Fuminobu Takahashi- Dark Matter

8/3/2019 Fuminobu Takahashi- Dark Matter

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Plan of talk

I. Dark matter and cosmic-rays

II. Affleck-Dine baryogenesisIII. Non-Gaussianity (if time allows)


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How can we know the presenceof dark matter?


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Gravity

It's not just a good idea.It's the law!


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lensingrotation curve CMB

Bullet cluster

+ large scale structures.


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(taken from WMAP webpage)

DM 0.2

The presence of DM hasbeen firmly established.

CMB observation

Rotation curvesStructure formation

Big bang nucleosynthesis


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(G. Bertone at COSMO-09)


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Must be electrically neutral, long-lived and cold.

e.g.) , gravitino, etc. (right-handed sneutrino, axino).

Little Higgs, UED, etc.

No DM candidates in SM.

LSP is long-lived if R-parity is a good symmetry.

The lightest T-parity/KK-parity particles

Others Q-ball, saxion, light moduli, sterile nu, etc...

Many


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Thermal relic abundance of WIMPs of massO(100)GeV - O(1)TeV is close to the observed

DM density.

WIMP =0.3

v /(pb)

Sounds reasonable, but it is betterkeep in mind other possibilities.

vthermal 3 1026

cm3

/sec


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Collider

Direct detection

Indirect search:annihilation/decay of dark matter

(http://pamela.roma2.infn.it/index.php)


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So, what is cosmic-rays?


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Cosmic-ray was discovered in 1912 by

Victor Hess using the balloon experiment.


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Total cosmic-ray spectrum

Main components:proton (+ alpha)

Electron: 1-0.1%

Positron: 0.1-0.01%Antiproton: 0.01%

Heavier nuclei: 1-0.1 %


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In particular, 1TeV electron/positron loses its most

of the energy in 105yrs, traveling about 1kpc.

The cosmic-ray particles diffuse in our Galaxy.

8.5kpc 1 pc = 3.26 lyr= 3x1016 m


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2. PAMELA, ATIC/PPB-BETS,

Fermi, and H.E.S.S. results


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Adriani et al,arXiv:0810.4995

Primary source?

naively expected b.g.

E-3.0

ATIC excess was not

confirmed by Fermi.


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Pulsars

Modification in propagation oracceleration/production in local SNR

Dark Matter decay/annihilation


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3. Dark Matter


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Energy

Flux Annihilation/decay mode

DM mass

Cross-sectionlifetime


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In particular, 1TeV electron/positron loses its most

of the energy in 105yrs, traveling about 1kpc.

The cosmic-ray particles diffuse in our Galaxy.

8.5kpc 1 pc = 3.26 lyr= 3x1016 m


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NFWAnnihilation

Meade et al, arXiv:0905.0480


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NFWDecay

Meade et al, arXiv:0905.0480


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Monochromatic electron production gives apoor fit to the Fermi data. (Good for ATIC)

Softer spectrum, e.g. (mu, tau) production isfavored by Fermi.

DM annihilation scenario is disfavored.

DM decay scenario can satisfy the

observational constraints.

DM mass must be in the TeV scale!


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Decaying DM scenario

Mass: a few TeV (or heavier)

Lifetime:

Dark matter particle with

The longevity of DM may be a puzzle,

especially if the mass is above 1TeV.

10

26

sec

Insensitive to the clumpy structure.


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Shirai, FT, Yanagida, arXiv:0905.0388Phys.Lett.B680:485-488,2009.


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The neutralino LSP scenario is interesting,

because thermal relic production can naturallyexplain the DM abundance.

The lightest neutralino is Bino-, Higgsino-,

or Wino-like, or a certain mixture of those.

Let us focus on the scenario,

which is realized in anomaly-mediation.


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Hisano et al (`07)

mW (2.7 3) TeV


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The must be a good

symmetry for the Wino LSP to

account for the observed DM.

Is the R-parity an symmetry

or just an one?


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The constant term breaks a continuous U(1)Rsymmetry down to the .

W C0 = m3/2M2

P

In order to have a (almost) vanishing cosmological

constant, the superpotential must have a constantterm:


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However, a continuous U(1)R may not be

the symmetry of the theory at highenergies.

