Risa Wechsler - Astronomy and Astrophysics
Risa Wechsler - Astronomy and Astrophysics
Risa Wechsler - Astronomy and Astrophysics
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M 200<br />
Lensing Mass<br />
Cluster Size<br />
10 14<br />
10 13<br />
10 12<br />
r 200 [h !1 Mpc]<br />
S<br />
M200 = A Ngal A= 2.1±0.4 ×10 11<br />
S= 1.56±0.07<br />
χ 2 = 11.1 DOF=10<br />
Sigma diff<br />
1000<br />
Real Data<br />
Sheldon et al 2005 (in prep) McKay et al 2005 (in prep)<br />
100<br />
1 10 100<br />
<br />
2.0<br />
1.0<br />
0.9<br />
0.8<br />
0.7<br />
0.6<br />
0.5<br />
Hansen et al 2005,<br />
ApJ in press<br />
0.4<br />
6 8 10 20 40 60 80 100<br />
N gals<br />
Velocity Dispersion<br />
1 10 100 1000<br />
N gals<br />
Now we know what the x-axis is.<br />
Since we have realistic clusters, we can now<br />
measure each of the y-axes for these plots in<br />
the same way in the models as they are<br />
measured in the data.<br />
Combining these constraints with the cluster<br />
abundance will provide powerful constraints on<br />
both cosmology <strong>and</strong> the true halo occupation.<br />
This extremely rich data set requires<br />
realistic simulations to make the most of it!
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