Neutralino Dark matter detection in the MSSM and NMSSM David G. - - PowerPoint PPT Presentation

24.5.2005 Seoul-The dark side of the Universe

• p. 1/55

Neutralino Dark matter detection in the MSSM and NMSSM David G. Cerdeño

D.G.C., C. Muñoz, JHEP 10 (2004) 015

• S. Baek, D.G.C., Y.G. Kim, P

. Ko, C. Muñoz, arXiv:hep-ph/0505019 D.G.C., C. Hugonie, D. López-Fogliani, C. Muñoz, A.M. Teixeira, JHEP 12 (2004) 048

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Outline

Introduction Motivation for Dark Matter in the Universe Supersymmetric dark matter Neutralino dark matter in Supersymmetric theories Theoretical predictions for neutralino direct detection in MSSM (General Supergravity theory) Next-to-MSSM Summary

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Introduction

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Motivation for Dark Matter

The motivation for dark matter appears at different scales in astrophysical observations. Luminous (visible) matter is insuf£cient to account for the observed gravitational effects Galactic scale Rotation curves in spiral galaxies Elliptic galaxies Clusters of galaxies Peculiar velocities X-ray measurements of the temperature of the gas Gravitational lensing Large scale ¤ows

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Motivation for Dark Matter

The motivation for dark matter appears at different scales in astrophysical observations. Luminous (visible) matter is insuf£cient to account for the observed gravitational effects The amount of dark matter is usually expressed in terms of the cosmological density parameter:

• ✁

is the density averaged over the Universe

is the critical density for obtaining a ¤at Universe.

Astrophysical observation seemed to favour

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Cosmological parameters from CMB

Observations of the Cosmic Microwave Background constitute a primary tool for determining the global properties of our Universe.

DASI, CBI, VSA, MAXIMA, BOOMERanG, COBE, WMAP , PLANCK, ...

Recently the WMAP experiment has provided high precision data from which cosmological parameters have been determined. Combining WMAP with other experiments the best £t is obtained for

Gyr From where a bound on the abundance of Cold Dark Matter can be extracted

(

c.l.)

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN)

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 7/55

Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics Neutrinos: (hot dark matter) constrained by structure formation.

Cowsik, McClelland ’72; Lee, Weinberg; Dicus, Kolb, Tepliz ’77

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics Neutrinos: (hot dark matter) constrained by structure formation. Axions: with a mass of

eV. Axions are spin 0 particles associated to the spontaneous breaking of the global

Peccei Quinn symmetry (postulated to solve the strong CP-Problem)

with

Ipser, Sikivie; Stecker, Sha£; Turner, Wilczek ’83

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 7/55

Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics Neutrinos: (hot dark matter) constrained by structure formation. Axions: with a mass of

eV. Weakly Interacting Massive Particles: They can be present in the right amount to explain the dark matter. The relic density of WIMPs ful£ls naturally

• ❆

Particles with weak-scale interactions have the appropriate value of the annihilation cross-section,

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 7/55

Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics Neutrinos: (hot dark matter) constrained by structure formation. Axions: with a mass of

eV. Weakly Interacting Massive Particles: They can be present in the right amount to explain the dark matter. Lightest Supersymmetric Particle: stable in Supersymmetric theories with R-parity. The LSP can be the lightest Neutralino,

, which is a WIMP . Other interesting possibilities are axino or gravitino dark matter.

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 7/55

Usual Suspects

The nature of Dark Matter is still to be deciphered. Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient (inconsistent with BBN) Non-Baryonic Candidates: are provided by particle physics Neutrinos: (hot dark matter) constrained by structure formation. Axions: with a mass of

eV. Weakly Interacting Massive Particles: They can be present in the right amount to explain the dark matter. Lightest Supersymmetric Particle: stable in Supersymmetric theories with R-parity. SIMPs, CHAMPs, SIDM, WIMPzillas, Scalar DM, KK, Light DM... The LSP can be the lightest Neutralino,

, which is a WIMP . Other interesting possibilities are axino or gravitino dark matter.

