LHC and Astroparticle Physics — The Next High Energy Frontier · The Next High Energy Frontier The Large Hadron Collider: • New threshold for new physics: q Spp = 14 TeV, sparton

LHC and Astroparticle Physics

— The Next High Energy Frontier

Tao Han

University of Wisconsin – Madison

TeV Particle Astrophysics II

(August 30, 2006)

LHC and Astroparticle Physics

— The Next High Energy Frontier

Tao Han

University of Wisconsin – Madison

TeV Particle Astrophysics II

(August 30, 2006)

Introduction to the Next HE Frontier

Physics Beyond the Standard Model

In the LHC Era

High-Energy Astroparticle Physics

The Next High Energy Frontier

The Large Hadron Collider:



• New threshold for new physics:√

Spp = 14 TeV, sparton = x1x2Spp

⇒ Mnew =√

sparton ∼ 0.2√

Spp ∼ 3 TeV.





⇒ Mnew =√

sparton ∼ 0.2√

Spp ∼ 3 TeV.

• Multiple channels, broad physics reach:qq′, gg, qg, bb → colored; Q = 0,±1; J = 0,1,2 states;

γγ, WW, WZ, ZZ → IW = 0,1,2; Q = 0,±1,±2; J = 0,1,2 states.





⇒ Mnew =√

sparton ∼ 0.2√

Spp ∼ 3 TeV.

• Multiple channels, broad physics reach:qq′, gg, qg, bb → colored; Q = 0,±1; J = 0,1,2 states;

γγ, WW, WZ, ZZ → IW = 0,1,2; Q = 0,±1,±2; J = 0,1,2 states.

• Higher luminosity, higher event rate:

L = 1033 − 1034 cm−2s−1 ⇒ 104 − 105 pb−1/yr.

HE cosmic Rays by Nature’s Accelerators


• Cosmic rays have historically led to new particle discoveries.



• The observed high energy events extend to

Elab ≈ 1011 GeV ⇒ Ecm =√

2mNElab ≈ 500 TeV.

beyond the GZK cutoff; higher than the conceivable collider energies.







• Variety of incoming particles:

γ, p, heavy nuclei, ν′s...

but the components not precisely known.







• Variety of incoming particles:

γ, p, heavy nuclei, ν′s...

but the components not precisely known.

• Main drawback:The flux (or the luminosity) falls rapidly faster than E−3.


The Highly successful SM:



• SU(3)C ⊗ SU(2)L ⊗ U(1)Y ⇒ SU(3)C ⊗ U(1)em

Experimentally tested to 0.1%!

150 160 170 180 190 200m t [GeV]

80.2

80.3

80.4

80.5

80.6

MW

[GeV

]

direct (1 σ)

indirect (1 σ)

all (90% CL)

MH [GeV]10

020

040

080

0



• SU(3)C ⊗ SU(2)L ⊗ U(1)Y ⇒ SU(3)C ⊗ U(1)em

Experimentally tested to 0.1%!

150 160 170 180 190 200m t [GeV]

80.2

80.3

80.4

80.5

80.6

MW

[GeV

]

direct (1 σ)

indirect (1 σ)

all (90% CL)

MH [GeV]10

020

040

080

0Triumph for the HEP theory and experiments!

Higgs boson (or alike) must exist !

• Mass generation for all elementary particles

• SM renormalizability

• Partial wave unitarity mH < O(TeV)

• Indirect experimental indication mH <∼ 200 GeV

Higgs boson (or alike) must exist !

• Mass generation for all elementary particles

• SM renormalizability

• Partial wave unitarity mH < O(TeV)

• Indirect experimental indication mH <∼ 200 GeV

A light Higgs boson is highly expected!

Light Higgs boson is sick !


Quantum corrections drag m2h to ultra-violet modes ∼ Λ2.

(a) (c)(b)

t

W,B

h

hh h h

h h

tc



(a) (c)(b)

t

W,B

h

hh h h

h h

tc

m2H = m2

H0 − 3

8π2y2t Λ

2 +1

16π2g2Λ2 +

1

16π2λ2Λ2



(a) (c)(b)

t

W,B

h

hh h h

h h

tc

m2H = m2

H0 − 3

8π2y2t Λ

2 +1

16π2g2Λ2 +

1

16π2λ2Λ2

(200 GeV)2 = m2H0 +

[

−(2 TeV)2 + (700 GeV)2 + (500 GeV)2]

(

Λ

10 TeV

)2

.



