The cosmography unveiled by the V-Web

Slides:



Advertisements
Similar presentations
John Walton Fall, Grows over shallow water table areas High amount of evapotranspiration Water balance component Q out of reach = Q into.
Advertisements

Our CMB Motion: The Local Void influence Voids Devoid of Dwarfs: Cosmology or Gastrophysics? Brent Tully Institute for Astronomy University of Hawaii.
When Galaxies Collide. It is not uncommon for galaxies to gravitationally interact with each other, and even collide!
Tracing the Halo – Cosmic Web Connection Marius Cautun Kapteyn Astronomical Institute Rien van de Weygaert, Wojciech Hellwing, Carlos Frenk, Bernard J.
Clusters & Super Clusters Large Scale Structure Chapter 22.
An Analytic Model for the Tidal Effect on Cosmic Voids Jounghun Lee & Daeseong Park Seoul National University Lee & Park 2006, ApJ, 652, 1 Park & Lee 2006,
Our Place in the Universe Drew Smith. Important Principles The Cosmological Principle ▫The universe is isotropic and homogenous (it “looks” the same in.
Astro 101 Test #4 Review When: Now available in two files Where: On the A101 homepage.
Astro 101 Test #4 Review When: Friday, May 9 at 2pm Where: Regener 103.
WMAP CMB Conclusions A flat universe with a scale-invariant spectrum of adiabatic Gaussian fluctuations, with re-ionization, is an acceptable fit to the.
Measuring the local Universe with peculiar velocities of Type Ia Supernovae MPI, August 2006 Troels Haugbølle Institute for Physics.
Identifying and Modeling Coronal Holes Observed by SDO/AIA, STEREO /A and B Using HMI Synchronic Frames X. P. Zhao, J. T. Hoeksema, Y. Liu, P. H. Scherrer.
Relating Mass and Light in the COSMOS Field J.E. Taylor, R.J. Massey ( California Institute of Technology), J. Rhodes ( Jet Propulsion Laboratory) & the.
A cosmic sling-shot mechanism Johan Samsing DARK, Niels Bohr Institute, University of Copenhagen.
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.
14 December 2006 Dark Matter Haloes in the Cosmic Web Cristiano Porciani (ETH Zurich) with OLIVER HAHN, Marcella Carollo, Avishai Dekel.
Type Ia Supernovae on a glass: The bread and butter of peculiar velocities Lunch meeting Aarhus, March 2007 Troels Haugbølle Institute.
The Structure of the Universe AST 112. Galaxy Groups and Clusters A few galaxies are all by themselves Most belong to groups or clusters Galaxy Groups:
Efficient Visualization of Lagrangian Coherent Structures by Filtered AMR Ridge Extraction October IEEE Vis Filip Sadlo, Ronald CGL -
Stars and Galaxies n Our sun is a star. n There are countless more like it in space.
NOTES: Characteristics of Galaxies Classification: The Hubble Tuning Fork Elliptical: E0--E7 Spheroids, E0 is spherical, E7 least spherical. Population.
General Astronomy Large Scale Structure of the Universe.
Chapter 24 Galaxies. Beyond the Milky Way are billions of other galaxies Some galaxies are spiral like the Milky Way while others are egg-shaped / elliptical.
Here and Now Chapter 1. Where are You? To find our place among the stars, we will zoom out from a familiar scene, to the largest scales in the universe.
Dark Energy. Expanding Universe Galaxies in the universe are spreading out over time. –Hubble’s law From Einstein’s general relativity this happens as.
Cosmology. We can simulate how a nearly smooth distribution of dark matter turns into our lumpy, grainy Universe with its hierarchy of structures -
Masses of Galaxy Groups Brent Tully University of Hawaii.
 SIM-Lite: 6 m baseline optical interferometer in space for precision/deep astrometry.  Pointing mode not survey (spinning).  SIM concept is finishing.
3D Flow Visualization Xiaohong Ye
Galaxy Dynamics Lab 11. The areas of the sky covered by various surveys.
Various Mostly Lagrangian Things Mark Neyrinck Johns Hopkins University Collaborators: Bridget Falck, Miguel Aragón-Calvo, Xin Wang, Donghui Jeong, Alex.
The Meaning of Einstein’s Equation*
Galaxy Distances - Then and Now Brent Tully, University of Hawaii with the essential collaboration of Rick Fisher, Ed Shaya, and Helene Courtois “I have.
A systematic analysis of caustic methods for galaxy clsuter masses
‘LABYRINTH’ 3D Visualisations of the Distribution of Galaxies and Large-Scale Structures Tony Fairall Software by Carl Hultquist and SameshamPerumal Depts.
Galaxy Formation Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity Disks are produced as the cloud.
Numerical simulations of wave/particle interactions in inhomogeneous auroral plasmas Vincent Génot (IRAP/UPS/CNRS, Toulouse) F. Mottez (LUTH/CNRS, Meudon)
Electric Fields Why electric charges can reach out and touch you.
The Biggest Things in the Universe Thursday, February 21.
BAO Damping and Reconstruction Cheng Zhao
Spherical Collapse and the Mass Function – Chameleon Dark Energy Stephen Appleby, APCTP-TUS dark energy workshop 5 th June, 2014 M. Kopp, S.A.A, I. Achitouv,
A novel approach to visualizing dark matter simulations
2MTF and Future TF Surveys Lister Staveley-Smith International Centre for Radio Astronomy Research University of Western Australia Vietnam 4 July
2MASS Tully-Fisher Survey
CE 3305 Engineering FLUID MECHANICS
LANIAKEA A TRIP THROUGH SPACE.
Fields: Forces and Energy
Aileen O’Donoghue (SLU),
Digital Elevation Model Based Watershed and Stream Network Delineation
Digital Elevation Model Based Watershed and Stream Network Delineation
The Universe.
Mapping the Universe With radio galaxies and quasars.
Thursday September 28, 2017 (Discussion – Galactic Superclusters; Video – HTUW Part 3; Continue Discovery Education Unit - Exploring Our Solar System,
Probing the Dark Universe with Weak Gravitational Lensing
Focus area: Galactic Motion
Distribution of Galaxies
Overview of our studies
Galaxy Clusters.
A Tour of the Messier Catalog
Faults-notes and model
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide.
Winner of several awards
Intrinsic Alignment of Galaxies and Weak Lensing Cluster Surveys Zuhui Fan Dept. of Astronomy, Peking University.
Yongmin Yoon, Myungshin Im, Gwang-ho Lee, Gu Lim, and Seong-kook Lee
How do multi streaming regions form and evolve?
Large Scale Structure Clusters and Groups Stellar systems
Critical Timing without a Timer for Embryonic Development
Core of Coma Cluster (optical)
Turbulence 1: Turbulent Boundary layer
Velocity field of the Local Universe
Presentation transcript:

