{"id":87,"date":"2015-07-27T12:49:34","date_gmt":"2015-07-27T12:49:34","guid":{"rendered":"https:\/\/www.clues-project.org\/cms\/?page_id=87"},"modified":"2020-10-28T20:07:24","modified_gmt":"2020-10-28T20:07:24","slug":"dark-matter","status":"publish","type":"page","link":"https:\/\/www.clues-project.org\/cms\/images-and-movies\/dark-matter\/","title":{"rendered":"Dark Matter"},"content":{"rendered":"

<\/a><\/p>\n

Images<\/h3>\n

These pictures show the large scale dark matter distribution and a selection of dark matter halos from our simulations.
\nThe brightness of colors indicates the density, if not stated otherwise.
\nCopyright [if not stated otherwise]: S. Gottl\u00f6ber, G. Yepes, A. Klypin, A. Khalatyan<\/em><\/p>\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n
\"\"<\/a><\/td>\nAll-sky map of the gamma-ray flux from dark matter decay<\/em> in Cartesian
\nprojection using galactic coordinates. This flux is assumed to be proportional to the dark matter density in the constrained cosmological simulation Box 160<\/a>.
\nKnown observed large structures reproduced by this simulation such as Virgo, Coma, and Perseus clusters, together with the Great Attractor, are labeled in this plot.
\n(A.J. Vazquez, F. Prada, F. Zandanel; Image generated with HEALPix<\/a>, see K.M. Gorski et al., 2005<\/a> for details)<\/em><\/p>\n

with labels\u00a0 [png, 1389×694, 812 KB]<\/a>
\nno labels\u00a0\u00a0\u00a0 [png, 1389×694, 738 KB]<\/a>
\neps-figure\u00a0 [eps, 997 KB]<\/a><\/td>\n<\/tr>\n

\"Box160AllSkyDMAnnihil\"<\/a><\/td>\nAnother all-sky map, this time of the gamma-ray flux from dark matter annihilation<\/em>. The flux is assumed to be proportional to the dark matter density squared<\/em> in the constrained cosmological simulation Box 160<\/a>.
\nAgain labels show the known observed large scale structured of the Local Universe.
\n(A.J. Vazquez, F. Prada, F. Zandanel; Image generated with HEALPix<\/a>, see K.M. Gorski et al., 2005<\/a>, for details)<\/em><\/p>\n

with labels\u00a0 [png, 1389×694, 827 KB]<\/a>
\nno labels\u00a0\u00a0\u00a0 [png, 1389×694, 748 KB]<\/a>
\neps-figure\u00a0 [eps, 997 KB]<\/a><\/td>\n<\/tr>\n

\"localgroup-180Mpc\"<\/a><\/td>\n\n
\"Box160_64CDM\"<\/a><\/td>\nLarge scale dark matter density distribution of the Local Universe simulation (Box 160<\/a>). 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.<\/p>\n

[jpg, 820×873, 533 KB]<\/a><\/td>\n<\/tr>\n

\"slice_box64-medium-labels\"<\/a><\/td>\n\n
\"Box160and64\"<\/a><\/td>\nA combination of two slices from two different CLUES simulations within a WMAP 3 cosmology:\u00a0 Box 160<\/a> and\u00a0Box 64-186592<\/a> (inset panel). The Local Supercluster (LSC) forms in both simulations and matches pretty well, despite the fact that the realizations were different.
\nLSC = Local Supercluster
\nGA = Great Attractor
\nPP = Perseus-Pisces-Cluster<\/p>\n

[png, 800×800, 543 KB]<\/a><\/td>\n<\/tr>\n

\u00a0\"Simulated_LG-1_info\"<\/a><\/td>\nAndromeda Galaxy (centre), Milky Way and Triangulum Galaxy in the high resolution region (2 Mpc\/h) of\u00a0Box 64-186592<\/a> plus some additional information.<\/p>\n

[jpg, 1000×745, 105 KB]<\/a><\/td>\n<\/tr>\n

\"yaniv4096\"<\/a><\/td>\nAndromeda Galaxy (centre), the Milky Way and Triangulum Galaxy in the high resolution region (2 Mpc\/h).<\/p>\n

