Statistical physics for cosmic structures: Gravitational structure formation and the cosmological problem Francesco Sylos Labini In collaboration with.

Slides:



Advertisements
Similar presentations
DM density profiles in non-extensive theory Eelco van Kampen Institute for Astro- and Particle Physics Innsbruck University In collaboration with Manfred.
Advertisements

P ROBING SIGNATURES OF MODIFIED GRAVITY MODELS OF DARK ENERGY Shinji Tsujikawa (Tokyo University of Science)
Simulating the joint evolution of quasars, galaxies and their large-scale distribution Springel et al., 2005 Presented by Eve LoCastro October 1, 2009.
Observational tests of an inhomogeneous cosmology by Christoph Saulder in collaboration with Steffen Mieske & Werner Zeilinger.
Wave-mechanics and the adhesion approximation Chris Short School of Physics and Astronomy The University of Nottingham UK.
Non-linear matter power spectrum to 1% accuracy between dynamical dark energy models Matt Francis University of Sydney Geraint Lewis (University of Sydney)
Cosmological Structure Formation A Short Course
Dark Matter-Baryon segregation in the non-linear evolution of coupled Dark Energy models Roberto Mainini Università di Milano Bicocca Mainini 2005, Phys.Rev.
Tomographic approach to Quantum Cosmology Cosimo Stornaiolo INFN – Sezione di Napoli Fourth Meeting on Constrained Dynamics and Quantum Gravity Cala Gonone.
Breakdown of the adiabatic approximation in low-dimensional gapless systems Anatoli Polkovnikov, Boston University Vladimir Gritsev Harvard University.
Lecture 2: Observational constraints on dark energy Shinji Tsujikawa (Tokyo University of Science)
Universe in a box: simulating formation of cosmic structures Andrey Kravtsov Department of Astronomy & Astrophysics Center for Cosmological Physics (CfCP)
Physics 133: Extragalactic Astronomy and Cosmology Lecture 12; February
IV Congresso Italiano di Fisica del Plasma Firenze, Gennaio 2004 Francesco Valentini Dipartimento di Fisica, Università della Calabria Rende (CS)
Coupled Dark Energy and Dark Matter from dilatation symmetry.
1 Latest Measurements in Cosmology and their Implications Λ. Περιβολαρόπουλος Φυσικό Τμήμα Παν/μιο Κρήτης και Ινστιτούτο Πυρηνικής Φυσικής Κέντρο Ερευνών.
A cosmic sling-shot mechanism Johan Samsing DARK, Niels Bohr Institute, University of Copenhagen.
THE GRACEFUL EXIT FROM INFLATION AND DARK ENERGY By Tomislav Prokopec Publications: Tomas Janssen and T. Prokopec, arXiv: ; Tomas Janssen, Shun-Pei.
Black hole production in preheating Teruaki Suyama (Kyoto University) Takahiro Tanaka (Kyoto University) Bruce Bassett (ICG, University of Portsmouth)
Galaxy bias with Gaussian/non- Gaussian initial condition: a pedagogical introduction Donghui Jeong Texas Cosmology Center The University of Texas at Austin.
Observational Evidence for Extra Dimensions from Dark Matter Bo Qin National Astronomical Observatories, China Bo Qin, Ue-Li Pen & Joseph Silk, PRL, submitted.
Connecting the Galactic and Cosmological Length Scales: Dark Energy and The Cuspy-Core Problem By Achilles D. Speliotopoulos Talk Given at the Academia.
Cosmological Reconstruction via Wave Mechanics Peter Coles School of Physics & Astronomy University of Nottingham.
Modern State of Cosmology V.N. Lukash Astro Space Centre of Lebedev Physics Institute Cherenkov Conference-2004.
Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN Cosmology and the origin of structure Rocky I : The universe observed Rocky.
Probing the Reheating with Astrophysical Observations Jérôme Martin Institut d’Astrophysique de Paris (IAP) 1 [In collaboration with K. Jedamzik & M. Lemoine,
Dark energy I : Observational constraints Shinji Tsujikawa (Tokyo University of Science)
What can we learn from galaxy clustering? David Weinberg, Ohio State University Berlind & Weinberg 2002, ApJ, 575, 587 Zheng, Tinker, Weinberg, & Berlind.
Clustering in the Sloan Digital Sky Survey Bob Nichol (ICG, Portsmouth) Many SDSS Colleagues.
