non-linear structure formation beyond the Newtonian approximation: a post-friedmann approach

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1 non-linear structure formation beyond the Newtonian approximation: a post-friedmann approach Marco Bruni, Institute of Cosmology and Gravitation University of Portsmouth, UK

2 Credits work with Irene Milillo (Rome, ICG), Daniele Bertacca (ICG, Cape Town) and Andrea Maselli (Rome), in progress MB, D. B. Thomas and D. Wands, Computing General Relativistic effects from Newto- nian N-body simulations: Frame dragging in the post- Friedmann approach, Physical Review D, in press, [arxiv: ] MB, J. C. Hidalgo, N. Meures, D. Wands, Non-Gaussian initial conditions in ΛCDM: Newtonian, relativistic and primordial contributions, Astrophysical Journal, in press, [arxiv:1307:1478] MB, R. Crittenden, K. Koyama, R. Maartens, C. Pitrou, D. Wands, Disentangling non- Gaussianity, bias and GR effects in the galaxy distribution, Physical Review D, 85, (R) (2012) [arxiv: ]

3 Standard ΛCDM Cosmology Recipe for modelling based on 3 main ingredients: 1. Homogeneous isotropic background, FLRW models 2. Relativistic Perturbations (e.g. CMB), good for large scales 3. Newtonian study of non-linear structure formation (N-body simulations or approx. techniques, e.g. 2LPT) at small scales on this basis, well supported by observations, the flat ΛCDM model has emerged as the Standard Concordance Model of cosmology.

4 picture credits: Daniel B. Thomas the universe at large scales

5

6 take home message it is important to consider relativistic effects in structure formations, even at small scales at large scales: matter power spectrum MB, Crittenden, Koyama, Maartens, Pitrou & Wands, Disentangling non-gaussianity, bias and GR effects in the galaxy distribution, arxiv: , PRD 85 (2012) see Bonvin & Durrer PRD 84 (2011) and Challinor & Lewis PRD 84 (2011)

7 Questions/Motivations Is the Newtonian approximation good enough to study non-linear structure formation? we are going to have more data: precision cosmology surveys and simulations covering large fraction of H-1 we also need accurate cosmology: not only we want accurate observations, we also need accurate theoretical predictions (Euclid target: 1% N-body simulations) We need to bridge the gap between small scale non-linear Newtonian approximation and large scale relativistic perturbation theory We need a relativistic framework ( dictionary ) to interprete N- body simulations [Chisari & Zaldarriaga (2011), Green & Wald (2012)]

8 post-friedmann approach current goals: develop a non-linear relativistic approximate framework, incorporating fully non-linear Newtonian theory at small scales and standard relativistic perturbations at large scales (~H -1 and beyond) extract leading order relativistic corrections from standard N-body simulations more accurate ΛCDM cosmology

9 Post-Newtonian cosmology post-newtonian: expansion in 1/c powers (more later) various attempts and studies: Tomita Prog. Theor. Phys. 79 (1988) and 85 (1991) Matarrese & Terranova, MN 283 (1996) Takada & Futamase, MN 306 (1999) Carbone & Matarrese, PRD 71 (2005) Hwang, Noh & Puetzfeld, JCAP 03 (2008) even in perturbation theory it is important to distinguish post-newtonian effects, e.g. in non-gaussianity and initial conditions. MB, J. C. Hidalgo, N. Meures, D. Wands, [arxiv: 1307:1478], cf. Bartolo et al. CQG 27 (2010) [arxiv: ]

10 post-n vs. post-f possible assumptions on the 1/c expansion: Newton: field is weak, appears only in g 00; small velocities post-newtonian: next order, in 1/c, add corrections to g 00 and gij post-minkowski (weak field): velocities can be large, time derivatives space derivative post-friedmann: something in between, using a FLRW background, Hubble flow is not slow but peculiar velocities are small tttttttttttttttttte ~r = H~r + a~v post-friedmann: we don t follow an iterative approach xt

11 metric and matter starting point: the 1-PN cosmological metric (Chandrasekhar 1965) we assume a Newtonian-Poisson gauge: Pi is solenoidal and hij is TT, at each order 2 scalar DoF in g00 and gij, 2 vector DoF in frame dragging potential Pi and 2 TT DoF in hij (not GW!)

