TeV-Scale Superpartners with an Unnatural Weak Scale Lawrence Hall - - PowerPoint PPT Presentation

TeV-Scale Superpartners with an Unnatural Weak Scale

Lawrence Hall University of California, Berkeley

Galileo Galilei Institute Beyond the SM after LHC 8 July 2013

OR

Multiverse SUSY

Outline

• 1. High Scale SUSY
• 3. TeV SUSY with
• 2. Spread SUSY

Hall, Nomura 0910.2235 Hall, Nomura 1111.4519 Bousso, Hall 1304.6407

ρD ∼ ρB

Outline

• 1. High Scale SUSY
• 3. TeV SUSY with
• 2. Spread SUSY

(multi)-TeV superpartners

Hall, Nomura 0910.2235 Hall, Nomura 1111.4519 Bousso, Hall 1304.6407

ρD ∼ ρB

Outline

• 1. High Scale SUSY
• 3. TeV SUSY with
• 2. Spread SUSY

All three have a fine-tuned weak scale Agnostic Multiverse

(multi)-TeV superpartners

Hall, Nomura 0910.2235 Hall, Nomura 1111.4519 Bousso, Hall 1304.6407

ρD ∼ ρB

Simplest Interpretation of LHC 8

125 GeV Higgs is fine tuned (to some degree)

v

Simplest Interpretation of LHC 8

125 GeV Higgs is fine tuned (to some degree)

v

v :

ΛCC :

A Simple Interpretation: tuning and size understood in the multiverse.

Simplest Interpretation of LHC 8

125 GeV Higgs is fine tuned (to some degree)

v

v :

ΛCC :

A Simple Interpretation: tuning and size understood in the multiverse.

˜ m

Multiverse arguments for the scale of superpartners?

Where are the Superpartners?

Cornered after 30+ years

• - of course, we need to be sure

TeV TeV

Munif Munif

Natural Susy

˜ mscalar ˜ mfermion

Without Naturalness

TeV TeV

Munif Munif

˜ mscalar ˜ mfermion

?

Where are the Superpartners?

Split SUSY

TeV TeV

Munif Munif

˜ mscalar ˜ mfermion

Arkani-Hamed, Dimopoulos hep-th/0405159

Gaugino/Higgsino dark matter

Pioneered multiverse reasoning in BSM particle physics Measurements could imply huge fine-tuning of weak scale

Anthropics for ΛCC



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Anthropics for ΛCC



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Martell, Shapiro, Weinberg astro-ph/9701099

−124 −123 −122 −121 −120 −119 log( ρΛ ) 0.0 0.2 0.4 0.6 0.8 Probability density 10

10

10

Fraction of virialized baryons

Anthropics for ΛCC



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Martell, Shapiro, Weinberg astro-ph/9701099

−124 −123 −122 −121 −120 −119 log( ρΛ ) 0.0 0.2 0.4 0.6 0.8 Probability density 10

10

10

Fraction of virialized baryons

−126 −125 −124 −123 −122 −121 −120 −119 log( ρΛ ) 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 Probability density

Bousso, Harnik, Kribs,Perez hep-th/0702115

Causal patch measure

Anthropics for v and ΛCC



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Agrawal, Barr, Donoghue, Seckel ph/9707380

v



No Complex Nuclei

rP

Anthropics for v and ΛCC

˜ m

??



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Agrawal, Barr, Donoghue, Seckel ph/9707380

v



No Complex Nuclei

rP

Scanning SUSY Breaking

Consider a power law distribution for in multiverse

dP ∝ ˜ mp d ln ˜ m ˜ m ≥ v

For include a factor for fine tuning of weak scale

dP ∝ ⇣ v ˜ m ⌘2 ˜ mp d ln ˜ m p 2

Natural weak scale Runaway to High Scale SUSY

˜ m

• 1. High Scale SUSY

Hall, Nomura 0910.2235

Runaway to High Scale SUSY

Runaway to High Scale SUSY

p > 2

dP d ln ˜ m

˜ m

v

Runaway to High Scale SUSY

Runaway to High Scale SUSY

p > 2

dP d ln ˜ m

˜ m

v

TeV TeV

Munif Munif

˜ ms

˜ mf

Higgs Mass Prediction

Hall, Nomura 0910.2235

Hu ↔ Hd

2 4 6 8 10 120 130 140 150

tanΒ MH GeV

mt = (173.1 ± 1.3) GeV

αs = 0.1176 ˜ m = 1014 GeV

Axion Dark Matter

˜ t loop ˜ m = 1014±2 GeV mh = (128 ± 3 ± 0.6 ± 1.0) GeV mt, αs

• 2. Spread SUSY

Hall, Nomura 1111.4519

Stabilizing SUSY Breaking at Multi-TeV

Runaway to High Scale SUSY

˜ m

dP d ln ˜ m

p > 2

v



?

