Inflationary particle production and non-gaussianity

Transcription

1 December 30th (2018) Inflationary particle production and non-gaussianity Yi-Peng Wu RESearch Center for the Early Universe (RESCEU) The University of Tokyo based on: arxiv[the last day of 2018?] see also Yi Wang, YPW, Jun ichi Yokoyama, Siyi Zhou JCAP (2018)

2 Heavy particles during inflation

3 Standard single-field inflation with Einstein gravity PLANCK (2018) Tensor-to-scalar ratio (r0.002) Convex Concave Primordial tilt (n s ) TT,TE,EE+lowE+lensing TT,TE,EE+lowE+lensing +BK14 TT,TE,EE+lowE+lensing +BK14+BAO Natural inflation Hilltop quartic model attractors Power-law inflation R 2 inflation V 2 V 4/3 V V 2/3 Low scale SB SUSY N =50 N =60 olarization at low and high multipol e n s = ± at 68 % CL. se is found to be consistent with sp No evidence beyond slow-roll (nor feature in the potential).

4 UV completion of single-field inflation m << H

5 UV completion of single-field inflation m H

6 The origin of heavy particles SUSY breaking / SUGRA? Baumann & Green [ ] Yamaguchi [ ] m ~ H heavy-lifted SM particles? Chen, Wang & Xianyu [ ] Kumar & Sundrum [ ] GUT / extra-dim? Kumar & Sundrum [ ]

7 Particle production & non-gaussianity

8 The resonance peaks Particle Data Group 2018 gure 10: Plot of R (e + e! hadrons)/ (e + e! µ + µ ) as a function of the center-of-mas gure adapted from [108]).

9 The Z resonance a slide from Daniel Baumann resonance Cross section (nb) EFT Center-of-mass energy (GeV)

10 The simplest non-gaussian observable h 3 i EFT particle production - k long /k short

11 wave interference The source 1(~r, t) =A 1 (~r)e i[!t 2(~r, t) =A 2 (~r)e i[!t 1(~r)] 2(~r)] The intensity Z I(~r) = dt A A A 1 A 2 cos[ 1 2 ] credit: physics@tutorvista.com = 1 + 2

12 cosmological quantum interference Two sources in de Sitter space (k, ) Ô(k) 3/2 analytic waves (k, ) Ô+ (k) + + Ô (k) analytic + non-analytic waves fixed by isometries of ds: ± = 3 r m 2 ± i 2 9 H 2 4 The correlation function D ˆQ[,,, ] E = (non-oscillatory) + (oscillatory) non-analytic effects

13 The signal of Higgs

14 h Chen, Wang & Xianyu [ ] Chen, Wang & Xianyu [ ] h Kumar & Sundrum [ ] h ) larger f NL

15 Spontaneous symmetry breaking during inflation 4 h4 hhi 6=0 tachyonic mass Kumar & Sundrum [ ] Rh 2 F µ )h 2

16 Heavy-lifting from EFT Kumar & Sundrum [ ] (weak-coupling) L inf-gauge int = c µ (H D µ H)+ c 2 2 (@ )2 H H + c 3 4 (@ )2 DH 2 + c 4 4 (@ )2 Z 2 µ + c 5 5 (@ µ (H D µ H)+ conclusion for non-gaussianity Goldstone EFT Goldstone EFT Slow-roll Models F with 5H with 10H with 60H h Z

17 Heavy-lifting from broken symmetry L h2 2 (@ µ ) (@ µh) 2 H = p h This work

18 Heavy-lifting from broken symmetry Equilibrium state: hhi = ± 0 / p m 2 h = R R =( 2 + h 2 ) 1/2, = /,

19 Heavy-lifting from broken symmetry θ!!! strong-coupling 1 3 2! weak-coupling Λ! Parameter space for the -h system with =0.01. The green area is the flat-dec / < p. The meshed area is incompatible with the Naturalness condition

20 (!"!#$%) scale of heavy Higgs µ h (m 2 h + µ 2 ) 1/2 = m h /c h, Λ " μ!! non-perturbative light Higgs heavy Higgs strong-coupling does not necessarily violate perturbativity.

21 dispersion relations ω + (1) ω + (2) 10 ω - (1) ω - (2) (1) µ h <H 5 (2) µ h >H ω /! ! / "

22 Power spectrum P : Higgs contribution to power spectrum Δ!ζ /! ζ * EoM EFT in-in 0.10 heavy Higgs θ /! two-field inflation quasi-single field inflation c 2 h! 1 c 2 h! 1/3

23 Bispectrum (equilateral limit) k 1 = k 2 = k 3 3 2!!" θ /! *

24 Bispectrum (from equilateral to squeezed) k 1 = k 2 = ck m h 2 = 0.9 m h 2 = m h 2 = 1.5 m h 2 = 2!! "θ / (-! ) 4 3 2!! "θ / (-! ) ! ! shapes beyond single-field inflation

25 Heavy Higgs production h X i Ô i i 10 6 δh - δh δ!! the non-analytic scaling with strong-coupling: r s µ 2 L h! h 9 H 2 4 = m 2 h 9 H 2 c 2 h 4 η See also An et. al [ ] for three-point functions

26 REMARKS and outlook Heavy particle production are encoded as non-analytic momentum scaling in primordial non-gaussianity. SM particles can be observable in non-gaussianity by heavy-lifting. Efficient particle production from spontaneous symmetry breaking and strong-couplings. Challenge for cosmological collider: SM signals or new physics? L h! r µ 2 h H = s m 2 h H 2 c 2 h 9 4

27 contact process m H exchange process m H