Publications (49)170.67 Total impact
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ABSTRACT: We have recently proposed a new class of gravitational scalartensor theories free from ghost instabilities. As they generalize Horndeski theories, or "generalized" galileons, we call them G$^3$. These theories possess a simple formulation when the time hypersurfaces are chosen to coincide with the uniform scalar field hypersurfaces. We confirm that they do not suffer from Ostrogradski instabilities by presenting the details of the Hamiltonian formulation. We examine the coupling between these theories and matter. Moreover, we investigate how they transform under a disformal redefinition of the metric. Remarkably, these theories are preserved by disformal transformations, which also allow subfamilies of G$^3$ to be mapped into Horndeski theories.08/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We show that the prediction for the primordial tensor power spectrum cannot be modified at leading order in derivatives. Indeed, one can always set to unity the speed of propagation of gravitational waves during inflation by a suitable disformal transformation of the metric, while a conformal one can make the Planck mass timeindependent. Therefore, the tensortoscalar ratio unambiguously fixes the energy scale of inflation. Using the Effective Field Theory of Inflation, we check that predictions are independent of the choice of frame, as expected. The first corrections to the standard prediction come from two parity violating operators with three derivatives. Also the correlator $\langle\gamma\gamma\gamma\rangle$ is standard and only receives higher derivative corrections. These results hold also in multifield models of inflation and in alternatives to inflation and make the connection between a (quasi) scaleinvariant tensor spectrum and inflation completely robust.07/2014; 
Article: Healthy theories beyond Horndeski
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ABSTRACT: We introduce a new class of scalartensor theories that extend Horndeski, or "generalized galileon", models. Despite possessing equations of motion of higher order in derivatives, we show that the true propagating degrees of freedom obey wellbehaved secondorder equations and are thus free from Ostrogradski instabilities, in contrast to the standard lore. Remarkably, the covariant versions of the original galileon Lagrangiansobtained by direct replacement of derivatives with covariant derivativesbelong to this class of theories. These extensions of Horndeski theories exhibit an uncommon, interesting phenomenology: the scalar degree of freedom affects the speed of sound of matter, even when the latter is minimally coupled to gravity.04/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We compute the full cosmic microwave background temperature bispectrum generated by nonlinearities after singlefield inflation. By integrating the photon temperature at second order along a perturbed geodesic in Newtonian gauge, we derive an expression for the observed temperature fluctuations that, for the first time, clarifies the separation of the gravitational lensing and timedelay effects from the purely secondorder contributions. We then use the secondorder Boltzmann code CosmoLib2nd to calculate these contributions and their bispectrum. Including the perturbations in the photon path, the numerically computed bispectrum exactly matches the expected squeezed limit. Moreover, the analytic squeezedlimit formula reproduces well the signaltonoise ratio and shape of the full bispectrum, potentially facilitating the subtraction of the bias induced by secondorder effects. For a cosmicvariance limited experiment with lmax=2000, the bias on a local signal is fNLloc=0.73 negligible for equilateral and orthogonal signals. The signaltonoise ratio is unity at lmax̃3000, suggesting that secondorder effects may hopefully be measured in the future.12/2013; 89(2).  [Show abstract] [Hide abstract]
ABSTRACT: The recently derived consistency relations for Large Scale Structure do not hold if the Equivalence Principle (EP) is violated. We show it explicitly in a toy model with two fluids, one of which is coupled to a fifth force. We explore the limits that galaxy surveys can set on EP violation looking at the squeezed limit of the 3point function involving two populations of objects. We find that one can explore EP violations of order 10^{3}  10^{4} on cosmological scales. Chameleon models are already very constrained by the requirement of screening within the Solar System and only a very tiny region of the parameter space can be explored with this method. We show that no violation of the consistency relations is expected in Galileon models.Journal of Cosmology and Astroparticle Physics 12/2013; 2014(06). · 6.04 Impact Factor 
