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

Galileo Galilei Institute Beyond the SM after LHC 8 July 2013 TeV-Scale Superpartners with an Unnatural Weak Scale Lawrence Hall University of California, Berkeley

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Multiverse SUSY

Outline 1. High Scale SUSY Hall, Nomura 0910.2235 2. Spread SUSY Hall, Nomura 1111.4519 3. TeV SUSY with ρ D ∼ ρ B Bousso, Hall 1304.6407

Outline 1. High Scale SUSY Hall, Nomura 0910.2235 2. Spread SUSY (multi)-TeV Hall, Nomura 1111.4519 superpartners 3. TeV SUSY with ρ D ∼ ρ B Bousso, Hall 1304.6407

Outline 1. High Scale SUSY Hall, Nomura 0910.2235 2. Spread SUSY (multi)-TeV Hall, Nomura 1111.4519 superpartners 3. TeV SUSY with ρ D ∼ ρ B Bousso, Hall 1304.6407 Agnostic All three have a fine-tuned weak scale Multiverse

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

Simplest Interpretation of LHC 8 125 GeV Higgs is fine tuned (to some degree) v A Simple Interpretation: Λ CC : tuning and size understood in the multiverse. v : Multiverse arguments for ˜ m the scale of superpartners?

Where are the Superpartners? ˜ m scalar M unif Natural Susy TeV TeV M unif ˜ m fermion Cornered after 30+ years -- of course, we need to be sure

Without Naturalness ˜ m scalar M unif ? TeV TeV M unif ˜ m fermion Where are the Superpartners?

Split SUSY Pioneered multiverse reasoning in BSM particle physics Arkani-Hamed, Dimopoulos ˜ hep-th/0405159 m scalar M unif TeV TeV M unif ˜ m fermion Gaugino/Higgsino dark matter Measurements could imply huge fine-tuning of weak scale

Anthropics for Λ CC r P No  Λ CC Large Scale Structure Weinberg PRL 1987

Anthropics for Λ CC r P No  Λ CC Large Scale Structure Weinberg PRL 1987 Fraction of virialized baryons 0.8 12 9 7 10 10 10 0.6 Probability density 0.4 0.2 0.0 − 124 − 123 − 122 − 121 − 120 − 119 log( ρ Λ ) Martell, Shapiro, Weinberg astro-ph/9701099

Anthropics for Λ CC r P No  Λ CC Large Scale Structure Weinberg PRL 1987 Fraction of virialized baryons Causal patch measure 0.8 0.7 12 9 7 10 10 10 0.6 0.6 0.5 Probability density Probability density 0.4 0.4 0.3 0.2 0.2 0.1 0.0 0.0 − 124 − 123 − 122 − 121 − 120 − 119 − 126 − 125 − 124 − 123 − 122 − 121 − 120 − 119 log( ρ Λ ) log( ρ Λ ) Martell, Shapiro, Weinberg astro-ph/9701099 Bousso, Harnik, Kribs,Perez hep-th/0702115

Anthropics for v and Λ CC r P No  Λ CC Large Scale Structure Weinberg PRL 1987 r P No  v Complex Nuclei Agrawal, Barr, Donoghue, Seckel ph/9707380

Anthropics for v and Λ CC r P No  Λ CC Large Scale Structure Weinberg PRL 1987 r P No  v Complex Nuclei Agrawal, Barr, Donoghue, Seckel ph/9707380 ?? ˜ m

Scanning SUSY Breaking Consider a power law distribution for in multiverse ˜ m m p d ln ˜ dP ∝ ˜ m For include a factor for fine tuning of weak scale ˜ m ≥ v ⇣ v ⌘ 2 m p d ln ˜ dP ∝ ˜ m m ˜ Runaway to Natural weak scale High Scale SUSY 2 p

1. High Scale SUSY Hall, Nomura 0910.2235

Runaway to High Scale SUSY p > 2 dP d ln ˜ m Runaway to High Scale SUSY ˜ m v

Runaway to High Scale SUSY p > 2 dP d ln ˜ m Runaway to M unif High Scale SUSY ˜ m s TeV ˜ m v TeV M unif ˜ m f

