Large extra dimensions Randall-Sundrum Supersymmetry Z - PowerPoint PPT Presentation

송희성 선생님과 공동연구 Large extra dimensions Randall-Sundrum Supersymmetry Z’ Radion Graviton 𝞯 ’/ 𝞯 in LR-model (g-2) Spin correlation rotating black holes

송희성 선생님과 공동 연구 (1999-2001)

3 Higgs as Inflaton 박성찬 ( 연세대 ) 고 송희성 교수님 추모 심포지움 2017.4.13.

Cut-off scale of the SM

Cut-off scale of the SM • In principle, we can ‘calculate’ everything E< 𝝡 SM with unlimited precision.

Cut-off scale of the SM • In principle, we can ‘calculate’ everything E< 𝝡 SM with unlimited precision. • 𝝡 SM > TeV, LHC

Cut-off scale of the SM • In principle, we can ‘calculate’ everything E< 𝝡 SM with unlimited precision. • 𝝡 SM > TeV, LHC • 𝝡 SM ~ M planck , in principle as the SM is renormalizable

Cut-off scale of the SM • In principle, we can ‘calculate’ everything E< 𝝡 SM with unlimited precision. • 𝝡 SM > TeV, LHC • 𝝡 SM ~ M planck , in principle as the SM is renormalizable • We may extrapolate all the way up to the Planck energy and see what would happen there.

dim>4 dim=4 Higgs + Gravity � 2 | H | 2 − v 2 / 2 � V ( H ) = λ  M 2 P + ξ | H | 2 � Z d 4 x √ g R + | DH | 2 − V ( H ) + L SM S = 2 O 4+ n X + M n Planck n =1

Higgs=R 2

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S =

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0 φ 2 = ξ -> 2 λ R

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0 φ 2 = ξ -> 2 λ R

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0 φ 2 = ξ -> 2 λ R R + ξ 2 ✓ ◆ Z 4 λ R 2 + · · · d 4 x √ g S =

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0 φ 2 = ξ -> 2 λ R Starobinski (R 2 ) inflation R + ξ 2 ✓ ◆ Z 4 λ R 2 + · · · d 4 x √ g S = α = ξ 2 4 λ

Higgs=R 2 Z d 4 x √ g (1 + ξφ 2 ) R + ( ∂φ ) 2 − λφ 4 � � S = **During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field. δφ : 2 ξφ R − 4 λφ 3 = 0 φ 2 = ξ -> 2 λ R Starobinski (R 2 ) inflation R + ξ 2 ✓ ◆ Z 4 λ R 2 + · · · d 4 x √ g S = α = ξ 2 4 λ

The Higgs potential in Einstein frame

The Higgs potential in Einstein frame inflation here

The Higgs potential in Einstein frame inflation here

The Higgs potential in Einstein frame inflation here 8 × 10 8 6 × 10 8 4 × 10 8 2 × 10 8 50 100 150 200 250 300 350 EWSB here

Planck [Astron.Astrophys. 594 (2016)] Higgs inflation provides very good fit to the data!

RG running of lambda self int. gauge int. This dominates over other interactions.

MC mass vs pole mass

criticality 2-loop effective coupling S. Moch, et al.,MITP report [1405.4781] Hamada, Kawai, Oda, SCP [PRL 2014, PRD2015]

M t & M H from Higgs inflation Hamada, Kawai, Oda, SCP, [PRD(2015)] Hamada, Kawai, Oda, SCP [PRL(2014)] n o i t a l f n I s g g i H check with full EWPT & Gfitter S. Heinemeyer, R. Kogler, SCP in progress

Potential Synergy Cosmological observation especially primordial gravitational wave = Precision particle physics experiments e.g. top quark mass