Current Status of Particle Theory Modelspeople.physics.tamu.edu/dutta/talks_2016/colloquiumUHv1.pdf · Direct Detection Experiments: DAMA, CDMS, XENON 100, CoGeNT, LUX etc. ... Presentation

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Bhaskar DuttaTexas A&M University

Current Status of Particle Theory Models

February 5, 2016

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QuestionsSome Outstanding Issues of High Energy Theory

1. Dark Matter content ( is 27%)

2. Electroweak Scale

3. Ordinary Matter (baryon) Content ( is 5%)

4. Rapid Expansion of the Early Universe

5. Neutrino Mass...

Need: Theory, Experiment and Observation

DMΩ

bΩ

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Questions

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Current Status

Collider Experiments: LHCDirect Detection Experiments: DAMA, CDMS, XENON 100,

CoGeNT, LUX etc.Indirect Detection Experiments: Fermi, AMS, PAMELACosmic Microwave Sky: Planck, WMAPNeutrino Experiments: T2K, Daya Bay, Double CHOOZ,

RENO etc.

What have we learnt? What is the status of theory models? What do we expect in the near future?Are we closing in?

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(i) What have we learnt so far?LHC, Direct and Indirect Detection Experiments, Planck Data, Neutrino Experiments

(ii) Dark Matter: History

(iii) Dark Matter and Ordinary MatterContents

(iv) Dark Matter at the LHC

(v) Concluding Insights

Presentation Outline

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Large Hadron Collider(LHC)

Proton-Proton Collision

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Higgs Boson has been found (Mass (mh) 125 GeV)+Completes Standard Model

3 families of quarks, leptons, Gauge Bosons (force carriers) : W±, Z, γ, g

LHC: Higgs

Higgs mechanism breaks the SM symmetry spontaneously and generates mass for quarks, leptons, W, Z and Higgs

Symmetry breaking scale(Electroweak scale): 246 GeV

Much lower than the Planck scale: 1.22 x 1019 GeV

Mz=91.18 GeV, Mw=80.22 GeV

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• Higgs mass increases rapidly with scale mh2= m0

2+k Λ2: divergence problem solution needs fine tuning (1 part in 1032)

• SM prediction: mh<850 GeV to satisfy the unitarity in W scattering

• Fine tuning problem solved in supersymmetry due to fermions ↔ bosons symmetry

• Higgs mass predicted in SUSY Model?Minimal Supersymmetry Standard Model (MSSM):

loop correction prediction: mh<135 GeV

•Measured mass (125 GeV) appears in the tight MSSM window

LHC: Higgs

+= β2222 CosMM Zh Mz=91.18 GeV

Fundamental law of nature hypothesized to besymmetric between bosons and fermions

Fermion ↔Boson

LHC: Supersymmetrized SM

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Lightest neutralinois in the final state dark matter candidate!!

New colored particles: Squarks, gluinosNew non-colored particles: Sleptons, Neutralinos, Charginos etc

Minimal SupersymmetricStandard Model (MSSM)

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LHC: SupersymmetryMotivation: supersymmetry (SUSY) or beyond the SMSM does not provide solutions to any of the outstanding issues

e.g., 27% of the Universe (DM) Higgs mass divergence problem Baryon content Origin of Electroweak scale (associated with Higgs Boson) Inflation Neutrino mass

SUSY is very useful in explaining some of these issues

Have we seen SUSY? Not yet

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LHC: Supersymmetry

Most models predict: 1-3 TeV (colored particle masses)So far: No colored particle up to 1.5 TeV

Non-colored SUSY particles: 100 GeV to 1-2 TeV(Major role in the DM content of the Universe)

Weak LHC bound for non-colored particles hole in searches!

Trouble in Models with very tight correlation between colored and non-colored particles , e.g., minimal SUGRA/CMSSM

LHC + Direct Detection + Indirect Detection quite constraining

New Excess at the LHC?

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Direct Detection Experiments

Any parameter space left?

DM

DM

CDMS, DAMA, CoGeNT:Signal for Low mass DM

LUX: No signal for Low or High DM mass

arXiv:1310.8214

Status of New physics/SUSY in the direct detection experiments:

• Astrophysical and nuclear matrix element uncertainties• No signal: some particle physics models are ruled out

Indirect Detection: Fermi

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: smaller than the thermal valueoannv ><σ

>< vannσ

Thermal DM 27%

Gamma-rays constraints: Dwarf spheroidals, Galactic center

Experimental constraints:

Fermi Collaboration: arXiv:1503.02641

LargeCross-sectionis constrained

Indirect Detection Excess of positrons has been found by both

AMS, PAMELA and Fermi

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Dark Matter Mass: More than 100 GeVNo anti-proton excess found?Theory Models predictions: The excess will fall off

Pulsar can produce this excess

Is this excess due toDM annihilation?

