def __init__(self, z=0.3, m200=1e13, c200=5., gammadm=1., mstar=1e11, reff=5., ra=0., dec=0., sources=None, \
cosmo=wl_cosmology.default_cosmo):
self.z = z
self.cosmo = cosmo
self.m200 = m200 # halo mass in M_Sun units
self.mstar = mstar # central point mass in M_Sun units
self.rhocrit = wl_cosmology.rhoc(self.z, cosmo=self.cosmo)
self.r200 = (self.m200 * 3. / 200. / (4. * pi) / self.rhocrit)**(
1 / 3.) #r200 in Mpc
self.c200 = c200
self.rs = self.r200 / self.c200
self.reff = reff # effective radius in kpc
self.gammadm = gammadm
self.angD = wl_cosmology.Dang(self.z, cosmo=self.cosmo)
self.Mpc2deg = np.rad2deg(1. / self.angD)
self.rs_ang = self.rs * self.Mpc2deg
self.reff_ang = self.reff * self.Mpc2deg / 1000.
self.halo_norm = self.m200 / gnfw.fast_M3d(self.r200, self.rs,
self.gammadm)
self.S_bulge = self.mstar / self.reff**2 * 1e6
self.sources = sources
if ra is not None:
self.ra = ra
if dec is not None:
self.dec = dec
def __init__(self, z=0.3, m200=1e13, c200=5., mstar=1e11, reff=5., ra=0., dec=0., sources=None, \
cosmo=wl_cosmology.default_cosmo):
self.z = z
self.cosmo = cosmo
self.m200 = m200 # halo mass in M_Sun units
self.mstar = mstar # stellar mass in M_Sun units
self.rhocrit = wl_cosmology.rhoc(self.z, cosmo=self.cosmo)
self.r200 = (self.m200*3./200./(4.*pi)/self.rhocrit)**(1/3.) #r200 in Mpc
self.c200 = c200
self.rs = self.r200/self.c200
self.reff = reff # effective radius in kpc
self.angD = wl_cosmology.Dang(self.z, cosmo=self.cosmo)
self.Mpc2deg = np.rad2deg(1./self.angD)
self.rs_ang = self.rs*self.Mpc2deg
self.reff_ang = self.reff*self.Mpc2deg/1000.
self.S_s = self.m200/(np.log(1. + self.c200) - self.c200/(1. + self.c200))/(4.*pi*self.rs**2)
self.S_bulge = self.mstar/self.reff**2*1e6
self.sources = sources
if ra is not None:
self.ra = ra
if dec is not None:
self.dec = dec
def __init__(self, z=0.3, m200=1e13, c200=5., mstar=1e11, reff=5., nser=4., nu=0., ra=0., dec=0., sources=None, \
cosmo=wl_cosmology.default_cosmo):
import adcontr
self.z = z
self.cosmo = cosmo
self.m200 = m200 # halo mass in M_Sun units
self.mstar = mstar # stellar mass in M_Sun units
self.fbar = self.mstar / (self.mstar + self.m200)
self.rhocrit = wl_cosmology.rhoc(self.z, cosmo=self.cosmo)
self.r200 = (self.m200 * 3. / 200. / (4. * pi) / self.rhocrit)**(
1 / 3.) #r200 in Mpc
self.c200 = c200
self.rs = self.r200 / self.c200
self.reff = reff # effective radius in kpc
self.nser = nser # Sersic index
self.nu = nu # adiabatic contraction efficiency parameter
self.angD = wl_cosmology.Dang(self.z, cosmo=self.cosmo)
self.Mpc2deg = np.rad2deg(1. / self.angD)
self.rs_ang = self.rs * self.Mpc2deg
self.reff_ang = self.reff * self.Mpc2deg / 1000.
self.S_h = self.m200 / self.rs**2
self.S_bulge = self.mstar / self.reff**2 * 1e6
self.sources = sources
if ra is not None:
self.ra = ra
if dec is not None:
self.dec = dec
def __init__(self, z=0.3, m200=1e13, c200=5., mstar=1e11, ra=0., dec=0., sources=None, \
cosmo=wl_cosmology.default_cosmo):
self.z = z
self.cosmo = cosmo
self.m200 = m200 # halo mass in M_Sun units
self.mstar = mstar # central point mass in M_Sun units
self.rhocrit = wl_cosmology.rhoc(self.z, cosmo=self.cosmo)
self.r200 = (self.m200*3./200./(4.*pi)/self.rhocrit)**(1/3.) #r200 in Mpc
self.c200 = c200
self.rs = self.r200/self.c200
self.angD = wl_cosmology.Dang(self.z, cosmo=self.cosmo)
self.Mpc2deg = np.rad2deg(1./self.angD)
self.rs_ang = self.rs*self.Mpc2deg
self.S_s = self.m200/(np.log(1. + self.c200) - self.c200/(1. + self.c200))/(4.*pi*self.rs**2)
self.sources = sources
if ra is not None:
self.ra = ra
if dec is not None:
self.dec = dec
def __init__(self, z=0.3, m200=1e13, c200=5., alpha=1., mstar=1e11, ra=0., dec=0., sources=None, \
cosmo=wl_cosmology.default_cosmo):
self.z = z
self.cosmo = cosmo
self.m200 = m200 # halo mass in M_Sun units
self.mstar = mstar # central point mass in M_Sun units
self.rhocrit = wl_cosmology.rhoc(self.z, cosmo=self.cosmo)
self.r200 = (self.m200*3./200./(4.*pi)/self.rhocrit)**(1/3.) #r200 in Mpc
self.c200 = c200
self.r2 = self.r200/self.c200
self.alpha = alpha
self.angD = wl_cosmology.Dang(self.z, cosmo=self.cosmo)
self.Mpc2deg = np.rad2deg(1./self.angD)
self.r2_ang = self.r2*self.Mpc2deg
self.halo_norm = self.m200/einasto.M3d(self.r200, self.r2, self.alpha)
self.sources = sources
if ra is not None:
self.ra = ra
if dec is not None:
self.dec = dec
for line in lines[1:]:
line = line.split()
name = line[0]
zd = float(line[1])
zs_here = float(line[2])
zs.append(zs_here)
tein_here = float(line[3])
tein_obs.append(tein_here)
tein_err.append(0.1 * tein_here)
lmchab_obs.append(float(line[6]))
lmchab_err.append(float(line[7]))
dd = wl_cosmology.Dang(zd)
ds = wl_cosmology.Dang(zs_here)
dds = wl_cosmology.Dang(zs_here, zd)
arcsec2kpc = np.deg2rad(1. / 3600.) * dd * 1000.
