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|
|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.
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).
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 npart
id= pFoF id of the halo
βi = undeflected angles (ie without lensing) in radian
θi= 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 βi by θi) to convert apparent angles into apparent normalized coordinates.
The (perturbed) redshifts zi are defined as follows:
z0 = a0/a
z1 = a0/a [ 1 – (φ-φ0)/c2 ]
z2 = a0/a [ 1 – (φ-φ0)/c2 +v·n/c ]
z3 = a0/a [ 1 – (φ-phi0)/c2 +v.n/c +0.5*|v.v|/c2 ]
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.
aij are the components of the distortion matrix aij=dβi/dθj, to be read as :
npart 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.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.data['COLUMN_NAME_1'] c2 = hdulist.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