Inflation Physics from the CMB and LSS Thursday, July 17, 14 What - PowerPoint PPT Presentation

Leonardo Senatore (Stanford) Inflation Physics from the CMB and LSS Thursday, July 17, 14

What are we seeing? • The only observable we are testing from the background solution is Ω K . 3 ⇥ 10 − 3 • All the rest, comes from the fluctuations • For the fluctuations – they are primordial – they are scale invariant ✓ 1 ◆ n s � 1 ' � 0 . 04 ⇠ O – they have a tilt N e – they are quite gaussian . h ⇣ 3 i h ⇣ 2 i 3 / 2 . 10 � 3 NG ⇠ ✓ – both tensors and scalar • Is this enough to conclude it is slow-roll Inflation? – and in general, what is the dynamics of this inflaton? Thursday, July 17, 14

The general theory of the fluctuations Thursday, July 17, 14

The Effective Field Theory of Inflation (Inflation as the Theory of a Goldstone Boson) with C. Cheung, P. Creminelli, L. Fitzpatrick, J. Kaplan JHEP 2008 Thursday, July 17, 14

The Effective Field Theory of Inflation Inflation: quasi dS phase with a privileged spacial slicing: Inflation: the Theory of the Goldstone Boson of time translations ⇧ ⇥ �⌥ • Analogous of the Chiral Lagrangian for the Pions and W bosons S. Weinberg PRL 17, 1966 • Goldstone boson equivalence principle • Used in WMAP9 and Planck papers (thanks!, but attributed to Weinberg) • Maybe because Weinberg is the true scientific father of all of us? Thursday, July 17, 14

The Effective Field Theory of Inflation Inflation: quasi dS phase with a privileged spacial slicing: Inflation: the Theory of the Goldstone Boson of time translations ⇧ ⇥ �⌥ • Dispersion relations s k 2 + k 4 ! 2 = c 2 M 2 Thursday, July 17, 14

The Effective Field Theory of Inflation Inflation: quasi dS phase with a privileged spacial slicing: Inflation: the Theory of the Goldstone Boson of time translations ⇧ ⇥ �⌥ • Dispersion relations s k 2 + k 4 ! 2 = c 2 M 2 Thursday, July 17, 14

The Effective Field Theory of Inflation Inflation: quasi dS phase with a privileged spacial slicing: Inflation: the Theory of the Goldstone Boson of time translations ⇧ ⇥ �⌥ • Dispersion relations s k 2 + k 4 ! 2 = c 2 M 2 Thursday, July 17, 14

The Effective Field Theory of Inflation Inflation: quasi dS phase with a privileged spacial slicing: Inflation: the Theory of the Goldstone Boson of time translations ⇧ ⇥ �⌥ • Interactions ⇡ 3 , ⇡ ( @ i ⇡ ) 2 , ( @ 2 ⇡ )( @⇡ ) 2 ˙ ˙ • at leading order in derivatives and in fluctuations Thursday, July 17, 14

A lesson from B-modes Thursday, July 17, 14

The amplitude and the tilt • This Lagrangian is fine to make all predictions H 4 h � 2 i ⇠ H 2 • The Amplitude h ⇣ 2 i ⇠ , ˙ M 2 HM 2 Pl c s Pl ˙ ¨ H H c s ˙ n s � 1 = H 2 + + • The tilt ˙ c s H HH Z • No potentials terms ◆ 2 ✓ V 0 V 00 M 2 M 2 , Pl Pl V V . – just symmetry – just how history of a mode depends on time Thursday, July 17, 14

No vacuum sources of B-modes with Silverstein and Zaldarriaga 1109 with Mirbabayi, Silverstein � n and Zaldarriaga in progress • Imagine at each step one produces � n n • Imagine decay to V ( φ ) • In this decay, – gravitational bremsstrahlung is produced φ HM χ ⇢ χ h h 2 i ⇠ M 2 ⇢ total Pl – This can be larger than standard signal – Also scalar are produced and they induce NG Thursday, July 17, 14

Non-Gaussianities • Large non-Gaussianities are possible and technically natural ⇡ 3 , ⇡ ( @ i ⇡ ) 2 , ( @ 2 ⇡ )( @⇡ ) 2 ˙ ˙ – Having these operators large is not in contrast with de Sitter epoch – Demystification of non-Gaussianities (after 25 years!)  Z • NG do not need to be tiny, but just small –Smallness of NG simply corresponds to weakly coupled field theory at E ⇠ H – EFT automatically gives operators and size: π 3 NG ' f NL ζ ⇠ H 2 ˙ c ) • Canonically normalize, and get NG: Example: Λ 2 Λ 2 U U ) »as for dim=6 operators Thursday, July 17, 14

Large non-Gaussianites with Smith and Zaldarriaga, JCAP2010 A function of two variables: like a scattering amplitude There are two templates With this, we could prove inflation Thursday, July 17, 14