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Direct detection of neutralinos

If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in galactic halos, raising the hope of their direct detection on Earth experiments. Direct detection of neutralinos would be possible through their elastic scattering with nuclei inside a detector.

Scattered WIMP Target crystal Recoiling nucleus

The recoiling energy can be detected by Ionization on solids Ionization in scintillators (measured by emission of photons) Increase in the temperature (measured by the released phonons)

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 8/55

Direct detection of neutralinos

If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in galactic halos, raising the hope of their direct detection on Earth experiments. Direct detection of neutralinos would be possible through their elastic scattering with nuclei inside a detector.

Sensitivity for WIMP detection (Spin-independent cross section)

Many experiments around the world Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, ZEPLIN, EDELWEISS, ...

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 8/55

Direct detection of neutralinos

If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in galactic halos, raising the hope of their direct detection on Earth experiments. Direct detection of neutralinos would be possible through their elastic scattering with nuclei inside a detector.

Sensitivity for WIMP detection (Spin-independent cross section)

Many experiments around the world Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, ZEPLIN, EDELWEISS, ... With increasing sensitivities and projected improvements ZEPLIN II and III, GENIUS, CDMSII, GEDEON, ...

» Outline Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters from CMB » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 8/55

Direct detection of neutralinos

If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in galactic halos, raising the hope of their direct detection on Earth experiments. Direct detection of neutralinos would be possible through their elastic scattering with nuclei inside a detector.

Sensitivity for WIMP detection (Spin-independent cross section)

Many experiments around the world Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, ZEPLIN, EDELWEISS, ... With increasing sensitivities and projected improvements ZEPLIN II and III, GENIUS, CDMSII, GEDEON, ... Could neutralinos be detected in the (near) future? How large can their detection cross section be?

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Neutralino dark matter in the MSSM

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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The Lightest Neutralino

The neutralinos in the MSSM are physical superpositions of the bino and wino (

) and Higgsinos (

).

The properties of the lightest neutralino,

, are very dependent on its composition.

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 11/55

Neutralino-nucleon cross section

One can evaluate the spin-independent part of the cross-section and analyse the feasibility of their direct detection.

Squark-exchange:

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 11/55

Neutralino-nucleon cross section

One can evaluate the spin-independent part of the cross-section and analyse the feasibility of their direct detection.

Squark-exchange:

Higgs-exchange:

This diagram is typically dominant and can be enhanced with Higgsino-like neutralinos (increase

) Light Higgses (decrease

)

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Supergravity scenarios

Working in the framework of SUGRA, several assumptions are made: The soft parameters are generated once SUSY is broken through gravitational interactions. They are given at a high energy scale (e.g., the GUT scale

GeV)

With these inputs, the RGEs are used to evaluate the low-energy supersymmetric spectrum. Radiative Electroweak Symmetry Breaking is imposed, and as a consequence the Higgsino mass parameter

is determined by the minimization of the Higgs effective

• potential. This implies

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 13/55

Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

GeV,

GeV

GeV, . . .

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

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Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

Higgs Mass (LEP2) :

GeV

(dependent on

in the MSSM)

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 13/55

Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

Higgs Mass (LEP2) :

GeV

(dependent on

in the MSSM)

Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04):

(from

data) (Bennett et al. ’04)

~ − ~ ~ 0 ~ χ νµ χ µ µ µ µ µ γ γ

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 13/55

Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

Higgs Mass (LEP2) :

GeV

(dependent on

in the MSSM)

Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04):

(from

data) (Bennett et al. ’04)

: (CLEO, BELLE)

~ 0 ~ − ~ ~ ~ b s γ χ χ b s γ , g u d

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 13/55

Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

Higgs Mass (LEP2) :

GeV

(dependent on

in the MSSM)

Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04):

(from

data) (Bennett et al. ’04)

: (CLEO, BELLE) B(

)

(CDF , D0)

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 13/55

Experimental Constraints

For consistency with experimental results, several constraints have to be imposed on the SUSY spectrum and low energy observables. Supersymmetric spectrum (LEP

, Tevatron):

Higgs Mass (LEP2) :

GeV

(dependent on

in the MSSM)

Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04):

(from

data) (Bennett et al. ’04)

: (CLEO, BELLE) B(

)

(CDF , D0)

Astrophysical Constraints

For the neutralino to be a solution to the problem of dark matter, its relic density has to be in agreement with observations Relic density:

• ❵❜❛

(

• ❵❜❛

)

» Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 14/55

Charge and Colour Breaking Constraints

The presence of scalar £elds with Colour and Electric Charge in SUSY theories may induce the appearance of dangerous charge and colour breaking minima (CCB) deeper than the realistic minimum.