(a) (c)(b)

t

W,B

h

hh h h

h h

tc

m2H = m2

H0 − 3

8π2y2t Λ

2 +1

16π2g2Λ2 +

1

16π2λ2Λ2

(200 GeV)2 = m2H0 +

[

−(2 TeV)2 + (700 GeV)2 + (500 GeV)2]

(

Λ

10 TeV

)2

.

• If Λ ∼ Mpl, then 1030-digits cancellation (Anthropic principle)!

• Naturalness: less than 90% cancellation on m2h ⇒ Λ <∼ 3 TeV.



(a) (c)(b)

t

W,B

h

hh h h

h h

tc

m2H = m2

H0 − 3

8π2y2t Λ

2 +1

16π2g2Λ2 +

1

16π2λ2Λ2

(200 GeV)2 = m2H0 +

[

−(2 TeV)2 + (700 GeV)2 + (500 GeV)2]

(

Λ

10 TeV

)2

.

• If Λ ∼ Mpl, then 1030-digits cancellation (Anthropic principle)!

• Naturalness: less than 90% cancellation on m2h ⇒ Λ <∼ 3 TeV.

Other New Physics must show up at TeV scale!

1. Symmetry/Cancellation at work?

• Super-symmetry (SUSY) (symmetry between opposite spin & statistics)

Natural cancellations: t versus t

W versus W

H versus H

Hd versus Hu,




W versus W

H versus H

Hd versus Hu,

∆m2H ∼ (M2

SUSY − M2SM)

λ2f

16π2ln

(

Λ

MSUSY

)

.

Weak scale SUSY is natural if MSUSY ∼ O (1 TeV).




W versus W

H versus H

Hd versus Hu,

∆m2H ∼ (M2

SUSY − M2SM)

λ2f

16π2ln

(

Λ

MSUSY

)

.

Weak scale SUSY is natural if MSUSY ∼ O (1 TeV).

• The Little Higgs idea – Strongly interacting dynamics:

An alternative way to keep H light (naturally).

Again, predicting new states:

W±, Z, B ↔ W±H , ZH , BH; t ↔ T ; H ↔ Φ.

(cancellation among same spin states!)

TeV scale new dynamics needed associated with a symmetry.

2. Low fundamental scale?

• With the help of Extra-dimensions, low-scale gravity/string theories

resolve the large hierarchy:

ADD:

tyi

x

SM

planck brane

gravity

Randall-Sundrum

Mply0

m ey0Mpl

2. Low fundamental scale?

• With the help of Extra-dimensions, low-scale gravity/string theories

resolve the large hierarchy:

ADD:

tyi

x

SM

planck brane

gravity

Randall-Sundrum

Mply0

m ey0MplMn+2

S ∼ M2PL/Rn −→ O(1 TeV2).

Consequently,

For R−1 <∼ E <∼ MS, march into extra-dimensions:

Kaluza-Klein (KK) states: M2n ∼ n2

k/R2;

Consequently,



k/R2;

For E >∼ MS, R−1, stringy effects:

String resonances: M2 ∼ nsM2S ;

Winding modes: M2n ∼ n2

wR2M4S .

Consequently,



k/R2;




wR2M4S .

Or other quantum gravity effects ...

⇒ testing the geometry of the extrad-dimensions!

Consequently,



k/R2;




wR2M4S .

Or other quantum gravity effects ...

⇒ testing the geometry of the extrad-dimensions!

For E ≫ MS, semi-classical gravity:

TeV-Scale Black Holes:

σ ≈ π r2bh,

rbh =1√

πMD

MBH

MD

8Γ(

n+32

)

n + 2

1n+1

→ MBH/M2pl in 4d

Unification of forces ?

Do the forces E & M/Weak/Strong all unify into a single force ?



YES if there is a TeV scale new physics threshold !

0

10

20

30

40

50

60

10 10 10 10 10 10 10 10 2 4 6 8 10 12 14 16

1/α i

µ(GeV)

1

1/α

2

1/α

3

1/α




0

10

20

30

40

50

60

10 10 10 10 10 10 10 10 2 4 6 8 10 12 14 16

1/α i

µ(GeV)

1

1/α

2

1/α

3

1/α

Motivation is strong for physics BSM at the TeV scale.




0

10

20

30

40

50

60

10 10 10 10 10 10 10 10 2 4 6 8 10 12 14 16

1/α i

µ(GeV)

1

1/α

2

1/α

3

1/α

Motivation is strong for physics BSM at the TeV scale.

(skip extensions of gauge, SUSY; ν masse and mixing ...)

We are entering a “data-rich” era:

B-factories (SLAC, KEK): test CP violation;

Neutrino Oscillation Experiments: Neutrino masses and mixing;

µ-magnetic moment: g − 2;

neutron/electron electric-dipole-moments ...






