Standard Model

(1)

Intro to Axions

Particle Physics @ Low Energies

J. Jaeckel^**

S. Abel^†, J. Berges^**, B. Doebrich^z, L. Gastaldo**, M. Goodsell^xx, H. Gies⁰, F. Kahlhoefer*, S. Knirck**,

V. Khoze^†, A. Lobanov^y, J. Redondo^x,

A. Ringwald*, U. Schmidt**, K. Schmidt-Hoberg*

and The FUNK Collaboration

**ITP Heidelberg, ^zCERN,^†IPPP Durham, *DESY,

YMPIfR Bonn, ^xU. Zaragoza, ^xxParis LPTHE, ⁰ITP Jena

Heidelberg University!

(2)

This used to be a funny slide.

(3)

Where we want to go…

Here be Dragons

The Standard Model Beyond the SM +

(directly accessible to colliders)

The Hidden Sector

(4)

We need...

Physics beyond the

Standard Model

(5)

(6)

Inventory of the Universe

Dark Energy 68%

Neutrinos 0.1-0.5%

Dark Matter 27%

Ordinary matter 5%

(7)

Where does it hide?

New physics

(8)

Exploring is ^{(at least)} 2 dimensional

ν,

^Fixed

target

(9)

ν,

^Fixed

target

“dark”

weakly coupled =

(10)

What are Axion?

And why do we need them?

(11)

A „visible“ Hint for new Physics

The strong CP Problem

(12)

A dirty little secret...

•  The θ-term violates time reversal (T=CP)!

+ -

T

+ -

(13)

A dirty little secret...

T

(14)

A dirty little secret...

CP

(15)

A dirty little secret...

T

(16)

A dirty little secret...

•  Connected to strong interactions!

Electric

dipole moment

of the neutron!

(17)

Measure neutron electric dipole moment

•  θ would cause neutron EDM Experiment

Measure transition frequency.

(18)

No neutron electric dipole moment...

(19)

What do we expect?

•  Two mass scales in the game:

(20)

Implications

•  Detailed calculation gives

Extremely unnatural!

(21)

Strong CP Problem

(22)

The axion solution

to the strong CP problem

(23)

In pictures…

(24)

The axion solution to the strong CP problem

•  Make µ dynamical è it can change its value

Classical potential

(25)

Classical potential With QCD

quantum corrections

(26)

With QCD

quantum corrections initially

(27)

With QCD

è QCD likes to be CP conserving (if we allow it)

after some time

(28)

With QCD

è Can still move

è new particle = axion

(29)

Axions

•  Classical flatness from symmetry

•  Quantum corrections are small

•  New light particle: The Axion

(itʼs a Weakly Interacting Sub-eV Particle)

Good motivation

for axion/WISP experiments

Dark matter candidate

(30)

In Equations…

(31)

A Dynamical θ

•  Idea:

–  Make θ a dynamical degree of freedom a –  Let a have no tree level potential

–  Let a have only derivative couplings

•  Then:

(32)

A Dynamical θ

•  Idea:

–  Make θ a dynamical degree of freedom a.

–  Let a have no tree level potential –  Let a have only derivative couplings

•  Then:

µ=a will evolve to a=θ=0

CP is conserved

(33)

What is a?

•  Properties:

–  Let a be a dynamical degree of freedom.

–  Let a have no tree level potential –  Let a have only derivative couplings

–  a2[0,2π] since

a is Goldstone boson

of a U(1) symmetry Axion!

(34)

Peccei-Quinn Symmetry

•  Toy model:

•  U(1):

•  If µ²<0 we have SSB

Phase is Goldstone Use it as Axion

(35)

The Coupling to and

•  A diagram

•  And a dimensional argument:

(36)

The Coupling to

•  Adler-Bell-Jackiw anomaly

•  Chiral rotations not a good symmetry: it is anomalous

(37)

The Coupling to

•  Adler-Bell-Jackiw anomaly

•  Chiral rotations not a good symmetry: it is anomalous

(38)

The mass of the Axion

•  U(1)_PQ is not exact. It‘s anomalous!

