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N-body Simulations and Gravitational Lensing with Dark Energy

N-body Simulations and Gravitational Lensing with Dark Energy. Beyond Einstein Meeting, May 13, 2004. Outline. Why Structure Formation and Dark Energy? Studying Dark Energy with Structure Formation: achievements and plans

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N-body Simulations and Gravitational Lensing with Dark Energy

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  1. N-body Simulations and Gravitational Lensing with Dark Energy Beyond Einstein Meeting, May 13, 2004

  2. Outline • Why Structure Formation and Dark Energy? • Studying Dark Energy with Structure Formation: achievements and plans • Dark Energy Models Considered: Minimally Coupled (Quintessence), Degenerate Today, Different in the Past • Cluster Concentrations (Dolag etal. 2003, A&A 416, 853) • Lensing (Arc Statistics, Meneghetti etal. 2004, A&A submitted, astro-ph/0405070) • Next Steps

  3. Why studying Dark Energy with Structure Formation? • Epochs of structure formation and cosmic acceleration overlap

  4. Why studying Dark Energy with Structure Formation? • Epochs of structure formation and cosmic acceleration overlap • Looking for signatures of a possible link between the two processes

  5. Why studying Dark Energy with Structure Formation? • Epochs of structure formation and cosmic acceleration overlap • Looking for signatures of a possible link between the two processes • Essential complement to the CMB data to compare the early, well behaving universe and the present weird cosmology Kuhlen etal. 2004, Dolag etal. 2004, Linder & Jenkins 2003, Klypin et al. 2003, …

  6. The Corrupted Universe L z=1000, Flat, sCDM f z=0, Accelerating, Large Scale Power Lack

  7. Background and Linear Perturbations Input to The N-body Machinery (gadget) Cluster Dependence on The Behavior of the Dark Energy Equation of State Imprint on Lensing Arc Statistics Large Boxes Merging Weak Lensing CMB Distortion Time Variation of G Dark Energy and Gravity Two Component Clustering Studying Dark Energy with Structure Formation: Achievements and Plans Dolag etal. A&A 416, 853, 2004, Meneghetti etal. A&A submitted, astro-ph/0405070, Bartelmann etal. A&A 409, 449, 2003, A&A 400, 19, 2003, A&A 396, 21, 2002

  8. DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi Trieste

  9. Lensing, Str.Form., Matthias Bartelmann Lensing, Massimo Meneghetti Heidelberg DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi

  10. Lensing, Str.Form., Matthias Bartelmann Lensing, Massimo Meneghetti DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi Padua N-body, Klaus Dolag Str. Form., Giuseppe Tormen Bologna Str. Form., Lauro Moscardini

  11. Lensing, Str.Form., Matthias Bartelmann Lensing, Massimo Meneghetti DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi N-body, Klaus Dolag Str. Form., Giuseppe Tormen Str. Form., Lauro Moscardini

  12. Dark Energy Models • Cosmological Constant (LCDM), Constant w=-0.6 Effective Dark Energy (DECDM), RP and SUGRA Quintessence, Open Cold Dark Matter (OCDM) • Criticalities: Equation of state behavior, Linear growth factor

  13. Clusters • Parent simulation: LCDM, 5123 particles in 479 h-1 kpc, 17 clusters identified at z=0 with radius between 5 and 10 h-1 Mpc, mass exceeding 3£ 1014 Mo . Clusters re-sampled with 106 particles • background evolution and initial conditions according to the underlying dark energy scenario • Mass resolution: 109 h-1 Mo

  14. Cluster Concentration • Radial profile binning and concentration found from a NFW fit • Comparison of the numerically determined concentrations with semi-analytical expectations

  15. Cluster Concentration

  16. Simulating Arcs • 52 equidistant time snapshots between z=0 and 1 • Surface density map from the central cluster region (3 h-1 Mpc comoving) • 2048£ 2048 light tracing grid in the central quarter of the lens plane • Deflection angle computed summing all contributions from the surface density map • Background galaxies at z=1 • Lensed images built out of the light rays lying within single sources

  17. Simulating Arcs

  18. Caustics, Critical Curves and Cross Sections

  19. Optical Depth

  20. Background and Linear Perturbations Input to The N-body Machinery (gadget) Cluster Dependence on The Behavior of the Dark Energy Equation of State Imprint on Lensing Arc Statistics Large Boxes Merging Weak Lensing CMB Distortion Time Variation of G Dark Energy and Gravity Two Component Clustering Studying Dark Energy with Structure Formation: Achievements and Plans

  21. Background and Linear Perturbations Input to The N-body Machinery (gadget) Cluster Dependence on The Behavior of the Dark Energy Equation of State Imprint on Lensing Arc Statistics Large Boxes Merging Weak Lensing CMB Distortion Time Variation of G Dark Energy and Gravity Two Component Clustering Studying Dark Energy with Structure Formation: Achievements and Plans

  22. CMB bispectrum L Q (W ) ´dT(W )/T alm=sQ (W )Ylm(W )dW Blm l`m`l``m``=alm al`m` al``m`` Bl l`l``=åm m` m`` (mlm`l`m``l``) alm al`m` al``m`` l f l`` l`

  23. CMB bispectrum & Structure Formation L < Blm l`m`l``m`` >=0 < Blm l`m`l``m`` >0 f

  24. L CMB bispectrum line of sight chronology z r z!1 :super-horizon scales in a flat CDM universe, dPY/dh =0, dQ/dz! 0 horizon crossing, Y decaying linearly, dQ/dz>0 onset of acceleration, change in cosmic equation of state, Y decaying linearly, dQ/dz>0 Non-linearity, Y grows, dQ/dz<0 f z! 0, l vanishes, dQ/dz! 0 l-1

  25. CMB bispectrum & Dark Energy L f Giovi, Baccigalupi, Perrotta PRD 2003, astro-ph/0308118

  26. Background and Linear Perturbations Input to The N-body Machinery (gadget) Cluster Dependence on The Behavior of the Dark Energy Equation of State Imprint on Lensing Arc Statistics Large Boxes Merging Weak Lensing CMB Distortion Time Variation of G Dark Energy and Gravity Two Component Clustering Studying Dark Energy with Structure Formation: Achievements and Plans

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