What do we know about
WIMPS & Neutrinos ?
G.G.Ross, Edinburgh, 9th February 2005
Neutrinos
They exist!
Massive
Mixing angles large
 3 neutrinos
 mLSND 2 1eV 2
Limited room for sterile neutrino – wait for MiniBoone
What do we know about
WIMPS & Neutrinos ?
WIMPS ?
What we don’t know about
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 ?
Dark Matter :
Does it exist?
MOND alternative
- Only visible matter
gives structure seen
- Gravitational lensing
- Density perturbations?
Milgrom, Beckenstein
What we don’t know about
WIMPS & Neutrinos ?
Dark Matter :
Does it exist?
Where is it?
The jury is still out Recent study shows one can get
excellent description of our galaxy
with local DM density < 101 0.3GeV/cm3
Basel group astro-ph/0212516,0312461
c. f .spiral galaxy rotation curves...
astro-ph/0403154
CDM successful at large scales (or MOND)
What we don’t know about
WIMPS & Neutrinos ?
Dark Matter :
(WIMPS)
Does it exist?
Where is it?
What is it?
Sterile neutrinos?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos,
axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Cryptons,…
Can we find it?
What we don’t know about
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?
 HH
Dirac or Majorana?
Majorana
M
 c <H0 >
Dirac
No cosmological problem as  R
If Dirac why is  so small?
not produced in early universe
 Propagate in new space dimensions -  small due to flux spreading

Right-handed  s in the bulk
n
1
2 RM *
 R, n ( x) einy / R
  d 4 x  L ( x) H ( x) R ( x, y  0)
m 
  H  M*
M Planck
 .10 eV
4
 Dirac see-saw
mD  H 
 
MD
L

MD
H
R
 
M*
TeV
L
R
m  2.05eV tritium  -decay
m  0.23eV CMB anisotropies
still room …
A degenerate spectrum is indicative of a non-Abelian family symmetry
e.g. SO(3) : m i i
Barbieri, Hall, Kane, GGR
Antush, King
Symmetries
Coherent picture of quark and lepton masses and mixing?
Family?
M
u
 M
GUT ?
SU (2)L  SU (2)R ?
Family?

SU (2)L  SU (2)R ?
M
d
 M
GUT ?
l
DATA :
Masses
? 

10 12

i
109
106

103
  li
  di



1
ui
103
GeV
Mixing
VCKM
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

1


10-1
10-2
10-3
10-4
eV


 



2
3
1
3
1
6
1
3
1
6
1
3
VMNS
 0.2 
 0.72  0.89 0.45  0.69


  0.24  0.58 0.39  0.76 0.52  0.84 
 0.24  0.58 0.39  0.76 0.53  0.84 


0  Bi-Tri Maximal

1
 2  Mixing …

1 
Non Abelian
2 
Structure?
Harrison
Scott
SO(3), SU(3)
Vacuum alignment
3
23
q i , li
SU(3)  SU(2)  ..
i
450
330
SU(3)  SU(2)'  ..
23

???
123
123
MD
m3
 8

  3   4
 3  4

1
 
  1  2
 1
 
3  4 3  4 

a 2   3 a 2   3 
a 2   3
1 
0
23   1  
1
 
Barbieri, Hall, Kane, GGR
De Madeiros, GGR
0
3   0 
1
 
P=1  i3 ic3  2  i23 ic23  3  i123 ic23  4  i23 ic123
SO(3), SU(3)
Vacuum alignment
MM
3
23
q i , li
SU(3)  SU(2)  ..
i
450
330
SU(3)  SU(2)'  ..
23
123

123

MD
m3
 8

  3   4
 3  4

1
 
  1  2
 1
 
3  4 3  4 

a 2   3 a 2   3 
a 2   3
1 
0
23   1  
1
 
 M1




M 1  M 2  M 3
0
3   0 
1
 
Neutrinos?
M  M D M M1 M DT
M2



M 3 
a
   
b
      e
What we don’t know about
WIMPS & Neutrinos ?
Dark Matter :
(WIMPS)
Does it exist?
Where is it?
What is it?
Sterile neutrinos?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos,
axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Cryptons,…
Can we find it?
What is dark matter?
3
Standard Model Neutrinos?
Sterile neutrinos?
mi
1 93eV
 0.07
(m  2.05eV tritium  -decay)
 0.007
(m  0.23eV CMB anisotropies)
 h  
2
-No SM interactions apart from mixing
-m s  10 KeV to avoid erasure of structure
if thermally produced
Axions?
-ma  0.01eV
-very weakly interacting 10-18  1020  EW
SUSY candidates
With R-parity conservation LSP stable
-nature of LSP model dependent
gravitinos, axinos – very weakly interacting, massive
10-32 EW , 10-18  1020  EW ; 106  103 GeV , 10 6  103 GeV
neutralinos, sneutrinos – (<)SM interactions
10-3  1010  EW ;
102  103 GeV
Neutralino mass matrix