Cosmological observations: Dark matter, mν, and dark energy ...







Astroparticle physics experiments:

Cosmic rays, neutrinos, dark matter, other new physics ...







Astroparticle physics experiments:

Cosmic rays, neutrinos, dark matter, other new physics ...

Tevatron: (pp at 1.96 TeV, FNAL, till 2009?)

top quark, new particle searches, Higgs (?) ...

LHC: (pp at 14 TeV at CERN, 2007)

comprehensive Higgs studies, extensive new particle searches ...

ILC: (e+e− at 500 GeV − 1 TeV)

more on top quark, precision Higgs and new light particles ...

Physics Expectations at the LHC

Major discoveries and excitement ahead ...

Feb.16, 2006: ATLAS (90m underground) CMS

(pilot run at the end of 2007.)

LHC Event rates for various SM processes:


Annual yield: 1B W±; 100M tt; 10M W+W−; 1M H0...


Annual yield: 1B W±; 100M tt; 10M W+W−; 1M H0...

Great potential to open a new chapter of HEP !Challenge: Small signal-to-background ratio!

Leptons(e, µ)

Photons

Taus

JetsMissing ET

y98014_416dPauss rd

H → WW→lνjjH → ZZ→lljjZZH

H→WW→lνlν

H→WW→lνlν

→ → νν

H →

Z Z

→

4 le

pton

s*(

(

H γγ→

H ZZ→0

n lept.+ x

∼g → n jets + E

MT

→ n leptons + Xq similar∼

H+→τν

0H, A , h0 0→ττ(H ) γγ→h0 0

g∼ → h + x0

χ χ∼ ∼0 +→

*( (

W'→lν

V,ρ →WZTC→ lνll

Z' → ll

unpredicted discovery

4l→

g, q →b jets + X∼ ∼

b- Jet-tag

WH→

lνbb

ttH→lν

bb+X

––

H ll→ ττZZ→

Leptons(e, µ)

Photons

Taus

JetsMissing ET

y98014_416dPauss rd

H → WW→lνjjH → ZZ→lljjZZH

H→WW→lνlν

H→WW→lνlν

→ → νν

H →

Z Z

→

4 le

pton

s*(

(

H γγ→

H ZZ→0

n lept.+ x

∼g → n jets + E

MT

→ n leptons + Xq similar∼

H+→τν

0H, A , h0 0→ττ(H ) γγ→h0 0

g∼ → h + x0

χ χ∼ ∼0 +→

*( (

W'→lν

V,ρ →WZTC→ lνll

Z' → ll

unpredicted discovery

4l→

g, q →b jets + X∼ ∼

b- Jet-tag

WH→

lνbb

ttH→lν

bb+X

––

H ll→ ττZZ→

With optimal triggering and kinematical selections:

pT ≥ 30 − 100 GeV, |η| ≤ 3 − 5; /ET ≥ 100 GeV.

For any scenario beyond SM, LHC WILL contribute:

• Higgs fully covered at the LHC:

1

10

10 2

102

103

mH (GeV)

Sig

nal s

igni

fica

nce

H → γ γ + WH, ttH (H → γ γ ) ttH (H → bb) H → ZZ(*) → 4 l

H → ZZ → llνν H → WW → lνjj

H → WW(*) → lνlν

Total significance

5 σ

∫ L dt = 100 fb-1

(no K-factors)

ATLAS

• LHC will have great chance for SUSY discovery: ∗m0 > 4000 GeV, m1/2 > 1400 GeV, tanβ >∼ 45.

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6

1.8

2

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

LHC, ET miss

-2

-5

-10

-30

5

4

5

mSUGRA: tanβ=45, A0=0, µ<0

m0(TeV)

m1/

2(T

eV)

LEP2no REWSB

Z~

1 no

t LS

P

mh LEP2 limit aµSUSY×1010 Br(b→sγ)×104

Br(Bs→µ+µ-)×108 0.094<Ωh2<0.129 stage 3

fσ(Z~

1p)×1011 pb 100 10 1

∗Baer, Balazs, Belyaev, O’Farrill, hep-ph/0305191.

• LH: The heavy T signal at LHC ∗

gg → T T phase-space suppression;

qb → q′T via t-channel WLb → T .

∗Han, Logan, McElrath, Wang, hep-ph/0301040.

ATLAS simulations for T → tZ, bW :∗

Invariant Mass (GeV)

0 500 1000 1500 2000

-1E

vent

s/40

GeV

/300

fb

0.5

1

1.5

2

2.5

3

3.5

4

ATLAS


0 500 1000 1500 2000

-1E

vent

s/40

GeV

/300

fb

50

100

150

200

250

300

350

400

ATLAS

Reach MT ∼ 1 (2) TeV for xλ = 1 (2).