Anthropics for v, , and

ΛCC

˜ m



ΛCC

No Large Scale Structure

Weinberg PRL 1987

rP

Agrawal, Barr, Donoghue, Seckel ph/9707380

v



No Complex Nuclei

rP

Hall, Nomura 1111.4519



Too much Dark Matter

˜ m

rP

A Boundary from LSP Freeze-Out

Assumptions:

• 1. The LSP is cosmologically stable

2.

TR ≥ ˜ m

• 3. No Dilution

The result:

Ωh2 / 1 hσAvi / m2

LSP / ˜

m2

ρD < ρc ˜ m < ˜ mc

A Boundary from LSP Freeze-Out

Assumptions:

• 1. The LSP is cosmologically stable

2.

TR ≥ ˜ m

• 3. No Dilution

The result:

Disks don’t fragment Tegmark, Aguirre, Rees, Wilczek astro-ph/0511774 Close encounters

{

Ωh2 / 1 hσAvi / m2

LSP / ˜

m2

ρD < ρc ˜ m < ˜ mc

A Boundary from LSP Freeze-Out

Assumptions:

• 1. The LSP is cosmologically stable

2.

TR ≥ ˜ m

• 3. No Dilution

The result:

mLSP ∼ αeff ⇤ TeqMP ≈ αeff 0.01 ⇥ 1 TeV

Unnatural Multi-TeV SUSY

Disks don’t fragment Tegmark, Aguirre, Rees, Wilczek astro-ph/0511774 Close encounters

{

Ωh2 / 1 hσAvi / m2

LSP / ˜

m2

ρD < ρc ˜ m < ˜ mc

Two Cases

Scalar Masses

X†X M 2 (Q†Q + . . . )

˜ m ∼ FX M ∼ m3/2

Two Cases

Scalar Masses

X†X M 2 (Q†Q + . . . )

˜ m ∼ FX M ∼ m3/2

X M W αWα

??

Two Cases

Scalar Masses

X†X M 2 (Q†Q + . . . )

˜ m ∼ FX M ∼ m3/2 TeV

˜ q, ˜ g, . . .

Multiverse MSSM Yes

X M W αWα

??

Two Cases

Scalar Masses

X†X M 2 (Q†Q + . . . )

˜ m ∼ FX M ∼ m3/2 TeV

˜ q, ˜ g, . . .

Multiverse MSSM Yes

X M W αWα

??

100 TeV

TeV

˜ q, . . . ˜ g, . . .

Spread SUSY No

1-loop anomaly mediation

Giudice, Luty, Murayama, Rattazzi hep-ph/9810442

Spread SUSY

TeV

Gaugino dark matter

TeV

Munif Munif

˜ ms

˜ mf

Spread SUSY

TeV

Gaugino dark matter

TeV

Munif Munif

˜ ms

˜ mf

125 GeV Scalar is “effortless”

˜ ms

Spread SUSY

TeV

Gaugino dark matter

Spread Hall, Nomura arXiv:1111.4519 Pure Gravity Mediation Ibe, Yanagida arXiv:1112.2462 Mini-Split Arvanitaki, Craig, Dimopoulos, Villadoro arXiv:1210.0555 Simply Unnatural Arkani-Hamed, Gupta, Kaplan, Weiner, Zorawski arXiv:1212.6971

TeV

Munif Munif

˜ ms

˜ mf

125 GeV Scalar is “effortless”

˜ ms

Susy Spectrum

Hall, Nomura, Shirai arXiv:1210.2395

0.2 0.5 1 2 10 100

12

M˜

g =10 TeV

5 TeV 3 TeV 2 TeV 1 TeV M ˜

W =3 TeV

1 TeV 500 GeV 200 GeV

Mass Spectrum

˜ m=102TeV ˜ m=103TeV =104TeV ˜ m=105TeV

10 100 1000

m3/2 [TeV]

m3/2

MP l MFund ∼ ˜ m m3/2

Dark Matter Abundance

Ω ˜

Wh2

cτ˜

g

1 < M˜

g < 3 TeV

AMS-02(KRA) AMS-02(MIN) Fermi Fermi(3×weaker)

Hall, Nomura, Shirai arXiv:1210.2395

10 100 1000

m3/2 [TeV]

1 0.1 0.01 10m 1m 0.1m 1cm 1mm 0.1mm

TR = 108 GeV

FI FO

m3/2

10 100 MP l MFund ∼ ˜ m m3/2

• 3. TeV Scale Superpartners with

Bousso, Hall 1304.6407

ρD ∼ ρB

No Catastrophic Boundary for Dark Matter

If this boundary does not exist,

• r is far from our universe,

are we forced to High Scale SUSY?

v ˜ m

dP d ln ˜ m



Too much Dark Matter

The Dark to Baryon Ratio

Why is ?