<H >

u,d

S.M. MINIMUM CCB MINIMUM <u,e...>

V φ

Also the (tree level) potential can become Unbounded from Below (UFB) along particular directions in the £eld space. Avoiding these cases leads to constraints on the parameter space, among which the UFB constraints are the most important ones.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 15/55

Supergravity models

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained:

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained: Experimentally accepted

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained: Experimentally accepted

• ❵❜❛

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained: Experimentally accepted

• ❵❜❛

• ❵❜❛

*

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained: Experimentally accepted

• ❵❜❛

• ❵❜❛

* Disfavoured by UFB constraints

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 16/55

mSUGRA

In mSUGRA, where soft terms are taken to be universal,

,

,

, the parameter space is very constrained: Experimentally accepted

• ❵❜❛

• ❵❜❛

* Disfavoured by UFB constraints

is disfavoured for any

Larger values can also be forbidden for certain

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 17/55

mSUGRA

Larger values of

lead to an increase of

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 17/55

mSUGRA

Larger values of

lead to an increase of

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 18/55

Increasing the detection cross section

Departures from the mSUGRA scenario can lead to an increase in the neutralino-nucleon cross section. Intermediate scales

(Gabrielli, Khalil, Muñoz, Torrente-Lujan ’00)

Non-universal soft parameters Non-universal scalar masses

(Bottino, Donato, Fornengo, Scopel ’99; Arnowitt, Nath ’99; Accomando, Arnowitt, Dutta, Santoso ’00)

Non-universalities in the Higgs sector induce the largest effects. Non-universal gaugino masses

(Corsetti, Nath ’00; D.G.C., Khalil, Muñoz ’01)

General case, with non-universal scalar and gauginos

(D.G.C, C. Muñoz ’04; Baek, D.G.C., Kim, Ko, Muñoz ’05)

Neutralinos within the reach of detectors in the near future can appear with a wide range

• f masses.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 19/55

Non-universal scalar masses

Non-universal scalar masses can help increasing

. The most important effect is due to non-universalities in the Higgs masses at the GUT scale, which can be parametrized by

and

:

M GUT MEW m

2

RGES for the Higgs parameters

2

u

δ < 0

1

m

d

H

2

δ > 0

2 H

m

The Higgsino components of the lightest neutralino increase and the Higgs masses decreaase, thus there is an increase in

. Also, new annihilation channels appear (with e.g.,

,

,

in the £nal products) and

• ❵

decreases.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 20/55

Non-universal scalar masses

Although in principle points ful£lling all the experimental constraints and with a consistent value for the relic density can be found within the reach of dark matter detectors, even for moderate

. . .

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 20/55

Non-universal scalar masses

(Baek, D.G.C., Kim, Ko, Muñoz ’05)

. . . the recent experimental constraint on B(

) rules out most of those regions.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 20/55

Non-universal scalar masses

(Baek, D.G.C., Kim, Ko, Muñoz ’05)

. . . the recent experimental constraint on B(

) rules out most of those regions. Especially in the large

regime, where neutralinos could escape detection in some

• f the projected experiments.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 21/55

Correlation between

and B( )

From the leading contribution to the B(

) process, the chargino mediated

transition one obtains the qualitative expression

Both observables, B(

) and

, increase for large

and small

.

Points with larger

are typically excluded.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 21/55

Correlation between

and B( )

From the leading contribution to the B(

) process, the chargino mediated

transition one obtains the qualitative expression

Both observables, B(

) and

, increase for large

and small

.