∗G. Azuelos et al.: hep-ph/0402037.

ATLAS simulations for T → tZ, bW :∗


0 500 1000 1500 2000

-1E

vent

s/40

GeV

/300

fb

0.5

1

1.5

2

2.5

3

3.5

4

ATLAS


0 500 1000 1500 2000

-1E

vent

s/40

GeV

/300

fb

50

100

150

200

250

300

350

400

ATLAS

Reach MT ∼ 1 (2) TeV for xλ = 1 (2).

Cross-sectiions measure coupling xλ.

Mass peak MT determines f : v/f = mt/MT (xλ + x−1λ )

=⇒ check consistency with f from MZH.∗

∗G. Azuelos et al.: hep-ph/0402037.∗Perelstein, Peskin, Pierce: hep-ph/0310039.

• Deep into extra-dimensions at the LHC:

Large extra-dim ADD & warped extra-dim RS: ∗

left: ADD with M⋆ = 20, 25, 30, 35 TeV;

right: RS with MKK = 16 TeV.

∗T. Rizzo

Black hole to ℓ and γ events at the LHC: ∗

1

10

10 210 310 410 510 610 710 8

0 2000 4000 6000 8000 10000MBH, GeV

dN/d

MB

H ×

500

GeV

MP = 1 TeV

MP = 3 TeV

MP = 5 TeV

MP = 7 TeV

∗Greg Landsberg

High Energy Astroparticle Physics

UHECRs exist:

+++++++ ++++++++++++

++++++++++++++++

++

+

+++++++

+++++++++

+++ + +

+

+

++++++++++++

++

+

++++

+

⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕

⊕ ⊕ ⊕

⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕

⊕ ⊕

⊕ ⊕

⊕ ⊕

⊕ ⊕ ⊕ ⊕

⊕ ⊕ ⊕ ⊕

⊕ ⊕

⊕ ⊕ ⊕

∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅

⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗

⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗

∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇

∇ ∇ ∇ ∇

⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄⁄ ⁄

⁄ ⁄ ⁄⁄ ⁄

⁄⁄

⁄

⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄⁄ ⁄ ⁄ ⁄ ⁄

⁄ ⁄⁄ ⁄

+ AGASA+ Akeno 20 km2+ Akeno 1 km2 AUGER

BLANCA CASA-MIA◊ DICE BASJE-MAS EAS-Top Fly’s Eye

Haverah ParkHaverah Park FeHaverah Park p HEGRA

⊕ HiRes-I⊕ HiRes-II

⊕ HiRes/MIA⁄ KASCADE (e/m QGSJET)⁄ KASCADE (e/m SIBYLL)

KASCADE (h/m) KASCADE (nn)∅ MSU

Mt. Norikura SUGAR⊗ Tibet ASγ⊗ Tibet ASγ-III∇ Tunka-25

Yakutsk

direct: JACEERUNJOBSOKOLGrigorov

Flu

x dΦ

/dE

× E

2.5

[m−2

s−1

sr−

1 G

eV1.

5]

104 105 106 107 108 109 1010 1011

103

104

102

10

1

Energy E [GeV]

ANKLE

KNEE

High Energy Astroparticle Physics

UHECRs exist:

+++++++ ++++++++++++

++++++++++++++++

++

+

+++++++

+++++++++

+++ + +

+

+

++++++++++++

++

+

++++

+

⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕

⊕ ⊕ ⊕

⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕ ⊕

⊕ ⊕

⊕ ⊕

⊕ ⊕

⊕ ⊕ ⊕ ⊕

⊕ ⊕ ⊕ ⊕

⊕ ⊕

⊕ ⊕ ⊕

∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅ ∅

⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗

⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗

∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇ ∇

∇ ∇ ∇ ∇

⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄⁄ ⁄

⁄ ⁄ ⁄⁄ ⁄

⁄⁄

⁄

⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄ ⁄⁄ ⁄ ⁄ ⁄ ⁄

⁄ ⁄⁄ ⁄

+ AGASA+ Akeno 20 km2+ Akeno 1 km2 AUGER

BLANCA CASA-MIA◊ DICE BASJE-MAS EAS-Top Fly’s Eye

Haverah ParkHaverah Park FeHaverah Park p HEGRA

⊕ HiRes-I⊕ HiRes-II

⊕ HiRes/MIA⁄ KASCADE (e/m QGSJET)⁄ KASCADE (e/m SIBYLL)

KASCADE (h/m) KASCADE (nn)∅ MSU

Mt. Norikura SUGAR⊗ Tibet ASγ⊗ Tibet ASγ-III∇ Tunka-25

Yakutsk

direct: JACEERUNJOBSOKOLGrigorov

Flu

x dΦ

/dE

× E

2.5

[m−2

s−1

sr−

1 G

eV1.