Need Larger Cross-section (larger than the thermal cross-section 3x 10-26 cm3/sec)

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Latest result from Planck

http://public.planck.fr/images/resultats/2014-matiere-noire/plot_constraints_planck2014.jpg

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Probing Dark Matter

SM

Dark Energy68%

Atoms5%

Dark Matter27% +

Collider experiments

Overlapping region

DM content (CMB) + overlapping region:

Thermal history, particle physics models, astrophysics

Planck MeasurementsAccurate measurement of cosmic microwave backgroundPrecision cosmology

Number of relativistic degrees of freedom: Neff = 3.04 ± 0.18 (neutrinos)

For Inflation:What is the scale of inflation?

Can we have more than one inflaton field?

What types of inflation models are okay?

Can we accommodate these models in particle physics framework?

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NeutrinosRecent Neutrino Data:Accurate measurements of 2 mass differences and 3 mixing angles

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Questions:Dirac or Majorana type? Charge-Parity violation? Exact masses? How many?

Status of GUT (Grand Unified Theory) ?

SO(10)?

Summary

Direct Production at the collider: SUSY lurking around? More Higgs?

Direct Detection and LHC: Low/high mass DM particle?

Indirect Detection and LHC: DM thermal/non-thermal/multi-component? Seen a signal already at AMS?

Neutrinos experiments: CP phase? More than 3 neutrinos? Do we have GUT (Grand Unified Theory) model?

Planck: Model of Inflation?

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DM

~ 0.0000001 seconds

Dark Matter: When?

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Now

Dark Matter: ThermalProduction of thermal non-relativistic DM:

particlesSMDMDM ⇔+

particlesSMDMDM ⇒+

Universe cools (T<mDM)

particlesSMDMDM ⇔+

Boltzmann equation

][3 2,

2eqDMDMeqDM

DM nnvHndt

dn−−=+ σ

∫

∫+−

+−

=

6

/)(2

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3

6

/)(2

31

3

)2(

)2(21

21

π

πσ

σ TEE

TEE

eq epdpd

vepdpd

vvolnostppfdgn /.

)2(),(

3

3

≡= ∫ π

m/T

3* Tgn

snY

s

==Y

Dark Matter: Thermal

Freeze-Out: Hubble expansion dominates over the interaction rate

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v1~DM σρc

DMDM nm=Ω

20~ DM

fmT

Dark Matter content:

Assuming : 2

2

~vχ

χασmf

αχ~O(10-2) with mχ ~ O(100) GeVleads to the correct relic abundance

m/T

freeze out

scm3

26103v −×=σY becomes constant for T>Tf

Nc G

Hπ

ρ83 2

0=

Y

Y~10-11 for mχ~100 GeVto satisfy the DM content

Thermal Dark Matter

DM particle + DM Particle SM particles

Annihilation Cross-section Rate:

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>< vannσ

DM

DM

DM

DM

f: SM particles; h, H, A: various Higgs, : SUSY particleNote: All the particles in the diagram are colorless

v1~DM σ

Ω

DM Abundance:

f~

scm3

26103v −×=σWe need to satisfy thermal DM requirement

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Suitable DM Candidate: Weakly Interacting Massive Particle (WIMP)

Typical in Physics beyond the SM (LSP, LKP, …)

Most Common: Neutralino (SUSY Models)

Neutralino: Mixture of Wino, Higgsino and Bino

Neutralino can give rise to larger/smaller annihilation rate

Larger/Smaller Annihilation Non-thermal Models

Thermal Dark Matter

Thermal Dark Matter

Dark Energy68%

Atoms5%

Dark Matter27%

v1~DM σ

Ω

20~ DM

fmT

Dark Matter content:

Weak scale physics :

2

2

~vχ

χασmf

αχ~O(10-2) with mχ ~ O(100) GeVleads to the correct relic abundance

freeze out

scm3

26103v −×=σ

Mp

Inflation

TeV

GeV

MeVBBN

~ WIMP freeze-out

Non-standard thermal history at is generic in some explicit high Scale theories.

fTfTT >

Acharya, Kumar, Bobkov, Kane, Shao’08Acharya, Kane, Watson, Kumar’09Allahverdi, Cicoli, Dutta, Sinha,’13

Status of Thermal DMThermal equilibrium above is an assumption.

DM content will be different in non-standard thermal histories

Barrow’82, Kamionkowski, Turner’90

DM will be a strong probe of the thermal history after it is discovered and a model is established.