Article: SingleField Consistency Relations of Large Scale Structure. Part II: Resummation and Redshift Space
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ABSTRACT: We generalize the recently derived singlefield consistency relations of Large Scale Structure in two directions. First, we treat the effect of the long modes (with momentum q) on the short ones (with momentum k) nonperturbatively, by writing resummed consistency relations which do not require k/q \delta_q << 1. These relations do not make any assumptions on the shortscales physics and are extended to include (an arbitrary number of) multiple long modes, internal lines with soft momenta and soft loops. We do several checks of these relations in perturbation theory and we verify that the effect of soft modes always cancels out in equaltime correlators. Second, we write the relations directly in redshift space, without assuming the singlestream approximation: not only the long mode affects the short scales as a homogeneous gravitational field, but it also displaces them by its velocity along the lineofsight. Redshift space consistency relations still vanish when short modes are taken at equal time: an observation of a signal in the squeezed limit would point towards multifield inflation or a violation of the equivalence principle.Journal of Cosmology and Astroparticle Physics 11/2013; 2014(02). · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We derive consistency relations for the late universe (CDM and \Lambda CDM): relations between an npoint function of the density contrast \delta and an (n+1)point function in the limit in which one of the (n+1) momenta becomes much smaller than the others. These are based on the observation that a long mode, in singlefield models of inflation, reduces to a diffeomorphism since its freezing during inflation all the way until the late universe, even when the long mode is inside the horizon (but out of the sound horizon). These results are derived in Newtonian gauge, at first and second order in the small momentum q of the long mode and they are valid nonperturbatively in the shortscale \delta. In the nonrelativistic limit our results match with (Kehagias and Riotto '12) and (Peloso and Pietroni '12). These relations are a consequence of diffeomorphism invariance; they are not satisfied in the presence of extra degrees of freedom during inflation or violation of the Equivalence Principle (extra forces) in the late universe.Journal of Cosmology and Astroparticle Physics 09/2013; · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: The effective field theory of cosmological perturbations stems from considering a cosmological background solution as a state displaying spontaneous breaking of time translations and (adiabatic) perturbations as the related NambuGoldstone modes. With this insight, one can systematically develop a theory for the cosmological perturbations during inflation and, with minor modifications, also describe in full generality the gravitational interactions of dark energy, which are relevant for latetime cosmology. The formalism displays a unique set of Lagrangian operators containing an increasing number of cosmological perturbations and derivatives. We give an introductory description of the unitary gauge formalism for theories with broken gauge symmetrythat allows to write down the most general Lagrangianand of the Stueckelberg "trick"that allows to recover gauge invariance and to make the scalar field explicit. We show how to apply this formalism to gravity and cosmology and we reproduce the detailed analysis of the action in the ADM variables. We also review some basic applications to inflation and dark energy.Classical and Quantum Gravity 07/2013; 30(21). · 3.56 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We propose a minimal description of single field dark energy/modified gravity within the effective field theory formalism for cosmological perturbations, which encompasses most existing models. We start from a generic Lagrangian given as an arbitrary function of the lapse and of the extrinsic and intrinsic curvature tensors of the time hypersurfaces in unitary gauge, i.e. choosing as time slicing the uniform scalar field hypersurfaces. Focusing on linear perturbations, we identify seven Lagrangian operators that lead to equations of motion containing at most two (space or time) derivatives, the background evolution being determined by the time dependent coefficients of only three of these operators. We then establish a dictionary that translates any existing or future model whose Lagrangian can be written in the above form into our parametrized framework. As an illustration, we study Horndeski'sor generalized Galileontheories and show that they can be described, up to linear order, by only six of the seven operators mentioned above. This implies, remarkably, that the dynamics of linear perturbations