5]

104 105 106 107 108 109 1010 1011

103

104

102

10

1

Energy E [GeV]

ANKLE

KNEE

To compare with collider experiments:Advantage: Higher energies.Disadvantage: Low and imprecise knowlege of fluxes.

Event reconstruction much harder.

protons/heavy ions below the “knee”:

Large event sample available for Ecm > 1 TeV,

the QCD interactions/showering become overwhelming.

• SUSY production simulated at Auger: ∗Signal hardly observable.

• TeV-scale BH production simulated at Auger: †Possible for observation if the cross section is high enough.

∗Cafarella, Coriano, Faraggi, hep-ph/0308169.†Cafarella, Coriano, Tomaras, hep-ph/0410358.






Particle multiplicity is the key for signal/background separation;

Can we make use of the “transverse energy”?

∗Cafarella, Coriano, Faraggi, hep-ph/0308169.†Cafarella, Coriano, Tomaras, hep-ph/0410358.






Particle multiplicity is the key for signal/background separation;

Can we make use of the “transverse energy”?

• The “near-by” sources from heavy particle annihilation: ‡Possible explanation/observation above GZK.

∗Cafarella, Coriano, Faraggi, hep-ph/0308169.†Cafarella, Coriano, Tomaras, hep-ph/0410358.‡Albuquerque, Farrar, Kolb, hep-ph/9805288; Protheroe, Stanev, (1996);Barbot, Drees, Halzen, Hooper, hep-ph/0207133.

High-energy cosmic neutrinos:

They serve as a better tool for new physics search!

⋄ No attenuation in Eν,

⋄ Avoid large QCD backgrounds.

⋄ ... ...

High-energy cosmic neutrinos:

They serve as a better tool for new physics search!

⋄ No attenuation in Eν,

⋄ Avoid large QCD backgrounds.

⋄ ... ...

• Enhanced νN cross section:†

νN → q, ℓq, ν8;

→ KK states, stringy states, BH′s...

→ EW instantons

→ ......

†M.Carena et al. (1998); Domokos, Kovesi-Domokos (1999); Nussinov, Shrock (1999);Jain, McKay, Panda, Ralston (2000); Ringwald, Tu (2002); Feng, Shapere (2002);Anchordoqui, Goldberg (2002); Kusenko Weiler (2002); Friess, Han, Hooper (2002);J.Alvarez-Muniz et al. (2002); Han, Hooper (2004).

For instance, BH signal at Auger: †

†L. Anchordoqui et al., hep-ph/0508312.

Possible EW instanton effects at IceCube: †

†T.Han, D.Hooper, hep-ph/0307120.

• Long-lived charged particles:‡

For instance, τR as the NLSP (next-lightest...).

SUSY production not enhanced,

but the long travel range of τR (∼ 103 km) compensates it.

Search for a pair of parallel upward charged tracks: τ+R τ−R .

Great potential for discovery!

‡I.Albuquerque, G.Burdman, Z.Chacko, hep-ph/0312197;M.H. Reno, I.Sarcevic, S.Su, hep-ph/0503030.

Dark Matter Searches:

• Collider/Indirect/Direct Dark Matter searches:†

†D.Hooper and A.Taylor, hep-ph/0607086.

Two points in order:


(1). Folk theorem: Precision EW data need a symmetry

(R, T, KK, Z2 ...), that leads to a CDM candidate.


(1). Folk theorem: Precision EW data need a symmetry

(R, T, KK, Z2 ...), that leads to a CDM candidate.

(2). More than “complementary”:

Indirect/Direct searches more conclusive than collider search!

A WIMP needs only to live for about 1 µs to be “DM” ...

Recap:

Recap:

• TeV scale new physics highly expected

EWSB, Naturalness/hierarchy problem with H.

Recap:



• LHC anticipated for major discovery

Higgs, weak-scale SUSY?

new strong dynamics?

extra-dimensions?

dark matter ...

Recap:






extra-dimensions?

dark matter ...

• TeV scale astroparticle physics complementary

Recap:






extra-dimensions?

dark matter ...

• TeV scale astroparticle physics complementary

Join the excitement!

Documents

LHC and Astroparticle Physics — The Next High Energy Frontier · The Next High Energy Frontier The Large Hadron Collider: • New threshold for new physics: q Spp = 14 TeV, sparton