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.

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Presentation transcript:

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

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

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

Study the morphological information in a density field: Where:

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

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

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

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

MMF: Main procedure

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

Particle distribution Application to a LCDM model

Density Field

The cosmic web seen with the MMF

Inventory of the cosmic web

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

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

Compressing filaments and walls: The spine of the cosmic web

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

But the Universe is not static

The cosmic web is shaped by its Dynamics

Clusters of galaxies: The nodes of the cosmic web

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

Dynamics of haloes in filaments

Walls…

And Voids

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

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

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

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

Formation time of haloes in the cosmic web

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

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

Evolution of orientations in the cosmic web: FilamentsWalls Inertia tensor

Evolution of orientations in the cosmic web: FilamentsWalls Spin Vector

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.