•  Dimensional considerations

–  SSB scale

–  Quark masses –  QCD scale

Goldstone Pseudogoldstone

PseudoGoldstone mass

(39)

LSW

LHCCDF

LEP

SN1987a

Y inv.

SN1987a

e⁺e^- inv.+

HB stars

Cosmology

CAST₊

SUMICO

Beam dump

-15 -12 -9 -6 -3 0 3 6 9 12 15

-18 -15 -12 -9 -6 -3 0

Log₁₀m_a[eV]

Log10gaBB[GeV-1 ]

Axion-like Particles

Axion band

¼⁰ mass/energy

Weaker interaction

(40)

LSW

LHCCDF

LEP

SN1987a

Y inv.

SN1987a

e⁺e^- inv.+

HB stars

Cosmology

CAST₊

SUMICO

Beam dump

-15 -12 -9 -6 -3 0 3 6 9 12 15

-18 -15 -12 -9 -6 -3 0

Log₁₀m_a[eV]

Log10gaBB[GeV-1 ]

Axion-like Particles

Axion band 750 GeV ALP mass/energy

(41)

LSW

LHCCDF

LEP

SN1987a

Y inv.

SN1987a

e⁺e^- inv.+

HB stars

Cosmology

CAST₊

SUMICO

Beam dump

-15 -12 -9 -6 -3 0 3 6 9 12 15

-18 -15 -12 -9 -6 -3 0

Log₁₀m_a[eV]

Log10gaBB[GeV-1 ]

Axion-like Particles

Axion band 750 GeV ALP mass/energy

(42)

How to find the Axion…

(43)

Exploring fundamental high energy physics…

•  The direct approach: MORE POWER

LHC, Tevatron + ILC,CLIC

•  Detects most things within energy range

•  E.g. may find SUSY particles, WIMPs etc.

(44)

But…

•  May miss very weakly interacting matter (Axions, WIMPs, WISPs…)

•  Current maximal energy few TeV

(45)

But…

•  Man it’s DANGEROUS…

(46)

But…

•  Or much much more horrifying:

No signal above background!

(47)

The Power of Low Energy Experiments

Complementary approaches

(48)

Light shining through walls

X X

(49)

Light shining through walls

•  Test

•  Enormous precision!

•  Study extremely weak couplings!

X X

(50)

Photons coming through the wall!

•  It could be Axion(-like particle)s!

•  Coupling to two photons:

a a

(51)

Light Shining Through Walls

•   A lot of activity –   ALPS

–   BMV

–   GammeV –   LIPPS

–   OSQAR

(52)

Small coupling, small mass

Axion band

¼⁰ mass/energy

(53)

Helioscopes CAST@CERN

SUMICO@Tokyo SHIPS@Hamburg

Sun Detector

Ion

(54)

Sensitivity

Axion band

(55)

Going to the future: IAXO

The International Axion Observatory

(56)

An interesting area…

TeV °

IAXO

Definite Test of TeV transparency

Test of QCD axion

+ white dwarf anomaly

Intermediate string scale models

(57)

WISPS=Weakly interacting sub-eV particles

•  Axions

•  Massive hidden photons (without B-field)

=analog ν-oscillations

•  Hidden photon +

minicharged particle (MCP)

a a

MCP MCP

(58)

Axions and ALPs

from

String Theory

(59)

String theory

•  Attempt to unify SM with gravity

•  New concept: strings instead of point particles

(60)

String theory: Moduli and Axions

•  String theory needs Extra Dimensions Must compactify

•  Shape and size deformations correspond to fields:

Moduli and Axions

Connected to the fundamental scale, here string scale

Axion/ALP candidates

(61)

Axion (like particles): Where are we?

