Search for supersymmetry
This presentation is the property of its rightful owner.
Sponsored Links
1 / 58

Search for Supersymmetry PowerPoint PPT Presentation


  • 54 Views
  • Uploaded on
  • Presentation posted in: General

Search for Supersymmetry. Outline. Introduction to supersymmetry Phenomenology of the CMSSM Non-universal scalar masses ? Non-universal Higgs masses (NUHM) Options for the LSP Gravitino dark matter New possibilities for collider phenomenology. Loop Corrections to Higgs Mass 2.

Download Presentation

Search for Supersymmetry

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Search for supersymmetry

Search for Supersymmetry


Outline

Outline

  • Introduction to supersymmetry

  • Phenomenology of the CMSSM

  • Non-universal scalar masses?

  • Non-universal Higgs masses (NUHM)

  • Options for the LSP

  • Gravitino dark matter

  • New possibilities for collider phenomenology


Loop corrections to higgs mass 2

Loop Corrections to Higgs Mass2

  • Consider generic fermion and boson loops:

  • Each is quadratically divergent: ∫Λd4k/k2

  • Leading divergence cancelled if

    Supersymmetry!

2

∙2


Other reasons to like susy

Other Reasons to like Susy

It enables the gauge couplings to unify

It predicts mH < 150 GeV

As suggested

by EW data

JE, Nanopoulos, Olive + Santoso: hep-ph/0509331

Approved by Fabiola Gianotti


Search for supersymmetry

Astronomers say

that most of the

matter in the

Universe is

invisible

Dark Matter

Lightest Supersymmetric particles ?

We shall look for

them with the

LHC


Minimal supersymmetric extension of standard model mssm

Minimal Supersymmetric Extension of Standard Model (MSSM)

  • Particles + spartners

  • 2 Higgs doublets, coupling μ, ratio of v.e.v.’s = tan β

  • Unknown supersymmetry-breaking parameters:

    Scalar massesm0, gaugino massesm1/2,

    trilinear soft couplingsAλ, bilinear soft couplingBμ

  • Often assume universality:

    Singlem0, singlem1/2, singleAλ,Bμ: not string?

  • Called constrained MSSM = CMSSM

  • Minimal supergravity (mSUGRA) predicts additional relations for gravitino mass, supersymmetry breaking:

    m3/2 = m0,Bμ = Aλ – m0


Lightest supersymmetric particle

Lightest Supersymmetric Particle

  • Stable in many models because of conservation of R parity:

    R = (-1) 2S –L + 3B

    where S = spin, L = lepton #, B = baryon #

  • Particles have R = +1, sparticles R = -1:

    Sparticles produced in pairs

    Heavier sparticles  lighter sparticles

  • Lightest supersymmetric particle (LSP) stable


Possible nature of lsp

Possible Nature of LSP

  • No strong or electromagnetic interactions

    Otherwise would bind to matter

    Detectable as anomalous heavy nucleus

  • Possible weakly-interacting scandidates

    Sneutrino

    (Excluded by LEP, direct searches)

    Lightest neutralino χ

    Gravitino

    (nightmare for astrophysical detection)


Constraints on supersymmetry

gμ - 2

Constraints on Supersymmetry

  • Absence of sparticles at LEP, Tevatron

    selectron, chargino > 100 GeV

    squarks, gluino > 250 GeV

  • Indirect constraints

    Higgs > 114 GeV, b -> s γ

  • Density of dark matter

    lightest sparticle χ:

    WMAP: 0.094 < Ωχh2 < 0.124


Current constraints on cmssm

Current Constraints on CMSSM

Assuming the

lightest sparticle

is a neutralino

Excluded because stau LSP

Excluded by b  s gamma

WMAP constraint on relic density

Excluded (?) by latest g - 2

JE + Olive + Santoso + Spanos


Current constraints on cmssm1

Current Constraints on CMSSM

Different

tan β

sign of μ

Impact of

Higgs

constraint

reduced

if larger mt

Focus-point

region far up

JE + Olive + Santoso + Spanos


Sparticles may not be very light

Sparticles may not be very light

Full

Model

samples

← Second lightest visible sparticle

Detectable

@ LHC

Provide

Dark Matter

Dark Matter

Detectable

Directly

Lightest visible sparticle →

JE + Olive + Santoso + Spanos


Missing energy detection @ lhc

Missing Energy Detection @ LHC

Sensitive to missing transverse energy

carried away by neutral particles:

e.g., neutrinos, neutralinos


Supersymmetry searches at lhc

Supersymmetry Searches at LHC

LHC reach in

supersymmetric

parameter space

`Typical’ supersymmetric

Event at the LHC

Can cover most

possibilities for

astrophysical

dark matter


Supersymmetric benchmark studies

Supersymmetric Benchmark Studies

Lines in

susy space

allowed by

accelerators,

WMAP data

Specific

benchmark

Points along

WMAP lines

Sparticle

detectability

Along one

WMAP line

Calculation

of relic

density at a

benchmark

point

Battaglia, De Roeck, Gianotti, JE, Olive, Pape


Sparticle signatures along wmap lines

SparticleSignaturesalongWMAPlines

Relatively small

branching ratios in CMSSM

Z

h

Average numbers

of particles per

sparticle event

τ

3l

Battaglia, De Roeck, Gianotti, JE, Olive, Pape


Summary of lhc scapabilities and other accelerators

Summary of LHCScapabilities … and OtherAccelerators

LHC almost

`guaranteed’

to discover

supersymmetry

if it is relevant

to the mass problem

Battaglia, De Roeck, Gianotti, JE, Olive, Pape


Tests of unification ideas

Tests of Unification Ideas

For gauge couplings

For sparticle masses


Precision observables in susy

Can one estimate the scale of supersymmetry?

Precision Observables in Susy

Sensitivity to m1/2

in CMSSM

along WMAP lines

for different A

mW

tan β = 10

tan β = 50

sin2θW

Present & possible

future errors

JE + Heinemeyer +Olive +Weiglein


Search for supersymmetry

MoreObservables

tan β = 10

tan β = 50

b → sγ

tan β = 10, 50

Bs → μμ

gμ- 2

JE + Heinemeyer +Olive +Weiglein


Global fits to present data

Global Fits to Present Data

Including mW , sin2θW, b → sγ, gμ - 2

As functions of m1/2 in CMSSM for tan β = 10, 50

JE + Heinemeyer +Olive +Weiglein


Global fits to present data1

χ

χ2,χ±

Global Fitsto Present Data

χ3,χ2±

τ1

Preferred

sparticle

masses for

tan β = 10

e1

e2

JE + Heinemeyer +Olive +Weiglein


Global fits to present data2

t1

t2

Global Fitsto Present Data

b1

b2

Preferred

sparticle

masses for

tan β = 10

g

A

Within reach of LHC!

JE + Heinemeyer +Olive +Weiglein


Beyond the cmssm

Beyond the CMSSM


More general supersymmetric models

More General Supersymmetric Models

  • MSSM with more general pattern of supersymmetry breaking:

    non-universal scalar masses m0

    and/or gaugino masses m½

    and/or trilinear couplings A0

  • Nature of the lightest supersymmetric particle (LSP)

  • Extended particle content:

    non-minimal supersymmetric model (NMSSM)


Non universal scalar masses

Non-Universal Scalar Masses

  • Different sfermions with same quantum #s?

    e.g., d, s squarks?

    disfavoured by upper limits on flavour-changing neutral interactions

  • Squarks with different #s, squarks and sleptons?

    disfavoured in various GUT models

    e.g., dR = eL, dL = uL = uR = eR in SU(5), all in SO(10)

  • Non-universal susy-breaking masses for Higgses?

    No reason why not!


