def H0_to_theta(hubble, omega_nu, omnuh2, omega_m, ommh2, omega_c, omch2,
omega_b, ombh2, omega_lambda, omlamh2):
h = hubble / 100.
if np.isnan(omnuh2):
omnuh2 = omega_nu * h**2
if np.isnan(omega_m):
omega_m = ommh2 / h**2
if np.isnan(omega_b):
omega_b = ombh2 / h**2
if np.isnan(omega_lambda):
omega_lambda = omlamh2 / h**2
if np.isnan(omega_c):
omega_c = omch2 / h**2
if np.isnan(omega_m):
omega_m = omega_c + omega_b + omega_nu
if np.isnan(omega_m):
omega_m = (omch2 + ombh2 + omnuh2) / h**2
if np.isnan([omnuh2, hubble, omega_m, omega_lambda, omega_b]).any():
return np.nan
m_nu = 93.14 * omnuh2 * units.eV
cosmo = LambdaCDM(hubble,
omega_m,
omega_lambda,
m_nu=m_nu / 3,
Ob0=omega_b,
Tcmb0=2.7255,
Neff=3.046)
ombh2 = cosmo.Ob0 * cosmo.h**2
omdmh2 = cosmo.Om0 * cosmo.h**2
zstar = 1048 * (1 + 0.00124 * ombh2**(-0.738)) * (
1 + (0.0783 * ombh2**(-0.238) / (1 + 39.5 * ombh2**0.763)) *
(omdmh2 + ombh2)**(0.560 / (1 + 21.1 * ombh2**1.81)))
astar = 1 / (1 + zstar)
rs = scipy.integrate.romberg(dsound_da,
1e-8,
astar,
rtol=5e-5,
args=(cosmo, ),
divmax=10) # in Mpc
DA = cosmo.angular_diameter_distance(zstar).to("Mpc").value / astar
return rs / DA
def partial_profile(RA0,DEC0,Z,angles,
RIN,ROUT,ndots,h,roff,phi_off):
ndots = int(ndots)
cosmo = LambdaCDM(H0=100*h, Om0=0.25, Ode0=0.75)
dl = cosmo.angular_diameter_distance(Z).value
KPCSCALE = dl*(((1.0/3600.0)*np.pi)/180.0)*1000.0
delta = ROUT/(3600*KPCSCALE)
t0 = time.time()
mask = (S.ra < (RA0+delta))&(S.ra > (RA0-delta))&(S.dec > (DEC0-delta))&(S.dec < (DEC0+delta))&(S.z_v > (Z+0.1))
t1 = time.time()
# print(t1-t0)
catdata = S[mask]
ds = cosmo.angular_diameter_distance(catdata.z_v).value
dls = cosmo.angular_diameter_distance_z1z2(Z, catdata.z_v).value
BETA_array = dls/ds
Dl = dl*1.e6*pc
sigma_c = (((cvel**2.0)/(4.0*np.pi*G*Dl))*(1./BETA_array))*(pc**2/Msun)
t2 = time.time()
# print(RA0,DEC0,t2-t1)
rads, theta, test1,test2 = eq2p2(np.deg2rad(catdata.ra),
np.deg2rad(catdata.dec),
np.deg2rad(RA0),
np.deg2rad(DEC0))
theta2 = (2.*np.pi - theta) +np.pi/2.
theta_ra = theta2
theta_ra[theta2 > 2.*np.pi] = theta2[theta2 > 2.*np.pi] - 2.*np.pi
e1 = catdata.gamma1
e2 = -1.*catdata.gamma2
#get tangential ellipticities
et = (-e1*np.cos(2*theta)-e2*np.sin(2*theta))*sigma_c
#get cross ellipticities
ex = (-e1*np.sin(2*theta)+e2*np.cos(2*theta))*sigma_c
# '''
k = catdata.kappa*sigma_c
del(e1)
del(e2)
r = np.rad2deg(rads)*3600*KPCSCALE
r = np.sqrt(roff**2 + r**2 + 2.*roff*r*np.cos(phi_off))
del(rads)
Ntot = len(catdata)
del(catdata)
bines = np.round(np.logspace(np.log10(RIN),np.log10(ROUT),num=ndots+1),0)
dig = np.digitize(r,bines)
t = np.tile(theta_ra,(3,1)).T
an = np.tile(angles,(len(theta_ra),1))
at = t - an
SIGMAwsum = []
DSIGMAwsum_T = []
DSIGMAwsum_X = []
N_inbin = []
GAMMATcos_wsum = np.zeros((ndots,3))
GAMMAXsin_wsum = np.zeros((ndots,3))
COS2_2theta = np.zeros((ndots,3))
SIN2_2theta = np.zeros((ndots,3))
for nbin in range(ndots):
mbin = dig == nbin+1
SIGMAwsum = np.append(SIGMAwsum,k[mbin].sum())
DSIGMAwsum_T = np.append(DSIGMAwsum_T,et[mbin].sum())
DSIGMAwsum_X = np.append(DSIGMAwsum_X,ex[mbin].sum())
GAMMATcos_wsum[nbin,:] = np.sum((np.tile(et[mbin],(3,1))*np.cos(2.*at[mbin]).T),axis=1)
GAMMAXsin_wsum[nbin,:] = np.sum((np.tile(ex[mbin],(3,1))*np.sin(2.*at[mbin]).T),axis=1)
COS2_2theta[nbin,:] = np.sum((np.cos(2.*at[mbin]).T)**2,axis=1)
SIN2_2theta[nbin,:] = np.sum((np.sin(2.*at[mbin]).T)**2,axis=1)
N_inbin = np.append(N_inbin,len(et[mbin]))
index = np.arange(mbin.sum())
output = {'SIGMAwsum':SIGMAwsum,'DSIGMAwsum_T':DSIGMAwsum_T,
'DSIGMAwsum_X':DSIGMAwsum_X,
'GAMMATcos_wsum': GAMMATcos_wsum, 'GAMMAXsin_wsum': GAMMAXsin_wsum,
'COS2_2theta_wsum':COS2_2theta,'SIN2_2theta_wsum':SIN2_2theta,
'N_inbin':N_inbin,'Ntot':Ntot}
return output
ra, dec = wcs.all_pix2world(x, y, 1)
dra, ddec = ra-centre[0], dec-centre[1]
dra *= 3600.
ddec *= 3600.
dist = ang_sep(centre[0],centre[1],ra,dec).T*3600
mask = dist < radius
return mass[mask].sum(),std[mask].sum(),np.median(sn[mask])
folder = '../main/grid1.0/'
z = 0.397
dl = cosmo.angular_diameter_distance(z).value # in kpc
kpcscale = dl*np.deg2rad(1.0/3600.0)*1000.0
r_100 = 100./kpcscale
r_200 = 200./kpcscale
S1c = [64.011542, -24.093647]
S2c = [64.016187, -24.075967]
S3c = [64.031547, -24.048917]
S4c = [64.061442, -24.053878]
S1p = [64.134196, -24.088425]
S1c_mass200 = []
S2c_mass200 = []
S3c_mass200 = []
S4c_mass200 = []
from astropy.cosmology import LambdaCDM
import numpy as np
d = open('./c_shape').readlines()
temp = open('./sqlcl.in').readlines()
cos = LambdaCDM(H0=73, Om0=0.27, Ode0=0.73)
ra = []
dec = []
z = []
#print( d )
for i in d:
t = i[:-1].split()
ra.append(float(t[0]))
dec.append(float(t[1]))
z.append(float(t[-3]))
cl = 'dbo.fGetNearbyObjEq(%f, %f, %f) AS GN\n'
R = 5.0
for i in range(len(ra)):
f = open('./sql/sql_%i' % (i), 'w')
r = R / cos.angular_diameter_distance(z[i]).value / np.pi * 180 * 60
for j in temp:
if (j[0:3] == 'dbo'):
f.write(cl % (ra[i], dec[i], r))
else:
f.write(j)
f.close()
#break