(62)

Axions and Moduli

•  Gauge field terms

+ Supersymmetry/supergravity

Scalar ALP/moduli coupling pseudoscalar ALP coupling

(63)

Axions and Moduli

•  Gauge couplings always field dependent (no free coupling constants)

•  Axions + Moduli always present in String theory

(64)

Masses and Couplings

•  “Axion scale” related to fundamental scale

•  If QCD axion: m_a fixed

•  However, if not QCD axion

(nearly) arbitrary

(65)

(66)

(67)

Intermediate strings Funny Higgs arguments

(68)

Dark Matter(s)

(69)

Can Dark Matter be Axiony/WISPy?

(Weakly Interacting Sub-eV Particley)

Slim

(70)

Properties of Dark Matter

•   Dark matter is dark, i.e.

it doesn‘t radiate!

(and also doesn‘t absorb)

è   very, very weak interactions with light and with ordinary matter

è Exactly the property of

Axions/WISPs

(71)

ν,

^Fixed

target

“dark”

weakly coupled =

(72)

A common prejudice

•  Dark Matter has to be heavy:

•  Prejudice based on thermal production!

and/or fermionic DM!

Both assumptions give minimal velocity

(thermal/Fermi) è galaxy, i.e. structure,

formation inhibited!

v>v

_escape

v<v

_escape

(73)

Weakly interacting

sub-eV

^DM

•  Has to be non-thermally (cold!!!) produced

•  Bosonic!

Axion(-like particles) Hidden Photons

See misalignment mechanism

(74)

Dark matter has to be heavy…

Dark matter has to be heavy

(75)

Dark matter has to be heavy…

Dark matter has to be heavy

(76)

SuperCold Dark Matter

(77)

The axion has no clue where to start

Field is stuck because of Hubble “breaking”

H>>m

(78)

The axion has no clue where to start

Can start moving…

H<<m

(79)

è Oscillations contain energy

è behave like non-relativistic particles (T=0)

(80)

Axion Dark Matter

•  è overdamped oscillator

•  è damped oscillator

è Dark Matter

(81)

Why Cold? Inflation!

Field value

space

(82)

Axion(-like particle) Dark Matter

~10¹² GeV

~10⁷ GeV

(83)

Detecting

Axiony/WISPy

DM

(84)

Use a plentiful source of axions

•  Photon Regeneration

axion

(dark matter)

Photon

(amplified in resonator)

(85)

Signal: Total energy of axion

Virial velocity in galaxy halo!

Receiver RF

(86)

An extremely sensitive probe!!!

(87)

A discovery possible any minute!

(88)

Electricity from Dark Matter ;-).

axion

(dark matter)

Photon

(amplified in resonator)

(89)

Really sustainable Energy

•  Galaxy contains (6-30)x10¹¹ solar masses of DM

è (3-15)x10⁴³ TWh

@100000 TWh per year (total world today) è 10³⁸ years J

DM power

½*v~300 MeV/cm³*300km/s~10 W/m²

compared to 2W/m² for wind

(90)

How “the axion” works

axion

B

Superconducting magnets

mirror

(91)

Encircling the axion…

(92)

Broadband

Search Strategy

(93)

Dark Matter Antenna

Antenna converts axion->photon Radiation concentrated in center

Detector

Probes here;

very sensitive!!

B

(94)

The FUNK Experiment Recycle Auger mirror

Detector

(95)

First Results

Coulomb's Law Solar physics

Dark Matter area

Haloscopes 3 - 15 GHz

15 - 100 GHz

0.1-4THz

FUNK optical

-9 -6 -3 0

-15 -12 -9 -6

Log₁₀m_X[eV]

Log10

(96)

Upgrade: The PMT 9000(+107)

Dark Matter area

15 - 100 GHz

0.1-4THz

FUNK optical

-9 -6 -3 0

-15 -12 -9 -6

Log₁₀m_X[eV]

Log10

Discovery Potential J !!!

(97)

The next years è Lower frequency

Dark Matter area

15 - 100 GHz

0.1-4THz

FUNK optical

-9 -6 -3 0

-15 -12 -9 -6

Log₁₀m_X[eV]

Log10

Discovery Potential J !!!