The dark universe SFB – Transregio Bonn – Munich - Heidelberg.
The Theory/Observation connection lecture 2 perturbations Will Percival The University of Portsmouth.
Higher Order Curvature Gravity in Finsler Geometry N.Mebarki and M.Boudjaada Département de Physique Mathématique et Subatomique Faculty of Science, Mentouri.
1 Three views on Landau damping A. Burov AD Talk, July 27, 2010.
Dynamical Instability of Differentially Rotating Polytropes Dept. of Earth Science & Astron., Grad. School of Arts & Sciences, Univ. of Tokyo S. Karino.
Michael Doran Institute for Theoretical Physics Universität Heidelberg Time Evolution of Dark Energy (if any …)
Racah Institute of physics, Hebrew University (Jerusalem, Israel)
How accurately do N body simulations reproduce the clustering of CDM? Michael Joyce LPNHE, Université Paris VI Work in collaboration with: T. Baertschiger.
23 Sep The Feasibility of Constraining Dark Energy Using LAMOST Redshift Survey L.Sun Peking Univ./ CPPM.
Cosmic shear and intrinsic alignments Rachel Mandelbaum April 2, 2007 Collaborators: Christopher Hirata (IAS), Mustapha Ishak (UT Dallas), Uros Seljak.
Probing cosmic structure formation in the wavelet representation Li-Zhi Fang University of Arizona IPAM, November 10, 2004.
The Feasibility of Constraining Dark Energy Using LAMOST Redshift Survey L.Sun.
Astro-2: History of the Universe Lecture 10; May
Gravitational collapse of massless scalar field Bin Wang Shanghai Jiao Tong University.
Black Hole Universe -BH in an expanding box- Yoo, Chulmoon ( YITP) Hiroyuki Abe (Osaka City Univ.) Ken-ichi Nakao (Osaka City Univ.) Yohsuke Takamori (Osaka.
Three theoretical issues in physical cosmology I. Nonlinear clustering II. Dark matter III. Dark energy J. Hwang (KNU), H. Noh (KASI)
GRAVITON BACKREACTION & COSMOLOGICAL CONSTANT
Quantum Noises and the Large Scale Structure Wo-Lung Lee Physics Department, National Taiwan Normal University Physics Department, National Taiwan Normal.
Stochastic Background Data Analysis Giancarlo Cella I.N.F.N. Pisa first ENTApP - GWA joint meeting Paris, January 23rd and 24th, 2006 Institute d'Astrophysique.
Feasibility of detecting dark energy using bispectrum Yipeng Jing Shanghai Astronomical Observatory Hong Guo and YPJ, in preparation.
NEUTRINOS IN THE INTERGALACTIC MEDIUM Matteo Viel, Martin Haehnelt. Volker Springel: arXiv today Rencontres de Moriond – La Thuile 15/03/2010.
Initial conditions for N-body simulations Hans A. Winther ITA, University of Oslo.
Evolution of perturbations and cosmological constraints in decaying dark matter models with arbitrary decay mass products Shohei Aoyama Nagoya University.
The HORIZON Quintessential Simulations A.Füzfa 1,2, J.-M. Alimi 2, V. Boucher 3, F. Roy 2 1 Chargé de recherches F.N.R.S., University of Namur, Belgium.
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,
Some bonus cosmological applications of BigBOSS ZHANG, Pengjie Shanghai Astronomical Observatory BigBOSS collaboration meeting, Paris, 2012 Refer to related.
3D Matter and Halo density fields with Standard Perturbation Theory and local bias Nina Roth BCTP Workshop Bad Honnef October 4 th 2010.
Breaking of spherical symmetry in gravitational collapse.
Collapse of Small Scales Density Perturbations
Theory group Michael Joyce *.
Theoretical Particle Physics Group (TPP)
Outline Part II. Structure Formation: Dark Matter
The influence of Dark Energy on the Large Scale Structure Formation
Cosmic Inflation and Quantum Mechanics I: Concepts
Quantum Spacetime and Cosmic Inflation
Shintaro Nakamura (Tokyo University of Science)
Global Defects near Black Holes
Outline Part II. Structure Formation: Dark Matter
Complexity in cosmic structures
The impact of non-linear evolution of the cosmological matter power spectrum on the measurement of neutrino masses ROE-JSPS workshop Edinburgh.
21cm Hydrogen spectrum anomaly and dark matter Qiaoli Yang Jian University Phys.Rev.Lett. 121 (2018) Nick Houston, Chuang Li, Tianjun Li, Qiaoli.
Presentation transcript:

