Dark Matter Connection of Dark Matter Connection of Particle Physics Models: Particle Physics Models:

Where Do We Stand?Where Do We Stand?

Bhaskar

Dutta

Texas A&M University

122nd September ’ 10

Upcoming Days…

2

The mechanism for generating masses

We will try to understand:

The physics behind the scale of W, Z boson mass scale ~ electroweak scale

The origin of dark matter

Do we have any further evidence of grand unification?

Is there any particle physics connection?

Mplanck

>>MW

The origin of inflation

Why Ωb(4%) ~ ΩDM (23%) ?...

The Standard Model (SM) describes all these particles and 3 of 4 forces. We have confirmed the existence of those in the laboratory experiments.

The Standard ModelThe Standard Model

+ Higgs boson

Higgs has not yet been discovered

The mass is constrained from data:

114 GeV<MH

<154 GeV

3

SM problems and solutionsSM problems and solutionsThe Standard Model :•

Cannot provide a dark matter candidate.

•

Has a serious Higgs mass divergence problem due to quantum correction.

•

Cannot accommodate masses for neutrinos.

•

Cannot provide enough matter- antimatter asymmetry.

• Standard Model has fallen!

4

•

Solves the Higgs mass problem in a very elegant way.

•

Supersymmetric grand unified models include neutrinos!

•

Can produce correct matter- antimatter asymmtery

• Can provide Inflation

• Can provide new sources of CP violation, e.g., Bs ψ φ

Supersymmetry

:Provides a candidate for dark matter ~ neutralino.

What is the new model?

[Recently observed 3.2σ

deviation at Tevatron]

Particle Physics and Cosmology

SUSY is an interesting class of models to provide a weakly interacting massive neutral particle (M ~ 100 GeV).

SUSY

SUSY

CDM CDM == NeutralinoNeutralino ( )( )01χ~

Ast

roph

ysic

sA

stro

phys

ics

{

{

8pb9.0

1~

23.0

2

2

ann

0

ann

2~ 0

1

M

dxv

h fx

πασ

σχ

=

Ω ∫

LHC

2010/9/20 5

LHC

LHCLHC

The fundamental law(s) of nature is hypothesized to be symmetric between bosons and fermions.

Fermion

↔Boson

Have they been observed? � Not yet.

SupersymmetrizedSupersymmetrized SMSM

6

SUSY partner of Z boson: neutralino

SUSY partner of W boson: chargino

Lightest neutralinos are always in the final state! This neutralino is the dark matter candidate!!

SUSY partner of τ lepton: stau

SUSY Interaction DiagramsSUSY Interaction Diagrams

7

The grand unification of

forces occur in SUSY models.

Dream of the UnificationDream of the Unification

☺U(1)Y ForceU(1)Y Force

Unification scale can also be pushed to 1017-18

GeVAmeliorates Proton decay problem in the very successful SO(10) modelDutta, Mimura, Mohapatra

,

Phys.Rev.Lett.100:181801,2008

8

Search for SUSY-upcoming days

9

Large Hadron

Collider-susy

particles will be directly produced

Higgs mass in the well motivated SUSY models: < 150 GeVCurrent experimental bound: 114 -

154 GeV

Direct detection experiment, CDMS, Xenon 100, LUX etc

Indirect detection experiments, e.g., PAMELA has already observed excess of positron excess in cosmic rayFermi Gamma Ray Space Telescope: Sensitive to gamma ray from Dark Matter annihilation

Tevatron

search for Bs μ+ μ− ( highest reach on SUSY masses)

Existence of Higgs will be explored

IceCube: Sensitive to neutrinos from DM annihilation e+

γ

ν

…

CDMS has observed two DM candidate events! Excess at DAMA/Libra,

COGENT

SUSY Models-CosmologySUSY Models and dark matter:

MSSM: supersymmetric

SM (more than 100 parameters)SUGRA: Gravity mediated mSUGRA (minimal model)Other possibilities: Gauge mediated, Moduli

mediated etc

DM candiates: Lightest neutralino

(most common)SneutrinoGravitino

Inflation: Low scale or High scale in these modelsLow scale can be tied to the SUSY breakings

01

~χv~G~ LHC, DM experiments

LHC, PLANCK data etc.