(98)

A Dream for Astrology ehhm Astronomy

V_DM =0 V_DM≠0=

Screen

•  Emission from moving dark matter

•  A picture of the DM-velocity distribution

(99)

New couplings:

A spin experiment

(100)

Looking for oscillating dipoles

•  Remember:

Axion field controls electric dipole moment:

•  Dipole moments follow the oscillating axion field è Tiny oscillating electric dipole

(101)

In an electric field

E d_e~s

T Energy in an elecxtric field

Torque tries to tilt dipole moment/spin

(102)

Dealing with oscillation

Problem: the dipole moment is rapidly oscillating ~m_a

è Danger of cancellation Solution: Rotate spin to compensate

è Use Spin Precession in magnetic field

S

Resonance when

(103)

Modification of Xenon EDM

Modification of Xenon EDM experiment

to be sensitive to time varying nuclear EDM

(104)

Sensitivity

Static

EDM 5

- 100Hz

100 -

1000Hz

SN1987a

Long

Measure QCD

Axion

-15 -14 -13 -12 -11 -10

-25 -20 -15 -10 -5

Log₁₀[m/eV]

Log 10[g dGeV2 ]

(105)

Conclusions

(106)

Conclusions

•  Good Physics Case for Axions and WISPs explore `The Low Energy Frontierʼ

•  Low energy experiments test energy scales much higher than accelerators

Complementary!

•  May provide information on hidden sectors and thereby into the underlying

fundamental theory

•  Dark Matter may be WISPy J

New cool Experiments underway.

(107)

a

(108)

Beyond ALPs

(109)

Hidden photons

Hidden photon

Photon

(amplified in resonator)

(110)

Also for hidden photons!!!

•  There are other very light DM candidates

•  E.g

extra (hidden) U(1) bosons=hidden photons!!!

(111)

@ DESY + Bonn: WISPDMX

New Results!

Standard Model

Intro to Axions

Here be Dragons

We need...

Physics beyond the

Standard Model

Inventory of the Universe

Where does it hide?

ν,

ν,

“dark”

weakly coupled =

What are Axion?

And why do we need them?

A „visible“ Hint for new Physics

The strong CP Problem

A dirty little secret...

A dirty little secret...

A dirty little secret...

A dirty little secret...

A dirty little secret...

Electric

dipole moment

of the neutron!

No neutron electric dipole moment...

What do we expect?

Implications

Extremely unnatural!

Strong CP Problem

The axion solution

to the strong CP problem

In pictures…

Good motivation

for axion/WISP experiments

In Equations…

A Dynamical θ

A Dynamical θ

µ=a will evolve to a=θ=0

CP is conserved

What is a?

Peccei-Quinn Symmetry

The Coupling to and

The Coupling to

The Coupling to

The mass of the Axion

Axion-like Particles

Axion-like Particles

Axion-like Particles

How to find the Axion…

LHC, Tevatron + ILC,CLIC

No signal above background!

The Power of Low Energy Experiments

Complementary approaches

• A lot of activity – ALPS

– BMV

– GammeV – LIPPS

– OSQAR

Small coupling, small mass

Going to the future: IAXO

An interesting area…

Axions and ALPs

from

String Theory

Axion/ALP candidates

Dark Matter(s)

Can Dark Matter be Axiony/WISPy?

(Weakly Interacting Sub-eV Particley)

Properties of Dark Matter

• Dark matter is dark, i.e.

it doesn‘t radiate!

(and also doesn‘t absorb)

è very, very weak interactions with light and with ordinary matter

è Exactly the property of

Axions/WISPs

ν,

“dark”

weakly coupled =

A common prejudice

v>v

v<v

•   A lot of activity –   ALPS

–   BMV

–   GammeV –   LIPPS

–   OSQAR

•   Dark matter is dark, i.e.

è   very, very weak interactions with light and with ordinary matter