Statistical physics for cosmic structures: Gravitational structure formation and the cosmological problem Francesco Sylos Labini In collaboration with T. Baertschiger, A. Gabrielli, L. Pietronero, B. Marcos Rome M. Joyce, Y. Baryshev, N. Vasilyev Paris Saint Petersburg “E. Fermi Center” & Institute for Complex Systems (ISC-CNR) Rome Italy

Summary The discrete gravitational N-body problem Primordial density fields and super-homogeneous distributions The observed distribution of galaxies Analogy with statistical physics systems Crucial observational tests for the standard theory of structure formation Role of dark matter

Early times density fields WMAP satellite 1st year, 2002 COBE DMR, 1992

150 Mpc/h (1990) 300 Mpc/h (2004) 5 Mpc/h Late times density fields

The problem of cosmological structure formation Initial conditions: Uniform distribution (small amplitude fluctuations) Final conditions: Stronlgy clustered, power-law correlations Dynamics: self-gravitating infinite system

Cosmological energy budget: the “standard model” Non baryonic dark matter (e.g. CDM): -never detected on Earth -needed to make structures compatible with anisotropies Dark Energy -never detected on Earth -needed to explain SN data -troubles with the contribution of quantum vacuum energy… What do we know about dark matter ? Fundamental and observational constraints

Statistical properties of fluctuations in FRW models (I)

Substantially Poisson (finite correlation length) Super-Poisson (infinite correlation length) Sub-Poisson (ordered or super-homogeneous) Statistical properties of fluctuations in FRW models (II) Extremely fine-tuned distributions

Statistical properties of fluctuations in FRW models (III) For CDM models: For HDM models: (integral constraint…)

Statistical properties of fluctuations in FRW models (IV) Anisotropies due to fluctuations in the gravitational potential (Sachs Wolfe)

Statistical properties of fluctuations in FRW models (V) Angular correlation function vanishes at > 60 deg (COBE/WMAP teams) Small quadrupole/octupole (COBE/WMAP teams) Planar octupole, aligned with quadrulpole (de Olivera Costa et al., 2003) Deficit of power in North ecliptic emisphere (Eriksen et al. 2003) Quadrupole and octopole aligned and correlated with Ecliptic (Schwartz et al. 2004)

Statistical properties of fluctuations in FRW models (VI)

Sampling fluctuations in FRW models (I)

Sampling fluctuations in FRW models (II)

Sampling fluctuations in FRW models (III) Normalization ? Origin the linear amplification? This is the only peculiar distinctive feature of HZ models in matter distribution

Conditional correlation properties (I)

Conditional correlation properties (II) Super-homogeneous Poisson-like Critical ?

Conditional correlation properties (III)

Conditional correlation properties (IV) Sampling Finite size

Conditional correlation properties (V) Sylos Labini, F., Montuori M. & Pietronero L. Phys Rep, 293, 66 (1998) Joyce M. & Sylos Labini F. Astrophys. J 554, L1 (2000)Hogg et al. (SDSS Collaboration) astro-ph/

Conditional correlation properties (VI)

Joyce M. & Sylos Labini F. Astrophys. J 554, L1 (2000) galaxies rotation curves Conditional correlation properties (VII)

Discrete gravitational N body problem (I) Classical interacting particles Collisionless Boltzmann Equation (Vlasov eq.)+ Poisson equation DM collisionless continuous medium Self-gravitating fluid equations in an expading universe Macro Particles N=10 10 (instead of N=10 80 ) as mass tracers Theoretical scheme of interpretation of numerical simulations Do the macro-particles correctly trace the evolution of the statistical and dynamical properties of theoretical models ? Statistical and dynamical effects of Discretization What Nbody really are

Problem: strong clustering up to scales ~ initial NN distance Self-gravitating continuous fluid interpretation: NO effects due to the granular nature of the particle distribution Convergence studies and stability No theory of discreteness Effects No theoretical knowledge of N dependence of the convergece Discrete gravitational N body problem (II)

Discrete gravitational N body problem (III) 1) Static (generation of IC): Effects of the pre-initial distribution on the correlations imposed with displacements by the ZA. 2) Early time evolution (up to shell crossing): Discreteness effects from spatial sampling 3) Growth of first correlations (two-body correlations): Strong collisions between particles 4) Late times (many body correlations): Self-similar evolution of the conditional density

Finite box + Periodic boundary conditions: infinite system (no center) Linear Perturbative Theory (I) Jeans swindle

Linear Perturbative Theory (II) Wigner crystal Bloch Theorem: diagonalization by plane waves

3X3 Real and symmetric matrix for each k Eigenmodes/ eigenvalues Wigner crystal: oscillations with plasma frequency Wigner crystal :unstable modes Gravity: Oscillating modes Wigner Crystal: oscillating modes Gravity: growing instabilities (even faster than fluid rate) Linear Perturbative Theory (III) Kohn sum rule Gravity: Fluid evolution (Lagrangian formalism)

