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Home , Axino, Axion, Hot dark matter, Neutralino

Neutralino dark Howard Baer University of Oklahoma

1 Evidence for : overwhelming, and from numerous disparate sources!

Properties: massive, neutral, cold (warm...)

Of in the (SM), only have the right properties: but they constitute , and their abundance is known

Dark matter must be some state not contained in the SM: NEW PHYSICS NEEDED!

2 Some dark matter candidates: vs. interaction strength plane

Some Dark Matter Candidate Particles

24 10 21 10 18 10 15 10 12 10 9 10 Q-ball 6 10 3 10 0 10 -3 10 neutrinos WIMPs : -6 10

(pb) -9 10 KK

int -12 10 branon ! wimpzilla -15 LTP 10 -18 Black Hole Remnant 10 -21 10 -24 10 -27 10 SuperWIMPs : -30 10 fuzzy CDM -33 10 KK -36 10 -39 10 -33 -30 -27 -24 -21 -18 -15 -12 -9 -6 -3 0 3 6 9 12 15 18 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 mass (GeV)

3 While some candidates are conjured by theorists specifically to solve the DM problem, others emerge as by-products of solutions to long standing problems in :

Peccei-Quinn solution to strong CP problem:

Supersymmetry: at least 3 viable DM candidates: neutralino, gravitino, axino/(axion)

4 SUSY motivations: in quantum field theory (no quadratic divergences for scalar fields) means to unification with (supergravity) gauge coupling unification provided at TeV scale precision EW corrections and Higgs mass radiative EWSB and the top mass accommodate baryogenesis: at least 3 ways

5 Supersymmetric models: how SUSY breaking is communicated from to visible sector

gauge mediation (GMSB): solves SUSY flavor problem, contains very light gravitino: does not naturally yield CDM

mediation (AMSB): mAMSB, HCAMSB, inoAMSB: solves flavor problem; need additional sources of CDM since thermal abundance too low

gravity mediation (SUGRA): 3 (or more) candidate DM particles: Z1 or χ, G,˜ a/a˜

6 ! Simplest: mSUGRA or CMSSM

embed MSSM into SUGRA gauge theory

SUSY breaking in simple hidden sector

parameter space: m0,m1/2,A0 tan β, sign(µ)

7 Neutralino: a WIMP DM candidate

The WIMP miracle

8 Calculation of relic density

9 mSUGRA parameter space

well-known regions: *bulk (low m0, mhf) *stau co-annihilation (low m0) *HB/FP (large m0) * A resonance (large tan(beta) * stop co-ann. * h-resonance

HB, Mustafayev, Park, Tata

10 More general: scan over 19 parameter SUGRA model

2 Ωχh too large for bino; too small for wino/

mχ < 500 GeV

HB, Box,Summy, arXiv:1005.2215 2 Ωχh 0.11 is most unlikely value! ∼ 11 Non-standard may be Standard! neutralino production from moduli decay

extra entropy production from moduli decay

neutralino production from gravitino decay

neutralino production from axino decay

entropy production from axino decay

axino or gravitino as LSP

presence of axion component to DM

12 Too much relic density? Dilute with additional entropy production (Lazarides, Schaeffer, Seckel and Shafi, NPB346 (1990) 193), or assume χ decay to lighter states e.g. axino or gravitino (Covi, Kim, Kim, Roszkowski, JHEP0105 (2001) 033)

Too little relic density? Add more via production from moduli/gravitino/axino decay: (Randall, Moroi, NPB570 (1999) 1731; Acharya, Kane, Watson, Kumar, PRD80 (2009)083529

Gelmini, Gondolo, PRD74 (2006) 023519

13 Production of SUSY (dark) matter at LHC7:

√s =7T eV

14 Simulated production of neutralino DM from SUSY at LHC

15 Search for mSUGRA at LHC

16 SM backgrounds to SUSY

17 Optimize cuts over parameter space

Then require, for some set of cuts and integrated luminosity:

18 Reach of LHC7 for various integrated luminosities:

HB, Barger, Lessa, Tata: JHEP

19 Smoking gun signature for LHC7: OS/SF dileptons Models with mass unification

m ˜ m ˜

mg˜ < 630 GeV dilepton mass edge below MZ!