[jpg, 981×922, 445 KB]<\/a><\/td>\n<\/tr>\n

\nAndromeda Galaxy<\/p>\n

[jpg, 978×710, 260 KB]<\/a><\/td>\n<\/tr>\n

\"yaniv4096_MW\"<\/a><\/td>\nMilky Way<\/p>\n

[jpg, 978×710, 265 KB]<\/a><\/td>\n<\/tr>\n

\"yaniv4096_M33\"<\/a><\/td>\nTriangulum galaxy (M33)<\/p>\n

[jpg, 978×710, 209 KB]<\/a><\/td>\n<\/tr>\n

\"LG_CDMvsWDM.avi\"<\/a><\/td>\nComparison of the three main halos in the Cold and Warm Dark Matter simulation.<\/p>\n
\"LG_dm\"<\/a><\/td>\nProjection of the three main halos (MW, M31, M33) along the z-direction (Box 64-186592<\/a>). The presented image has a size of 1.3 Mpc\/h per side.<\/p>\n

[png, 1574×1154, 503 KB]<\/a><\/p>\n

Versions with gas and star distribution are available at:
\ngas [png, 1574×1154, 357 KB]<\/a>
\nstars [png, 1574×1154, 22 KB]<\/a><\/td>\n<\/tr>\n<\/tbody>\n<\/table>\n

\n

<\/a><\/p>\n

Movies<\/h3>\n

All movies were created by simulations of the CLUES team (PI’s: S. Gottl\u00f6ber, Y. Hoffman, A. Klypin, G. Yepes). The simulations have been performed at LRZ Munich, NIC J\u00fclich and BSC Barcelona and are described in the simulations section<\/a>.<\/p>\n\n\n\n\n\n\n\n\n\n\n\n\n\n
For the production of movies for the Adler planetarium Chicago we were
\nrerunning the Box 64 – 10909<\/a> simulation (dark matter only) on the pleiades computer of NAS Ames. For this special purpose 7200 outputs in equal distance delta_a_expn = 0.0001362 were stored. The movie shows the evolution of the Local Group in spherical projection.
\nCredit:\u00a0 C. Henze, N. McCurdy, J. Primack and CLUES team. <\/em>Fast preview movie (4x speed)<\/a> [avi, 1024×1024, 22 MB]
\nFast preview movie (4x speed)<\/a> [mp4, 1024×1024, 23 MB]
\nLower quality, small<\/a> [mp4, 640×640, 23 MB]
\nLower quality<\/a> [mp4, 1024×1024, 45 MB]
\nFull resolution<\/a> [mpg, 1024×1024, 134 MB]
\nSnapshot<\/a> [jpg, 1024×1024, 109 KB]<\/td>\n<\/tr>\n
Same as above, but no spherical projection. At the end of evolution the camera zooms inward and the Local Group, Virgo Cluster and Fornax are labeled.
\nCredit: C. Henze, N. McCurdy, J. Primack and CLUES team.\u00a0 <\/em>Fast preview movie (4x speed)<\/a> [avi, 1024×1024, 9.3 MB]
\nFast preview movie (4x speed)<\/a> [mp4, 1024×1024, 13 MB]
\nLow quality<\/a> [mp4, 1024×1024, 50 MB]
\nSmall size, full quality<\/a> [mp4, 640×640, 113 MB]
\nFull size, full quality<\/a> [mp4, 1024×1024, 345 MB]<\/p>\n

Snapshot<\/a> [jpg, 1024×1024, 113 KB]<\/td>\n<\/tr>\n

Flight through the whole simulation box, WMAP5 (dark matter only, Box 64 – 10909<\/a>. Visualized using pgplot<\/a>.
\nCredit: G. Yepes and the CLUES team<\/em><\/p>\n

[avi, 1520×1142, 17 MB]<\/a>
\n[mp4, 1520×1142, 19 MB]<\/a><\/td>\n<\/tr>\n

Evolution of Andromeda (center), Milky Way (upper right) and M33 (lower right) in a ~ 2 Mpc\/h box (Box 64 – 186592<\/a>), starting at redshift z=42. The colours represent the dark matter density. A similar movie for the gas density evolution can be found in the Gas<\/a>-section. Visualized using\u00a0PMViewer<\/a>.
\nCredit: K. Riebe and the CLUES team<\/em><\/p>\n

