MSSM in view of PAMELA and Fermi-LAT

Ts. Enkhbat2nd workshop on LHC physics, CYCU, Chungli

Based on: arXiv: 1002.3631B. Bajc, Ts. E, D. K. Ghosh , G. Senjanovic, Y. Zhang

Outline

• Introduction• Decaying gravitino as the MSSM dark matter– Simple case

• Pamela and Fermi-LAT vs MSSM• Phenomenological and cosmological implications• Conclusions

Introduction The MSSM* is the main extension of the SM Virtues of the MSSM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidateIn addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008]

Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006]

*Here we define the MSSM as supersymmetrization of the SM + gravitinoThe last item is the topic of the present talk:The dark matter candidate in light of recent Sattillete experiments:

PAMELA & Fermi-LAT

Sattellite experiments

• Pamela: 1.5 to 100GeV antiproton &positron flux

PAMELA collaboration, arXiv: 0810.4995

Fermi-LAT

Measures electron spectrum from 7GeV to 1TeV

Fermi LAT collaboration, arXiv: 0905.0025, 1008.3999

Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration]

- Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008

Dark Matter - Annihilating DM - Decaying DM• A viable mechanism must induce excess leptons not hadrons.• We address this question in general MSSM

MSSM & decaying gravitino DM

In its most general form, MSSM contains

Constraints : nucleon decay

A. Y. Smirnov & F. Vissani, 1996

: oscillation

S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

uccccc

R LHdduQLdLLeW ''''

2

1

2

1

2~27'''

30010

GeV

ml

2/1~

2~87''

1001001010

GeV

m

GeV

mq nn

Neutrino masses

~

22

2~

2

2~

2'

2~

2

2~

2 ~;

16

3;

16 m

g

m

mm

m

mmm

q

bLRq

l

LRl

(or )dominates : 2/1

2

2~

2/1~3

)100(1.0110

GeV

m

eV

m

TeV

mLRll

dominates : a seesaw mechanism with the gaugino playing the role of the right handed neutrinos.

~

'

The size of the neutrino masses

Large values for RPV couplings

: Neutralinos cannot be DM! sec)1(0~ OLSP

The only viable candidate for DM is the Gravitino!

Gravitino decays

• Relevant gravitino interactions in SUGRA

..242

1chF

iD

Maa

L

Pl

• Effective 2&3-body decay operators

..2

..2

'

296

2~

3

3

2~

2

2~

2

chLPLPeePLPLMm

chWPgBPg

WPg

Mm

mi

L

c

LRR

Pl

eff

body

RRR

Pl

LReff

body

��

e

hadrons

ZW

h

mm

mmm

mm

Mm

mm

22/3

2/3

2/3

,2/3

2/3

0

0

'

/'

,0

0

qq

WZ

h

Mass ranges Gravitino decay modes

Photon & Neutrino mode

m

TeV

GeV

mGeV

M

m

m

m

Pl

1

510

32

13

2/350

2

3

2/3

Takayama & Yamaguchi, 2000

Monochromatic photons and neutrinos

• No such signal observed by Fermi-LAT

• If neutrino mass is dominated by sneutrino VEV

GeV50

2/3 10 or GeVm 52/3

This case cannot explain PAMELA or Fermi-LAT!

2 & 3-body decay rates

2

3

2/3

4~

22~

5

22

2 18432 Pl

LR

M

m

m

mgW

WZW

220

2 cos2

1

WM

mh

W 22

22/30

2 864

2

3

2/3

4~

4

2/3

3

2

3 18432 PlM

m

m

m

2&3-body diagrams• Neutrino channels

• Charged lepton channels

• Higgs channels

• Three-body decay channels

• Criteria to fit neutrino mass and PAMELA and/or Fermi-LAT

4

10/

1010

3.003.0

2

32

49

3

51

GeVGeV

eVmeV (ν mass)

(PAMELA/Fermi-LAT)

(leptophilic DM)

(perturbativity bound)

4/1

51

3

2/5

2/3

4/124

~

49

3

2/12/5

2/3~

10400410

101.0400600

GeVGeV

mTeVm

GeVeV

m

GeV

mTeVm v

3/1

49

3

2/33/124/12

2/32/3

101.0435.05.0

3

GeVeV

m

TeV

m

TeV

m v

• The lower and upper bound on the slepton mass

• The upper limit on the gravitino mass

•An optimal fit for Fermi-LAT }14,5.1,14.0{4

2

for eVmv }3.0,1.0,03.0{

this leaves narrow range for gravitino mass

Allowed region compatible with PAMELA

The dashed line is the perturbativity bound. Blue (red) region is excluded by the gravitino (neutrino) mass.

Allowed region for Fermi-LAT

The dashed line is the perturbativity bound

eVmGeVGeVm v 2.0),103.0sec(103.2,400 50

3

26

2/32/3

• The fit for PAMELA only

•The allowed region in the 2/3~ mm plane (for PAMELA)

eVmGeVTeVm v 03.0),104.1sec(105,3.3 50

3

25

2/32/3

The simultaneous fit for PAMELA positron excess and Fermi-LAT due to 3-body gravitino decay

• Fit for PAMELA

• The fit for Fermi-LAT

eVmGeVTeVm v 03.0),104.1sec(105,3.3 50

3

25

2/32/3

Phenomenological consequences• There is no LHC signatures if both PAMELA and Fermi-LAT are to be explained by gravitino decay:

• Phenomenologically interesting case is if gravitino is behind PAMELA only

Gaugino NLSP:

metersdGeV

m

m

mMg

m

mgv Pl

30,600

sec10

6

3072~

~

5

~7~

2/37

2/3

5~

22

4~

5~

3

2200

for GeVGeVm 50

32/3 103.0,400

Sizable amount decays inside detector.If charged wino is NLSP, leave highly ionized tracks.

Light slepton (with vanishing RPV coupling) as NLSP

2

~~3

~

2/3

7

2/3

~

2~

23

4~

2~

7~

55

24

1

1600sec10

1010

~

01

0

1

00

1

TeV

m

GeV

m

m

m

m

M

mm

mgv Pl

In this case the NLSP decays outside the detector

Light slepton with 7

2/3

5

132

1

400600106

8

GeV

m

GeV

mGeV

m NLSPNLSPNLSP

If charged Displaced vertex /ionizing track, dilepton+If sneutrino 2 charged lepton final states

E

1

Conclusions The MSSM even if taken as the theory of the neutrino masses it explain

PAMELA excess. The sleptons are heavy with masses in the range 500 to 10^6 TeV The gravitino mass can be as light as 300 GeV Phenomenologically there is no constraint on the squark masses The Fermi-LAT data can be explaind only if the gravitino is around 3TeV.

Perturbativity pushes the gravitino to lighter values. The decaying gravitino as the explanation of Fermi-LAT will kill any chance

of MSSM being in the LHC range