1010

SUSY Models-Cosmology…What we hope for:The upcoming data from the LHC + Direct –Indirect detection experiments + WMAP-PLANCK data Establish a model

whether our dark matter picture is correct

explain the observed baryon density, inflation etc.

The model would tell us:

The origin of the electroweak scale

11

The signal : jets + leptons + missing Energy

Establishing a Model at the LHC

(or l+l-, τ+τ−)

DM

DM

Colored particles get produced and decay into weakly interacting stable particles

High energy jet[mass difference is large]

The energy of jets and leptons depend on the sparticle masses which are given by models R-parity conserving

12

(or l+l-, τ+τ−)

MW

,MZ

SUSY at the LHCFinal states Model Parameters

We may not be able to solve for masses of all the sparticles from a model

Reconstruct sparticle masses, e.g.,

Solving for the MSSM : Very difficult due to too many parameters

01

~~ χ++→ lqQ0

1~~ χ+→ lL

01

04,3,2

~,,~ χχ +→ llhZ etc.

Identifying one sideis very tricky!

13

SUSY at the LHC

The best strategy:

Solve for the minimal model: mSUGRA4 parameters: m0, m1/2, A0, tanβ and Sign(μ)

The cascades can be understood in a simpler way [hopefully!]

Next step:Next to minimal model (Higgs nonuniversality)Then …

We can use simpler models to understand the cascades and solve for the model parameters

Calculate the Dark Matter content

14

4 parameters + 1 signtanβ

<Hu >/<Hd > at MZm1/2 Common gaugino mass at MGUTm0 Common scalar mass at MGUTA0 Trilinear couping at MGUTsign(μ) Sign of μ in W(2) = μ Hu Hd

MHiggs > 114 GeVMchargino > 104 GeV2.2x10−4 <B(b → s γ) <4.5x10−4

(g−2)μ : 3 σ deviation from SM

Key Experimental Constraints

12900940 201

.h. ~ <<χ

Ω

Minimal Minimal SupergravitySupergravity ((mSUGRAmSUGRA))

<Hd >

<Hu >

<H> =

246 G

eVβ

SUSY model in the framework of unification:

+

Arnowitt, Chamesdinne, Nath, PRL 49 (1982) 970; NPB 227 (1983) 121. Barbieri, Ferrara, Savoy, PLB 119 (1982) 343.Lykken, Hall, Weinberg, PRD 27 (1983) 2359.

15

Dark Matter Allowed RegionDark Matter Allowed Region

16

GeV 15~5Δ =M

Co-annihilation RegionCo-annihilation Region

17

( )

2

1CDM

⎥⎥⎥⎥⎥⎥

⎦

⎤

⎢⎢⎢⎢⎢⎢

⎣

⎡

∝−Ω + ….

A near degeneracy occurs naturally for light stau

in mSUGRA.A near degeneracy occurs naturally for light stau

in mSUGRA.

011 ~~ MMM

χτ −≡Δ

fTMe k/Δ

2

−

⎥⎥⎥⎥⎥⎥

⎦

⎤

⎢⎢⎢⎢⎢⎢

⎣

⎡01χ~

1τ~+ + ….

Co-annihilation (CA) ProcessCo-annihilation (CA) Process

Griest, Seckel ’91

Anatomy of Anatomy of σσ annann <v>in a Model<v>in a Model

pbM

vann 1~~ 2

2ασ ><

Goal for the analysisGoal for the analysis

Establish the “dark matter allowed region” signal

Measure SUSY masses

Determine Model parameters

Calculate Ωχh2 and compare with ΩCDM h

2

18

DM Allowed Regions in mSUGRA

[Stau-Neutralino

CA region]

[Focus point region]the lightest neutralino

has a larger

Higgsino

component

Feng, Matchev, Wilczek, PLB482 388,2000.