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Non-Thermal DM

Decay of moduli/heavy field occurs at:

)MeV5(TeV100

~2/3

2/1

φmcTr

Tr ~ MeV : Not allowed by BBN

[Moduli : heavy scalar fields gravitationally coupled to matter]

>< vannσ : different from thermal average, is not 27% Non-thermal DM can be a solution

DM from the decay of heavy scalar field, e.g., Moduli decay

For Tr<Tf: Non-thermal dark matter

v1~DM σ

Ω

Decay of moduli produce both DM and ordinary matter

Moroi, Randall’99; Acharya, Kane, Watson’08,Randall; Kitano, Murayama, Ratz’08; Dutta, Leblond, Sinha’09; Allahverdi, Cicoli, Dutta, Sinha,’13

MpInflatio

TeV

GeV

MeV

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Non-thermal DM

Non-thermal DM Production from moduli decay

Ordinary Matter and DM from moduli decay ⇒ Cladogenesis of DM and Ordinary Matter (Baryons) [Allaverdi, Dutta, Sinha’11]

Cladogenesis: is an evolutionary splitting event in a species in which each branch and its smaller branches forms a "clade", an evolutionary mechanism and a process of adaptive evolution that leads to the development of a greater variety of sister species.

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Mp

Inflation

TeV

GeV

MeVBBN

~ WIMP freeze-out

Mp

Inflation

TeV

GeV

MeVBBN

Non-thermal DM

Large multicomponent/non-thermal; Small Non-thermal

Probe directly at Indirect and Collider experiments

>< vannσ

DM content: summary

>< vannσ

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Dark Matter at the LHCAnnihilation of lightest neutralinos (DM particles) quarks, leptons etc.At the LHC: proton + proton DM particles

DM Annihilation diagrams: mostly non-colored particlese.g., sleptons, staus, charginos, neutralinos, etc.

How do we produce these non-colored particles and the DM particle at the LHC? Can we measure the annihilation cross-section ?

1. Cascade decays of squarks and gluinos2. Vector Boson fusion

>< vannσ

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The signal : SM particles + DM particle(Missing energy)

Via Cascade decays at the LHC

(or l+l-, τ+τ−)DM

DMColored particles are produced and they decay finally into the weakly interacting stable particle

High PT jet

(or l+l-, τ+τ−)LHC is very complicated

DM at the LHC Via VBF

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LHC has a blind spot for productions of non-colored particle

The W boson (colorless) coming out of high energy protons can produce colorless particlesVector Boson Fusion(VBF

Special search strategy needed to extract the signal

New way of understanding DM or new physicssector at the LHC

Refs (For example): A. Datta, P. Konar, and B. Mukhopadhyaya, 02. G. Giudice, T. Han, K. Wang, and L.T. Wang, 13

A.G. Delannoy, B. Dutta, A. Gurrola, W. Johns, T. Kamon, E. Luiggi, A. Melo, P. Sheldon, K. Sinha, K. Wang, S. Wu, ‘13

Dutta, Gurrola, Kamon, John, Sinha, Shledon; ‘13

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Cross Sections via VBFDM Via W at the LHCjjpp 0

10

1~~ χχ→

DM

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DM Content via VBF

Simultaneous fit of various observables:

How to check that LHC observations lead to correct dark matter content? Measure Ω at the LHC (Ω is 27%: Planck Measurement)

New particle at the LHC?

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Q

g New Quarks: Q, New Leptons: L New scalar particles: X

Do we need dark matter particles to explain the data?

Dutta, Gao, Ghosh, Gogoladze, Li, e-Print: e-Print: arXiv:1512.05439Dutta, Gao, Ghosh, Gogoladze, Li, Walker, e-Print: e-Print: arXiv:1601.00866

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Concluding Insights Model ideas have constraints from LHC, Planck,

Neutrino data, direct and indirect detection constraints Higgs mass is within the supersymmetry model prediction

window LHC measurements so far seem to be preferring

Non-thermal DMNon-thermal scenarios can allow us to understand the

Ordinary Matter-Dark Matter coincidence puzzle

Determination of the property of DM is crucial: LHC and Indirect detections identify DM model

Need to investigate colorless particles (suitable for DM calculation) at the LHC

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Acknowledgement

Kechen Wang (PhD 2014), Tathagata Ghosh, Sean Wu,Yu GaoStudents/Post-Doctoral Fellow:

Rouzbeh Allahverdi, Richard Arnowitt, Michele Cicoli, James Dent, Ricardo Eusebi, Ilia Gogoladze, Alfredo Gurrola, Teruki Kamon, Tainjun Li, Rabindra Mohapatra, Dimitri Nanopoulos, Farinaldo Queirez, Fernando Quevedo, Qaisar Shafi, Kuver Sinha, Louis Strigari, David Toback, Joel Walker

Research Funded by Department of Energy (DOE)

Faculty from TAMU and other places: