Halos

12 to 15 million halos (with more than 100 particles) were detected on the light-cones with a Friends-of-Friends algorithm (with a linking-length b given in the table). The resulting relativistic catalogs (produced through ray-tracing) are provided here. The format is explained below.

	FoF b=0.2 ASCII angle/red/WL
Narrow 2500 deg2 LCDM	link (12M)
Narrow 2500 deg2 wCDM	link (13M)
Fullsky 41253 deg2 LCDM	link (13M)
Fullsky 41253 deg2 wCDM	link (15M)

Remark: The deeper (z < 10) light-cone is available upon demand to Michel-Andrès Breton (breton at ice.csic.es). Beyond z > 3 one has to take extra care of finite resolution effects at scales of order few coarse cells.

Particle subsample

Subsamples of about 200 million particles, 400 million particles and 1.4 billion particles were ray-traced. The resulting relativistic catalogs are provided here (the format is explained below).

Narrow lightcone 2500 deg2 z<2.0 LCDM 400M particles (fits)

Narrow lightcone 2500 deg2 z<2.0 wCDM 400M particles (fits)

———————————————————————-

Fullsky lightcone 41253 deg2 z<0.5 LCDM 1400M particles (fits)

Fullsky lightcone 41253 deg2 z<0.5 LCDM 200M particles (light fits)

Fullsky lightcone 41253 deg2 z<0.5 wCDM 1400M particles (fits)

Fullsky lightcone 41253 deg2 z<0.5 wCDM 200M particles (light fits)

FILE CONTENT AND FORMAT

The catalogs are displayed as ASCII files for halo or FITS file for particles, the different columns refers to :

id β₁ β₂ θ₁ θ₂ error₁ error₂ z₀ z₁ z₂ z₃ z₄ z₅ a₁₁ a₁₂ a₂₁ a₂₂ n_part

id= pFoF id of the halo 
β_i = undeflected angles (ie without lensing) in radian
θ_i= apparent angles (ie with lensing) in radian

The angles are defined as in spherical coordinates. The normalized comoving coordinates are recovered as :
x = cos(β₁)*sin(β₂)
y = sin(β₁)*sin(β₂)
z = cos(β₂)
The same formula can be used (replacing β_i by θ_i) to convert apparent angles into apparent normalized coordinates.

The (perturbed) redshifts z_i are defined as follows:

1+z₀ = a₀/a
1+z₁ = a₀/a [ 1 – (φ-φ₀)/c² ]
1+z₂ = a₀/a [ 1 – (φ-φ₀)/c² +v·n/c ]
1+z₃ = a₀/a [ 1 – (φ-phi0)/c² +v.n/c +0.5*|v.v|/c² ]
1+z₄ = a₀/a [ 1 – (φ-φ₀)/c² +v·n/c +0.5*|v·v|/c² – 2 int(∂φ∂η dη)/c² ]
z₅ = exact redshift computation from GR definition (in principle the resulting redshift should be very close to z₄)

a is the expansion factor, φ is the potential, c is the square of the speed of light, v is the peculiar velocity of the source, n the direction of observation and ∂φ∂η the derivative of the potential with respect to the conformal time η. The subscript 0 indicates quantities evaluated at the observer location, while those without subscript indicates quantities evaluated at the source location. The observer is assumed to have no velocity in the adopted system of coordinates.

a_ij are the components of the distortion matrix a_ij=dβ_i/dθ_j, to be read as :

     a₁₁       a₁₂
     a₂₁       a₂₂

n_part is the number of particles in the halo.

How to read the file?

ASCII files are straightforward to read. For instance in Python

import numpy as np
data=np.loadtxt(filename)

Light fits files are straightforward to read. For instance in Python:

from astropy.io import fits
hdulist = fits.open(filename)
data = hdulist[0].data # This gives the same array as for ASCII files

Standard fits can be read column by column. For instance in Python:

from astropy.io import fits
hdulist = fits.open(filename)
c1 = hdulist[1].data['COLUMN_NAME_1']
c2 = hdulist[1].data['COLUMN_NAME_2']

where COLUMN_NAME_I can be id,beta1,beta2,theta1,theta2,error,iteration,z0,z1,z2,z3,z4,z5,a11,a12,a21,a22,npart

Go back to relativistic catalogs and lightcone data page