fingerprinting models of first-order phase transitions by the ......white dwarf bbo gw spectrum ^ f...

Fingerprinting models of first-order phase transitions by the synergy between collider and gravitational-wave experiments

Katsuya Hashino 1

Collaborators: M. Kakizaki 1 , S. Kanemura 1 , P. Ko 2 , T. Matsui 2

　　　 ( 1. University of Toyama, 2. KIAS )

Katsuya Hashino 1, 2

K. H, R. Jinno, M. Kakizaki, S. Kanemura, T. Takahashi and M. Takimoto, arXiv:1809.04994 [hep-ph]

2018/06/28 Touhoku Univ

Collaborators: R. Jinno 3, 4 , M. Kakizaki 1 , S Kanemura 2 , T. Takahashi 5 , M Takimoto 4, 6

(1. Univ. Toyama , 2. Osaka Univ. , 3. IBS, 4. KEK, 5. Saga Univ. , 6. Weizmann Institute of Science)

Introduction

2

❖ Exploring the Higgs sector is important to understand

→

Baryon asymmetry of the Universe (BAU)

❖ Phenomena beyond the SM have been reported.

❖ Electroweak Baryogenesis (EWBG) is a senario explaining BAU.

Sakharov’s conditions → Sphaleron process

→ Extended Higgs sector

→ Strongly first order electroweak phase transition (1st EWPT)

● Baryon number violation

● Departure from equilibrium

● C and CP violation

(φc / Tc ≳1 )

[A. D. Sakharov, Pisma Zh. Eksp. Teor. Fiz. 5, 32 (1967)]

❖ Higgs boson which is predicted in the Standard Model(SM) was detected at the Large Hadron Collider(LHC).

❖ We can realize strongly 1st EWPT by extended Higgs models.

How do we search extended Higgs models?

Collider experiments

❖ We can search the extended Higgs sectors by collider experiments.

3

★ Direct searches of additional Higgs boson

今年の２月と６月にLIGOが直接観測

したと発表

★ Indirect test by the deviation of the SM-like Higgs boson couplings from the SM (hγγ, hWW, hZZ, hbb…)

❖ I mainly use the deviations in the Higgs boson couplings from the SM to test the model by collider experiments. PRL 119, no. 16, 161101 (2017)

For example… The accuracy about the scaling factor of hZZ

about 8% (current data) → 2-4% (HL-LHC) → 0.38% (ILC 250 2000 fb-1)

[“ATLAS and CMS Collaborations” JHEP 1608, 045 (2016), “Working Group Report: Higgs Boson” arXiv:1310.8361 [hep-ex], K. Fujii et al., arXiv:1710.07621 [hep-ex]]

Higgs couplings will be precisely measured.

(h : SM-like Higgs boson)

Spectrum of gravitational waves from 1st EWPT

❖ The bubble nucleation rate per unit volume per unit time:

4

α ≃ Normalized latent heat released by PT, β ≃ 1/(The duration of PT)

(S3 : the three dimensional Euclidean action)

❖ Transition temperature Tt :

❖ The GW spectrum is characterized by α and β :

(The temperature at the end of phase transition)

Sources of GWs : 1.Collision of wall 2.Plasma turbulence 3.Compression wave of plasma

❖ α and β parameters are determined by the effective potential.

　→ Parameters in the model can be fixed by the GW spectrum.

GWs occur by broken the spherical symmetry of babble.

❖ The gravitational waves (GWs) occur from 1st EWPT.

( H : the Hubble parameter)

In this talk

5

❖ We adopt the Fisher matrix analysis to analyze the expected constraints in future space-based interferometers for parameters of the extended Higgs model (the model with a real isospin singlet scalar field).

GWs occur by broken the spherical symmetry of babble.

❖ We quantitatively discuss the testability of real Higgs singlet model by the synergy between the collider and GW experiment.

❖ We discuss what constraints on parameters in the model can be derived when future GW experiments actually give us the data.

many papers have investigated the possibility of detecting GWs from phasetransition at future experiments, most of them perform a relatively simple analysis in whichit is discussed whether the predicted GW spectrum comes above or below the sensitivitycurves.what constraints can be derived when future experiments actually give us the data

The model with a real isospin singlet scalar field ❖ Tree-level potential

❖ Independent parameters

❖ The deviation in the Higgs couplings

,

[K. Fuyuto and E. Senaha, Phys. Rev. D 90, 015015 (2014)]Scanned range

❖ The model can realize strongly 1stOPT.

Detectable GWs from EWPT may be able to occur.

→

GW spectrum in the real Higgs singlet model

7

❖ The scanned range

[C. L. Wainwright, Comput. Phys. Commun. 183, 2006 (2012)]

❖ We obtain φc/Tc ,Tt ,α and by numerical analysis in the space of 2 classical fields.