Points with larger

are typically excluded. The correlation can be diluted if the term in parenthesis is reduced by

• Decreasing the stop mixing (e.g., with

)

• Decreasing the Higgsino mixing (e.g., with

non-universal Higgses)

• Increasing the stop mass (e.g., with

)

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 21/55

Correlation between

and B( )

From the leading contribution to the B(

) process, the chargino mediated

transition one obtains the qualitative expression

Both observables, B(

) and

, increase for large

and small

.

Points with larger

are typically excluded. The correlation can be diluted if the term in parenthesis is reduced by

• Decreasing the stop mixing (e.g., with

)

• Decreasing the Higgsino mixing (e.g., with

non-universal Higgses)

• Increasing the stop mass (e.g., with

) As a consequence, points with large

are still attainable.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 22/55

Non-universal scalar and gaugino masses

Non-universal gaugino masses can also induce an increase of

.

Decreasing

(

) leads to an increase in the value of

through the corresponding RGEs. Thus, the

parameter is reduced and the cross section increases.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 22/55

Non-universal scalar and gaugino masses

Non-universal gaugino masses can also induce an increase of

.

Decreasing

(

) leads to an increase in the value of

through the corresponding RGEs. Thus, the

parameter is reduced and the cross section increases. In the general case, a combination of these and scalar non-universalities

provides more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 23/55

Non-universal scalar and gaugino masses

In the general case, non-universalities in scalars and gauginos provide more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. Decrease

The

parameter decreases through the in¤uence of

• n the RGEs of the Higgs

parameters Heavier neutralinos are found with a larger Higgsino composition. The Higgs-exchanging interaction becomes more important and there is a slight increase of

. There is also a reduction of

• ❵

. Also, due to the decrease in

, and the reduction in the stop mixing, B(

) slightly decreases. As a consequence, larger

are obtained.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 23/55

Non-universal scalar and gaugino masses

In the general case, non-universalities in scalars and gauginos provide more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. Decrease

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 23/55

Non-universal scalar and gaugino masses

In the general case, non-universalities in scalars and gauginos provide more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. Decrease

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 24/55

Non-universal scalar and gaugino masses

In the general case, non-universalities in scalars and gauginos provide more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. Increase

The

parameter increases Lighter neutralinos are obtained, which have a larger Bino composition. In this case, due to the increase in the

parameter, and in the the stop mixing, B(

) increases, and smaller

are obtained.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 24/55

Non-universal scalar and gaugino masses

In the general case, non-universalities in scalars and gauginos provide more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. Increase

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 25/55

Very light neutralinos

With

very light (Bino-like) neutralinos can be obtained, which are compatible with experimental constraints.

(Griest, Roszkowski ’92; Gabutti, Olechowski, Cooper, Pokorski, Stodolski ’96; Hooper, Plehn ’02)

Despite them having typically a too high relic density, a signi£cant reduction in

• ❵❜❛

can be obtained for large

if the mass of the CP-odd Higgs is small (

GeV).

(Bottino, Fornengo, Scopel ’02; Bottino, Donato, Fornengo, Scopel ’03 ’04) (Bélanger, Boudjema, Cottrant, Pukhov, Rosier-Lees ’03)

Although this can be achieved precisely with non-universalities in the Higgs masses, this entails a very large increase in B(

) and makes this possibility very constrained.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 25/55

Very light neutralinos

With

very light (Bino-like) neutralinos can be obtained, which are compatible with experimental constraints. Still, for moderate values of

, neutralinos as light as

GeV can be

• btained with very large values for the detection cross section,

.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 26/55

Summary (MSSM)

Supersymmetric theories provide a natural dark matter candidate in terms of the Lightest SUSY particle. The impressive experimental efforts in dark matter detection, in particular of WIMPS motivate the theoretical analysis of the theoretical predictions for neutralino detection MSSM Experimental and astrophysical constraints play a leading role in restricting the parameter

• space. In particular, the recent constraint on B(

) typically rules out regions with larger

. Departures from the mSUGRA case, allowing intermediate initial scales and/or non-universal soft parameters can induce an increase of

. Non-universalities in the scalar and gaugino sectors allow for ¤exibility in the neutralino sector. Points of the parameter space can be obtained, where the experimental constraints are satis£ed and

is within the sensitivity of detectors in the near future for a wide range

• f neutralino masses (

GeV).