[Bulk region] is almost ruled out

19

Arnowitt, Dutta, Santoso, NPB 606:59,2001.

Ellis, Falk, Olive, PLB 444:367,1998.

Overdense

region

Signals of the Allowed RegionsSignals of the Allowed RegionsNeutralino-stau coannihilation(CA) region: jets + taus (low energy) +

missing energy[ArnowittArnowitt, Dutta, , Dutta, GurrolaGurrola, , KamonKamon, , KrislockKrislock, , TobackToback, , PRL, 100, (2008) 231802PRL, 100, (2008) 231802;ArnowittArnowitt, Dutta, , Dutta, KamonKamon, , KolevKolev, , TobackToback,,

PLB 639 (2006) 46;PLB 639 (2006) 46;ArnowittArnowitt, , AurisanoAurisano, Dutta, , Dutta, KamonKamon, , KolevKolev, Simeon, , Simeon, TobackToback, Wagner; , Wagner; PLB 649 PLB 649 (2007)73(2007)73]

Focus point: jets+ leptons +missing energy[Dutta, Flanagan, Dutta, Flanagan, KamonKamon, , KrislockKrislock, to appear;, to appear;ToveyTovey, PPC 2007; Baer, Barger, , PPC 2007; Baer, Barger, SalughnessySalughnessy, , SummySummy, Wang , PRD, 75, 095010 , Wang , PRD, 75, 095010 (2007)(2007)]]

Bulk region: jets+ leptons +missing energy [Nojiri, Polsello, Tovey’05]

Overdense regions: Higgs+Jets, Z+jets, taus+jets+missing energy [Dutta, [Dutta, GurrolaGurrola, , KamonKamon, , KrislockKrislock, , LahanasLahanas, , MavromatosMavromatos, , NanopoulosNanopoulos, arXiv:0808.1372 ], arXiv:0808.1372 ]

Non Universal Higgs Models: W+jets+taus +missing energy [Dutta, Kamon, Krislock, Kolev, Oh, arxiV:1008.3380 20

Smoking Gun of CA RegionSmoking Gun of CA Region

100%1τ~

τ

τ

Lu~

01χ~

02χ~

g~

97%

u

u

SU

SY

Ma

sse

s

(CDM)

2 quarks+2 τ’s+missing energy

Uniq

ue k

inem

atics

21

Low energy taus

exist in theCA regionHowever, one needs to measure the model parameters to predict thedark matter content in this scenario

