(Neutrino indirect) detection of neutralino dark matter in (non) universals SUSY GUT models

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Submitted on 20 Feb 2003

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(Neutrino indirect) detection of neutralino dark matter

in (non) universals SUSY GUT models

E. Nezri

To cite this version:

(Neutrino Indirect) Detection of Neutralino Dark Matter in

(non-)Universals SUSY GUT Models.

Emmanuel Nezri

Laboratoire de Physique Corpusculaire de Clermont-Ferrand : Theory

Centre de Physique des Particules de Marseille : Antares

⇒ V.Bertin, E.N., J.Orloff, non-Universal models, hep-ph/0210034

⇒ V.Bertin, E.N., J.Orloff, hep-ph/0204135 accepted in EPJ C (mSugra)

see also: J.L.Feng, K.T. Matchev, F. Wilczek, PRD63(01)040524

V. Barger, F. Halzen, D. Hooper, C. Kao, PRD65(02)075022

and: L. Bergström, J. Edsjö, P. Gondolo; PRD58(98)103519

Contents

Detecting cold dark matter (WIMPS) in neutrino telescopes

mSugra summary

DM indirect detection with a neutrino telescope: ingredients

? A colddark matter canditate: choose χ, lightest neutralino in Constrained MSSM

? A relic density: depends on (co-)annihilation processes σA

? A cosmic storage ring: to re-start annihilation, need to concentrate nχ; halo, clumps? too small forν’s! Need

big, nearby, heavy body with large capture rate (C) _⇒ depends on σ_χpel . Sun: OK! Earth: small.

? χ = Majorana fermion: can self-annihilate, limiting the total population Nχ:

˙

Nχ = C − CAN_χ2

Annihilation rate: ΓA = 1₂CAN_χ2 = C₂ tanh2√CCAt eq

∼ C2 can be insensitive to σA

? among decay products χχ _{→ b¯b, t¯}t, W W, ZZ, . . . _{→ ν + · · ·}, onlyν’s can escape the sun and reach a

detector. Φ(Eν) depends on dominant annihilation channel

Neutralino

- group SU (3) _{× SU(2) × U(1)}

SM _{−−−−−→}SU SY MSSM - 2 Higgs doublets : tan β = vu_vd , 5 scalars : h, A, H, H±

- R-parity conservation_→ stable LSP

- mp 6= mp˜ ⇒ Soft breaking termsLsoft

In the basis (_{−i ˜}B,_{−i ˜}W3_{, ˜H}0

Parameters at GUT scale _{∼ 2. 10}16 GeV:

? a common gaugino mass m1/2

? a common scalar mass m0

? a common trilinear coupling A0

? a common bilinear coupling B0

? Higgs parameter µ0

+ Renormalization group equations and radiative ElectroWeak Symmetry Breaking:

1 2m 2 Z = m2_Hd QEW SB − m 2 Hu    QEW SB tan 2 β tan2 _{β − 1} −µ2|_{QEW SB} achieved at QEW SB ∼ pm_t1˜ m_t2˜ ⇒ Input parameters : m0, m1/2, A0, tan β, sgn(µ)

Advantages: REWSB, less free parameters, contact

with acc. analyses, but also addressing CCB, Landau poles, high energy extrapoll.

Thanks to Suspect authors

http://www.lpm.univ-montp2.fr:7082/ kneur/suspect.html

(study of the CMSSM with Suspect :

hep-ph/0107316, A. Djouadi, M. Drees,J.L. Kneur)

mSugra/CMSSM models

Composition of the lightest neutralino :

? bino χ : for low m0, RGE drive

M1|_{QEW SB} =

M2|_{QEW SB}

2

= 0.41m1/2 << |µ|_{QEW SB}

? mixed bino-higgsino χ : EWSB

∼ −m2_Hu|_{QEW SB} − µ2|_{QEW SB} if

tan β _{≥ 5}

for m0 large (> 1000),

increasing m0⇒ m2_Hu less negative ⇒ µ

decreases _{⇒ µ ∼ M}1

“Focus point region” hep-ph/9909334 Feng,

Experiment sensitivities in the

(m

, m

)

plane

m0 (GeV)

m1/2 (GeV)

ICECUBE

ANTARES 0.1 km2

Exp. Excluded

not LSP

χ

=1

h

Ω

0.3

0.1

0.025

no EWSB

m0 (GeV)

m1/2 (GeV)