❖ LISA and DECIGO may be capable of detecting GWs from EWPT.

(We use the public code "CosmoTransitions".)

[K. Fuyuto and E. Senaha, Phys. Rev. D 90, 015015 (2014)]

DECIGO: [Class. Quant. Grav. 28, 094011(2011)]

LISA: [arXiv:1512.06239 [astro-ph.CO]]

The peaks of the GW spectrum

Fisher matrix analysis❖ Fisher matrix analysis is essentially a Gaussian approximation of the likelihood function.

❖ Likelihood function

LISA, White dwarf : [A. Klein et al., Phys. Rev. D93 no. 2, (2016) 024003]

DECIGO, BBO : [K. Yagi and N. Seto, Phys. Rev. D83 (2011) 044011]

❖ Sample point

ΩGW, peak LISA

DECIGO

White dwarfBBO

GW spectrum

^

fGW, peak^

(We assume that we can apply the expression to one detector (LISA).)

The inverse matrix of Fab is the covariance matrix.

1σ contours (LISA)

❖ The expected constraints on the GW spectrum propagate to the parameters in the model.

9

❖ Δλhhh/λhhhSM and detectable GWs are described

in scaling factors (κF and κV) and mH.

,,

Testability of real Higgs singlet model

❖ Fiducial point (mH, κ) = (166.4 GeV, 0.96)

❖ From the current κ, Δλhhh which can be observed by ILC and the GWs from EWPT spectrum might be detected.

10

[The ATLAS and CMS Collaborations, ATLAS-CONF-2015-044.]

Testability of real Higgs singlet model❖ Δλhhh/λhhh

SM and detectable GWs are described in scaling factors (κF and κV) and mH.

,,

ILC : ΔκZ ~ 0.38%

❖ Fiducial point (mH, κ) = (166.4 GeV, 0.96)

❖ We might be able to test the model by the synergy between measurements of the Higgs boson couplings and the spectrum of GW.

[K. Fujii et al., arXiv:1710.07621 [hep-ex]]

[K. H, R. Jinno, M. Kakizaki, S. Kanemura, T. Takahashi and M. Takimoto, arXiv:1809.04994 [hep-ph]]

Direct searches by LHC Run-II : [A. Ilnicka, T. Robens, and T. Stefaniak, Mod. Phys. Lett. A33 no. 10n11, (2018) 1830007]

Summary

11

❖ We may be able to use the gravitational-wave spectrum to explore the form of the Higgs potential.

❖ We might be able to test the models by the measurements of the various Higgs boson couplings at the collider experiments and the spectrum of gravitational wave at the future space-based interferometers.

❖ We have quantitatively discussed this possibility by adopting the Fisher matrix analysis and analyzed the expected constraints in future space-based interferometers for parameters of the extended models.

Backup

12

Gravitational waves interferometers

❖ If electroweak phase transition (EWPT) is 1st order, gravitational waves (GWs) occur from EWPT.

13

★ Ground-based GWs interferometers (LIGO, KAGRA, Advanced Virgo, …)

今年の２月と６月にLIGOが直接観測

したと発表

These experiments can detect GWs from the early universe such as electroweak 1stOPT, and so on.

★ Future space-based GWs interferometers ( LISA, DECIGO, ... )

These experiments can detect GWs from astronomical origin.→

LIGO detected GWs directly.

→

[PRL.116, no. 6,061102(2016), PRL.116, no. 24, 241103(2016), PRL. 118, no. 22, 221101 (2017), PRL. 119, no. 14, 141101 (2017), PRL 119, no. 16, 161101 (2017)]

PRL 119, no. 16, 161101 (2017)

LISA is scheduled to launch into space in 2034.

The model with a real singlet scalar field

❖ Tree-level potential

❖ Diagonalized mass matrix

❖ Independent parameters

❖ Effective potential(T=0) : ci=3/2 (5/6) for scalars and fermions (gauge bosons)

1stOPT in the model mainly occurs the mixing effects at tree-level

In this model, ϕc/Tc > 1 does not have to give a large deviation in the hhh coupling.[A. Ashoorioon and T. Konstandin, JHEP 0907, 086 (2009)]

We take the benchmark point where ϕc/Tc depend on hhh and θ.

There are 2 order parameters.


❖ The benchmark point and scanned range

[K. Fuyuto and E. Senaha, Phys. Rev. D 90, 015015 (2014)]In the benchmark point, ϕc/Tc depend on hhh coupling and θ.

❖ The deviation of 3 point Higgs boson coupling

❖ The model realize strongly 1stOPT.

❖ The scaling factors for Higgs couplings

,

Detectable GWs from electroweak 1stOPT might be able to occur.