20 Reach of LHC14 compared to Tevatron and ILC

21 Precision sparticle measurements at LHC

22 Precision SUSY measurements and cosmology Find which parameter space choices lead to precision measurements

Map parameters onto e.g. relic density, DD , ID Allanach, Belanger, Boudjema, Pukhov -> Collider Nojiri, Polesello, Tovey measurement of Baltz, Battaglia, Peskin, Wisansky Arnowitt, Dutta, Kamon, .. Ω h2, σ(χp), σ v , χ ! · " ···

Beware: points chosen are SPS1a or accessible to ILC500

23 IDD via telescopes

IDD via WIMP annihilation to gammas or

24 Direct WIMP detection via WIMP- scattering

25 DD in mSUGRA model: Xenon-100 should cover FP region!

26 Reach of LHC14, ILC compared to DD/ID WIMP search

HB, Park, Tata

27 Well-tempered Arkani-Hamed, Delgado, Giudice Scan over 10 models with and without universality; keep only models with correct relic abundance

Bulk of models asymptote at 10^-8 pb! Accessible to next Xenon-100 run! HB, Mustafayev, Park, Tata

28 DD of relic winos in various AMSB models

HB, Dermisek, Rajagopalan,Summy: JCAP 1007 (2010) 014

*unlike SUGRA models, these are bounded from below *reach of Xe 1 ton well beyond that of LHC

29 If a WIMP signal is found, do we declare victory and go home? NO! Era of WIMP astronomy will have just begun!

Check SI scattering on different target nuclei (A^2 dependence)

Extract WIMP mass from recoil E distribution

Check SD WIMP scattering rate; sensitive to of WIMP

Extract WIMP velocity distribution

Directional detectors: seasonal, day/night eff.

30 If WIMP seen in DD, then mass measurement

Study by Schnee; Green; Drees&Shan shows m(WIMP) may be extracted from energy spectrum in DD experiments, for lower range of WIMP : crucial input for LHC?

31 Role of SI vs. SI WIMP search

Bertone, Cerdeno, Collar, Odom, PRL99 (2007)151301

32 Directional WIMP recoil detectors ala DRIFT

WIMP wind

seasonal

day/night

33 Gravitino production in early (gravitino problem)

Gravitinos can be produced thermally in early universe

Gravitino lifetime suppressed by M_Pl^-2

Late decays disrupt successful BBN predictions

Need either m_grav > 5 TeV or T_R<10^5 GeV (but then problems with baryogenesis)

Kawasaki et al; Ellis et al.

34 Baryogenesis and gravitino problem

EW baryogenesis in MSSM: mt1<125 GeV

Leptogenesis: need T(reheat)>10^9 GeV (conflicts with gravitino problem)

Non-thermal leptogenesis: TR>10^6 GeV

Affleck-Dine leptogenesis: can have TR~10^6 GeV

....

35 Gravitino (superWIMP) dark matter: BBN constraints on gravitino as LSP are severe unless it is very light, as in GMSB

(Case of bino NLSP)

Kawasaki, Kohri, Moroi, Yatsuyanagi, PRD78, 065011(2008)

36 Axion dark matter

Axion DM: forms BEC, suppresses small scale structure, gives mechanism for galactic rotation Sikivie, Wang arXiv:0901.1106

37 Axion cavity seach

38 Axions+ SUSY=> axinos

axino is spin-1/2, R-odd spartner of axion

axino mass is model dependent: keV-> GeV

axino is an EWIMP; coupling suppressed by Peccei-Quinn scale f : 10 9 10 12 GeV a − good candidate for cold DM

for review, see Covi, Kim, Kim, Roszkowski JHEP 0105 (2001) 033

39 Peccei-Quinn + SUSY Two scenarios: Axino is LSP

DM is mixture of axions plus thermally produced and non-thermal (decay produced) axinos

no WIMP signals Axino is not LSP: * DM consists of WIMP+axion mixture: TeV scale axinos decay to WIMPs, augmenting production as in AMSB models *Possible DD of WIMP and axion!

40 Conclusions: SUSY neutralino is excellent candidate for CDM

Role of LHC: produce matter states associated with dark matter; decay to stable DM candidate (LHT, UED, SUSY, etc) usually gives ETMISS signature (charged stable NLSP counter-example)

In case of WIMP dark matter, additional signals from DD/ID of DM will provide complementary information (e.g. WIMP mass?)

Xenon-100 will soon test FP region of mSUGRA and well-tempered neutralino models with mixed bino-higgsino CDM precision measurements may allow collider measurement of relic density, associated quantities

If WIMP signal is found, era of WIMP astronomy will begin!

A-dependence; recoil spectrum; SD scatter; WIMP mass/velocity dist’n; directional detectors;compare to LHC; IDD signals;...

DUSEL will be essential for program of WIMP astronomy!

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