[avi, 1024×768, 27 MB]<\/a>
\n[mp4, 1024×768, 13 MB]<\/a><\/td>\n<\/tr>\n

Evolution of Milky Way and Andromeda Galaxy (M31) in a 1.5 Mpc box (Box 64 – 10909<\/a>). Visualized using pgplot<\/a>.
\nCredit: G. Yepes and the CLUES team<\/em><\/p>\n

[avi, 1520×1140, 19 MB]<\/a>
\n[mp4, 1520×1140, 20 MB]<\/a><\/td>\n<\/tr>\n

Evolution of M31 in a 250 kpc box (Box 64 – 10909<\/a>). Visualized using pgplot<\/a>.
\nCredit: G. Yepes and the CLUES team<\/em><\/p>\n

[avi, 1520×1142, 19 MB]<\/a>
\n[mp4, 1520×1142, 20 MB]<\/a><\/td>\n<\/tr>\n

Evolution of the Milky Way in a 250 kpc box (Box 64 – 10909<\/a>). Visualized using pgplot<\/a>.
\nCredit: G. Yepes and the CLUES team<\/em><\/p>\n

[avi, 1520×1142, 19 MB]<\/a>
\n[avi, 1520×1142, 20 MB]<\/a><\/td>\n<\/tr>\n

A comparison between cold and warm dark matter, Box 64 – 186592<\/a>. Visualized using PMViewer<\/a>.
\nCredit: A. Khalatyan and the CLUES team<\/em><\/p>\n

[avi, 720×576, 8.8 MB]<\/a>
\n[mp4, 720×576, 14 MB]<\/a><\/td>\n<\/tr>\n

Comparison between cold and warm dark matter for the three main halos of the Local Group, Box 64 – 186592<\/a>. Visualized using PMViewer<\/a>.
\nCredit: A. Khalatyan and the CLUES team<\/em><\/p>\n

[avi, 640×480, 2.3 MB]<\/a>
\n[mp4, 640×480, 15 MB]<\/a><\/td>\n<\/tr>\n

Comparison of dark matter (left) and gas (right) density distribution of the Local Group at z=0 (Box 64 – 186592<\/a>, 2048^3
\nparticles effective resolution). Visualized using PMViewer<\/a>.
\nCredit: K. Riebe and the CLUES team<\/em><\/p>\n

[avi, 1220×610, 38 MB]<\/a>
\n[avi, 1024×512, 38 MB]<\/a>
\n[mp4, 1024×512, 24 MB]<\/a><\/td>\n<\/tr>\n

A flight through the whole simulation box (dark matter distribution), Box 64 – 186592<\/a>. Visualized using pgplot<\/a>.
\nCredit: G. Yepes and the CLUES team<\/em><\/p>\n

[avi, 1520×1142, 16 MB]<\/a>
\n[mp4, 1520×1142, 9.2 MB]<\/a><\/td>\n<\/tr>\n<\/tbody>\n<\/table>\n","protected":false},"excerpt":{"rendered":"

Images 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 [if not stated otherwise]: S. Gottl\u00f6ber, G. Yepes, A. Klypin, A. Khalatyan All-sky map of the gamma-ray flux from dark matter decay in […]<\/p>\n","protected":false},"author":3,"featured_media":0,"parent":46,"menu_order":0,"comment_status":"closed","ping_status":"open","template":"","meta":{"footnotes":""},"class_list":["post-87","page","type-page","status-publish","hentry"],"_links":{"self":[{"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/pages\/87","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/users\/3"}],"replies":[{"embeddable":true,"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/comments?post=87"}],"version-history":[{"count":13,"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/pages\/87\/revisions"}],"predecessor-version":[{"id":712,"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/pages\/87\/revisions\/712"}],"up":[{"embeddable":true,"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/pages\/46"}],"wp:attachment":[{"href":"https:\/\/www.clues-project.org\/cms\/wp-json\/wp\/v2\/media?parent=87"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}