can be more general than that of Horndeski while remaining second order. Finally, in order to make the link with observations, we provide the entire set of linear perturbation equations in Newtonian gauge, the effective Newton constant in the quasistatic approximation and the ratio of the two gravitational potentials, in terms of the timedependent coefficients of our Lagrangian.Journal of Cosmology and Astroparticle Physics 04/2013; 2013(08). · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We compute the cosmic microwave background temperature bispectrum generated by nonlinearities at recombination on all scales. We use CosmoLib2nd, a numerical Boltzmann code at second order to compute cosmic microwave background bispectra on the full sky. We consistently include all effects except gravitational lensing, which can be added to our result using standard methods. The bispectrum is peaked on squeezed triangles and agrees with the analytic approximation in the squeezed limit at the few percent level for all the scales where this is applicable. On smaller scales, we recover previous results on perturbed recombination. For cosmicvariance limited data to l_{max}=2000, its signaltonoise ratio is S/N=0.47, corresponding to f_{NL}^{eff}=2.79, and will bias a local signal by f_{NL}^{loc}≃0.82.Physical Review Letters 03/2013; 110(10):101303. · 7.73 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We use the socalled eikonal approximation, recently introduced in the context of cosmological perturbation theory, to compute power spectra for multicomponent fluids. We demonstrate that, at any given order in standard perturbation theory, multipoint power spectra do not depend on the largescale adiabatic modes. Moreover, we employ perturbation theories to decipher how nonadiabatic modes, such as a relative velocity between two different components, damp the smallscale matter power spectrum, a mechanism recently described in the literature. In particular, we do an explicit calculation at oneloop order of this effect. While the oneloop result eventually breaks down, we show how the damping effect can be fully captured by the help of the eikonal approximation. A relative velocity not only induces mode damping but also creates largescale anisotropic modulations of the matter power spectrum amplitude. We illustrate this for the Local Group environment.Physical review D: Particles and fields 02/2013; 87(4).  [Show abstract] [Hide abstract]
ABSTRACT: We compute the cosmic microwave background temperature bispectrum generated by nonlinearities at recombination on all scales. We use CosmoLib$2^{\rm nd}$, a numerical Boltzmann code at secondorder to compute CMB bispectra on the full sky. We consistently include all effects except gravitational lensing, which can be added to our result using standard methods. The bispectrum is peaked on squeezed triangles and agrees with the analytic approximation in the squeezed limit at the few per cent level for all the scales where this is applicable. On smaller scales, we recover previous results on perturbed recombination. For cosmicvariance limited data to $l_{\rm max} =2000$, its signaltonoise is $S/N=0.47$ and will bias a local signal by $f_{\rm NL}^{\rm loc}\simeq 0.82$.12/2012;  [Show abstract] [Hide abstract]
ABSTRACT: We propose a universal description of dark energy and modified gravity that includes all singlefield models. By extending a formalism previously applied to inflation, we consider the metric universally coupled to matter fields and we write in terms of it the most general unitary gauge action consistent with the residual unbroken symmetries of spatial diffeomorphisms. Our action is particularly suited for cosmological perturbation theory: the background evolution depends on only three operators. All other operators start at least at quadratic order in the perturbations and their effects can be studied independently and systematically. In particular, we focus on the properties of a few operators which appear in nonminimally coupled scalartensor gravity and galileon theories. In this context, we study the mixing between gravity and the scalar degree of freedom. We assess the quantum and classical stability, derive the speed of sound of fluctuations and the renormalization of the Newton constant. The scalar can always be demixed from gravity at quadratic order in the perturbations, but not necessarily through a conformal rescaling of the metric. We show how to express covariant fieldoperators in our formalism and give several explicit examples of dark energy and modified gravity models in our language. Finally, we discuss the relation with the covariant EFT methods recently appeared in the literature.Journal of Cosmology and Astroparticle Physics 09/2012; 1302(2013):032. · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Euclid is a European Space Agency medium class mission selected for launch in 2019 within the Cosmic Vision 20152025 programme. The main goal of Euclid is to understand the origin of the accelerated expansion of the Universe. Euclid will explore the expansion history of the Universe and the evolution of cosmic structures by measuring shapes and redshifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid's Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission.06/2012;  [Show abstract] [Hide abstract]
ABSTRACT: We compute the matter bispectrum in the presence of primordial local nonGaussianity over a wide range of scales, including the very small nonlinear ones. We use the Halo Model approach, considering nonGaussian corrections to the halo profiles, the halo mass function and the bias functions. We compare our results in the linear and mildly nonlinear scales to a large ensemble of Gaussian and nonGaussian numerical simulations. We consider both squeezed and equilateral configurations, at redshift z = 0 and z = 1. For z = 0, the deviations between the Halo Model and the simulations are smaller than 10% in the squeezed limit, both in the Gaussian and nonGaussian cases. The Halo Model allows to make predictions on scales much smaller than those reached by numerical simulations. For local nonGaussian initial conditions with a parameter fNL = 100, we find an enhancement of the bispectrum in the squeezed configuration k = k3 = k2 >> k1 \sim 0.01 h^{1} Mpc, of \sim 15% and \sim 25% on scales k \sim 1 h^{1} Mpc, at z = 0 and z = 1 respectively. This is mainly due to the nonGaussian corrections in the linear bias. Finally we provide a very simple expression valid for any scenario, i.e. for any choice of the halo profile, mass and bias functions, which allow for a fast evaluation of the bispectrum on squeezed configurations.Journal of Cosmology and Astroparticle Physics 05/2012; 2012(08). · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We introduce the eikonal approximation to study the effect of the largescale motion of cosmic fluids on their smallscale evolution. This approach consists in collecting the impact of the longwavelength displacement field into a single or finite number of random variables, whose statistical properties can be computed from the initial conditions. For a single dark matter fluid, we show that we can recover the nonlinear propagators of renormalized perturbation theory. These are obtained with no need to assume that the displacement field follows the linear theory. Then we extend the eikonal approximation to many fluids. In particular, we study the case of two nonrelativistic components and we derive their resummed propagators in the presence of isodensity modes. Unlike the adiabatic case, where only the phase of smallscale modes is affected by the largescale advection field, the isodensity modes change also the amplitude on small scales. We explicitly solve the case of cold dark matterbaryon mixing and find that the isodensity modes induce only very small corrections to the resummed propagators.Physical review D: Particles and fields 03/2012; 85(6).  [Show abstract] [Hide abstract]
ABSTRACT: With future galaxy surveys, a huge number of Fourier modes of the distribution of the large scale structures in the Universe will become available. These modes are complementary to those of the CMB and can be used to set constraints on models of the early universe, such as inflation. Using a MCMC analysis, we compare the power of the CMB with that of the combination of CMB and galaxy survey data, to constrain the power spectrum of primordial fluctuations generated during inflation. We base our analysis on the Planck satellite and a spectroscopic redshift survey with configuration parameters close to those of the Euclid mission as examples. We first consider models of slowroll inflation, and show that the inclusion of large scale structure data improves the constraints by nearly halving the error bars on the scalar spectral index and its running. If we attempt to reconstruct the inflationary singlefield potential, a similar conclusion can be reached on the parameters characterizing the potential. We then study models with features in the power spectrum. In particular, we consider ringing features produced by a break in the potential and oscillations such as in axion monodromy. Adding large scale structures improves the constraints on features by more than a factor of two. In axion monodromy we show that there are oscillations with small amplitude and frequency in momentum space that are undetected by CMB alone but can be measured by including galaxy surveys in the analysis.Journal of Cosmology and Astroparticle Physics 01/2012; 2012(04). · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Future lensing surveys will be nearly fullsky and reach an unprecedented depth, probing scales closer and closer to the Hubble