 |
Figure 1:
Left panel:
in units of the background density,
 ,
we show the 3D density profile for the halo (black), for the caustics in a
perfectly cold medium (red) and for the caustics smoothed out by a
warm/hot dark matter with velocity dispersion
(green). Red spikes are all singular with infinite density and
limited here to finite values because of finite resolution.
Right panel: the same colour-coding for the projected 2D
density profiles in units of
 .
When projected,
caustic peaks are smoother and look like a flight of stairs.
Therefore, we expect low lensing magnifications close to
the caustics (see Sect. 3).
|
| Open with DEXTER | |
In the text
 |
Figure 2:
contribution of caustics for two
values of  :
cold medium 
(black curve) and warm medium
 km s-1 (red curve). The green (resp. blue) "binned''
curve is the noise level for one (resp. 100 stacked) halo(es). |
| Open with DEXTER | |
In the text
 |
Figure 3:
Difference between the
contribution
of cold caustics and the smooth component. We illustrate the blurring
effect of an imperfect knowledge of the turnaround radius of stacked
haloes. The solid black line, dashed green line and dot-dashed
blue line correspond to zero, 3% and 10% uncertainties, respectively.
As in Fig. 2, the binned curve represents
the noise level achieved with 600 stacked haloes. The convolution effect
of error in the assumed/measured value of
is important and a
significant detection of caustics requires well-determined turnaround
radii (
a few percent relative accuracy). The very small scale
oscillations in the plot are numerical artifacts and ideally the only
sawtooth patterns are those due to caustics. |
| Open with DEXTER | |
In the text