Non universal higgs masses nuhm

Non-Universal Higgs Masses (NUHM)

  • Generalize CMSSM (+)

    mHi2 = m02(1 + δi)

  • Free Higgs mixing μ,

    pseudoscalar mass mA

  • Larger parameter space

  • Constrained by vacuum

    stability


Sampling of m 1 2 m 0 planes in nuhm

Sampling of (m1/2, m0) Planes in NUHM

New vertical

allowed strips

appear

JE + Olive + Santoso + Spanos


Low energy effective supersymmetric theory

Low-Energy Effective Supersymmetric Theory

  • Assume universality for sfermions with same quantum numbers (but different generations)

  • Require electroweak vacuum to be stable (RGE not → negative mass2)

    up to GUT scale (LEEST)

    up to 10 TeV (LEEST10)

  • Qualitatively similar to NUHM

    not much freedom to adjust squarks/sleptons


Sparticles may not be very light1

Sparticles may not be very light

Full

Model

samples

← Second lightest visible sparticle

Detectable

@ LHC

Provide

Dark Matter

Dark Matter

Detectable

Directly

Lightest visible sparticle →

JE + Olive + Santoso + Spanos


Gravitino dark matter

Gravitino Dark Matter?


Possible nature of lsp1

Possible Nature of LSP

  • No strong or electromagnetic interactions

    Otherwise would bind to matter

    Detectable as anomalous heavy nucleus

  • Possible weakly-interacting scandidates

    Sneutrino

    (Excluded by LEP, direct searches)

    Lightest neutralino χ

    Gravitino

    (nightmare for astrophysical detection)


Possible nature of nlsp

Possible Nature of NLSP

  • NLSP = next-to-lightest sparticle

  • Very long lifetime due to gravitational decay, e.g.:

  • Could be hours, days, weeks, months or years!

  • Generic possibilities:

    lightest neutralino χ

    lightest slepton, probably lighter stau

  • Constrained by astrophysics/cosmology


Different regions of sparticle parameter space if gravitino lsp

Different

Gravitino

masses

DifferentRegions of SparticleParameterSpace ifGravitino LSP

χ NLSP

stau NLSP

Density below

WMAP limit

Decays do not affect

BBN/CMB agreement

JE + Olive + Santoso + Spanos


Minimal supergravity model msugra

Neutralino LSP

region

stau LSP

(excluded)

Gravitino LSP

region

tan β fixed by vacuum conditions

Minimal Supergravity Model (mSUGRA)

More constrained than CMSSM: m3/2 = m0, Bλ = Aλ – 1

Excluded by b  s γ

LEP constraints

Onmh, chargino

JE + Olive + Santoso + Spanos


Light nuclei bbn vs cmb

Light Nuclei: BBN vs CMB

Good agreement for D/H, 4He: discrepancy for 7Li?

Observations

Calculations

Cyburt + Fields + Olive + Skillman


Constraints on unstable relics

Constraints on Unstable Relics

  • 7Li < BBN?

  • Effect of relic decays?

  • Problems with D/H

  • 3He/D too high!

  • Interpret as upper

    limits on abundance

    of metastable heavy

    relics

JE + Olive + Vangioni


Different regions of sparticle parameter space if gravitino lsp1

DifferentRegions of SparticleParameterSpace ifGravitino LSP

χ NLSP

stau NLSP

Density below

WMAP limit

Decays do not affect

BBN/CMB agreement

JE + Olive + Santoso + Spanos


Regions allowed in different scenarios for supersymmetry breaking

CMSSM

Benchmarks

GDM

Benchmarks

Regions Allowedin Different Scenarios forSupersymmetryBreaking

NUHM

Benchmarks

with neutralino NLSP

with stau NLSP

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Spectra in nuhm and gdm benchmark scenarios

Spectra inNUHM and GDMBenchmarkScenarios

Typical example of

non-universal Higgs masses:

Models with gravitino LSP

Models with stau NLSP

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Properties of nuhm and gdm models

Properties of NUHM and GDM Models

  • Relic density ~ WMAP in NUHM models

  • Generally < WMAP in GDM models

    Need extra source of gravitinos at high temperatures, after inflation?