Low EnergyLow Energy ττ and and MMττττ

Low energy τ’s

are an enormous challenge for the detectors

22

Num

ber

of C

ount

s / 1

GeV

ETvis(true) > 20, 20 GeV

ETvis(true) > 40, 20 GeV

ETvis(true) > 40, 40 GeV

GeV) 5.7(

011

02

=→→

M

~~~

Δχττττχ

Arnowitt, Dutta, Kamon, Kolev, Toback PLB 639 (2006) 46PLB 639 (2006) 46

We need to involve the low energy τ’sIn our analysis

Low energy τ

23

We use ISAJET + PGS4PLB 639 (2006) 46PLB 639 (2006) 46Arnowitt, Dutta, Kamon, Kolev, Toback

EE TT missmiss+2+2ττ+2j Analysis+2j Analysis

SUSY Anatomy

Mjττ

Mττ

pT(τ)

100%1τ~

τ

τ

Lu~

01χ~

02χ~

g~

97%

u

u

SU

SY

Ma

sse

s

(CDM)

24

Meff

Extracting One side: jττOS-LS selection of ditaus selects , but if we need to reconstruct the entire side

02χ~

We use the following subtraction scheme:

2 t

BEST: Bi Event Subtraction Technique

Dutta, Kamon,Krislock, Kolev, Oh, arXiv: 1008.3380

25

Observables

SM+SUSY Background gets reduced±±± −ττττ

NN m

• Ditau invariant mass: Mττ• Jet-τ-τ

invariant mass: Mjττ

• Jet-τ

invariant mass: Mjτ• PT of the low energy τ• Meff : 4 jets +missing energy• Meff (b) : 4 jets +missing energy

Since we are using 7 variables, we can measure the model parameters and the grand unified scale symmetry (a major ingredient of this model)

1. Sort τ’s by ET (ET1 > ET

2 > …)• Use OS−LS method to extract τ

pairs from the decays

All these variables depend on masses model parameters

26

7 Eqs

(as functions of SUSY parameters)

)~,~(

)~,~,,~(

)~,~,,~ (

)~,~,~(

)~,(

)~,~,(

6peakeff

01

025

(2)peak2

01

024

(2)peak1

01

023

(2)peak

012

01

021

peak

L

Lj

Lj

Lj

qgfM

MqfM

MqfM

qfM

MfSlope

MfM

=

Δ=

Δ=

=

Δ=

Δ=

χχ

χχ

χχ

χ

χχ

τ

τ

ττ

ττ

Invert the equations to Invert the equations to determine the massesdetermine the masses

Determining SUSY Masses (10 fbDetermining SUSY Masses (10 fb−−11))

1σ ellipse

)91.5( 8.09.5/

)19.3( 2.01.3/0.26.10

;19141;15260

;21831 ;25748

01

02

01

02

~~

~~

~~

~~

=±=

=±=±=Δ

±=±=

±=±=

theoryMM

theoryMMM

MM

MM

g

g

gqL

χ

χ

χχ

10 fb-1

27

Phys. Rev. Phys. Rev. LettLett. 100, (2008) 231802. 100, (2008) 231802

Meff

(b) = f7

(g, qL

, t, b)~ ~ ~ ~

ArnowittArnowitt, Dutta, , Dutta, GurrolaGurrola, , KamonKamon, , KrislockKrislock, , TobackToback

[1] Established the CA region by detecting low energy τ’s (pT

vis > 20 GeV)

[2] Determined SUSY masses using:Mττ

, Slope, Mjττ

, Mjτ

, Meff

e.g., Peak(Mττ

) = f (Mgluino , Mstau , M , M )

[3] Predict the dark matter relic density by determining m0 , m1/2 , tanβ, and A0

DM Relic Density in DM Relic Density in mSUGRAmSUGRA

01χ~0

2χ~

28

[4] We can also predict the dark matter-nucleon scattering cross section but it has large theoretical error

p−01χ

σ

Determining Determining mSUGRAmSUGRA ParametersParameters

),tan,,(),(

002/14)(

eff

02/13eff

AmmfMmmfM

b β==

),tan,,(),(

002/12

02/11

AmmfMmmfM j

βττ

ττ

==

Solved by inverting the following functions:

140tan160

43505210

0

2/1

0

±=±=

±=±=

βA

mm

10 fb-1

),tan,( 02/102

~01

AmmZh βχ

=Ω

1fb 10 −=L1fb 50 −

29

Phys. Rev. Phys. Rev. LettLett. 100, (2008) 231802. 100, (2008) 231802

)fb 30( %7/ 1~~ 0

101

−−−

≈pp χχσδσ

)fb 70( %1.4)fb 30( %2.6/

1

12~

2~ 0

101

−

−

=

=ΩΩ hhχχ

δ

Direct Detection

DeterminingDetermining ΩΩhh2 2 in different modelsin different models

3030

Dutta, Gurrola, Kamon, Krislock , Nanopoulos, Lahanas, Mavromatos, PRD 09

