[PPT] - Where is SUSY? Lawrence Hall University of California, Berkeley PowerPoint Presentation

SLIDE 1

Where is SUSY?

Lawrence Hall University of California, Berkeley

Johns Hopkins 36th Workshop Galileo Galilei Institute October 2012

SLIDE 2

SUSY Spectrum, 1984

Text

SLIDE 3

SUSY Spectrum, 1984

Text

Over 3 decades of susy: seismic shifts!

SLIDE 4

(I) 2011- A New Era of Data

SLIDE 5

A 125 GeV Higgs Boson

Is good news for perturbative Susy

SLIDE 6

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

v

Origin of ?

SLIDE 7

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

v

Origin of ?

mh

125 150 100

Natural Unnatural

Inconclusive

SLIDE 8

Large Range of is Possible in MSSM

˜ m

tan β

Giudice and Strumia 1108.6077

A) SM below ˜

m

B) Split SUSY

(Fermionic superparters at 1 TeV)

SLIDE 9

No Superpartners Yet!!

Jets + missing transverse energy from squark and gluino production 8/13/12 A compilation of CMS results from 2011 data

SLIDE 10

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

Any superpartners at the TeV scale?

SLIDE 11

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

Any superpartners at the TeV scale?

R parity violation: udd A compressed spectrum

SLIDE 12

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

Any superpartners at the TeV scale?

Adding a singlet R parity violation: udd A compressed spectrum

SLIDE 13

Is SUSY Natural?

Natural Unnatural

˜ m v

˜ m ∼ v

Any superpartners at the TeV scale?

Adding a singlet R parity violation: udd A compressed spectrum Dark Matter Yukawa unification Spread Susy

SLIDE 14

2012 Result on Direct Detection

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

45

10

44

10

43

10

42

10

41

10

40

10

39

10

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

45

10

44

10

43

10

42

10

41

10

40

10

39

10

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

45

10

44

10

43

10

42

10

41

10

40

10

39

10

DAMA/I DAMA/Na CoGeNT CDMS (2010/11) EDELWEISS (2011/12) XENON10 (2011) XENON100 (2011) COUPP (2012) SIMPLE (2012) ZEPLIN-III (2012) CRESST-II (2012)

XENON100 (2012)

bserved limit (90% CL)

Expected limit of this run: expected σ 2 ± expected σ 1 ±

SLIDE 15

Implications for Neutralino DM

10-46 10-45 10-45 10-44 100 1000 30 300 100 1000 30 300 m in GeV M1 in GeV

well tempered binoêhiggsino, tan b = 10

m

D M

= m

h

ê 2 m

D M

= m

Z

ê 2

“The Well-Tempered Region is excluded”

Farina, Kadastik, Raidal, Pappadopulo, Pata, Strumia 1104.3572 revised Aug 2012

˜ b/˜ h

SLIDE 16

Indirect Detection via Gamma Rays

FIG. 2. Derived 95% C.L. upper limits on a WIMP annihila-

tion cross section for the b¯ b channel, the τ +τ − channel, the µ+µ− channel, and the W +W − channel. The most generic cross section (∼ 3·10−26 cm3s−1 for a purely s-wave cross section) is plotted as a reference. Uncertainties in the J factor are included.

Fermi LAT 1108.3546

SLIDE 17

(II) Natural SUSY

2. Adding a singlet
1. MSSM ??

SLIDE 18

Fine-Tuning in the MSSM: 2012

SLIDE 19

Fine-Tuning in the MSSM: 2012

mh = 124 − 126 GeV

Minimize

messenger scale

f 10 TeV

∆

tan β > 10

mQ3 = mU3 = m˜

t

∆ = ∂ ln mh ∂ ln p

David Pinner, Josh Ruderman, LJH 1112.2703

∆ > 100 The MSSM is fine-tuned

SLIDE 20

Adding a Singlet:

λ SHuHd

SLIDE 21

Adding a Singlet:

λ SHuHd

David Pinner, Josh Ruderman, LJH 1112.2703

λ < 0.7

SLIDE 22

Adding a Singlet:

λ SHuHd

David Pinner, Josh Ruderman, LJH 1112.2703

λ < 0.7

Why not go to larger ?

