1. Morphology and dynamics of the cosmic web Miguel Angel Aragon-Calvo Rien v.d. Weygaert Bernard Jones Thijs v.d. Hulst “Cosmic Voids” Amsterdam, 2006

3. Gravity naturally gives rise to: ● Walls ● Filaments ● Clusters ● Voids

4. Characterizing the morphological components of the cosmic web: The Multiscale Morphology Filter (MMF) (A small review)

5. Study the morphological information in a density field: Where:

6. The eigenvalues of the Hessian matrix encode shape information, i.e. how the field changes locally The Hessian Matrix

7. How do we account for the multiscale nature of the LSS? Scale integration: Smooth the field over the range of relevant scales Select the characteristic scale across all scales scale

8. Recovering the underlying density field (DTFE): W. Schaap & Rien v. d. Weygaert Advantages: Follows scale – Preserves original structure. Does not introduce artifacts Volume filling

9. Disadvantages Linear interpolation Smoothing length must be larger than delaunay triangle- tetrahedra.

10. MMF: Main procedure

11. Galaxies located at the vertices of voronoi cells (clusters), joined by edges resembling filaments which define planes (walls) Small test with Voronoi models

12. Particle distribution Application to a LCDM model

13. Density Field

14. The cosmic web seen with the MMF

15. Inventory of the cosmic web

16. Density of the cosmic web Density alone can not separate the morphological components!!! Blobs Filaments Walls Voids

17. Studying the cosmic web in more detail Properties of: ● Filaments Filaments ● Walls Walls

18. Compressing filaments and walls: The spine of the cosmic web

19. Density profiles FilamentsWalls Walls define the boundaries of voids!!!

20. But the Universe is not static

25. The cosmic web is shaped by its Dynamics

26. Clusters of galaxies: The nodes of the cosmic web

27. Clusters of galaxies: The nodes of the cosmic web (in time)

28. Dynamics of haloes in filaments

30. Walls…

32. And Voids

34. FilamentsWalls Peculiar velocities Dynamics of the cosmic web traced by dark matter haloes Flowing with the filamentAnd along the wall…

35. FilamentsWalls Peculiar velocities as function of distance from the spine of the cosmic web

36. Filaments Walls Peculiar velocities in time Zeldovich pancacke? Dynamical environment determines the interaction between haloes and their surroundings

37. Mass function Some properties of haloes in the cosmic web Haloes (FoF)Subhaloes (FracHop)

38. Formation time of haloes in the cosmic web

39. Formation times as function of morphology, mass and density All densities0<delta<10

40. Orientation of haloes in the cosmic web Aragon-Calvo et al 2006, in press

41. Evolution of orientations in the cosmic web: FilamentsWalls Inertia tensor

42. Evolution of orientations in the cosmic web: FilamentsWalls Spin Vector

43. Conclusions Advertisement: We developed a method (MMF) that characterizes the morphological components of the matter distribution: Blobs, Filaments Walls and Voids, allowing us to obtain a Qualitative and Quantitative description of the Large Scale Structure. The cosmic Web: The dynamics of the cosmic web are closely related to its morphology. In fact, they shape it. Environment plays a crucial role in the determination of the properties of haloes not only in terms of their local density but by defining a dynamical environment which determines the interaction between haloes and its surroundings and with other haloes.