Overdense region

Region where χ20 decays to Higgs (signal: Higgs (signal: Higgs+jets+missingHiggs+jets+missing energy)energy)

δΩCDM /ΩCDM ~ 150% (1000 fb-1)

Region where χ20 decays to staustau and HiggsHiggs

δΩCDM /ΩCDM ~ 20% (500 fb-1)

)300%(28~ 12

2−

ΩΩ fb

hhδ Dutta, Flanagan,

Kamon, Krislock, to appear

Signal: jets+ dileptons+missing energy

)fb 70( %1.4)fb 30( %2.6/

1

12~

2~ 0

101

−

−

=

=ΩΩ hhχχ

δ

Signal: jets+ditaus+missing energy

NonNon--Universal SUGRAUniversal SUGRA

107.0038.0

2

0

1/20

094.0h

GeV343A3.8,39.5 tanGeV,9.97.726m ,GeV2.35.499m,GeV26366m

+−=Ω

±=±=±=±=±=

βuH

Dutta, Kamon, Kolev, Krislock,Oh, arXiv: 1008.3380

189.0018.0

2

0

1/20

08.0h

GeV730A,6.439.5 tanGeV,13727m ,GeV3.96.499m,GeV57367m

+−=Ω

±=±=±=±=±=

βuH

For 1000 fb-1

For 100 fb-1

Nature may not be so kind Nature may not be so kind …… Our studies have been done based on a minimal scenario(= mSUGRA)…Let’s consider a non-universal scenario: Higgs non-

universality: mHu

, mHd

m0 (most plausible extension)easy to explain the DM content:

Signal: W+jets+taus

+missing energy

≠

31

Dark Matter particle

DM Particle: Direct Detection?

detector

µ(*)

The measurement at the LHC will pinpoint the parameters of SUSY models. We can predict the direct detection probability of dark matter particles.

Complementary

measurements !

32

Ongoing/future projects: CDMS, LUX, XENON100, COGENT, EDELWEISS etcStatus:–

DAMA/LIBRA, COGENT claim to have observed some events.

–

CDMS

claims to have observed two events–

Xenon 100 is taking more data

Status - Direct Detection

10-8 pb

33

DAMA

CDMSXENON100

mSUGRA Parameter space

Allahverdi, Dutta, SantosoPLB 687:225 ,2010

CoannihilationRegion

Focus point

• The bounds from CDMS/Xenon 100 have started becoming competitive with b s γ and Higgs mass constraints. 34

PAMELAPAMELA

3535

Recent results on anti-particle flux:

PAMELA has reported an excess of positrons up to 100 GeV, but no excess in anti-proton

PAMELAPAMELA……

3636

MSSM x U(1)MSSM x U(1)BB--LL

and PAMELAand PAMELA

3737

Dark Matter and positron excess:Wimp annihilation rate today: n B <sv>

B

is the boost factor<sv>f

=3x10-26

cm3/s annihilation cross-section around the freeze-out time

Model independent analysis shows: B ~ 10 (ee) -103(tt)Source of Boost: Astrophysics, particle physics

MSSM is further suppressed since the annihilation cross-section mostly is p-wave suppressed

<sv> v2 => <sv>today

=10-5<sv>f ∝

Non-thermal scenario can explain PAMELA anti proton/positron data

MSSM needs to be extended, e.g., with a U(1)_B-L

Leblond, Dutta, Sinha, PRD, 09; Allahverdi, Dutta, Santoso, PLB 09

ConclusionConclusion

38

SM of particle physics has fallen.Supersymmetry seems to be natural in the rescue act and the dark matter content of the universe can be explained in this theory.

The SUGRA model is consistent with the existing experimental results.

[1] LHC can probe the minimal SUGRA, non-

universal SUGRA model directly.All the dark matter allowed regions can be probed at the LHC

The dark matter content can be measured with a good accuracy

This accuracy depends on the final states

[2] This analysis can be applied to any SUSY model

Conclusion…[3] Direct detection experiments will simultaneously

confirm the existence of these models.

[4] Indirect detection experiments will also confirm

the existence of SUSY models

[5] Very exciting time ahead…

39