λ λ

To very large ?

Natural theory with heavy Higgs

SLIDE 23

Adding a Singlet:

λ SHuHd

David Pinner, Josh Ruderman, LJH 1112.2703

1 < λ< 2

SLIDE 24

Adding a Singlet:

λ SHuHd

David Pinner, Josh Ruderman, LJH 1112.2703

1 < λ< 2

∆ < 10

SLIDE 25

Adding a Singlet:

Explains why we haven’t seen superpartners yet

λ SHuHd

David Pinner, Josh Ruderman, LJH 1112.2703

1 < λ< 2

∆ < 10

SLIDE 26

(III) TeV Susy

Dark Matter

Coupling Unification Spread Susy

SLIDE 27

Direct Detection of Dark Matter

500 1000 1500 2000 10-43 10-44 10-45 10-46 10-47

0.01 0.1

mDM @GeVD sp,n @cm2D

spin independent

ccch

Xenon100 LUX Xenon1T

@ D

Exciting times ahead:

Cliff Cheung, David Pinner, Josh Ruderman, LJH 1210...

SLIDE 28

TeV Scale from Cosmological Abundance

R parity LSP is a SM superpartner

˜ m < TR

˜ m ∼ TeV

No dilution

SLIDE 29

TeV Scale from Cosmological Abundance

R parity LSP is a SM superpartner

˜ m < TR

˜ m ∼ TeV

,c

∼ TeV ≈ TR

The forbidden window

˜ m

ρDM

ρDMobs

No dilution

SLIDE 30

TeV Scale from Cosmological Abundance

R parity LSP is a SM superpartner

˜ m < TR

˜ m ∼ TeV

,c

∼ TeV ≈ TR

The forbidden window

˜ m

ρDM

ρDMobs

˜ m ∼ α p TeqMP l

No dilution

SLIDE 31

Current Limits on Bino/Higgsino DM

Cliff Cheung, David Pinner, Josh Ruderman, LJH 1210...

Parameter space

(M1, µ, tan β)

chχχ / M1 + µ sin 2β = 0

“Blind Spot”

1 1

0.1 0.1 10 10 100 100

1000
500

500 1000 200 400 600 800 1000

m @GeVD M1 @GeVD

tan b = 2

Wthermal Wcdm XENON100 SI XENON100 SD IceCube W-W+ Fermi

LEP c- c+

chcc = 0

1

0.1 0.1 10 10 100 100 1000 1000

1

1000
500

500 1000 200 400 600 800 1000

m @GeVD M1 @GeVD

tan b = 20

Wthermal Wcdm XENON100 SI XENON100 SD Fermi IceCube W-W+

LEP c- c+

chcc = 0

ΩLSP = Ωobs

Assume

SLIDE 32

Future Probes of Bino/Higgsino DM

Cliff Cheung, David Pinner, Josh Ruderman, LJH 1210...

Parameter space

(M1, µ, tan β)

chχχ / M1 + µ sin 2β = 0

“Blind Spot”

ΩLSP = Ωobs

Assume

1000
5000
100 100

1000 5000 100 1000 5000

m @GeVD M1 @GeVD

tan b = 2

Wthermal = Wcdm XENON1T SI XENON1T SD Fermi LUX SI LEP c- c+ chcc = 0

1000
5000
100 100

1000 5000 100 1000 5000

m @GeVD M1 @GeVD

tan b = 20

Wthermal = Wcdm XENON1T SI XENON1T SD Fermi LUX SI LEP c- c+ chcc = 0

SLIDE 33

Bino/Higgsino DM from Freeze-out

Cliff Cheung, David Pinner, Josh Ruderman, LJH 1210...

Parameter space

chχχ / M1 + µ sin 2β = 0

“Blind Spot” Assume

1000
500

500 1000 1 2 5 10 20 40

m @GeVD tan b

current limits

LEP c- c+ Xenon100 SI IceCube W+W- Xenon100 SD chcc = 0

1000
500

500 1000 1 2 5 10 20 40

m @GeVD tan b

LUX and IceCube reach H~2013L

LEP c- c+ LUX SI IceCube W+W- HreachL IceCube tt HreachL chcc = 0

1000
500

500 1000 1 2 5 10 20 40

m @GeVD tan b

XENON 1T reach H~2017L

LEP c- c+ Xenon1T SI Xenon1T SD chcc = 0

ΩF O

LSP = Ωobs

(M1, µ, tan β) → (µ, tan β)

SLIDE 34

LSP Dark Matter Summary

˜ m ∼ TeV

Current experiments LUX and Xenon1T have removed about half the space will explore most of the space Cosmological abundance of LSP provides independent argument for For freeze-out (bino/Higgsino and bino/wino)

SLIDE 35

(III) TeV Susy

Dark Matter

Coupling Unification Spread Susy

SLIDE 36

Gauge Coupling Unification

102 104 106 108 1010 1012 1014 0.2 0.4 0.6 0.8 1. 1.2 1.4

E GeV ga

SLIDE 37

Gauge Coupling Unification

102 104 106 108 1010 1012 1014 0.2 0.4 0.6 0.8 1. 1.2 1.4

E GeV ga

ccurs in the Standard Model!

Weak scale susy improves the precision:

✏g = 0.12 → ✏g = 0.014

SLIDE 38

Gauge Coupling Unification

But does not usefully constrain the superparticle masses

100 105 108 1011 1014 1017 1020 10 20 30 40 50 60 m @GeVD ai-1 105 108 1011 1014 1017 1020 10 20 30 40 50 60 m @GeVD ai-1

msusy = 100 GeV msusy = 100 TeV

✏g = 0.014 → ✏g = 0.017

Logarithmic evolution! Weak scale susy improves the precision:

✏g = 0.12 → ✏g = 0.014

SLIDE 39

Yukawa Coupling Unification

Once again, weak scale susy improves the precision

100 105 108 1011 1014 1017 0.10 0.15 0.20 0.25 0.30 0.35 0.40

m @GeVD yi

tan b = 20

yb yt

t-b-

100 105 108 1011 1014 1017 0.4 0.5 0.6 0.7 0.8 0.9 1.0

m @GeVD yi

tan b = 50

yt yb yt

need

τ

b − τ

t − b − τ

✏g = 0.60 → δfin

b

= 0.12

SLIDE 40

Yukawa Coupling Unification

Once again, weak scale susy improves the precision

100 105 108 1011 1014 1017 0.10 0.15 0.20 0.25 0.30 0.35 0.40

m @GeVD yi

tan b = 20

yb yt

t-b-

100 105 108 1011 1014 1017 0.4 0.5 0.6 0.7 0.8 0.9 1.0

m @GeVD yi

tan b = 50

yt yb yt

need

τ

b − τ

t − b − τ

Yukawas span 6 decades: Is a hint?

b/τ

✏g = 0.60 → δfin

b

= 0.12

SLIDE 41

Constraining δfin

b

δfin

b

∝ µ m˜

q

tan β

Gilly Elor, David Pinner, Josh Ruderman, LJH 1206.5301

˜ m

SLIDE 42

Constraining δfin

b

δfin

b

∝ µ m˜

q

tan β

Gilly Elor, David Pinner, Josh Ruderman, LJH 1206.5301

˜ m

bino/Higgsino LSP dark matter Cannot decouple squarks Need large

tan β

Power law behavior!

SLIDE 43

Constraining δfin

b

δfin

b

∝ µ m˜

q

tan β

Gilly Elor, David Pinner, Josh Ruderman, LJH 1206.5301

˜ m

m˜

q < 10 TeVtan β

50 bino/Higgsino LSP dark matter Cannot decouple squarks Need large

tan β

Power law behavior!

SLIDE 44

(III) TeV Susy

Dark Matter

Coupling Unification Spread Susy

SLIDE 45

A Mildly Split Spectrum

/TeV

˜ m

1 102 − 105

scalar gauginos

1. 1-loop gaugino masses

from Anomaly Mediation 2.

