WIMPS & Neutrinos

G.G.Ross, Edinburgh, 9th February 2005

What do we know about

?

They exist!

Massive

3 neutrinos

Mixing angles large

Limited room for sterile neutrino – wait for MiniBoone

2 21LSNDm eV

Neutrinos

WIMPS & Neutrinos

What do we know about

?

WIMPS ?

WIMPS & Neutrinos ?

Neutrinos : Majorana or Dirac?

Hierarchical or nearly degenerate?

Inverted hierarchy or normal hierarchy?

Origin of small mass - seesaw?

(Non-Abelian) family symmetry?

mixing lepton # violation?

What we don’t know about

WIMPS & Neutrinos

What we don’t know about

?

Dark Matter : Does it exist? MOND alternative

Milgrom, Beckenstein

- Only visible mattergives structure seen

- Gravitational lensing

- Density perturbations?

WIMPS & Neutrinos

What we don’t know about

?

Dark Matter : Does it exist?

Where is it?

3110

The jury is still out -

Recent study shows one can get

excellent description of our galaxy

with local DM density < 0.3GeV/cm

Basel group astro-ph/0212516,0312461

. .spiral galaxy rotation curves...c f

astro-ph/0403154

CDM successful at large scales (or MOND)

WIMPS & Neutrinos

What we don’t know about

?

Dark Matter : Does it exist?

Where is it?

What is it?

Can we find it?

Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

(WIMPS)

WIMPS & Neutrinos ?

Neutrinos : Majorana or Dirac?

Hierarchical or nearly degenerate?

Inverted hierarchy or normal hierarchy?

Origin of small mass - seesaw?

(Non-Abelian) family symmetry?

mixing lepton # violation?

What we don’t know about

Dirac or Majorana? MajoranaHH

M

0<H > Diracc

If Dirac why is so small?

Propagate in new space dimensions - small due to flux spreading

Right-handed in the bulks

4 ( ) ( ) ( , 0)L Rd x x H x x y

*

/1,2

( ) iny RR nRM

n

x e

* *4.10Planck

HM TeV

M Mm eV

Dirac see-saw

L RR

L

DMH

DD

m HM

R No cosmological problem as

not produced in early universe

2.05 tritium -decaym eV

0.23 anisotropiesm eV CMB

A degenerate spectrum is indicative of a non-Abelian family symmetry

still room …

. . (3) : m i ie g SO Barbieri, Hall, Kane, GGRAntush, King

?u GUTM M

?d lGUTM M

(2) (2) ?L RSU SU(2) (2) ?L RSU SU

Family?Family?

Symmetries Coherent picture of quark and lepton masses and mixing?

DATA :

iu?

1GeV

i id il

1210 910 610 310 310

Masses

Mixing

1 0.218 0.224 0.002 0.005

0.218 0.224 1 0.032 0.048

0.004 0.015 0.03 0.048 1CKMV

0.72 0.89 0.45 0.69 0.2

0.24 0.58 0.39 0.76 0.52 0.84

0.24 0.58 0.39 0.76 0.53 0.84MNSV

2 13 3

1 1 16 3 2

1 1 16 3 2

0

10-1

10-2

10-3

10-4

eV

Bi-Tri Maximal Mixing …

HarrisonScott

Non AbelianStructure?

D

3

8 3 4 3 4

3 4 2 3 2 3

3 4 2 3

Mm

1

a a

a

Vacuum alignment

3

0

0

1

23

0

1

1

2123

1

1

1

Barbieri, Hall, Kane, GGRDe Madeiros, GGR

0 0

3 23

i i

23 123

45 33

SU(

3) SU(2) ..

SU(3) SU(2)

' ..

q , l

i

???

1 i 3 3 2 i 23 23 3 i 123 23 4 i 23 123P= c c c ci i i i

(3), SU(3)SO

D

3

8 3 4 3 4

3 4 2 3 2 3

3 4 2 3

Mm

1

a a

a

Vacuum alignment

3

0

0

1

23

0

1

1

2123

1

1

1

0 0

3 23

i i

23 123

45 33

SU(

3) SU(2) ..

SU(3) SU(2)

' ..

q , l

i

(3), SU(3)SO1

2

3

1 2 3

M

M

M

M

M M

M

M

b e a

1M

TD DM MM M

Neutrinos?

WIMPS & Neutrinos

What we don’t know about

?

Dark Matter : Does it exist?

Where is it?

What is it?

Can we find it?

Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

(WIMPS)

Sterile neutrinos?

Axions?

