Introduction to Cosmology

Virially Bound Systems 201 in stars, the halo mass and the length scale. A frequently used radial density profile parametrizatio ...

202 Dark Matter emission. One may assume that the electron density distribution associated with the X-ray brightness is in hydro ...

Galaxies 203 Most of the dark matter in the Universe, or about two thirds of it, is not associ- ated with groups and clusters o ...

204 Dark Matter dynamics may easily be modified by such fields [6]. But this argument works only on the gas halo, and does not a ...

Galaxies 205 <MI> = –18.5 <MI> = –20.5 .5 0 V(R)/V(R )apt V(R)/V(R apt ) V(R)/V(R )apt V(R)/V(R apt ) 0 .5 1 1.5 2 1 ...

206 Dark Matter is in some tension with the Virial Theorem, perhaps due to variations in the central dispersions,휎 0 , of the st ...

Galaxies 207 Ultra-compact dwarf galaxies (UCDs) are stellar systems with masses of around 107 –10^8 Msunand half-mass radii of ...

208 Dark Matter The very general question arises whether the galaxies could at all have formed from primordial density fluctuati ...

Clusters 209 and the matter overdensity are related. Mass profile estimation is thus possible once the infall pattern of galaxie ...

210 Dark Matter 20 10 0 10 20 20 20 – 10 01020 – 20 – 10 01020 10 20 10 0 π/ h 1 Mpc σ/h–^1 Mpc σ/h–^1 Mpc π/ h 1 Mpc Fi ...

Merging Galaxy Clusters 211 9.4 Merging Galaxy Clusters In isolated galaxies and galaxy clusters all matter components contribut ...

212 Dark Matter The Baby Bullet. Another merging system with similar characteristics but with lower spatial resolution is the po ...

Dark Matter Candidates 213 Another major cluster merger is DLSCL J0916.2+2951 [17] at푧=0.53, in which the collisional cluster ga ...

214 Dark Matter The shocking conclusion is that the predominant form of matter in the Universe is nonbaryonic, and we do not eve ...

Dark Matter Candidates 215 level of particle physics. At the cosmological level there are two new parameters, the ratio푥of the t ...

216 Dark Matter interactions, in which case they froze out early when their interaction rate became smaller than the expansion r ...

Dark Matter Candidates 217 0 1 2 3 4 log(a) a^0 DM baryons log(δp/p) aeq = 3 10–5adec = 10 –3 Figure 9.3Time-dependence of the ...

218 Dark Matter An intermediate category is constituted by possible sterile neutrinos and by the gravitino, which is a SUSY part ...

The Cold Dark Matter Paradigm 219 15 h 18 h h 21 h^0 h^3 12 h (^9) h (^6) h 0.5 1 1.5 2 Lookback time (billions of years) 2.5 2. ...

220 Dark Matter blue galaxies at 1⩽푧⩽ 3 .5, which obviously are very young. There is also evidence that the galaxy merger rate w ...