Dark Matter - PowerPoint Presentation

Slide1

Dark Matter

Axion Dark Matter

Georg G.

Raffelt, Max-Planck-Institut für Physik, München

Physics Colloquium, University of Sydney, 3 March 2014Slide2

Axions

as Cold Dark Matter of the Universe

Dark

Energy ~70%

(

Cosmological Constant)

Neutrinos

0.1

-2%

Dark Matter~25%

Ordinary Matter

~

5%

(of this only about

10% luminous)Slide3

Neutron

Proton

Gravitation (Gravitons?)

Weak

Interaction (W and Z Bosons)

Periodic System of Elementary Particles

Electromagnetic

Interaction (Photon)

Strong

Interaction (8 Gluons)

Down

Strange

Bottom

Electron

Muon

Tau

e-Neutrino

m

-Neutrino

t

-Neutrino

n

t

n

m

n

e

e

m

t

d

s

b

1

st

Family

2

nd

Family

3

rd

Family

Up

Charm

Top

u

c

t

Quarks

Leptons

Charge

-

1/3

Down

Charge

-

1

Electron

Charge

0

e-Neutrino

n

e

e

d

Charge

+

2/3

Up

u

HiggsSlide4

Supersymmetric Extension of Particle Physics

In

supersymmetric

extensions of the particle-physics standard model, every boson has a fermionic partner and vice versa

Sleptons

(

,

,

…)

Squarks

(

,

,

…)

Spin

Superpartner

0

1/2

Gluinos

Wino

Zino

Photino

(

)

1/2

3/2

Higgsino

Gravitino

1/2

Leptons (e,

n

e

, …)

Quarks (u, d, …)

1

Gluons

W



Z

0

Photon (

g

)

0

2

Higgs

Graviton

Spin

Standard particle

If R-Parity is conserved, the lightest SUSY-particle (LSP) is stable

Most plausible candidate for dark matter is the

neutralino

,

similar to a massive

Majorana

neutrino

Neutralino

= C

1

Photino

+ C

2

Zino

+ C

3

HiggsinoSlide5

Laboratory Searches for WIMP Dark Matter

Energy

deposition

Recoil energy

(few keV) is

measured by

Ionisation

Scintillation

Cryogenic

Galactic

dark matter

particle

(e.g

. neutralino

)Slide6

WIMP Searches (Underground Physics)

COUPP

PICASSO

XENON

LUX, ZEPLIN

WARP, ArDM

DEAP/CLEAN

DAMA/LIBRA

KIMS, XMASS

DRIFT

GERDA

CDMS

EDELWEISS

CRESST

ROSEBUD

Heat

Phonons

Charge

LightSlide7

WIMP Cross Section Limits 2014

Klaus Eitel, 2014Slide8

High- and Low-Energy Frontiers in Particle Physics

eV

Planck

mass

GUT

scale

Electroweak

scale

QCD

scale

Cosmological

constant

WIMP dark matter

(related to EW scale, perhaps SUSY)

Axion dark matter

(related to Peccei-Quinn symmetry)

Accelerator Frontier

CERNSlide9

Axion Physics in a Nut Shell

CP conservation in QCD by

Peccei-Quinn mechanism

For fa

≫

f

p

axions are “invisible”

and very light

 Axions a ~ p0

m

p

f

p



m

a

fa

g

g

a

Particle-Physics Motivation

Axions

thermally produced in

stars,

e.g

. by Primakoff production

Limits from avoiding excessive

energy drain

Solar

axion searches

(CAST, Sumico)

a

g

Solar and Stellar Axions

In spite of small mass, axions are born

non-relativistically

(non-thermal relics)

Cold

dark matter

candidate

m

a

~

10

m

eV

(or much smaller or larger)

Cosmology

Search for Axion Dark Matter

S

N

g

a

B

ext

Microwave

resonator

(1 GHz = 4

m

eV)

Primakoff

conversion

ADMX-LF

(UW Seattle)

ADMX-HF (Yale)Slide10

CP Violation in Particle Physics

Physics Nobel Prize 2008

Discrete symmetries in particle

physics

C

–

Charge

conjugation, transforms particles to antiparticles

violated by weak interactionsP – Parity, changes left-handedness to right-handedness

violated by weak interactionsT –

Time

reversal, changes direction of motion (forward to backward

)

CPT

–

exactly

conserved in quantum field

theoryCP – conserved

by all gauge interactions

violated by three-flavor quark mixing matrix

M. Kobayashi

T. Maskawa

All

measured CP-violating effects derive

from a single phase in the quark mass matrix (Kobayashi-Maskawa phase),

i.e. from complex Yukawa couplings

Cosmic matter-antimatter asymmetry requires new ingredientsSlide11

The CP Problem of Strong Interactions

Real quark

mass

Phase from

Yukawa coupling

Angle

variable

CP-odd

q

uantity

Remove phase of mass term by

chiral transformation

of quark fields

can

be traded between quark phases and

term

No physical impact if at least one

Induces

a large neutron electric dipole moment (a T-violating quantity)

Experimental

limits:

Why

so small?