12 metric and matter velocities, matter and the energy momentum tensor

13 metric and matter velocities, matter and the energy momentum tensor note: ρ is a non-perturbative quantity

14 Quiz Time! Which metric would you say is right in the Newtonian regime? Which terms would you retain?

15 Answer The question is not well posed: the answer depends on what you are interest in! equations of motion: passive approach, gravitational field is given (geodesics): particle or fluid motion: just U is relevant; photons: U and V (Bertschinger talk) field equations: active approach, matter tells space how to curve, curvature tells matter how to move self-consistent derivation of Newtonian equations from Einstein equations requires U, V and Pi (i.e. all leading order terms)

16 Newtonian ΛCDM, with a bonus insert leading order terms in E.M. conservation and Einstein equations subtract the background, getting usual Friedmann equations introduce usual density contrast by ρ=ρb(1+δ) from E.M. conservation: Continuity & Euler equations Poisson

17 Newtonian ΛCDM, with a bonus insert leading order terms in E.M. conservation and Einstein equations subtract the background, getting usual Friedmann equations introduce usual density contrast by ρ=ρb(1+δ) from E.M. conservation: Continuity & Euler equations cf. Bertschinger weak field lecture notes gr6.pdf Poisson

18 Newtonian ΛCDM, with a bonus what do we get from the ij and 0i Einstein equations? zero Slip bonus Newtonian dynamics at leading order, with a bonus: the frame dragging potential Pi is not dynamical at this order, but cannot be set to zero: doing so would forces a constraint on Newtonian dynamics result entirely consistent with vector relativistic perturbation theory in a relativistic framework, gravitomagnetic effects cannot be set to zero even in the Newtonian regime, cf. Kofman & Pogosyan (1995), ApJ 442: magnetic Weyl tensor at leading order

19 Post-Friedmannian ΛCDM next to leading order: the 1-PF variables resummed scalar potentials resummed gravitational potential resummed Slip potential resummed vector frame dragging potential Chandrasekhar velocity:

20 Post-Friedmannian ΛCDM The 1-PF equations: scalar sector Continuity & Euler generalized Poisson: a non-linear wave eq. for ϕg non-dynamical Slip

21 Post-Friedmannian ΛCDM The 1-PF equations: vector and tensor sectors the frame dragging vector potential becomes dynamical at this order the TT metric tensor hij is not dynamical at this order, but it is instead determined by a non-linear constraint in terms of the scalar and vector potentials

22 linearized equations linearized equations: standard scalar and vector perturbation equations in the Poisson gauge cf. Ma & Bertschinger, ApJ (1994)

23 frame-dragging potential from N-body simulations first calculation of an intrinsically relativistic quantity in fully non-linear cosmology three runs of N-body simulations with particles and 160 h -1 Mpc (Gadget-2) publicly available Delauney Tessellation Field Estimator (DTFE) used to extract the velocity field. cf. Pueblas & Scoccimarro (2009) MB, D. B. Thomas and D. Wands, Physical Review D, in press, [arxiv: ]

24 Power Spectra

25 power spectra: sources linear and non-linear matter power spectra (vorticity)

26 scalar and vector potentials linear and non-linear scalar potential vector potential

27 ratio of the potentials

28 ratio of the potentials similar ratio than in second order perturbation theory but here the scalar potential (sources) is fully nonlinear: vector potential about 10 2 larger than in IIOPT cf. Lu, Ananda, Clarkson & Maartens (2009)

29 Initial conditions and non-g standard assumption on initial conditions in N-body simulations based on Poisson equation Poisson equation is linear, hence Gaussian initial conditions in the primordial curvature perturbation (=scalar potential) translate in a Gaussian density field incorrect at large scales, where relativistic corrections come in at second order. MB, Hidalgo, Meures, Wands, ApJ, in press, [arxiv:1307:1478], cf. Bartolo et al. CQG 27 (2010) [arxiv: ]

30 Summary Resummed PF equations include Newtonian and 1-PF non-linear terms together at leading Newtonian order in the dynamics, consistency of Einstein equations requires a non-zero gravito-magnetic vector potential PF framework provides a straightforward relativistic interpretation of Newtonian simulations: quantities are those of Newton-Poisson gauge linearised equations coincide with 1-order relativistic perturbation theory in Poisson gauge (probably OK up to II-order) 2 scalar potentials, become 1 in the Newtonian regime and in the linear regime, valid at horizon scales: slip non-zero in relativistic mildly non-linear (intermediate scales?) regime gravitomagnetic vector potential extracted from N-body sim.; need to work on observational consequences: effects on convergence/weak lensing E-modes probably negligible; B-modes? lensing of CMB photon polarization?

31 Outlook and work in progress gravitomagnetic vector potential extracted from N-body sim.; need to work on observational consequences: effects on convergence/weak lensing E-modes probably negligible; B-modes? lensing of CMB photon polarization? applications of Post Friedmann formalism in many directions: quantify Slip, linear/non-linear power spectrum, lensing, etc... need to apply approx. methods to solve eqs. (e.g. 2LP theory), then consider modifying N-body codes extension to parametrised non-linear post-f to complement existing linear post-f work