M N  B W3
0
H1
0
H2

M1


0

  M Z cos  sin W

 M Z sin  sin W
0
M2
 M Z cos  sin W
M Z cos  cos W
M Z cos  cos W
0
 M Z sin  cos W

LSP sensitive to parameters
CMSSM :
m0 , m1/ 2 ,  , M 2 , tan  , Ai
M Z sin  sin W   B 

 M Z sin  cos W   W3 


  H 10 

 

0
  H 02 


CMSSM
Ellis, Olive, Santoso, Spanos
mQi  muc  md c  mH  m0
i
i
mQi3  muc  md c  mH  m0
i
i
mQ3  mQi 3 (1  0.2)
3 family symmetry breaking
Ramage,GGR
KK state
For some compactifications LKP stable
e.g . T 2 / Z 2 , S / Z 2
For low scale of compactification LKP can make up dark matter :
e.g. in SM with all states propagating in bulk B1 can be LKP
v 
Wimpzilla
0.6 pb
mB21 (TeV )
DM : mB1  400 1200GeV
mDM  34GeV
 v at unitarity bound and initial thermal abundance
mDM  1010 GeV
non thermal production (e.g. gravitational)
Can we find WIMPS?
Sterile neutrinos?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos,
axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Cryptons,…
Can we find WIMPS?
Sterile neutrinos?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos,
axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Cryptons,…
Very low scattering cross sections
Can we find WIMPS?
Sterile neutrinos?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos,
axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Cryptons,…
Neutralino interactions exhaustively studied
CMSSM : Neutralino searches
  45MeV , 64MeV
independent
 spin
contours
N  N
Ellis, Olive, Santoso, Spanos
CDMS II excluded
Ellis, Olive, Santoso, Spanos
Kaluza Klein searches
v 
0.6 pb
mB21 (TeV )
Annihilation products ;
not visible by current searches
e e .. 60%
 .. 4%
qq ..
35%
c. f . Neutralino decay to bb,  ...
Look for galactic annihilation production of
 , e
Signals could be visible if galactic cusps exist
– for LKP sharp cutoff on positron energy
SUMMARY
What we could know about
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?
Wimps
Sterile neutrinos?


Indirect detection
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Direct detection possible
Cryptons,…
M quark , M lepton structure

Third generation heavy
hb  h  (?)ht

Hierarchy :
ht ,b
g
OK
(specific string calculations + IRFP)
(not expected to be precise with Wilson line breaking)
 spontaneously broken family symmetry
0.2
  
 L R H 

M 
n
 spatial separation
Yijk h qu


A ijk 
n
d n e
H D
n
M ,a a ,ijk
2

2

e 2 iijk n . #
Froggatt-Nielsen mixing
3R  n( R  R )
M quark , M lepton structure
P   M 
 (i , j )
Cannot align Yukawa and A terms
Qi q cj H a  ..
c
c
Aij Yij Qi q j H a  (3   (i, j ))  P*  Yij Qi q j H a
( md , S  0 Q  0)
Md
mb
 4

  3
 2

S  0 Q  0
( A )
Similar structure for charged leptons
3
2
2
CP
( A )
 3 

2



1 
SUGRA
Gauge mediation ?
Vives, GGR
Neutrino mixing not related to large RH mixing
SUMMARY
What we could know about
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?
Wimps
Sterile neutrinos?


Indirect detection
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
Little Higgs candidate?
KK state?
Wimpzilla?
Direct detection possible
Cryptons,…
CMSSM
m10 / m16  1.25, D  0
mQ ,u
2
R , eR
 m16 2  g10 2 D 2
md R , L 2  m16 2  3 g10 2 D 2
SO(10)
meR 2  m16 2  g10 2 D 2
mH1 2  m10 2  2 g10 2 D 2
mH 2 2  m10 2  2 g10 2 D 2
m10 / m16  0, D  0.4
Ramage, GGR