Theoretical scheme for a perturbative treatment of the discrete N-body Especially relevant because of the method to set up IC in cosmological N-body Precise formalism up to shell crossing for calculating discreteness corrections Oscillating modes Breaking of isotropy Divergence from fluid behavior Extension of the perturbative treatment to higher orders Body-centered cubic lattice is stable (only unstable mode for gravity) If initial perturbations contain modes such that Same results as Lagrangian formalism of a pressureless self-gravitating fluid Zeldovich approximation as asymptotic form of the discrete solutions Linear Perturbative Theory (IV) What’s new

Poisson initial conditions (no correlations) Zero initial velocities Periodic Boundary conditions Growth of correlation in the gravitational problem (I) Two body collapse time No expansion

A simple test: NN force versus full gravity Most of particles are mutually NN Gravitational force is dominated by NN Our hypothesis: The full distribution can be treated for a time of the order of the dynamical time as an ensamble of isolated two-body systems Growth of correlation in the gravitational problem (II)

Discrete fluctuations give rise to early non-linear correlation (structures). How discrete effects are “exported” at larger scales and longer times ? Growth of correlation in the gravitational problem (III)

As for the Poisson and SL case: 1.Formation of first structures from discrete fluctuations 2. Propagation of correlation from small to large scales Growth of correlation in the gravitational problem (IV)

Usual picture Dynamical evolution of the small fluctuations in the initial continuous field (non-linear regime of the set of fluid equations in an expanding universe) dependence on: - Initial conditions - Space expansion Our Conclusion: Non-linear dynamics of cosmological NBS is essentially the same as the non-expanding Poisson case and it is driven by the discrete fluctuations at the smallest scales in the distribution: -independent on IC -Space expansion Growth of correlation in the gravitational problem (VI)

Discreteness of the gravitational field causes first correlations (interaction of nearest neighbors and formation of small groups) Each group begins to act as a single particle and the groups themselves become correlated and more and more massive clusters are build up. The clustering is rescaled to larger and larger distances whose limit is determined by the time available for structure to form (W.C. Saslaw “The distribution of the galaxies” 2002, CUP) Coarse Grain approach: Interplay between discrete effects and fluid linear evolution Growth of correlation in the gravitational problem (VII)

Growth of correlation in the gravitational problem (VIII)

Summary HZ tail: the only distinctive feature of FRW-IC in matter distribution is the behavior of the large scales tail of the correlation function Problem with large angle CMBR anisotropies Homogeneity scale: not yet identified with galaxy distribution Amplification (i.e.Bias): is due to a finite size effect and not to selection different mechanism in simulations and galaxies Structures in N-Body simulations: too small and maybe different in nature from galaxy structures Discrete gravitational clustering: results of N-body must be taken with great care when interpreted as evolution of DM fluid Discrete fluctuations play a central role for non-linear structures Universality and independence on IC Perturbative theory for the treatment of discrete systems

Conclusion: Plans for the Future…. Study of galaxy distribution in the SDSS survey -- Homogeneity scale -- Clustering of galaxies of different luminosity Formation of non linear structures -- Study of modified potentials (cut-off, softnening) -- Non linear study of perturbed lattices -- Coarse grain approach for the formation of structures -- Statisical characterization of structures (Tsallis, Saslaw…) Study of CMBR density fields -- Real space analysis -- Test for angular isotrotpy

Some references A.Gabrielli, B. Jancovici, M. Joyce, J.L. Lebowitz, L. Pietronero and F. Sylos Labini Generation of primordial cosmological perturbations from statistical mechanicalmodels, Phys.Rev. D67, (2003) T. Baertschiger, M. Joyce and F. Sylos Labini Power law and discreteness in cosmological N-body simulations, Astrophys.J.Lett 581, L63 (2002) F. Sylos Labini, T. Baertschiger and M. Joyce Universality of power-law correlation in the gravitational clustering, Europhys.Lett. 66,171, (2004) T. Baertschiger and F. Sylos Labini On the problem of initial conditions in cosmological N-body simulations Europhs.Lett. 57, 322 (2002) A. Gabrielli, M. Joyce and F. Sylos Labini The Glass-like universe: real space statistical properties of standard cosmological models, Phys.Rev.D, 65, (2002) T. Baertschiger and F. Sylos Labini Growth of correlations in gravitational N-body simulations Phys.Rev.D 69, , 2004 M. Joyce, B. Marcos, A. Gabrielli, T. Baertschiger, F. Sylos Labini Gravitational evolution of a perturbed lattice and its fluid limit Phys.Rev.Lett R. Durrer, A. Gabrielli, M. Joyce and F. Sylos Labini,``Bias and the power spectrum beyond the turn-over'' Astrophys.J.Lett,585, L1-L4 (2003) A.Gabrielli, F. Sylos Labini, M. Joyce, L. Pietronero Statistical physics for cosmic structures Springer Verlag 2005