Extra Dimensions: From Colliders to Cosmology

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Extra Dimensions From Colliders to Cosmology

• Large Extra Dimensions (Primordial Black Holes)
• Universal Extra Dimensions (KK Bino)
• Warped Extra Dimensions (KK ?R )

Collider signals DM properties
Thanks to T. Tait!
J. Hewett
Michell Symposium 2007
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Kaluza-Klein tower of particles

• E2 (pxc)2 (pyc)2 (pzc)2 (pextrac)2
  (mc2)2

In 4 dimensions, looks like a mass!
pextra is quantized n/R
Tower of massive particles
Large radius gives finely separated Kaluza-Klein
particles
Small radius gives well separated Kaluza-Klein
particles
Small radius
Large radius
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Large Extra Dimensions
Arkani-Hamed, Dimopoulos, Dvali, SLAC-PUB-7801

• Motivation solve the hierarchy problem by
  removing it!
• SM
  fields confined to 3-brane
• 
  Gravity becomes strong in the bulk

Gauss Law MPl2 V? MD2? , V? Rc ?
MD Fundamental scale in the bulk TeV
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Kaluza-Klein Modes in a Detector
Indirect Signature
Missing Energy Signature pp ? g Gn
Vacavant, Hinchliffe
JLH
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Graviton Exchange Modified with Running
Gravitational Coupling

• Insert Form Factor in
• coupling to parameterize
• running
• MD-2 1q2/t2M2 -1
• Could reduce signal!

t?
1
SM
0.5
D34 M 4 TeV
JLH, Rizzo, to appear
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Constraints from Astrophysics/Cosmology
Cullen, Perelstein Barger etal, Savage etal

• Supernova Cooling
• NN ? NN Gn can cool supernova too rapidly
• Cosmic Diffuse ? Rays
• NN ? NN Gn ???
• ?? ? Gn ? ??
• Matter Dominated Universe
• too many KK states
• Neutron Star Heat Excess
• NN ? NN Gn
• becomes
  trapped in neutron star halo
• and heats
  it

Hannestad, Raffelt Hall, Smith
-
Fairbairn
Hannestad, Raffelt
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Astrophysical Constaints MD in TeV
Hannestad, Raffelt

• ?
  2 3 4 5
• Supernova Cooling 9
  0.66 0.01
• Cosmic Diffuse ?-rays
• Sne
  28 1.65 0.02
• Sne Cas A 14
  1.2 0.02
• Neutron Star 39
  2.6 0.4
• Matter Dominated Universe 85 7
  1.5
• Neutron Star Heat Excess 700 25
  2.8 0.57

Low MD disfavored for ? 3
Can be evaded with hyperbolic manifolds
- Starkman, Stojkovic, Trodden
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Black Hole Production _at_ LHC
Dimopoulos, Landsberg Giddings, Thomas

• Black Holes produced when ?s gt M
• Classical Approximation space curvature
  ltlt E

E/2
b lt Rs(E) ? BH forms
b
E/2
Geometric Considerations ?Naïve ?Rs2(E),
details show this holds up to a factor
of a few
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Black Hole event simulation _at_ LHC
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Decay Properties of Black Holes (after Balding)

• Decay proceeds by thermal emission of Hawking
  radiation

n determined to ?n 0.75 _at_ 68 CL for n2-6 from
TH and ? This procedure doesnt work for large n
At fixed MBH, higher dimensional BHs are hotter
?N? 1/?T? ? higher dimensional BHs emit fewer
quanta, with each quanta having higher energy
Multiplicity for n 2 to n 6
Harris etal hep-ph/0411022
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pT distributions of Black Hole decays
Provide good discriminating power for value of
n Generated using modified CHARYBDIS linked to
PYTHIA with M 1 TeV
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Production rate is enormous!
Determination of Number of Large Extra Dimensions
1 per sec at LHC!
JLH, Lillie, Rizzo
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Primordial Microscopic Black Holes

• Produced in high-energy collisions in early
  universe
• Rapid growth by absorption of matter from
  surrounding plasma

Empty Bulk
Mass density determined by TI
Excluded

• Demand
• Black Holes not overclose the universe
• Must not dominate energy density during BBN

Thermalized Bulk
Conley, Wizansky
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Universal Extra Dimensions
Appelquist, Cheng, Dobrescu

• All SM fields in TeV-1, 5d, S1/Z2 bulk
• No branes! ? translational invariance is
  preserved
• ? tree-level conservation
  of p5
• KK number conserved at tree-level
• broken at higher order by boundary
  terms
• KK parity conserved to all orders, (-1)n
• Consequences
• KK excitations only produced in pairs
• Relaxation of collider precision EW constraints
• Rc-1 300 GeV!
• Lightest KK particle is stable (LKP) and is Dark
  Matter candidate
• Boundary terms separate masses and give SUSY-like
  spectrum

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Universal Extra Dimensions Bosonic SUSY
Spectrum looks like SUSY !