 Slide12

Neutron Electric Dipole Moment

Violates time reversal (T) and

space reflection (P) symmetries

Natural scale

Experimental limit

Limit on coefficient

 Slide13

Strong CP Problem

QCD vacuum energy

• CP conserving vacuum has

(Vafa and Witten 1984)

•

QCD could have any

, is “constant of nature”

•

Energy can not be minimized:

not dynamical

Equivalent

Equivalent

Peccei-Quinn solution:

Make

dynamical, let system relax to lowest

energy

 Slide14

The Pool Table Analogy (Pierre Sikivie 1996)

Gravity

Symmetric

relative

to gravity

Pool table

New degree

of freedom



Axion

(Weinberg 1978, Wilczek 1978)

Axis

Symmetry

dynamically

restored

(Peccei & Quinn 1977)

Symmetry

broken

Floor

inclined

f

aSlide15

35 Years of AxionsSlide16

The Cleansing Axion

Frank Wilczek

“I named them after a laundry

detergent, since they clean up

a problem with an axial current.”

(Nobel lecture 2004)Slide17

Axion Bounds and Searches

10

3

10

6

10

9

10

12

[GeV] f

a

eV

keV

meV

m

eV

m

a

neV

10

15

Direct

searches

Too

much CDM

(misalignment)

Tele

scope

Experiments

Globular clusters

(a-

g

-coupling)

SN 1987A

Too many events

Too much

energy loss

Too much

hot dark

matter

CAST

ADMX

(Seattle & Yale)

Globular clusters (He ignition), WD cooling

(a-e coupling)

Too

much cold dark matter

(re-alignment with

Q

i

= 1)

Classic

region

Anthropic

regionSlide18

Dark

Energy

~

70% (Cosmological Constant)

Neutrinos

0.1

-

2%

Dark Matter

~25%

Ordinary Matter

~

5%

(of this only about

10% luminous)

Axions as Cold Dark Matter of the UniverseSlide19

Creation of Cosmological Axions

(very early universe)

U

PQ

(1) spontaneously broken

Higgs field settles in

“Mexican hat”

Axion field sits fixed at

(

eV)

Axion mass turns on quickly

by thermal

instanton gas

Field starts oscillating when

Classical field oscillations

(axions at rest)

Axions are born as nonrelativistic, classical field oscillations

Very small mass, yet cold dark matterSlide20

Axion Cosmology in PLB 120 (1983)Slide21

Killing Two Birds With One Stone

Peccei-Quinn mechanism

Solves strong CP problem

Provides dark matter in the form of axionsSlide22

Cosmic Axion Density

Modern values for QCD parameters and temperature-dependent axion mass

imply (Bae, Huh & Kim, arXiv:0806.0497)

If axions provide the cold dark matter:

•

implies

GeV

and

m

eV

(“classic window

”)

•

GeV

(GUT scale) or larger (string inspired) requi

res

(“

anthropic window”)

 Slide23

Axion Production by Domain Wall and String Decay

Recent numerical studies of collapse

of string-domain wall system

Implies a CDM axion mass of

Hiramatsu

, Kawasaki,

Saikawa

&

Sekiguchi, arXiv:1202.5851 (2012

)

Remains to be confirmed,

interpretation of numerical studies

not entirely straightforward

 Slide24

BEC Formation

• Axions

~ WIMP dark matter on scales axion Compton wavelength?