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 27/55

Neutralino dark matter in the NMSSM

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 28/55

Motivation

The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated extension of the MSSM. Offers an elegant solution to the

• problem of the MSSM

The

• term in the MSSM, present in the superpotential faces a naturaleness

problem:

Whereas a natural value for

is

, minimisation of the scalar potential implies

In the NMSSM

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 28/55

Motivation

The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated extension of the MSSM. Offers an elegant solution to the

• problem of the MSSM

Less severe “Higgs-little £ne tuning” problem of the MSSM In the MSSM

and so far it has not been detected. This problem is less severe in the NMSSM, since the upper bound for the Higgs mass is larger than in the MSSM.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 28/55

Motivation

The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated extension of the MSSM. Offers an elegant solution to the

• problem of the MSSM

Less severe “Higgs-little £ne tuning” problem of the MSSM Rich phenomenology Very light Higgses and neutralinos are experimentally viable. Although the Higgs phenomenology has been thoroughly studied, there are only a few works on the implications for neutralino dark matter.

Flores, Olive, Thomas ’91 Bednyakov, Klapdor-Kleingrothaus ’98

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 28/55

Motivation

The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated extension of the MSSM. Offers an elegant solution to the

• problem of the MSSM

Less severe “Higgs-little £ne tuning” problem of the MSSM Rich phenomenology Very light Higgses and neutralinos are experimentally viable. Although the Higgs phenomenology has been thoroughly studied, there are only a few works on the implications for neutralino dark matter.

Flores, Olive, Thomas ’91 Bednyakov, Klapdor-Kleingrothaus ’98

Thorough analysis of the NMSSM parameter space, calculating the particle spectrum and the experimental constraints from LEP . Implications for Neutralino-nucleon cross section.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 29/55

Overview of the NMSSM

In the NMSSM the £eld structure of the MSSM is modi£ed by the addition of a new super£eld

, which is a singlet under the SM gauge group:

This leads to the following new terms in the superpotential

and in the Lagrangian

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 29/55

Overview of the NMSSM

In the NMSSM the £eld structure of the MSSM is modi£ed by the addition of a new super£eld

, which is a singlet under the SM gauge group:

This leads to the following new terms in the superpotential

and in the Lagrangian

When Electroweak Symmetry Breaking occurs the Higgs £eld takes non-vanishing VEVs:

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 30/55

Higgs Sector

The minimisation conditions for the scalar potential can be used to reexpress the soft breaking Higgs masses in terms of the rest of the parameters:

And restrictions on the signs of

,

and

appear After rotating away the CP-odd would-be Goldstone boson we are left with £ve neutral Higgs states, and two charged states. CP-even and CP-odd states do not mix, since we made the assumption of no CP-violation

• n the Higgs sectors. Thus the mass matrices are written in the corresponding basis:

CP-odd Higgs:

CP-even Higgs:

The lightest Higgs has a singlet component:

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 31/55

The neutralino in the NMSSM

The lightest neutralino

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 31/55

The neutralino in the NMSSM

The lightest neutralino has now a singlino component

This, together with changes in the Higgs sector, alters the neutralino direct detection properties, in particular, the Neutralino-nucleon cross section has to be re-evaluated.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 32/55

Neutralino-nucleon cross section

We only concentrate on the spin-independent part of the cross-section

Squark-exchange: formally identical to MSSM; new mixings in

coupling

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 32/55

Neutralino-nucleon cross section

We only concentrate on the spin-independent part of the cross-section

Squark-exchange: formally identical to MSSM; new mixings in

coupling

Higgs-exchange:

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 33/55

Enhancing the cross section

In the MSSM larger predictions for

can be obtained when the Higgs-exchange diagrams are enhanced by Increasing the Higgsino content of

(

and

) Decreasing the mass of the exchanged Higgses (

and

)

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 33/55

Enhancing the cross section

In the MSSM larger predictions for

can be obtained when the Higgs-exchange diagrams are enhanced by Increasing the Higgsino content of

(

and

) Decreasing the mass of the exchanged Higgses (

and

) The second possibility is particularly important in the NMSSM Very light Higgses can be obtained, considerably enhancing the

• channel.