Higgs Mass Prediction Hall, Nomura 0910.2235 150 m t = (173 . 1 ± 1 . 3) GeV 140 M H � GeV � α s = 0 . 1176 m = 10 14 GeV 130 ˜ 120 2 4 6 8 10 tan Β H u ↔ H d Axion m h = (128 ± 3 ± 0 . 6 ± 1 . 0) GeV Dark Matter m = 10 14 ± 2 GeV ˜ m t , α s ˜ t loop

2. Spread SUSY Hall, Nomura 1111.4519

Stabilizing SUSY Breaking at Multi-TeV p > 2 dP d ln ˜ m Runaway to High Scale SUSY  ˜ ? m v

Anthropics for v, , and Λ CC ˜ m r P No  Λ CC Large Scale Structure Weinberg PRL 1987 r P No  v Complex Nuclei Agrawal, Barr, Donoghue, Seckel ph/9707380 r P Too much ˜  m Dark Matter Hall, Nomura 1111.4519

A Boundary from LSP Freeze-Out Assumptions: 1. The LSP is cosmologically stable 2. T R ≥ ˜ m 3. No Dilution 1 Ω h 2 / The result: h σ A v i / m 2 m 2 LSP / ˜ m < ˜ ˜ ρ D < ρ c m c

A Boundary from LSP Freeze-Out Assumptions: 1. The LSP is cosmologically stable 2. T R ≥ ˜ m 3. No Dilution 1 Ω h 2 / The result: h σ A v i / m 2 m 2 LSP / ˜ m < ˜ ˜ ρ D < ρ c m c { Disks don’t fragment Tegmark, Aguirre, Rees, Wilczek astro-ph/0511774 Close encounters

A Boundary from LSP Freeze-Out Assumptions: 1. The LSP is cosmologically stable 2. T R ≥ ˜ m 3. No Dilution 1 Ω h 2 / The result: h σ A v i / m 2 m 2 LSP / ˜ m < ˜ ˜ ρ D < ρ c m c { Disks don’t fragment Tegmark, Aguirre, Rees, Wilczek astro-ph/0511774 Close encounters Unnatural � α e ff ⇥ ⇤ m LSP ∼ α e ff T eq M P ≈ 1 TeV 0 . 01 Multi-TeV SUSY

Two Cases X † X m ∼ F X Scalar Masses M 2 ( Q † Q + . . . ) M ∼ m 3 / 2 ˜

Two Cases X † X m ∼ F X Scalar Masses M 2 ( Q † Q + . . . ) M ∼ m 3 / 2 ˜ ?? X M W α W α

Two Cases X † X m ∼ F X Scalar Masses M 2 ( Q † Q + . . . ) M ∼ m 3 / 2 ˜ ?? X Yes M W α W α q, ˜ ˜ g, . . . TeV Multiverse MSSM

Two Cases X † X m ∼ F X Scalar Masses M 2 ( Q † Q + . . . ) M ∼ m 3 / 2 ˜ ?? X Yes No M W α W α ˜ q, . . . 100 TeV 1-loop anomaly mediation Giudice, Luty, Murayama, Rattazzi q, ˜ ˜ ˜ g, . . . g, . . . hep-ph/9810442 TeV TeV Spread SUSY Multiverse MSSM

Spread SUSY M unif ˜ m s TeV TeV M unif ˜ m f Gaugino dark matter

Spread SUSY 125 GeV Scalar is “effortless” M unif ˜ m s TeV TeV M unif ˜ ˜ m s m f Gaugino dark matter

Spread SUSY 125 GeV Scalar is “effortless” M unif ˜ m s TeV TeV M unif ˜ ˜ m s m f Spread Hall, Nomura arXiv:1111.4519 Pure Gravity Mediation Ibe, Yanagida arXiv:1112.2462 Gaugino dark matter Arvanitaki, Craig, Dimopoulos, Mini-Split Villadoro arXiv:1210.0555 Arkani-Hamed, Gupta, Kaplan, Simply Unnatural Weiner, Zorawski arXiv:1212.6971