  • NLSP lifetime: 104s < τ < few X 106s

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Neutralino masses and decay modes

χh, χZ may be

large in NUHM

Neutralino Masses and Decay Modes

χh, χZ small

in CMSSM

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Final states in gdm models with stau nlsp

Final States in GDM Models with Stau NLSP

  • All decay chains

    end with lighter stau

  • Generally via χ

  • Often via heavier

    sleptons

  • Final states contain

    2 staus, 2 τ,

    often other leptons

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Kinematic distributions point

Kinematic Distributions: Point ε

  • Staus come with

    many jets & leptons

    with pT hundreds of GeV,

    produced centrally

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Kinematic distributions point1

Kinematic Distributions: Point ζ

  • Staus come with

    many jets & leptons

    with pT hundreds of GeV,

    produced centrally

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Stau mass measurements by time of flight

Stau Mass Measurements by Time-of-Flight

  • Event-by-event

    accuracy < 10%

  • < 1% with full sample

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Numbers of visible sparticle species

Numbers of Visible Sparticle Species

At different

colliders


Slepton trapping at the lhc

Slepton Trapping at the LHC?

If stau next-to-lightest sparticle (NLSP)

may be metastable

may be stopped in detector/water tank?

Trapping

rate

Kinematics

Feng + Smith

Hamaguchi +Kuno + Nakaya + Nojiri


Stau momentum spectra

Stau Momentum Spectra

  • βγ typically peaked ~ 2

  • Staus with βγ < 1 leave central tracker

    after next beam crossing

  • Staus with βγ < ¼ trapped inside calorimeter

  • Staus with βγ < ½ stopped within 10m

  • Can they be dug out?

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Extract cores from surrounding rock

Very little room for water tank in LHC caverns,

only in forward directions where few staus

Extract Cores from Surrounding Rock?

  • Use muon system to locate impact point on cavern wall with uncertainty < 1cm

  • Fix impact angle with accuracy 10-3

  • Bore into cavern wall and remove core of size 1cm × 1cm × 10m = 10-3m3 ~ 100 times/year

  • Can this be done before staus decay?

    Caveat radioactivity induced by collisions!

    2-day technical stop ~ 1/month

  • Not possible if lifetime ~104s, possible if ~106s?

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Detect staus in mass spectrometer

Detect Staus in Mass Spectrometer?

  • Each core ~ 1cm × 1cm × 10m

  • ‘Region of interest’ ~ 1m long

  • Contains ~ 2 × 1027 nucleons, i.e., 1027 protons

  • Present best limits from water ~ 10-29/proton

  • Sensitivity possible in principle

  • How quickly could the volume be searched?

  • Have at most a few weeks!

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Detect supersymmetric decay albedo

Detect Supersymmetric Decay Albedo?

  • Look for staus stopping ~ 10m from detector

  • Later decay → τ + gravitino

  • τ → μ with branching ratio ~ 16%

  • Characteristic energies ~ (1/6) mstau

    ~ 25 to 50 GeV

  • Geometric acceptance for upward-going μ ~ 1/12 → ~ 1.3% of stau decays detectable

    → ~ 100 events/year in benchmark scenario ε

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Caveat cosmic ray background

Caveat Cosmic-RayBackground

  • Background of cosmic-ray μ

    ~ 100 events/year

  • Similar energy range

  • Signal might be visible in

    benchmark scenario ε

  • Not in scenarios ζ and η

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Potential measurement accuracies

Potential Measurement Accuracies

Gravitino Dark Matter even more interesting

than Neutralino Dark Matter!

Measure staumass to 1%

Measure m½ to 1%

via cross section, other masses?

Distinguish points ζ, η

De Roeck, JE, Gianotti, Moortgat, Olive + Pape: hep-ph/0508198


Summary

Summary

  • The ‘C’ in CMSSM signifies ‘conservative’

  • Many more exotic supersymmetric phenomenologies are possible

  • Gravitino dark matter is one example

  • Not to mention breaking of R parity …

    … nor split supersymmetry

  • Supersymmetry is the most ‘expected’ surprise at the LHC

  • Expect it to appear in an unexpected way!


Elastic scattering cross sections

Elastic Scattering Cross Sections

From global fit to accelerator data

Latest experimental upper limit

JE + Olive + Santoso + Spanos: hep-ph/0502001


Direct cdm detection in nuhm leest

Direct CDM detection in NUHM/LEEST

Cross section similar

in NUHM/LEEST

Cross section depends

on πN σ term

Cross section depends

on sign of μ

Some NUHM/LEEST

models already excluded

JE + Olive + Santoso + Spanos


  • Login