radius. This motivates the study of the cosmic shear beyond the smallangle approximation and including general relativistic corrections that are usually suppressed on subHubble scales. The complete expression of the reduced cosmic shear at second order including all relativistic effects was derived in [1]. In the present paper we compute the resulting cosmic shear bispectrum when all these effects are properly taken into account and we compare it to primordial nonGaussianity of the local type. The new general relativistic effects are generically smaller than the standard nonlinear couplings. However, their relative importance increases at small multipoles and for small redshifts of the sources. The dominant effect among these non standard corrections is due to the inhomogeneity of the source redshift. In the squeezed limit, its amplitude can become of the order of the standard couplings when the redshift of the sources is below 0.5. Moreover, while the standard nonlinear couplings depend on the angle between the short and long mode, the relativistic corrections do not and overlap almost totally with local type nonGaussianity. We find that they can contaminate the search for a primordial local signal by f_NL>10.Physical review D: Particles and fields 12/2011; 86(2).  [Show abstract] [Hide abstract]
ABSTRACT: The CMB bispectrum generated by secondorder effects at recombination can be calculated analytically when one of the three modes has a wavelength much longer than the other two and is outside the horizon at recombination. This was pointed out in \cite{Creminelli:2004pv} and here we correct their results. We derive a simple formula for the bispectrum, $f_{NL}^{loc} =  (1/6+ \cos 2 \theta) \cdot (1 1/2 \cdot d \ln (l_S^2 C_{S})/d \ln l_S)$, where $C_S$ is the short scale spectrum and $\theta$ the relative orientation between the long and the short modes. This formula is exact and takes into account all effects at recombination, including recombinationlensing, but neglects all latetime effects such as ISWlensing. The induced bispectrum in the squeezed limit is small and will negligibly contaminate the Planck search for a local primordial signal: this will be biased only by $f_{NL}^{loc}\approx0.4$. The above analytic formula includes the primordial nonGaussianity of any singlefield model. It also represents a consistency check for secondorder Boltzmann codes: we find substantial agreement with the CMBquick code.Journal of Cosmology and Astroparticle Physics 09/2011; 11(11). · 6.04 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We study largescale structure formation in the presence of a quintessence component with zero speed of sound in the framework of Eulerian Perturbation Theory. Due to the absence of pressure gradients, quintessence and dark matter are comoving and can be studied as a unique fluid in terms of the total energy density contrast and the common velocity. In this description the clustering of quintessence enhances the linear term proportional to the velocity divergence in the continuity equation by a factor (1+w) Omega_Q / Omega_m. This is responsible for a rapid evolution of the growth rate at low redshifts, and modifies the standard relation between the velocity divergence and the growth factor. For the total fluid, the solutions for the linear growth function and growth rate can be written in integral forms and admit simple fitting formulae, as in the LambdaCDM case. At second order in perturbation theory, we derive an explicit expression for the kernels F_2 and G_2. They receive modifications of the order of the ratio between quintessence and total energy density perturbations, which affect the corresponding treelevel bispectra. We finally compute the cumulative signaltonoise in the power spectrum, bispectrum and reduced bispectrum, expected for departures from a LambdaCDM cosmology both in the clustering and smooth quintessence scenarios. The reduced bispectrum, in particular, receives sensible modifications only in the clustering case and can potentially be used to detect or rule out the model.Journal of Cosmology and Astroparticle Physics 01/2011; 3(03). · 6.04 Impact Factor
Publication Stats
1k  Citations  
170.67  Total Impact Points  
Top Journals
Institutions

2013

Université ParisSud 11
Orsay, ÎledeFrance, France 
Columbia University
 Institute for Strings, Cosmology, and Astroparticle Physics
New York City, New York, United States


2003–2013

French National Centre for Scientific Research
Lutetia Parisorum, ÎledeFrance, France


2005–2012

Cea Leti
Grenoble, RhôneAlpes, France


2001–2012

University of Geneva
 Department of Theoretical Physics
Genève, Geneva, Switzerland 
University of Oxford
 Department of Physics
Oxford, England, United Kingdom


2004–2007

University of Helsinki
 Department of Physical Sciences
Helsinki, Southern Finland Province, Finland