If the R symmetry in the high energy isa , the R parityis broken by C0.


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In addition to the SM Yukawa interactions, the

following operator is allowed by the symmetry.

W = ijk

(C0)2eiLjLk,

and similar terms for quark multiplets.

2x2+1+1+1 = 7 2 (mod 5)

O(1)w/

In our model the Wino DM of mass 3TeV is not


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In our model, the Wino DM of mass 3TeV is notabsolutely stable, and decays through the R-parity

violating operator, eLL.

e.g.)

1027

sec1

2 m3/2

103 TeV4

mfW03 TeV

5

m5 TeV

4

,

N t th t b th th Wi d th i f th R


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Wino mass

(=3TeV)

R-parity

violation

Gravitino mass(= 103TeV)

The overall scale is determined by the thermal relic abundance.

A

nomaly

mediation dis

crete

Z5

R-sym.

MW0 g22

162m3/2 W

1

M2Pm23/2eLL

Note that both the Wino mass and the size of the R-parity violation are determined by the gravitino mass.

Electron + Positron flux:


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Electron + Positron flux:

Propagation through the galactic magnetic field is described

by a diffusion equation

electron/positron

fet = K(E)

2

fe(E, x) +

E[b(E)fe(E, x)] + Q(E, x)

diffusion energy loss source

Dark Matter

Mass &

Decay rate

The Wino DM decay may account for the observed


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y y

PAMELA/Fermi excesses in the CR e-+e+.

I: e1L2L3, II: e2L2L3, III: e3L2L3


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C-R.Chen, S. Mandal, FT, arXiv:0910.2639

1024

1025

1026

[sec]

1027

103 10

410

2

Fermi (b=10-20)

HESS GC

Fermi (iso)

+ -

[GeV]mDM

1024

1025

1026

[sec]

1027

103 10

410

2

Fermi (b=10-20)

HESS GC

Fermi (iso)

+ -

[GeV]mDM

Although the decay mode is slightly different from thesetwo, it should be still allowed by the latest Fermi data.


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...yet another

coincidence??

New inflation model with Z5 R-symmetry


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New inflation model with Z5 R symmetryIzawa and Yanagida ,`97

Consistent with the discrete Z5 R-symmetry.

V

K(, ) = ||2 + k4||4,

W() = v2g

6

6.

R[] = 2 R[6] = 12 2 (mod 5)

V() v4 k

2v42

g

2

5

21

v25 +g2

2510

(v2

/g)1/5

Inflaton acquires non-vanishing VEV:


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m3/2 = W(0) 5v2

6

v2

g

15

The gravitino mass is related to the inflaton

parameters!

O(106)GeV g = O(1)for

The WMAP normalization = 10-5

is imposed.


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It is likely that the and found anexcess in the CR positrons/electrons.

If so, we need to modify the conventional model

of CR electron/positron. The possible sources are

In the case of DM, other observational channels,especially , could refute/support thescenario.


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The of mass 3TeV can

explain the observed PAMELA/Fermi anomalies inthis framework.

We have proposed a model based on thein which R-parity is broken by

the constant term in W (= gravitino mass).

The model based on Z5 R symmetrycan give rise to the gravitino mass of 103TeV.


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Focus week on ``Indirect DM search7-11 Dec. 2009 at IPMU

Invited speakers include: Marco Casolino (INFN, University of Rome Tor Vergata) Paolo Gondolo (University of Utah)

Kouichi Hirotani (National Tsing Hua University) Masahiro Hoshino (University of Tokyo) Dan Hooper (FNAL) Alejandro Ibarra (Technische Universitat Munchen) Tesla Jeltema (UCO/Lick Observatories)

Philipp Mertsch (Oxford) Igor Moskalenko (Stanford University)* Stefano Profumo (UCSC) Surjeet Rajendran (MIT) Pasquale Serpico (CERN)

Shoji Torii (Waseda University) Carsten Rott (Ohio State University)

Organizers:Dan HooperStefano Profumo

Fuminobu Takahashi


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Fuminobu Takahashi- Dark Matter