy_peculiar_z = 1.0 * self.galaxy_peculiar_vr / (
astropy.constants.c.value / 1.0e3)
self.cosmological_redshift = np.zeros_like(self.RA_deg)
for i, index in enumerate(ci):
self.cosmological_redshift[i] = np.float64(
z_at_value(WMAP7.comoving_distance,
self.galaxy_comoving_z_mpc[i] * u.megaparsec,
ztol=1e-12,
maxfun=2000))
self.hubble_velocity = self.cosmological_redshift * astropy.constants.c.value / 1.0e3 #in km/s
self.galaxy_observed_z = 1.0 * self.cosmological_redshift + self.galaxy_peculiar_z
#self.galaxy_comoving_x_mpc = self.galaxy_camera_posx*(1.0 + self.cosmological_redshift)
#self.galaxy_comoving_y_mpc = self.galaxy_camera_posy*(1.0 + self.cosmological_redshift)
#self.galaxy_comoving_z_mpc = self.galaxy_camera_posz*(1.0 + self.cosmological_redshift)
self.galaxy_camera_posx = self.galaxy_comoving_x_mpc / (
1.0 + self.cosmological_redshift)
self.galaxy_camera_posy = self.galaxy_comoving_y_mpc / (
1.0 + self.cosmological_redshift)
self.galaxy_camera_posz = self.galaxy_comoving_z_mpc / (
1.0 + self.cosmological_redshift)
self.angdiam_mpc = np.asarray(
WMAP7.angular_diameter_distance(self.cosmological_redshift))
self.kpc_per_arcsec = np.asarray(
WMAP7.kpc_proper_per_arcmin(self.cosmological_redshift) / 60.0)
self.observed_angdiam_mpc = np.asarray(
WMAP7.angular_diameter_distance(self.galaxy_observed_z))
self.observed_comoving_mpc = np.asarray(
WMAP7.comoving_distance(self.galaxy_observed_z))
self.observed_kpc_per_arcsec = np.asarray(
WMAP7.kpc_proper_per_arcmin(self.galaxy_observed_z) / 60.0)
self.RA_kpc = self.RA_deg * 3600.0 * self.kpc_per_arcsec
self.DEC_kpc = self.DEC_deg * 3600.0 * self.kpc_per_arcsec
self.observed_RA_kpc = self.RA_deg * 3600.0 * self.observed_kpc_per_arcsec
self.observed_DEC_kpc = self.DEC_deg * 3600.0 * self.observed_kpc_per_arcsec
self.mstar_msun = subhalos['SubhaloMassInRadType'][self.subhalo_index,
4] * (1.0e10) / ilh
self.mgas_msun = subhalos['SubhaloMassInRadType'][
self.subhalo_index, 0] * (1.0e10) / ilh #includes wind mass
self.mbh_msun = subhalos['SubhaloMassInRadType'][self.subhalo_index,
5] * (1.0e10) / ilh
self.mhalo_msun = subhalos['SubhaloMass'][self.subhalo_index] * (
1.0e10) / ilh
self.baryonmass_msun = self.mstar_msun + self.mgas_msun + self.mbh_msun #within 2x stellar half mass radius... best?