rhoc.append(wl_cosmology.rhoc(zd))
rein_phys_here = tein_here * arcsec2kpc
rein_phys.append(rein_phys_here)
s_cr = c**2 / (4. * np.pi * G) * ds / dds / dd / Mpc / M_Sun * kpc**2
mein_here = np.pi * rein_phys_here**2 * s_cr
reff1 = float(line[4])
nser1 = float(line[5])
def S_cr(self, z):
Ds = wl_cosmology.Dang(z, cosmo=self.cosmo)
Dds = wl_cosmology.Dang(z, self.z, cosmo=self.cosmo)
return c**2/(4.*pi*G)*Ds/Dds/self.angD*Mpc/M_Sun
from scipy.interpolate import splrep, splev
from astropy.io import fits as pyfits
calib_dir = '/Users/sonnen/hsc_weaklensing/hsc-unblinded-Aug2017/'
# reads in the shear calibration info
calib_file = h5py.File(calib_dir + 'hsc_16a_mandelbaum_shear.hdf5', 'r')
rmax = 0.5 # maximum radius for the WL analysis, in Mpc (physical)
rmin = 0.03 # minimum radius for the WL analysis, in Mpc (physical)
nz = 1001
zd_grid = np.linspace(0.01, 1., nz)
dd_grid = 0. * zd_grid
for i in range(nz):
dd_grid[i] = wl_cosmology.Dang(zd_grid[i])
dd_spline = splrep(zd_grid, dd_grid)
# reads in the shape measurement and photo-z table
wl_table = h5py.File(
'/gdrive/projects/hsc_weaklensing/HSC_S16A_2.0_minimal.hdf5', 'r')
# reads in the lens sample catalog
f = open('sdss_legacy_hscoverlap_mcut11.0.cat', 'r')
ra, dec, zd, mstar, mstar_err = np.loadtxt(f,
usecols=(0, 1, 2, 3, 4),
unpack=True)
f.close()
ngal = len(ra)
# defines the stellar profile
ein_frac = sersic.M2d(rein, nser, reff)
def bulge_M2d(R):
return sersic.M2d(R, nser, reff * arcsec2kpc)
def bulge_Sigma(R):
return sersic.Sigma(R, nser, reff * arcsec2kpc)
lmchab_obs = float(line[6])
lmchab_err = float(line[7])
dd = wl_cosmology.Dang(zd)
ds = wl_cosmology.Dang(zs)
dds = wl_cosmology.Dang(zs, zd)
rhoc = wl_cosmology.rhoc(
zd) # critical density of the Universe in M_Sun/Mpc**3
s_cr = c**2 / (
4. * np.pi * G
) * ds / dds / dd / Mpc / M_Sun * kpc**2 # critical surface mass density in M_Sun/kpc**2
arcsec2kpc = arcsec2rad * dd * 1000.
rein_phys = rein * arcsec2kpc # Einstein radius in kpc
nm200 = 30
nmstar = 30
def S_cr(self, z): # critical surface mass density in M_Sun/Mpc^2
Ds = wl_cosmology.Dang(z, cosmo=self.cosmo)
Dds = wl_cosmology.Dang(z, self.z, cosmo=self.cosmo)
return c**2 / (4. * pi * G) * Ds / Dds / self.angD * Mpc / M_Sun
lnser_samp = nser_mu + nser_beta * (lmchab_samp - mchab_piv)
lreff_samp = reff_mu + reff_nu * (lnser_samp - np.log10(4.)) + reff_beta * (
lmchab_samp - mchab_piv)
# prepares arrays to store values of theta_ein and the lensing cross-section for each point of the sample
tein_samp = np.zeros(nsamp)
crosssect_samp = np.zeros(nsamp)
for i in range(nsamp): # loops over the sample
if zs_samp[i] < zd_samp[i] + 0.01:
# source is in front of the lens
tein_samp[i] = 0.
crosssect_samp[i] = 0.
else:
dd = wl_cosmology.Dang(zd_samp[i])
rhoc = wl_cosmology.rhoc(
zd_samp[i]) # critical density of the Universe in M_Sun/Mpc**3
arcsec2kpc = arcsec2rad * dd * 1000.
ds = wl_cosmology.Dang(zs_samp[i])
dds = wl_cosmology.Dang(zs_samp[i], zd_samp[i])
s_cr = c**2 / (
4. * np.pi * G
) * ds / dds / dd / Mpc / M_Sun * kpc**2 # critical surface mass density, in M_Sun/kpc**2
r200 = (10.**lm200_samp[i] * 3. / 200. /
(4. * np.pi) / rhoc)**(1. / 3.) * 1000.
c200 = 10.**lc200_samp[i]