→

1stOPT in the model mainly occurs the mixing effects at tree-level

16


[C. L. Wainwright, Comput. Phys. Commun. 183, 2006 (2012)]

❖ We obtain φc/Tc ,Tt ,α and by numerical analysis in the space of 2 classical fields.

[K.H, M.Kakizaki, S.Kanemura, P.Ko and T.Matsui, Phys.Lett.B766(2017)49 ]

❖ LISA and DECIGO might be capable of detecting GWs originated from 1st order EWPT.

(We use the public code "CosmoTransitions".)


In the benchmark point, ϕc/Tc depend on hhh coupling and θ.


17


❖ The condition of strongly 1stOPT is satisfied in the green region.

[K.H, M.Kakizaki, S.Kanemura, P.Ko and T.Matsui, Phys.Lett.B766(2017)49 ]


In the benchmark point, ϕc/Tc depend on hhh coupling and θ.

❖ We show the parameter region where the detectable GW spectrum occur.


❖ From the current κ, Δλhhh which can be observed by ILC and the GWs from EWPT spectrum might be detected.

18

[The ATLAS and CMS Collaborations, ATLAS-CONF-2015-044.]

❖ By the deviation in the hFF and hVV coupling(κ=κF=κV) and additional scalar mass mH, detectable of GWs and the deviation in the hhh coupling(Δλhhh) are described in figure.

❖ The real Higgs singlet model can be verified by combining the measurements of hFF,hVV,hhh coupling and GWs.

,,

[K.H, M.Kakizaki, S.Kanemura, P.Ko and T.Matsui, Phys. Lett. B766 (2017) 49 ]


19

The measurements of the deviations[Snowmass Higgs Working Group Report (1310.8361)]❖ The measurement of κ

[K.Fujii et al., arXiv:1506.05992][S.Dawson et al.,arXiv:1310.8361]❖ The measurement of λhhh

λhhh

HL-LHC 14 TeV 3000fb-1　　ILC 500GeV 4000fb-1　　ILC 1TeV 2000fb-1(5000fb-1)　　　

50% 27% 16% (10%)

%%%%%%

%%

ILC 250GeV

2000fb-1

[ K. Fujii et al., arXiv:1710.07621 [hep-ex]]

20

The measurements of the deviations

[“ATLAS and CMS Collaborations” JHEP 1608, 045 (2016)]

21


Snowmass Higgs Working Group Report (1310.8361)

-

22


K. Fujii et al., arXiv:1710.07621 [hep-ex] (New physics effects)

For example,

23

[G. Aad et al. [ATLAS and CMS Collaborations], JHEP 1608, 045 (2016)]

24 H. Baer et al., arXiv:1306.6352 [hep-ph].

Landau pole

26

We take the same benchmarkpoint as case S2 in [K.Fuyuto, E. Senaha, Phys.Rev.D90 (2014) no.1, 015015]

170 -20

❖ Potential

Running of scalar coupling

❖ Benchmark point

　Constraints

28


❖ Perturbative unitarity

❖ Vacuum stability

❖ Oblique parameters

[S. Baek, P. Ko, W. I. Park and E. Senaha, JHEP 1211, 116 (2012)]

　Direct search

29


[T. Robens and T. Stefaniak, Eur. Phys. J. C 76, no. 5, 268 (2016)]

Allowed region

　Direct search

30


[A. IlnickaT. Robens and T. Stefaniak, arXiv:1803.03594]

Allowed region

Excluded region.

x : VEV for singlet scalar field

The constraint on singlet scalar field HL-LHC

31


[M. Carena, Z. Liu and M. Riembau, Phys. Rev. D 97, 095032 (2018)]

~ -0.15

32



~ -0.15

Allowed region0.989



33



GW spectrum from 1stOPT


34


(S3 : the three dimensional Euclidean action H : the Hubble parameter)




[M. Kamionkowski, A. Kosowsky and M. S. Turner, Phys. Rev. D 49, 2837 (1994)]“Bubble collision(Envelope approximation) n=2, m=2”

,

GW spectrum from 1stOPT


35


(S3 : the three dimensional Euclidean action H : the Hubble parameter)




[M. Kamionkowski, A. Kosowsky and M. S. Turner, Phys. Rev. D 49, 2837 (1994)]“Bubble collision(Envelope approximation) n=2, m=2”

,


36

Phase transition

❖ The bounce solution φb is obtained by equation of motion.

Boundary condition

37

Phase transition❖ The bounce solution φb is obtained by equation of motion.

❖ We can obtain Sb by the bounce solution φb.

(We can obtain Tt by the equation.)→

Boundary condition

38[J.R.Espinosa,T.Konstandin, J.M.No and G. Servant,JCAP 1006,028 (2010)]

fingerprinting models of first-order phase transitions by the ......white dwarf bbo gw spectrum ^ f...

Documents