Limits in terms of parameters of a Lagrangian •. • These are contour plots of parameters of a fundamental Lagrangian with Smith and Zaldarriaga, JCAP2010 Planck Collaboration 2013 • Same as in particle accelerator Precision Electroweak Tests. • Thanks to the EFT: A qualitatively new (and superior) way to use the cosmological data • Universal limit c s & 0 . 02 Thursday, July 17, 14

Enhanced Symmetries with Behbahani, Mirbabayi, Smith to appear ⌃ ⌃ • Higher derivative opts can be the leading ones ⌃ 1 d 4 x ( � µ � ) 2 + – QFT fact: the following theory is technically natural Λ 4 n ( � n � ) 4 S ⇥ • loops do not generate lower derivative opts. ∂ 4 φ ∂ 4 φ • it could come from integrating out a high spin particle ∂ 4 φ ∂ 4 φ ∂ 4 φ • Apply this logic to the EFT of Inflation – we can start at very high number of derivatives ∂ 4 φ ∂ 4 φ ∂ 4 φ – Many shapes are similar – The first non-trivial ones are at 7- and 9-derivs • and Thursday, July 17, 14

Enhanced Symmetries with Behbahani, Mirbabayi, Smith to appear • Optimal analysis of WMAP9 (could not do Planck) • Results • About 2.5 – we know with Planck goes down,.... wait and see Thursday, July 17, 14

The EFT of Multifield Inflation with Zaldarriaga 1109 • Multifield Inflation offers a plethora of interesting signatures. Multiple fields can be – goldstone bosons • abelian • non-abelian – Susy (introduced in the EFT to study NG for the first time) • unless coupled to inflaton sector, SUSY broken just by • But if BICEP is true?! multiple fields must dominate the signal of fluctuations – Call with – Since • some room left, but not very large • Many signals, analysis in progress Thursday, July 17, 14

Particles in intermediate states with Nacir, Porto, and Zaldarriaga 1109 • Another option is to have particles in intermediate states ˙ π – If they are not observed, but they are light • Several examples � OOO � – effective opts – Conformally coupled sector ˙ ˙ π π with Green, Lewandowski, Silverstein, and Zaldarriaga 1301 – Quasi single field Chen and Wand 0909 • a scalar –protected as a Pseudo Goldstone Senatore in progress Senatore and Zaldarriaga 1109 –protected by SUSY Baumann and Green 1205 Craig and Green 1404 • All this quite unconstrained Thursday, July 17, 14

What has Planck done to theory? • Planck improve limits wrt WMAP by a factor of ~3.  � Z ⇡ 3 ˙ • We can think of Inflation as being characterized by higher dimension opt.s Λ 2 U NG ⇠ H 2 p • Since Λ min , Planck 3 Λ min , WMAP ) ' U U Λ 2 U • Given the absence of known or nearby threshold, this is not much. • Planck is great • but Planck is not good enough – not Plank’s fault, but Nature’s faults • Please complain with Nature • Planck was an opportunity for a detection, not much an opportunity to change the theory in absence of detection • On theory side, little changes – contrary for example to LHC, which was crossing thresholds • Any result from LHC is changing the theory Thursday, July 17, 14

NG and the future • No matter BICEP, non-Gaussianities crucial to increase our understanding • In order to increase our knowledge of interactions in Inflation, we need more modes – Planck will not do it, nor BICEP • Large Scale Structures offer the ideal place for hunting for more modes – I will show results from the EFTofLSS that, if verified and extended to all observable, can increase limits to f equil , orthog , loc . . 1 NL 2 2 – We can argue that absence of detection of NG up to this level implies observational proof of slow-roll inflation • Because every other theory gives larger non-Gaussianities • This is learning even without detection • This also offers us a way to study large scale structures (which are nice) Thursday, July 17, 14

Leonardo Senatore (Stanford) The Effective Field Theory of Cosmological Large Scale Structures Thursday, July 17, 14

What is next? • Plank will increase by a factor of less than 2. • Next are Large Scale Structures • Like moving from LEP to LHC: – much dirtier, but much more potential • How many modes are there? – this is the question Thursday, July 17, 14

The Effective Field Theory of Cosmological Large Scale Structures Bias in the EFTofLSS Senatore alone 1306 with Angulo, Foreman, Schmittful 1306 The one-loop bispectrum in the EFTofLSS see also Baldauf, Mirbabayi, Mercolli,Pajer 1306 The IR-resummed with Zaldarriaga 1304 EFTofLSS The Lagrangian-space with Porto and Zaldarriaga 1311 EFTofLSS The EFTofLSS at 2-loops with Carrasco, Foreman and Green 1310 The 2-loop power spectrum with Carrasco, Foreman and Green 1304 and the IR safe integrand The Effective Theory of Large with Carrasco and Hertzberg JHEP 2012 Scale Structure (EFTofLSS) Cosmological Non-linearities with Baumann, Nicolis and Zaldarriaga JCAP 2012 as an Effective Fluid Thursday, July 17, 14

A well defined perturbation theory • Non-linearities at short scale Thursday, July 17, 14

A well defined perturbation theory • Non-linearities at short scale Thursday, July 17, 14