ζ = ρD ρB ∼ 1

The Dark to Baryon Ratio

Why is ?

ζ = ρD ρB ∼ 1

A multiverse explanation:

dP ∼ ζp/2 1 1 + ζ d ln ζ dP d ln ζ ζ 1

Same Causal Patch measure as for CC

0 < p < 2

LSP Dark Matter from Freeze-Out

ζ ∝ ρD ∝ ˜ m2

Electroweak fine-tune Measure

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

LSP Dark Matter from Freeze-Out

ζ ∝ ρD ∝ ˜ m2

Electroweak fine-tune Measure

Little SUSY Hierarchy

2 < p < 4

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

LSP Dark Matter from Freeze-Out

ζ ∝ ρD ∝ ˜ m2

Electroweak fine-tune Measure

Little SUSY Hierarchy

2 < p < 4

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

Bonus:

ρD ρB ∼ 1

• 4. Gravitino LSP

Hall, Ruderman, Volansky 1302.2620

TeV scale superpartners in unnatural theories rest on LSP freeze-out DM (multiverse or not) What if LSP does not reach Thermal Equilibrium?

m3/2 ∼ F MP l

Gravitino is often the LSP

Large Loop-hole?

TeV scale superpartners in unnatural theories rest on LSP freeze-out DM (multiverse or not) What if LSP does not reach Thermal Equilibrium?

m3/2 ∼ F MP l

Gravitino is often the LSP

Large Loop-hole?

Josh’s talk: No! Must include all production mechanisms

TR ˜ m = 103

˜ m . 9 TeV

10-6 10-5 10-4 10-3 10-2 10-1 1 101 102 103 104 102 103 104 105

m3ê2 @GeVD m é @GeVD

• verclosed

aeff = 0.03 HwinoL FO UV

m3ê2 > m é

BBN TR m é = 103

˜ m :

TeV multi-TeV

Summary: SUSY in the Multiverse

A Remarkable Situation

1973-2013: 40 years without BSM discovery 1998: 2013: SM Higgs, apparently tuned

ΛCC ∼ 1 GN t2

• bs

A Remarkable Situation

Naturalness/Symmetry may be in trouble A New Framework 1973-2013: 40 years without BSM discovery 1998: 2013: SM Higgs, apparently tuned

ΛCC ∼ 1 GN t2

• bs

A Remarkable Situation

Naturalness/Symmetry may be in trouble A New Framework

dP ∝ ˜ mp d ln ˜ m

A Multiverse

scanning mass scales: ΛCC, v, ... investigate

1973-2013: 40 years without BSM discovery 1998: 2013: SM Higgs, apparently tuned

ΛCC ∼ 1 GN t2

• bs

Natural SUSY

˜ m

dP d ln ˜ m

v

0 < p < 2

Natural SUSY

TeV TeV

Munif Munif

˜ ms

˜ mf

Cornered after 30+ years -- we need to be sure

Runaway to High Scale SUSY

p > 2

˜ m

dP d ln ˜ m

v

TeV TeV

Munif Munif

˜ ms

˜ mf

High Scale SUSY

mh = (128.0 ± 0.6 ± 1.0) GeV

Hu ↔ Hd

Axion Dark Matter

Stabilizing SUSY Breaking at Multi-TeV p > 2

v

˜ m

dP d ln ˜ m

Too much Dark Matter

OR

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

2 < p < 4

Stabilizing SUSY Breaking at Multi-TeV p > 2

v

˜ m

dP d ln ˜ m

Too much Dark Matter

TeV TeV

Munif Munif

˜ mf

˜ ms

Multiverse MSSM

TeV

Munif Munif

˜ ms

˜ mf Spread SUSY

OR

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

2 < p < 4

Stabilizing SUSY Breaking at Multi-TeV p > 2

v

˜ m

dP d ln ˜ m

Too much Dark Matter

TeV TeV

Munif Munif

˜ mf

˜ ms

Multiverse MSSM

TeV

Munif Munif

˜ ms

˜ mf Spread SUSY

1-20 TeV May need 100 TeV Collider

OR

˜ m

dP d ln ˜ m

v

˜ mc

˜ mp ˜ mp ✓ v2 ˜ m2 ◆ ˜ mp ✓ v2 ˜ m2 ◆ ✓ ˜ m2

c

˜ m2 ◆

2 < p < 4