Galileon Cosmology ASTR448 final project. Yin Li December 2012
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1 Galileon Cosmology ASTR448 final project Yin Li December 2012
2 Outline Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime. Phenomenology and Constraints background, de Sitter attractor linear perturbation, ghost and laplace instability; CMB, lensing, matter power spectrum, etc; tension between expansion and growth.
3 Part One Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime.
4 Part One Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime.
5 Why modified gravity? Cosmological Constant (CC)? No compelling field theory explanation for cosmic acceleration vacuum energy? 120 order of magnitude larger than CC In general there is high-order quantum correction A dynamical theory, protected against loop correction by symmetry
6 What qualifies? Modify GR in the infrared, acceleration without CC Nonlinearity, screening mechanism to pass solar system test Vainshtein mechanism: DGP, Galileon, Massive Gravity Chameleon mechanism: f(r) Symmetron...
7 Part One Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime.
8 Ostrogradski's theorem In general higher-derivative theories have extra DoF and usually plagued by instabilities Ostrogradski's theorem: linear instability in the Hamiltonians associated with Lagrangians which depend upon more than one time derivative non-degenerately 1D unrelativistic point particle example: Euler-Lagrange eqn: M. Ostrogradski, Mem. Ac. St. Petersbourg VI 4, 385 (1850) R. Woodard, Lect. Notes Phys. 720, 403 (2007) [arxiv:astro-ph/ ]
9 Ostrogradski's theorem EoM: Canonical coordinates inversion M. Ostrogradski, Mem. Ac. St. Petersbourg VI 4, 385 (1850) R. Woodard, Lect. Notes Phys. 720, 403 (2007) [arxiv:astro-ph/ ]
10 Ostrogradski's theorem Legendre transformation Hamiltonian eqns hold Hamiltonian linear in P1, thus unstable M. Ostrogradski, Mem. Ac. St. Petersbourg VI 4, 385 (1850) R. Woodard, Lect. Notes Phys. 720, 403 (2007) [arxiv:astro-ph/ ]
11 Horndeski's theory Suppress Ostrogradski's instability by requiring 2nd order E-L eqns Starting from the general form Horndeski proved the most general 2nd-order E-L eqn can be obtained from a Lagrange density of the above form with p=q=2, 10 free functions with 6 PDE's No new DoF, but not necessarily stable DGP and Galileon as subsets G. W. Horndeski, Int. J. Theor. Phys. 10 (1974)
12 Part One Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime.
13 DGP 4D gravity in 5D Minkowski spacetime Galilean and shift symmetry in decoupling limit Vainshtein mechanism Self-accelerating branch, plagued by ghost (kinetic term has the wrong sign)
14 Motivation of Galileon gravity Most general 4D Lagrangian with galilean and shift symmetry. Protection from radiative loop correction? Vainshtein mechanism No-ghost de Sitter attractor solution Other motivation of Galilean symmetry: higher dimension symmetry massive gravity A. Nicolis, R. Rattazzi and E. Trincherini, arxiv: [hep-th]
15 Part One Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski and curved spacetime.
16 Galileon in flat spacetime A. Nicolis, R. Rattazzi and E. Trincherini, arxiv: [hep-th]
17 Galileon in flat spacetime Only 2nd deriv appear in EoM's A. Nicolis, R. Rattazzi and E. Trincherini, arxiv: [hep-th]
18 Covariant Galileon Minimally coupled Galileon In curved spacetime, 3rd and 4th order derivatives appear in EoM and energymomentum tensor C. Deffayet, G. Esposito-Farese, A. Vikman, Phys. Rev. D 79, (2009) [arxiv: ]
19 Covariant Galileon Unique non-minimal couplings to curvature eliminate higher derivatives, thus retain only one scalar C. Deffayet, G. Esposito-Farese, A. Vikman, Phys. Rev. D 79, (2009) [arxiv: ]
20 Part Two Phenomenology and Constraints background, de Sitter attractor; linear perturbation, ghost and laplace instability; CMB, lensing, matter power spectrum, etc; tension between expansion and growth.
21 Einstein and Jordan Frames Action in Einstein frame In the weak field limit, the action can be transformed into a linearized form in Jordan frame, after which we can promote it to its full, nonlinear form Einstein field eqn and EoM of scalar by variation S. A. Appleby and E. V. Linder, JCAP 1203, 043 (2012), arxiv: [astro-ph.co]
22 Background Assuming flat FLRW Homogeneous evolution De Sitter attractor S. A. Appleby and E. V. Linder, JCAP 1203, 043 (2012), arxiv: [astro-ph.co]
23 Expansion A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
24 Part Two Phenomenology and Constraints background, de Sitter attractor; linear perturbation, ghost and laplace instability; CMB, lensing, matter power spectrum, etc; tension between expansion and growth.
25 Linear Perturbation Consider only scalar mode in Newtonian gauge Subhorizon, quasi-static approximation S. A. Appleby and E. V. Linder, JCAP 1203, 043 (2012), arxiv: [astro-ph.co] Covariant Gauge Invariant perturbation using 3+1 decomposition, with modified CAMB A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co] No-ghost and Laplace stability constrains the parameter space
26 Part Two Phenomenology and Constraints background, de Sitter attractor; linear perturbation, ghost and laplace instability; CMB, lensing, matter power spectrum, etc; tension between expansion and growth.
27 CMB A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
28 Weyl potential A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
29 Weak lensing potential A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
30 Matter power spectrum A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
31 Galileon clustering A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
32 Quasi-static approximation A. Barreira, B. Li, C. Baugh and S. Pascoli, arxiv: [astro-ph.co]
33 Part Two Phenomenology and Constraints background, de Sitter attractor; linear perturbation, ghost and laplace instability; CMB, lensing, matter power spectrum, etc; tension between expansion and growth.
34 Growth vs Expansion (uncoupled Galileon) Linear perturbation, scalar mode and quasi-static approx. Modified Poisson eqn Effective Gravitational strengths S. A. Appleby and E. V. Linder, JCAP 1203, 043 (2012), arxiv: [astro-ph.co] S. A. Appleby and E. V. Linder(2012), arxiv: [astro-ph.co]
35 Trial of (uncoupled) Galileon CosmoMC CMB data from WMAP7 is applied in the form of the covariance matrix for the shift parameter, acoustic peak multipole, and redshift of decoupling Distances from Type Ia supernovae in the Union2.1 data compilation constrain the expansion history at z Distances from the baryon acoustic oscillation feature in the galaxy distribution, measured to 6 redshifts at z = growth rate from the WiggleZ survey at four redshifts z = , and from the BOSS survey at z = 0.57, plus the EG growth probe S. A. Appleby and E. V. Linder(2012), arxiv: [astro-ph.co]
36 Trial of (uncoupled) Galileon Best fit yields with respect to the best fit LCDM, despite having 4 extra fit parameters: S. A. Appleby and E. V. Linder(2012), arxiv: [astro-ph.co]
37 Trial of (uncoupled) Galileon Best fit model Gravitational strengths diverges in the near future due to Laplace instability S. A. Appleby and E. V. Linder(2012), arxiv: [astro-ph.co]
38 Trial of (uncoupled) Galileon Narrow region of degeneracy S. A. Appleby and E. V. Linder(2012), arxiv: [astro-ph.co]
39 Other interesting aspects Tensor perturbation Generalized galileon G-inflation Connection to massive gravity Nonlinearity and Vainshtein mechanism
40 Thank you!
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