Such light Higges (

), which have a relatively large singlet composition, can induce an increase in

• f several orders of magnitude.

The lightest Higgs cannot be pure singlet, since the

coupling vanishes.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 34/55

Constraints on the parameter space

We work with the following input parameters, given at the EW scale:

The Higgs potential is minimised numerically with the code

.

Ellwanger, Gunion, Hugonie ’04

The NMSSM spectrum is then obtained and the following constraints applied Absence of Landau poles below

Experimental constraints from LEP Neutralino:

, direct production (

); Chargino and

Neutral Higgs: Constraints on production rates

(IHDM)

(DHDM)

(APM)

The constraint on the neutralino relic density is not imposed.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 35/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 35/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Landau Pole

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 35/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Landau Pole Higgs tachyons

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 35/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Landau Pole Higgs tachyons False minima

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 35/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Landau Pole Higgs tachyons False minima LEP constraints

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 36/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Higgsino Singlino Neutralino sector: The Singlino composition increases for small

and

, and the mass decreases.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 36/55

Results (

,

)

, (i)

For £xed values of

,

,

,

, we analyse the constraints on the

plane:

GeV

GeV

GeV Neutralino sector: The Singlino composition increases for small

and

, and the mass decreases. Doublet Singlet Higgs sector: Light Higgses which are mainly Singlets are found for small

and

.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 37/55

Results (

,

)

, (i)

The corresponding neutralino-nucleon cross section as a function of the neutralino mass

GeV

GeV

GeV Black dots ful£l all the constraints. Grey dots are excluded by LEP .

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 37/55

Results (

,

)

, (i)

The corresponding neutralino-nucleon cross section as a function of the neutralino mass

GeV

GeV

GeV Black dots ful£l all the constraints. Grey dots are excluded by LEP . Large values for the cross section

pb are obtained for very light singlet-like Higgses. Lightest Higgs:

GeV with

Lightest Neutralino:

and

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 38/55

Overview

, (i-iii)

The GUT relation is £xed

GeV, with

GeV

GeV ,

GeV ,

Large values for

correspond to: Very light singlet-like Higgses (

GeV),

, and neutralinos which are Higgsino-singlino with

.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 39/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 39/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV,

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

When

increases, the gaugino components of

become more important and

decreases.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe

• p. 39/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV,

GeV,

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

When

increases, the gaugino components of

become more important and

decreases. For large

is bino-like and

is beyond experimental sensitivity.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary » Summary (NMSSM) 24.5.2005 Seoul-The dark side of the Universe

• p. 40/55

Summary

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary » Summary (NMSSM) 24.5.2005 Seoul-The dark side of the Universe

• p. 41/55

Summary (NMSSM)

Supersymmetric theories provide a natural dark matter candidate in terms of the Lightest SUSY particle. The impressive experimental efforts in dark matter detection, in particular of WIMPS motivate the theoretical analysis of the theoretical predictions for neutralino detection Next-to-MSSM Large values of

are attainable, within the reach of future dark matter experiments The increase in

is due to an enhancement of Higgs-exchanging diagrams, due to the presence of very light Higgses (

GeV) with a signi£cant singlet composition. The lightest neutralino is a mixed singlino-Higgsino state with

GeV In progress: Include calculation of the relic density and constraints on low energy

• bservables.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 42/55

Extra Slides MSSM

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 43/55

Rotation curves in spiral galaxies

r v

rot

rot

= distance to the center of the galaxy

= mass contained within that radius

Beyond the luminous disk

rot

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 44/55

Rotation curves in spiral galaxies

Roy ’00, data from Corbelli, Salucci ’99

rot

rot

= distance to the center of the galaxy

= mass contained within that radius

Beyond the luminous disk

rot

However, observations show

rot

for

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 45/55

Rotation curves in spiral galaxies

The galaxy is surrounded by a spherical halo of Dark Matter with

rot

(i.e., self gravitational ball of ideal gas)