• Phenomenology looks like Supersymmetry
• Heavier KK particles cascade down to LKP
• LKP Photon KK state
• appears as missing ET
• SUSY-like Spectroscopy
• Confusion with SUSY if discovered _at_ LHC !

Chang, Matchev,Schmaltz
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How to distinguish SUSY from UED I

• Observe KK states in ee- annihilation
• Measure their spin via
• Threshold production, s-wave
• vs p-wave
• Distribution of decay products
• However, could require CLIC
• energies...

JLH, Rizzo, Tait Datta, Kong, Matchev
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How to distinguish SUSY from UED II
Datta, Kong, Matchev

• Observe higher level (n 2) KK
• states
• Pair production of q2q2, q2g2, V2 V2
• Single production of V2 via (1) small KK number
  breaking couplings and (2) from cascade decays of
  q2

Discovery reach _at_ LHC
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How to distinguish SUSY from UED III

• Measure the spins of the KK states _at_ LHC
  Difficult!
• Decay chains in SUSY and UED

Form charge asymmetry
Works for some, but not all, regions of parameter
space
Smillie, Webber
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Identity of the LKP

• Boundary terms (similar to SUSY soft-masses)
• Induced _at_ loop-level (vanish _at_ cut-off)
• Determine masses couplings of entire KK tower
• ?1 ?2 ?3
• Smallest corrections to U(1) KK state
• NLKP is eR(1)
• ?M 1/R gt v
• LKP is almost pure Bino KK B?(1)

Bino-Wino mass matrix, n1
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Thermal Production and Freeze Out

• Assume LKP in thermal equilibrium in early
  universe
• Falls out of equilibrium as universe expands
• Below freeze-out, density of LKP WIMPS per
  co-moving volume is fixed

For 1 TeV KK, Tf 40 TeV
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Co-annihilation

• eR(1) may substantially affect relic density if
  it is close in mass to B(1)
• eR(1) has same interaction efficiency
• freeze-out temp is unaffected
• eR(1) left after freeze-out
• Eventually eR(1) ? e(0) B(1)
• Net relic density of B(1) is increased

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Relic Density

• ? scaled mass splitting between eR(1) and B(1)
• ? 0.05
• 0.01
• ?h2 0.11 ? 0.006 yields for R

1 flavor 5 flavors
B(1) alone
5d range of 600-900 GeV
6d range of 425-625 GeV
Tait, Servant
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More Complete Calculations
WMAP
? 0.01 solid 0.05 dashed
Quasi-degenerate KK quarks and gluons
Quasi-degenerate KK eL(1)
Kong, Matchev
Burnell, Kribs
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Add Gravity in the Bulk
mG1 gt mB1
mG1 lt mB1
KK graviton decays into B(1) (mWG KK scale from
relic density without graviton)
Super-WIMPS!
Feng, Rajaraman, Takayama
Shah, Wagner
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Direct Detection of LKP

• LKP nucleon scattering

Tait, Servant
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Localized Gravity Warped Extra Dimensions
Randall, Sundrum
Bulk Slice of AdS5 ?5 -24M53k2 k curvature
scale
Naturally stablized via Goldberger-Wise
Hierarchy is generated by exponential!
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Kaluza-Klein Modes in a Detector SM on the brane
Number of Events in Drell-Yan _at_ LHC
For this same model embedded in a string theory
AdS5 x S?
Unequal spacing signals curved space
Davoudiasl, JLH, Rizzo
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Kaluza-Klein Modes in a Detector SM off the brane
Fermion wavefunctions in the bulk decreased
couplings to light fermions for gauge graviton
KK states
-
gg ? gn ? tt _at_ LHC
gg ? Gn ? ZZ _at_ LHC
Lillie, Randall, Wang
Agashe, Davoudiasl, Perez, Soni
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Issue Top Collimation
-
gg ? gn ? tt
g1 4 TeV
g1 2 TeV
Lillie, Randall, Wang
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Warped Extra Dimension with SO(10) in the bulk

• Splits families amongst 16 of SO(10) with
  different Z3 charges Baryon symmetry in bulk
• Lightest Z-odd particle, ?R KK state, is stable

Bold-face particles have zero-modes
Gives correct relic density for wide range of
masses
Agashe, Servant
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Cosmic Ray Sensitivity to Black Hole Production
No suppression
Ringwald, Tu
Anchordoqui etal
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Summary of Expt Constraints on MD
Anchordoqui, Feng Goldberg, Shapere