The cosmography unveiled by the V-Web Daniel Pomarède (CEA/Saclay – IRFU) Yehuda Hoffman, R. Brent Tully, Hélène Courtois XIIth Rencontres du Vietnam – Large Scale Structures and Galaxy Flows

The V-Web classification Hoffman et al. MNRAS 425 (2012) 2049 The Cosmicflows-2 catalog of 8161 peculiar velocities is used as input to a Wiener filter and constrained realizations to reconstruct the velocity field Information on local collapse and expansion is provided by the shear tensor: The analysis of the eigenvalues of the shear tensor allows to reconstruct the Velocity Web: 3 ordered eigenvalues λ1 > λ2 > λ3 at each position in space, 4 possible conditions: λ1 > λ2 > λ3 > 0 is condition for a knot (flow is inward in 3 directions) λ1 > λ2 > 0 > λ3 is condition for a filament (flow is inward in 2 directions, outward on the third) λ1 > 0 > λ2 > λ3 is condition for a sheet (flow is inward in 1 direction, outward on the 2 others) 0 > λ1 > λ2 > λ3 is condition for a void (flow is outward in all 3 directions) A few examples at selected locations: the Milky Way: λ1=0.277, λ2=0.086, λ3=-0.173 => the Milky Way resides in a filament the Perseus Cluster λ1=0.357, λ2=0.215, λ3=0.065 => the Perseus cluster is located in a knot somewhere in the middle of the Hercules Void λ1=-0.013, λ2=-0.128, λ3=-0.300 => this location is in a void

V-Web classification V-Web classification scheme: 3 ordered eigenvalues λ1 > λ2 > λ3 at each position in space, 4 possible conditions: λ1 > λ2 > λ3 > 0 is condition for a knot (flow is inward in 3 directions) λ1 > λ2 > 0 > λ3 is condition for a filament (flow is inward in 2 directions, outward on the third) λ1 > 0 > λ2 > λ3 is condition for a sheet (flow is inward in 1 direction, outward on the 2 others) 0 > λ1 > λ2 > λ3 is condition for a void (flow is outward in all 3 directions) Use of multiple non-null thresholds to reconstruct surfaces of constant values: Void cells Sheet cells Filament cells Knot cells λ1 λ2 λ3

Analysis of the V-Web using the SDvision visualization software Visualization of the knots using 5 surface levels of λ3 1) Set the desired level of λ2 2) Get the corresponding filament surface λ2= 0.075 Using a high λ2 level to materialize the filaments and several levels of λ3 to materialize the knots

Analysis of the V-Web using the SDvision visualization software Visualization of the knots using 5 surface levels of λ3 1) Set the desired level of λ2 2) Get the corresponding filament surface λ2= 0.046 A right balance between high level (surface is vanishing) and low level (surface fills the whole space) for λ2

V-Web cartography a three-dimensional network Reconstruction of the filaments that run through the uncharted Zone of Avoidance

V-Web cartography Reconstruction of the filaments that run through the Zone of Avoidance

V-Web versus Full Flow The structure of the full flow is determined by the gravitational potential, not by the V-Web that is a tracer of local collapse and expansion. Shapley is the dominant sink of velocity flows.

V-Web versus local (divergent) flows Each streamline benefits from its own local field obtained by the separation of the divergent and tidal flows Local flows run along filaments; shearing points are observed at each filaments midsections Local flows delineate Basins of Attractions (superclusters)

V-Web versus Laniakea BoA The Laniakea basin of attraction reaches out to: the voids surrounding the Great Attractor the midsections of filaments where local flows shear appart

Zoom map The Arch is a filament where flows headed to the Great Attractor and Perseus-Pisces shear apart

Immersive maps Perseus-Pisces: a node of the V-Web where several filaments converge

Immersive maps Coma: a node of the V-Web where several filaments converge

VIDEO a special shorter/faster edit of a 13min video (to be submitted)

What about sheets and voids? preliminary results The sheets and voids are organized in a three dimensional network of nodes (voids) connected by filamentary sheets. The network of knots connected by filaments and the network of voids connected by sheets are complementary.

The V-Web versus the Great Repeller