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The richest superclusters: SCL126 and SCL9

The richest superclusters: SCL126 and SCL9. Maret Einasto, J. Einasto, E. Saar, E. Tago, L.J. Liivamägi, and others Tartu Observatory. SCL126 and SCL9 in the 2dF Redshift Survey. SCL9 – 2dF Southern slice. S CL126 - 2dF Northern slice. Supercluster data.

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The richest superclusters: SCL126 and SCL9

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  1. The richest superclusters:SCL126 and SCL9 Maret Einasto, J. Einasto, E. Saar, E. Tago,L.J. Liivamägi, and others Tartu Observatory

  2. SCL126 and SCL9 in the 2dF Redshift Survey SCL9 – 2dF Southern slice SCL126 - 2dF Northern slice

  3. Supercluster data Center: 196h, -1.75 deg, 250 Mpc 10h, -29 deg, 326 Mpc N(2dFgroups) 42 26 N(Abell clusters) 9 12(25) N(X-ray clusters) 4 2(6) N(galaxies) 3591 3175 δ(mean) 7.7 8.1 L(tot) 0.4x1014Lsun mass > 2 x 1016 Msun 0.5x1014Lsun Length 70 Mpc 150 Mpc For comparison: The Shapley Supercluster: N(Ab) = 28, N(X)= 8, length > 100 Mpc, mass > 2 x 1016 Msun The Horologium-Reticulum Supercluster: N(Ab) = 35, N(X)= 10, length > 100 Mpc, mass > 2 x 1016 Msun

  4. Supercluster SCL126 SCL126 in 2dF A1750 A1651, 1650, A1663: Very compact high-density core region (~10 Mpc) Multiple mergers Evidence of a filament with X-ray clusters (Belsole etal 2004, Donelly etal 2001) Imprints of such superclusters on CMB maps (SZ, RS effects, Rubino-Martin etal 2004)

  5. Supercluster SCL9 A2811, A2829

  6. Substructures in superclusters SCL126 SCL9 P – passive, non-star-forming, red galaxies (early type) A – actively star forming, blue galaxies (late type)

  7. Galaxy populations in superclusters:luminosity SCL126 SCL9 Luminosity functions of galaxies in groups. G10: rich groups (Ngal >= 10), G2: poor groups (Ngal < 10), IG: isolated galaxies (those not in groups)

  8. Galaxy populations in superclusters: colours blue red blue red P/A SCL126: 2.77 SCL9: 2.45 Colour index col: col > 1.07 – red, passive galaxies (P) col < 1.07 – blue, actively star-forming galaxies (A)

  9. Quantifying morphology with Minkowski functional V3 (Euler characteristic) V3 – the number of isolated clumps, mf – mass fraction: the ratio of the mass in regions with density lower than the density on the surface, to the total mass of the supercluster

  10. Rich superclusters – a challenge for cosmological models There are too many of them. Galaxy formation and evolution depend on both local and global environment. Richness of groups and their galaxy content depend of environment. Bright/faint galaxy distribution more clumpy than in models.

  11. Rich superclusters – a challenge for cosmological models There are large differences between the richest superclusters: 1. SCL126 contains very compact core with X-ray clusters. Collapsing core? In models such cores are very rare (Gramann and Suhhonenko2002) 2. Structure SCL9 more similar to model superclusters than SCL126. 3. Galaxy populations and distribution/clumpiness in SCL126 the fraction of red galaxies higher than in SCL9 – SCL126 – older? One of the first superclusters? z=2 z=0

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