• Larger-range correlation established by BEC dynamics? (Observable?)• Axions born as classical field oscillations → Issue of classical field dynamics (not a quantum effect)• BEC formation caused by gravitational interactions possible ???See also • Erken, Sikivie, Tam & Yang, arXiv:1111.1157 • Saikawa & Yamaguchi, arXiv:1210.7080

• Noumi

,

Saikawa

,

Sato & Yamaguchi, arXiv:1310.0167 • Davidson & Elmer, arXiv:1307.8024 • Berges & Jaeckel,

arXiv:1402.4776 ~100 citationsSlide25

High- and Low-Energy Frontiers in Particle Physics

eV

Planck

mass

GUT

scale

Electroweak

scale

QCD

scale

Cosmological

constant

WIMP dark matter

(related to EW scale, perhaps SUSY)

Axion dark matter

(related to Peccei-Quinn symmetry)

Accelerator Frontier

CERNSlide26

Searching for Solar Axions

Searching for

Axion-Like ParticlesSlide27

Experimental Tests of Invisible Axions

Primakoff effect:

Axion-photon transition in external

static E or B field(Originally discussed for by Henri Primakoff 1951)

Pierre Sikivie:

Macroscopic B-field can provide a

large coherent transition rate over

a big volume (low-mass axions)

Axion helioscope:

Look at the Sun through a dipole magnet

Axion haloscope:

Look for dark-matter axions with

A microwave resonant cavitySlide28

Search for Solar Axions

g

a

Sun

Primakoff

production

Axion Helioscope

(Sikivie 1983)

g

Magnet

S

N

a

Axion-Photon-Oscillation

Tokyo

Axion Helioscope (“Sumico”)

(

Results since 1998, up again 2008)

CERN

Axion Solar Telescope (CAST)

(

Data since 2003)

Axion flux

Alternative technique:

Bragg conversion in crystal

Experimental limits on solar axion flux

from dark-matter experiments

(SOLAX, COSME, DAMA, CDMS ...)Slide29

Tokyo Axion Helioscope (“Sumico”)

Moriyama, Minowa, Namba, Inoue, Takasu &

YamamotoPLB 434 (1998) 147Inoue, Akimoto,

Ohta, Mizumoto,

Yamamoto & Minowa

PLB 668 (2008) 93

m

 Slide30

CAST at CERNSlide31

Recent “shining-light-through-a-wall” or vacuum birefringence experiments:

ALPS

BMV BFRT GammeV

LIPPS OSQAR PVLAS Photon Regeneration Experiments

Ehret et al. (ALPS Collaboration), arXiv:1004.1313

(DESY, using HERA dipole magnet)

(Laboratoire National des Champs Magnétiques Intens, Toulouse)

(Brookhaven, 1993)

(Fermilab)

(Jefferson Lab) (CERN, using LHC dipole magnets)

(INFN Trieste)Slide32

Shining TeV Gamma Rays through the Universe

Figure from a talk by Manuel Meyer (Univ. Hamburg)Slide33

Parameter Space for Axion-Like Particles

Invisible

axion (DM)

Axion Line

Invisible

axion (DM)

Axion Line

HB

Stars

Invisible

axion (DM)

Axion Line

HB

Stars

CAST

Solar Axions

Invisible

axion (DM)

Axion Line

HB

Stars

Laser

Experiments

CAST

Solar Axions

TeV

g

rays

How to make

progress?Slide34

Next Generation Axion Helioscope (IAXO) at CERN

• Irastorza et al.: Towards a new generation axion helioscope, arXiv:1103.5334• Armengaud et al.: Conceptual Design of the International Axion Observatory

(IAXO), arXiv:1401.3233

Need new magnet w/– Much bigger aperture:

per

bore

–

Lighter

(no

iron yoke)– Bores at Troom Slide35

Searching for Axion Dark Matter

Searching for

Axion Dark MatterSlide36

Search for Galactic Axions (Cold Dark Matter)

Power

Frequency

m

a

Axion Signal

Thermal noise of

cavity & detector

Power of galactic axion signal

Microwave Energies

(1 GHz

 4

m

eV)

Dark matter axions

Velocities in galaxy

Energies therefore

m

a

= 1

-

100

m

eV

v

a

 10

-

3

c

E

a



(1



10

-

6

) m

a

Axion Haloscope

(Sikivie

1983)

B

ext

 8 Tesla

Microwave

Resonator

Q

 10

5

Primakoff Conversion

g

a

B

ext

Cavity

overcomes

momentum

mismatch

 Slide37

Axion Dark Matter Experiment (ADMX), Seattle

Adapted from Gianpaolo CarosiSlide38

SQUID Microwave Amplifiers in ADMX

Adapted from Gianpaolo CarosiSlide39

Axion Dark Matter Searches

1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) 3153

2. University of Florida PRD 42 (1990) 12973. US Axion Search ApJL 571 (2002) L27

4. CARRACK I (Kyoto)

hep-ph/0101200

1

2

3

4

Limits

assuming axions are the galactic dark

matter with standard halo

KSVZ

DFSZ

ADMX-LF (Seattle) search range (2015+)Slide40

ADMX-HF at

Yale (Steve Lamoreaux Group)

