Dark matter distribution

These pictures show the large scale dark matter distribution and a selection of dark matter halos from our simulations.
The brightness of colors indicates the density, if not stated otherwise.
Copyright: S. Gottlöber, G. Yepes, A. Klypin, A. Khalatyan

	All-sky map of the gamma-ray flux from dark matter decay in Cartesian projection using galactic coordinates. This flux is assumed to be proportional to the dark matter density in the constrained cosmological simulation Box 160. Known observed large structures reproduced by this simulation such as Virgo, Coma, and Perseus clusters, together with the Great Attractor, are labeled in this plot. (A.J. Vazquez, F. Prada, F. Zandanel; Image generated with HEALPix, see K.M. Gorski et al., 2005 for details) with labels [png, 1389x694, 812 KB] no labels [png, 1389x694, 738 KB] eps-figure [eps, 997 KB]
	Another all-sky map, this time of the gamma-ray flux from dark matter annihilation. The flux is assumed to be proportional to the dark matter density squared in the constrained cosmological simulation Box 160. Again labels show the known observed large scale structured of the Local Universe. (A.J. Vazquez, F. Prada, F. Zandanel; Image generated with HEALPix, see K.M. Gorski et al., 2005, for details) with labels [png, 1389x694, 827 KB] no labels [png, 1389x694, 748 KB] eps-figure [eps, 997 KB]
	Large scale dark matter density distribution of the Local Universe (Box 160). The image shows a slice through the center of the box and its boundary is periodically wrapped to get a side length of 180 Mpc/h. Also see Anatoly Klypin - Box 160. [jpg, 740x673, 430 KB]
	Large scale dark matter density distribution of the Local Universe simulation (Box 160). The image covers the full box range of 160 Mpc/h. Several objects of the real universe are identified: the circle shows the position of our Local Group, a blown up panel shows the detailed structure of the simulated Local Group. The resolution of this small region of 2 Mpc/h radius is equivalent to having a total of 4096^3 (70 billion) particles in the whole box, which translates in a dynamical range of more than 106. [jpg, 820x873, 533 KB]
	Dark matter distribution in the 64 Mpc/h box (Box 64-186592). with labels [png, 800x800, 708 KB] medium [png, 800x800, 694 KB] large [png, 1024x1024, 1.1 MB] huge [png, 8000x8000, 28 MB]
	A combination of two slices from two different CLUES simulations within a WMAP 3 cosmology: Box 160 and Box 64-186592 (inset panel). The Local Supercluster (LSC) forms in both simulations and matches pretty well, despite the fact that the realizations were different. LSC = Local Supercluster GA = Great Attractor PP = Perseus-Pisces-Cluster [png, 800x800, 543 KB]
	Andromeda Galaxy (centre), Milky Way and Triangulum Galaxy in the high resolution region (2 Mpc/h) of Box 64-186592 plus some additional information. [jpg, 1000x745, 105 KB]
	Andromeda Galaxy (centre), the Milky Way and Triangulum Galaxy in the high resolution region (2 Mpc/h). [jpg, 981x922, 445 KB]
	Andromeda Galaxy [jpg, 978x710, 260 KB]
	Milky Way [jpg, 978x710, 265 KB]
	Triangulum galaxy (M33) [jpg, 978x710, 209 KB]
	Comparison of the three main halos in the Cold and Warm Dark Matter simulation. (also see Movies) [jpg, 640x480, 36 KB]
	Projection of the three main halos (MW, M31, M33) along the z-direction (Box 64-186592). The presented image has a size of 1.3 Mpc/h per side. [png, 1574x1154, 503 KB] Versions with gas and star distribution are available at: gas [png, 1574x1154, 357 KB] stars [png, 1574x1154, 22 KB]