Susy Spectrum M P l m ˜ ∼ m 3 / 2 M Fund m 3 / 2 100 10 12 m =10 5 TeV ˜ Mass Spectrum 1000 2 g =10 TeV M ˜ M ˜ W =3 TeV m 3 / 2 [TeV] 1 5 TeV 3 TeV 100 2 TeV 1 TeV 0.5 500 GeV 1 TeV =10 4 TeV 200 GeV Hall, Nomura, Shirai 10 0.2 m =10 3 TeV m =10 2 TeV ˜ ˜ arXiv:1210.2395

Dark Matter Abundance M P l m ˜ m 3 / 2 100 ∼ 10 M Fund m 3 / 2 T R = 10 8 GeV 1000 0.1m 1mm 10m 1m 1cm 0.1mm FO m 3 / 2 [TeV] 100 FI Hall, Nomura, Shirai 0.01 arXiv:1210.2395 0.1 10 1 W h 2 Ω ˜ AMS-02(KRA) Fermi c τ ˜ g AMS-02(MIN) Fermi(3 × weaker) 1 < M ˜ g < 3 TeV

3. TeV Scale Superpartners with ρ D ∼ ρ B Bousso, Hall 1304.6407

No Catastrophic Boundary for Dark Matter dP d ln ˜ m Too much  Dark Matter ˜ m v If this boundary does not exist, or is far from our universe, are we forced to High Scale SUSY?

The Dark to Baryon Ratio ζ = ρ D Why is ? ∼ 1 ρ B

The Dark to Baryon Ratio ζ = ρ D Why is ? ∼ 1 ρ B 1 A multiverse explanation: dP ∼ ζ p/ 2 1 + ζ d ln ζ dP Same Causal Patch 0 < p < 2 d ln ζ measure as for CC ζ 1

LSP Dark Matter from Freeze-Out m 2 ζ ∝ ρ D ∝ ˜ Electroweak Measure fine-tune ✓ v 2 ◆ ✓ ˜ ✓ v 2 ◆ dP m 2 ◆ m p ˜ c m p ˜ m 2 ˜ d ln ˜ m m 2 m 2 ˜ ˜ m p ˜ ˜ m ˜ v m c

LSP Dark Matter from Freeze-Out m 2 ζ ∝ ρ D ∝ ˜ Electroweak Measure fine-tune ✓ v 2 ◆ ✓ ˜ ✓ v 2 ◆ dP m 2 ◆ m p ˜ c m p ˜ m 2 ˜ d ln ˜ m m 2 m 2 ˜ ˜ m p ˜ ˜ m ˜ v m c 2 < p < 4 Little SUSY Hierarchy

LSP Dark Matter from Freeze-Out m 2 ζ ∝ ρ D ∝ ˜ Electroweak Measure fine-tune ✓ v 2 ◆ ✓ ˜ ✓ v 2 ◆ dP m 2 ◆ m p ˜ c m p ˜ m 2 ˜ d ln ˜ m m 2 m 2 ˜ ˜ m p ˜ ˜ m ˜ v m c 2 < p < 4 ρ D Bonus: ∼ 1 Little SUSY Hierarchy ρ B

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? F Gravitino is often the LSP m 3 / 2 ∼ M P l 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? F Gravitino is often the LSP m 3 / 2 ∼ M P l Large Loop-hole? Josh’s talk: No! Must include all production mechanisms

multi-TeV TeV m : ˜ 10 5 T R a eff = 0.03 H wino L T R m = 10 3 é = 10 3 m ˜ m . 9 TeV 10 4 ˜ overclosed FO é @ GeV D m BBN 10 3 UV é m 3 ê 2 > m 10 2 10 - 6 10 - 5 10 - 4 10 - 3 10 - 2 10 - 1 10 1 10 2 10 3 10 4 1 m 3 ê 2 @ GeV D

Summary: SUSY in the Multiverse

A Remarkable Situation 1973-2013: 40 years without BSM discovery 1 1998: Λ CC ∼ G N t 2 obs 2013: SM Higgs, apparently tuned