Design of

cavity & magnetDilution refrigerator above & below deck

ADMX-HF will also be a test-bed for

innovative concepts,

e.g

. thin-film superconducting cavities

Adapted from Karl van BibberSlide41

WISPDMX at DESY and MPIfR

208 MHz microwave cavities

H1 detector

Microwave

cavities: HERA – 50, 208,

500

MHz

208

MHz cavity

:

resonant modes at 199, 295, 433, 524, 579, 707, 765, 832 MHzMagnets: DESY H1 1.1 T

(solenoid

),

HERA

5

T

(dipole

),

Receiver technology: MPIfR, Tn

~ 100 KPhase 1,2 – searches using available facilities

Phase 3 – advanced searches with specially designed facilitiesSlide42

Broadband Approaches

„

Focusing“ the DM signal w/ spherical reflector

Feasible above 10 GHz

TOKAMAKs:

- Optimize

B

2

V

factor in a radiometer mode

- Good at low frequencies- Design study under way (Lobanov et al. 2013) 

TOKAMAK

Facility

B

[T]

V

[m

3

]

B

2

V

[T2 m3]

ToreSupra

4

30480

JET4

200

3200ITER5

1200

30000MPP ASDEX

3.1

14

135TEXTOR

3.0

763

Microwave cavity experiment

B

[T]V

[m3]B2V

[T

2 m3]

ADMX7.6

0.211.5WISPDMX

1.1

0.460.6

Horns et al. 2013Slide43

Center for Axion and Precision Physics (CAPP)

New Institute for Basic Science (IBS), Korea

The plan is to launch a competitive Axion Dark Matter Experiment in Korea, participate in state-of-the-art axion experiments around the world, play a leading role in the proposed proton electric-dipole-moment (EDM) experiment and take a significant role in storage-ring precision physics involving EDM and muon g–2 experiments.

15 Oct 2013

Yannis

SemertzidisSlide44

What if the axion is found?Slide45

1D Infall and the Folding of Phase SpaceSlide46

Fine Structure in the Axion Spectrum

Axion distribution on a 3-dim sheet in 6-dim phase space

Is “folded up” by galaxy formation

Velocity distribution shows narrow peaks that can be resolved More detectable information than local dark matter density

P.Sikivie

& collaboratorsSlide47

Axion Bounds and Searches

10

3

10

6

10

9

10

12

[GeV] f

a

eV

keV

meV

m

eV

m

a

neV

10

15

Direct

searches

Too

much CDM

(misalignment)

Tele

scope

Experiments

Globular clusters

(a-

g

-coupling)

SN 1987A

Too many events

Too much

energy loss

Too much

hot dark

matter

CAST

ADMX

(Seattle & Yale)

Globular clusters (He ignition), WD cooling

(a-e coupling)

Too

much cold dark matter

(re-alignment with

Q

i

= 1)

Classic

region

Anthropic

regionSlide48

Oscillating Neutron EDM by Axion Dark Matter

Assume axions are galactic dark matter:

300 MeV/cm3

Independently of

expect

Expect

time-varying neutron EDM, MHz frequency for

GeV

8 orders of magnitude below limit on static EDM, but oscillates!

Oscillating axion field (DM)

→ Oscillating

Q

term

→

Oscillating neutron EDMSlide49

Searching for Axions in the Anthropic Window

Graham & Rajendran,

arXiv:1101.2691Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089

CASPEr experiment

P

recise

magnetometry to measure

tiny deviations from Larmor

frequencySlide50

Cosmic Axion Spin Precession Experiment (CASPEr)

Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089

Time-varying nucleon EDM caused by axion DM in Lead Titanate magnetometerPhase I

Phase IIMagnetometer noise limitSlide51

Helmholtz Institute Mainz (HIM)

Building under construction

New institute onStructure, symmetry and stability of matter and antimatter

Dmitry BudkerMoving from Berkeley to HIMPlans to pursue CASPErSlide52

Dow Jones Index of Axion Physics

inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar)Slide53

Pie Chart of Dark Universe

Dark

Energy

~70%

(

Cosmological Constant)

Neutrinos

0.1

-2%

Dark Matter~25%

Ordinary Matter

~

5

%

(of this only about

10% luminous)