ZEPLIN Max

EDELWEISS II

Exp. Excluded

=1

h

Ω

0.3

0.1

0.025

not LSP

χ

no EWSB

A

= 0 ; tan β = 45 ; µ > 0

Calculation with Suspect + Darksusy package :

mSugra : Direct Detection Experiments vs Neutrino Telescopes

µ flux

: m

σ

: m

mSugra with 5 GeV threshold vs neutrino Indirect Dection

(GeV) χ m 100 200 300 400 500

)

.yr

flux from sun (km

µ

log10

ANTARES 3 years

ICECUBE

mSugra models vs Direct Detection

(GeV) χ m 100 200 300 400 500

(pb)

σ

log10

CDMS

_EDELWEISS

EDELWEISS II

ZEPLIN MAX

Non-universal scalar soft terms

? Sfermions : non-universality in sfermions matrices can lead to light third generation sfermions

→coannihilations χ˜τ , χ˜t can modify the relic density but happend in region out of reach of detectors.

Detection imply “real” quarks mainly on u and d valence and due to their low Yukawa couplings RGE

evolutions of the first and second generation squarks depend on gaugino soft masses _→ their masses can

not be lowered by changing scalar soft terms to enhance σ_χscal_−q and σ_χspin_−q through the process χq _{−→ χq}q˜ .

? Higgses : relax universality m_Hi|MGUT = (1 + δi)m0 →modify REWSB relation parameters , mA, µ can

non universal Higgs masses effects in the

(

m

, m

)

plane

m0 (GeV)

m1/2 (GeV)

yr

km

flux = 10

µ

yr

flux = 10 km

µ

Exp. Excluded

not LSP

χ

=0.3

h

Ω

0.1

0.025

no EWSB

m0 (GeV)

m1/2 (GeV)

ZEPLIN Max

EDELWEISS II

Exp. Excluded

=0.3

h

Ω

0.1

0.025

not LSP

χ

no EWSB

m

= m

; m

= 0.5m

;

A0

= 0 ; tan β = 45 ; µ > 0

? wider noREWSB region ? mA(H) < mA(H)|mSugra → good for relic density (χχ A

−→ b¯b) and direct detection at low m0 (χq

H

Free relations in gaugino

mass parameters

M2|GU T parameter

? essentially modify neutralino composition (and

slightly low energy values of fields whitout

SU (3) charge through RGE).

Increasing the wino component of the

neutralino favours _→ χχ χ

+ 1 , χ02

−−−−−→

W+W−, ZZ and enhance the

annihila-tion cross secannihila-tion σA_χ−χ. the strong χχ0₂

and χχ+₁ coannihilations become actives and

Ωχh2 strongly decreases.

? larger coupling entering in σ_χscal_{−p →} increases the direct detection

? favours neutralino annihilations into the hard

W+W− spectrum_→ increases the indirect

detection muon fluxes

? However, the relevant value of M2 is very

critical : = fine-tunning (except moduli decays

giving wino in AMSB models. Moroi, Randall hep-ph/9906527).

M3|GU T parameter

? 1-loop RGE analyse _→ M3|GU T is the main

pa-rameter for non-universality in the MSSM (Kazakov, Moultaka hep-ph/9912271).

(M_{sof t}scal_|low)2 = (M_{sof t}scal|GU T)2+ c3f3+ c2f2+

c1f1 + corrections with fi = (M GU T_i )2 bi  1 ₋ 1 (1+biα0t)2 

and c3 strongly dominant.

→ M3|GU T < m1/2 decreases mA, m2_H2, µ (and mq˜) ? increase annihilation χχ _{−→ b¯b}A (χχ _{−→ f ¯}f˜ f) χχ _{−→ t¯}Z t, χχ χ + i ,χi −−−−→ W+W−, ZZ _∝ higgsino fraction

→ very favourable for Ωχh2

Gain for detection :

? direct detection : increase σscal_χ−p via χq _{−→ χq}H

(mH lower and z11(2)z13(4) %)

? indirect detection : increase capture σ_χspin_−p via

χq _{−→ χq}Z (higgsino fraction _%) and annihilation

Effects of

x =

1/2

on relic density and detection rate

Ω

h

µ flux

σ

flux from sun (km

Conclusion

RGE models OK with neutrino indirect detection :

?

very heavy scalars (beyond reach of LHC)

?

neutrino telescope signal in mSugra

_→

m

< 300

− 350

GeV

?

Ωh

_{∼ 0.15}

can be accomodated for

all

“mSugra” points using

x = M3

_|

/m

∼ 0.6(±0.1) + corrections(m

, tan β, mb

)

with

a

strong enhancement

of detection rates improving the experiment possibilities.

?

Earth out of reach neutrino telescopes in those framework.