self.xpos_ckh = subhalos['SubhaloPos'][self.subhalo_index,
0] #in cKpc/h of max bound part
self.ypos_ckh = subhalos['SubhaloPos'][self.subhalo_index, 1]
self.zpos_ckh = subhalos['SubhaloPos'][self.subhalo_index, 2]
self.xpos_pmpc = (self.xpos_ckh * 1.0 / (1.0 + snapz) / ilh) / 1.0e3
self.ypos_pmpc = (self.ypos_ckh * 1.0 / (1.0 + snapz) / ilh) / 1.0e3
self.zpos_pmpc = (self.zpos_ckh * 1.0 / (1.0 + snapz) / ilh) / 1.0e3
self.xvel_kms = subhalos['SubhaloVel'][self.subhalo_index, 0]
self.yvel_kms = subhalos['SubhaloVel'][self.subhalo_index, 1]
self.zvel_kms = subhalos['SubhaloVel'][self.subhalo_index, 2]
self.sfr = subhalos['SubhaloSFRinRad'][self.subhalo_index]
self.bhmdot = subhalos['SubhaloBHMdot'][self.subhalo_index]
self.gmag = subhalos['SubhaloStellarPhotometrics'][self.subhalo_index,
4]
self.rmag = subhalos['SubhaloStellarPhotometrics'][self.subhalo_index,
5]
self.imag = subhalos['SubhaloStellarPhotometrics'][self.subhalo_index,
6]
self.zmag = subhalos['SubhaloStellarPhotometrics'][self.subhalo_index,
7]
self.gmag_apparent = gmag[ci]
#self.total_redshift =
return
def Dc2(z1, z2):
Dcz1 = (p15.comoving_distance(z1).value * p15.h)
Dcz2 = (p15.comoving_distance(z2).value * p15.h)
res = Dcz2 - Dcz1 + 1e-8
return res
def Da2(z1, z2):
# return the proper distance to redshift z in Mpc/h
Dcz1 = (cosmo.comoving_distance(z1).value * cosmo.h)
Dcz2 = (cosmo.comoving_distance(z2).value * cosmo.h)
res = (Dcz2 - Dcz1 + 1e-8) / (1 + z2)
return res
def Da(z):
# return the proper distance to redshift z in Mpc/h
res = cosmo.comoving_distance(z).value * cosmo.h / (1 + z)
return res
def Dc2(z1, z2):
# return the comoving distance between redshifts z1 and z2 in Mpc/h
Dcz1 = (cosmo.comoving_distance(z1).value * cosmo.h)
Dcz2 = (cosmo.comoving_distance(z2).value * cosmo.h)
res = (Dcz2 - Dcz1 + 1e-8)
return res
def Dc(z):
# return the comoving distance to redshift z in Mpc/h
res = cosmo.comoving_distance(z).value * cosmo.h
return res
def getcoords(a,d,z):
comdis = WMAP7.comoving_distance(z)
i = (comdis)*(math.cos(math.radians(d)))*(math.cos(math.radians(a)))
j = (comdis)*(math.cos(math.radians(d)))*(math.sin(math.radians(a)))
k = (comdis)*(math.sin(math.radians(d)))
return(i,j,k,z)
def Dc(z):
res = p15.comoving_distance(z).value*p15.h
return res
"""Dc(z) returns comoving distance at a particular redshift z"""
"""Parameters
# Planck13.comoving_distance(ar_z)) # # plt.plot(ar_z, Planck13.comoving_distance(ar_z) / Planck13.comoving_distance(ar_z)) # plt.plot(ar_z, Planck13.comoving_distance(ar_z + ar_delta_z_planck13 - ar_delta_z_wmap7) / # Planck13.comoving_distance(ar_z)) # plt.show() # print(scipy.misc.derivative(func=Planck13.comoving_distance, x0=2, dx=0.1)) # ar_dcmv_dz_planck13 = np.array([scipy.misc.derivative( # func=lambda x: Planck13.comoving_distance(x).value, x0=z, dx=0.01) for z in ar_z]) # ar_dcmv_dz_wmap7 = np.array([scipy.misc.derivative( # func=lambda x: WMAP7.comoving_distance(x).value, x0=z, dx=0.01) for z in ar_z]) # plt.plot(ar_z, -(ar_dcmv_dz_planck13 - ar_dcmv_dz_wmap7) * ar_delta_z_planck13) # plt.show() del scipy.misc ar_base_cmvd_planck13 = Planck13.comoving_distance(ar_z) ar_true_planck13_cmvd = Planck13.comoving_distance(ar_z + ar_delta_z_planck13) ar_base_cmvd_wmap5 = WMAP5.comoving_distance(ar_z) ar_wmap5_apparent_cmvd = WMAP5.comoving_distance(ar_z + ar_delta_z_planck13) ar_base_cmvd_wmap7 = WMAP7.comoving_distance(ar_z) ar_wmap7_apparent_cmvd = WMAP7.comoving_distance(ar_z + ar_delta_z_planck13) ar_base_cmvd_wmap9 = WMAP9.comoving_distance(ar_z) ar_wmap9_apparent_cmvd = WMAP9.comoving_distance(ar_z + ar_delta_z_planck13) plt.plot(ar_z, ar_true_planck13_cmvd - ar_base_cmvd_planck13) plt.plot(ar_z, ar_wmap5_apparent_cmvd - ar_base_cmvd_wmap5) plt.plot(ar_z, ar_wmap7_apparent_cmvd - ar_base_cmvd_wmap7) plt.plot(ar_z, ar_wmap9_apparent_cmvd - ar_base_cmvd_wmap9) # plt.plot(ar_z, ar_wmap7_apparent_cmvd - ar_true_planck13_cmvd) plt.show()