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 46/55

Clusters of galaxies

Coma Cluster Measurement of peculiar velocities

(Zwicky ’33)

X-ray measurements of the temperature of the gas

(Briel, Henry, Bohringer ’92; White ’93)

Gravitational lensing

(Tyson ’94)

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 47/55

mSUGRA

The constraint on the relic density leaves narrow accepted regions. Bulk region Coannihilation “tail” with Next-to-LSP (in this case the

)

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe

• p. 47/55

mSUGRA

The constraint on the relic density leaves narrow accepted regions. Bulk region Coannihilation “tail” with Next-to-LSP (in this case the

) Rapid annihilation through CP-odd Higgs

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 48/55

Extra Slides NMSSM

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 49/55

Higgs Sector

CP-odd Higgs:

CP-even Higgs:

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 50/55

Variations of the parameters

, (i)

Decrease

: Despite the decrease in the tachyonic region, the region excluded experimentally by

(IHDM and DHDM) is much larger and imply

pb.

,

GeV ,

GeV ,

GeV

GeV with

Mixed singlino-Higgsino neutralinos with

GeV

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 50/55

Variations of the parameters

, (i)

Variations in

: Low values of

are more experimentally constrained, but allow for lighter Higgses with a large singlet component and thus large

,

GeV ,

GeV ,

GeV For large

tachyonic regions are larger, the Higgs is mainly a doublet and the Neutralino is Higgsino-like. Similar results to those in the MSSM are obtained.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 50/55

Variations of the parameters

, (i)

Variations in

: There is a range of “optimal” values for

• utside of which tachyons appear more easily in

the Higgs sector and experimental constraints are more important. large

,

GeV ,

GeV ,

GeV

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 51/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 51/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV,

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

When

increases, the gaugino components of

become more important and

decreases.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 51/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Preserving the GUT relation

GeV,

GeV,

GeV

GeV

GeV

GeV For low

,

is singlino-Higgsino like

When

increases, the gaugino components of

become more important and

decreases. For large

is bino-like and

is beyond experimental sensitivity.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 52/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Relaxing the GUT relation

GeV

GeV

GeV

GeV The Wino composition becomes more important as

• increases. The cross section,

, is larger than in the Bino case.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 52/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Relaxing the GUT relation

GeV,

GeV

GeV

GeV

GeV The Wino composition becomes more important as

• increases. The cross section,

, is larger than in the Bino case.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 52/55

Variations in the gaugino masses

, (i)

So far we have analysed the case

. Let us now address variations in the gaugino mass parameters Relaxing the GUT relation

GeV,

GeV,

GeV

GeV

GeV

GeV The Wino composition becomes more important as

• increases. The cross section,

, is larger than in the Bino case. Because of the experimental bound on the chargino mass, Wino-like neutralinos cannot be obtained below

GeV.

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 53/55

Case (ii)

, (ii)

In contrast with the previous examples, in case (ii), for

, the Neutralino is Higgsino-like in all the parameter space and the cross section is bounded by

. The lightest Higgs is doublet-like.

,

GeV ,

GeV ,

GeV Most of the parameter space is excluded due to tachyons in both the CP-odd and CP-even Higgs sectors.

and

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 54/55

Case (iii)

, (iii)

In case (iii), for

, the parameter space is again plagued with tachyons in the Higgs

• sector. Despite this, large

can be found when the Higgs is light and singlet-like.

,

GeV ,

GeV ,

GeV The Neutralino is a mixed singlino-Higgsino state with

.

GeV and

GeV

» Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe

• p. 55/55

Case (iv)

, (iv)

The results for case (iv), with

, are qualitatively similar to those of case (ii). The Neutralino is Higgsino-like and a doublet-like lightest Higgs is obtained.

,

GeV ,

GeV ,

GeV The neutralino-nucleon cross-section is bounded by

pb by experimental constraints.

and

GeV