MF und MP l ∼ 1 − 10−2

Spread SUSY

SLIDE 46

Yasunori Nomura, LJH 1111.4519

Different

rigins for

Higgsino LSP Wino LSP

mass [TeV]

1 103 106

˜ h ˜ W ˜ B ˜ g ˜ G ˜ q, ˜ , H0,±, A Ω mass [TeV]

1 103 106

˜ W ˜ B ˜ g ˜ h, ˜ G ˜ q, ˜ , H0,±, A

Wells hep-ph/0411041 Arkani-Hamed, Delgado, Giudice ph/0601041 Giudice, Luty, Murayama, Rattazzi hep-ph/9810442

µ

Two Versions

SLIDE 47

Higgs Mass in Spread SUSY

Higgsino LSP Wino LSP

Yasunori Nomura, LJH 1111.4519

1 2 3 4 5 102 103 104 1 0.9 0.8 0.7 0.6 0.5 0.4 tan β sin 2β ˜ m [TeV] µ =10 TeV µ =100 TeV 130 GeV 125 GeV 120 GeV

Yasunori Nomura, Satoshi Shirai, LJH 1210.2395

δmt = 1 GeV

SLIDE 48

Higgs Mass in Spread SUSY

Higgsino LSP Wino LSP

Yasunori Nomura, LJH 1111.4519

1 2 3 4 5 102 103 104 1 0.9 0.8 0.7 0.6 0.5 0.4 tan β sin 2β ˜ m [TeV] µ =10 TeV µ =100 TeV 130 GeV 125 GeV 120 GeV

Yasunori Nomura, Satoshi Shirai, LJH 1210.2395

δmt = 1 GeV

LHC gluino signal

SLIDE 49

(IV) High Scale Susy

˜ m ∼ Mu ∼ 1014 GeV v

Standard Model

SLIDE 50

Higgs Mass

λ( ˜ m) = g2( ˜ m) + g2( ˜ m) 8 cos22β

2 4 6 8 10 120 130 140 150

tanΒ MH GeV

mt = (173.1 ± 1.3) GeV

αs = 0.1176 ˜ m = 1014 GeV

Hall, Nomura 0910.2235

SLIDE 51

Higgs Mass

λ( ˜ m) = g2( ˜ m) + g2( ˜ m) 8 cos22β

2 4 6 8 10 120 130 140 150

tanΒ MH GeV

mt = (173.1 ± 1.3) GeV

αs = 0.1176 ˜ m = 1014 GeV

Hall, Nomura 0910.2235

Uncertainties from

unified thresholds (not stops)

αs, mt

NNLO (1205.6497) from experiment (1207.0980)

SLIDE 52

Higgs Mass

λ( ˜ m) = g2( ˜ m) + g2( ˜ m) 8 cos22β

2 4 6 8 10 120 130 140 150

tanΒ MH GeV

mt = (173.1 ± 1.3) GeV

αs = 0.1176 ˜ m = 1014 GeV

An Alarming Possibility!!

Hall, Nomura 0910.2235

Uncertainties from

unified thresholds (not stops)

αs, mt

NNLO (1205.6497) from experiment (1207.0980)

SLIDE 53

SM Quartic Trajectory

Close to zero

Hall, Salem, Watari hep-ph/0608121

Close to catastrophic vacuum tunneling

Elias-Miro et al 1112.3022

SLIDE 54

Standard Model Phase Diagram

Degrassi et al 1205.6497

Catastrophic vacuum tunneling boundary

λ(MP l) = 0

SLIDE 55

R parity violation Adding S helps ...

Status of SUSY in 2012

Dark Matter suggests SUSY at 1-10 TeV Moderately Split Spectra like 125 GeV Higgs

b/τ

TeV-scale Susy Natural Susy High Scale SUSY MSSM

A worry! Fine tuning is worse than 1 in a 100

SLIDE 56

Predicted Signals of Spread SUSY

0.2 0.5 1 2 10 100

√FX [GeV] r∗ ×1012

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 ˜ m=104TeV ˜ m=105TeV

10 100 1000

m3/2 [TeV]

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

TR = 108 GeV

1016 1017 1018 10 100 1000

m3/2 [TeV] M∗ [GeV]

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

TR = 3×109 GeV

(Fixed Higgsino mass) Fundamental Scale Susy Breaking Scale

τ˜

g

Ωh2

Fermi AMS-02 (proj)