Higgs inflation after the BICEP2 & Planck results. Seong Chan Park (SKKU & KIAS)

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1 Higgs inflation after the BICEP2 & Planck results Seong Chan Park (SKKU & KIAS) The 4th KIAS workshop on Particle Physics and Cosmology, Oct Refs 1. Higgs inflation is still alive by Yuta Hamada, Hikaru Kawai, Kin-ya Oda, and SCP, Phys. Rev. Lett (2014) arxiv: Higgs inflation from Standard Model criticality by the same authors arxiv: for full analysis

2 Disclaimer note After excellent talks on the related topics in the morning session, I may add a little more information. However, I found it always pleasure to hear something that I already know about. So I hope you enjoy my talk, too. Also, I would describe what I could see as a particle phenomenologist which may be useful for some people in audience. Disclaimer note 2 I assume: SM is good to Planck scale, which is unlikely. But, as long as corrections are by weak (gauge) interactions or higher loops, their effects are subdominant anyway. Higher order operators are suppressed even though some non-zero contribution (~10-9 ) actually helps to fit the running of spectral index.

3 A key message today We may learn about LHC physics from cosmological data in Higgs inflation! Higgs inflation An economical and predictive idea : Higgs=Inflaton at low scale (~100 GeV) responsible for EWSB at high scale (~10 17 GeV) responsible for cosmic inflation See Bezrukov s talk

4 Higgs potential e.g., precise measurement of top quark mass may be achievable in Higgs inflation This is not a small thing!

Current top quark mass measurement CMS PAS TOP-14-001 NEW July!2014! [CMS!PAS!TOP-14-002] Mt=175->173->172 Error remains still big~gev To reduce the error, one should have better understanding of MC mass but this is tough in LHC!

5 Current top quark mass measurement CMS PAS TOP NEW July!2014! [CMS!PAS!TOP ] Mt=175->173->172 Error remains still big~gev To reduce the error, one should have better understanding of MC mass but this is tough in LHC! ILC scan around 350 GeV allows Mt=100 MeV Higgs in the SM A scalar field (s=0) (2,1/2) of : doublet Tachyonic, develops non-zero VEV two free parameters in the general renormalizable action

6 Higgs in the SM W-mass and gauge coupling measurement or equivalently G F : from the LHC! are experimentally measured! Current status of Higgs mass measurement

7 Decay pattern is consistent with the SM! The Higgs in the SM plays two main roles: EWSB (or gauge boson masses) and fermion masses. Both have been experimentally checked! Yuta Takahashi s

Inflation solves problem Era of inflation space inflates > e 60 our patch time space Inflation is exponential expanding stage of Universe in an early era gives chance to have causal connection in our

8 Inflation solves problem Era of inflation space inflates > e 60 our patch time space Inflation is exponential expanding stage of Universe in an early era gives chance to have causal connection in our patch of universe Then, homogeneity, isotropy and no observation of monopole, domain wall etc are explained. also provides seed for structure formation provided. In particle physics, inflation takes place due to a scalar particle slow-roll conditions N.B. This guy is scalar or a composite state with s=0. Q. WHY? (ex)

9 Higgs vs Inflaton Higgs Chaotic Inflation look very different But! The Higgs potential becomes flat at high scale by RGE! The SM Higgs quartic coupling

10 2-loop effective potential arxiv: criticality [Hamada, Kawai, Oda, SCP, PRL 2014] Criticality of the SM +loop [Hamada, Kawai, Oda, SCP, , PRL], [Bezrukov, Shaposhinikov, ]

11 % of woman science major Criticality of the SM [Hamada, Kawai, Oda, SCP, PRL 2014] Plateau! This helps. But, not enough for 60 efoldings. +loop

12 Another source of flatness : non-minimal coupling Generically allowed in SUGRA. In effective theory, this term should be included as long as Inflation by non-minimal couplings [SCP, S.Yamaguchi (2008)] (ex) monomial Thus, as long as V/K 2 is asymptotically flat, the slow-roll inflation can take place!

13 An interesting topic for model building (ex) monomial m=2 Higgs Inflation [Bezrukov,Shaposhinikov (2008)] COBE normalization: (hard to swallow )

14 At low scale, Higgs potential with/without non-minimal coupling term look just same. GeV consistent with the low energy measurements! At high scale, the potential becomes flat with NMC: minimal non-minimal good for inflation!

15 Two (and more) cosmological observables Scalar spectral Index Tensor-to-scalar ratio scale invariance how fast? ( also running spectral index, Non-Gaussianity etc ) Tensor-to-scalar ratio is seen in B-mode polarization in CMBR

16 Any massless field experiences quantum fluctuations during inflation: gravitational field too.

18 There are two polarization modes of a gravitational wave:

20 Helmholtz theorem curl-free divergence free Not surprising!

21 BICEP2 w/o foreground noise r~how fast the inflaton moves ~the slope in potential

-Foreground dust must be better understood! 1405.

22 -Foreground dust must be better understood! by Faluger, Hill and Spergel Also, astro-5 sigmas often disappear (rate~50%)

Planck showed that the power spectrum indicates that the uncertainty is comparable in magnitude to the BICEP2 measurements at these multipoles. arxiv:1409.5738 Planck intermediate results. XXX.

23 Planck showed that the power spectrum indicates that the uncertainty is comparable in magnitude to the BICEP2 measurements at these multipoles. arxiv: Planck intermediate results. XXX. Assessing the dust contribution to the B-mode power measured by the BICEP2 experiment requires a dedicated joint analysis with Planck, incorporating all pertinent observational details of the two data sets, such as masking, filtering, and color corrections. (Further analysis is needed to rule out any sign of B-Mode observation by BICEP2.) W/O RGE [SCP, S.Yamaguchi (2008)] n is around r is expected to be small ~0.003!

24 Higgs Inflation w/o RGE =R 2 inflation Higgs inflation=r 2 inflation Higgs [COBE] R2

25 w/ RGE larger NM coupling [Hamada, Kawai, Oda, SCP, PRL 2014] Higgs inflation w/ RGE, criticality

26 higher order terms negative running M t in Higgs Inflation

summary BICEP + Planck, if confirmed, fantastic!! If not, we will learn more about dust any way. Higgs may play a role of inflaton and Higgs inflation is compatible with data: n=0.967 and r=0.

27 summary BICEP + Planck, if confirmed, fantastic!! If not, we will learn more about dust any way. Higgs may play a role of inflaton and Higgs inflation is compatible with data: n=0.967 and r=0.003 or ~0.1 wo/w criticality. (greater possibility is open for Higgs inflation with criticality) With criticality (r~0.1), Mt may be (best) measured by cosmological data! PLANCK and BICEP upgrades(bicep3, KECK array) result will tell us more. Let s stay tuned. Thank you!

From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology

From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology Yi-Fu Cai June 18, 2013 in Hefei CYF, Chang, Chen, Easson & Qiu, 1304.6938 Two Standard Models Cosmology CMB: Cobe (1989), WMAP (2001),