Standard Model Neutrinos?3

2

1 93

0.07

0.007

imheV

( 2.05 tritium -decay)m eV

( 0.23 anisotropies)m eV CMB

-No SM interactions apart from mixing

- 10 to avoid erasure of structures

m KeV

if thermally produced

What is dark matter?

a-m 0.01eV-18 20-very weakly interacting 10 10 EW

SUSY candidates

gravitinos, axinos – very weakly interacting, massive

With R-parity conservation LSP stable-nature of LSP model dependent

neutralinos, sneutrinos – (<)SM interactions

-32 -18 20 6 3 6 3EW10 , 10 10 ; 10 10 , 10 10EW GeV GeV

-3 10 2 310 10 ; 10 10EW GeV

1

0 0 321 2 03

1

02

0 cos sin sin sin

0 cos cos sin cos

cos sin cos cos 0

sin sin sin cos 0

Z W Z W

Z W Z WN

Z W Z W

Z W Z W

BM M MWM M M

M B W H HM M HM M

H

Neutralino mass matrix

LSP sensitive to parameters

0 1/ 2 2, , , , tan , im m M A CMSSM :

Ellis, Olive, Santoso, Spanos

CMSSM

0c ci i i

Q u Hdm m m m m

3 0c ci i id HQ u

m m m m m

3 3(1 0.2)Q Qim m

3 family symmetry brea king

Ramage,GGR

KK state For some compactifications LKP stable2

2 2. . / , /e g T Z S Z

For low scale of compactification LKP can make up dark matter :

1. . in SM with all states propagating in bulk can be LKPB e g

1

2

0.6v

( )B

pb

m TeV

1400: 1200Bm eVDM G

Wimpzilla 34DMm GeV v at unitarity bound and initial thermal abundance

1010DMm GeV non thermal production (e.g. gravitational)

Can we find WIMPS?

Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

Can we find WIMPS?

Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

Very low scattering cross sections

Can we find WIMPS?

Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

Neutralino interactions exhaustively studied

Ellis, Olive, Santoso, Spanos

CMSSM : Neutralino searches

spin independentN N contours

, 445 6MeV MeV

Ellis, Olive, Santoso, Spanos

CDMS II excluded

Kaluza Klein searches

1

2

0.6v

( )B

pb

m TeV not visible by current searches

Annihilation products ; .. 60%e e

.. 4%qq .. 35%

. . Neutralino de bcay to b, ...c f

Look for galactic annihilation production of , e

Signals could be visible if galactic cusps exist

– for LKP sharp cutoff on positron energy

WIMPS & Neutrinos ?

Neutrinos : Majorana or Dirac?

Hierarchical or nearly degenerate?

Inverted hierarchy or normal hierarchy?

Origin of small mass - seesaw?

(Non-Abelian) family symmetry?

mixing lepton # viola ? tion

What we could know about SUMMARY

?

?

Wimps Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

Indirect detection

Direct detection possible

Hierarchy : spontaneously broken family symm y etr

n

L RH M

spatial separ n atio

Yijk hqu n H2

DM , a a,ijk

dn e

Aijk n

2 e 2 i ijkn. #

Froggatt-Nielsen mixing

3 ( )R n R R

, structurequark leptonM M

, (specific string calc ulations + IRFP OK ) t bh gThird generation heavy

(?) b th h h (not expected to be precise with Wilson line break ing)

0.2

4 3 3

2

23

2

2

1

d

b

M

m

( , 0 0)dm S Q

0 0

( )

S Q

A

( )

CP

A

?Gauge mediat

S GRA

ion

U

Vives, GGR

( , )..

i j ci j aMP Q q H

Cannot align Yukawa and A terms

(3 ( , )) *c c

ij ij a ij ai j i jA Y Q q H i j P Y Q q H

, structurequark leptonM M

Similar structure for charged leptons Neutrino mixing not related to large RH mixing

WIMPS & Neutrinos ?

Neutrinos : Majorana or Dirac?

Hierarchical or nearly degenerate?

Inverted hierarchy or normal hierarchy?

Origin of small mass - seesaw?

(Non-Abelian) family symmetry?

mixing lepton # viola ? tion

What we could know about SUMMARY

?

?

Wimps Sterile neutrinos?

Little Higgs candidate?

Axions?

SUSY – neutralinos, sneutrinos, gravitinos, axinos

KK state?

Wimpzilla?

Cryptons,…

Indirect detection

Direct detection possible

CMSSM10 16/ 1.25, 0m m D

10 16/ 0, 0.4m m D Ramage, GGR

1

2

2 2 2 216 10, ,

2 2 2 216 10,

2 2 2 216 10

2 2 2 210 10

2 2 2 210 10

3

2

2

R R

R

R

Q u e

d L

e

H

H

m m g D

m m g D

m m g D

m m g D

m m g D

SO(10)