Ultralight dark matter

Javier RedondoRamón y Cajal fellowUniversidad de Zaragoza (Spain)

Javier Redondo (Zaragoza U)

MIAPP Munich, Dec 1st 2015

Outline

- mass < eV, Fermions, bosons

- Theoretical motivation

- Relic abundance

- Ultralight is different

- Direct Detection

- Laboratory searches

- Indirect Detection ... not much

Low mass bosons (technically natural)

- Pseudo-Goldstone bosons Very generic BSM Axions motivated by the strong CP problem Majorons, familons, etc...

- Axion-like particles in string theories Non-perturbative masses O(100) ALPs in compactifications ... an Axiverse! - Gauge U(1) vector bosons Stuckelberg mass Hidden sectors of string theory?

- The value of controls matter-antimatter differences in QCD✓

Axions and strong CP (bottom up)

✓↵s

8⇡Gµ⌫

eGµ⌫

P, T (CP) violating

✓0 ⇡�⇡

- The value of controls matter-antimatter differences in QCD

n

n

n

n

✓

n

n

Measured today |✓| < 10�10 (strong CP problem)

Axions and strong CP (bottom up)

0 ⇡�⇡

- is it a dynamical field?

n

n

Energy

✓

Measured today |✓| < 10�10 (strong CP problem)

✓(t,x)

generated by QCD!

Axions and strong CP (bottom up)

0 ⇡�⇡

time

n

n

Energy

Measured today |✓| < 10�10 (strong CP problem)

- is it a dynamical field? ✓(t,x)generated by QCD!

✓(t) = ✓0 cos(mat)

Axions and strong CP (bottom up)

0 ⇡�⇡

time

n

n

Energy

~ One parameter theory

axion mass✓(t, x) = a(t, x)/fa

ma = 6meV109 GeV

fa

Measured today |✓| < 10�10 (strong CP problem)

- is it a dynamical field? ✓(t,x)generated by QCD!

✓(t) = ✓0 cos(mat)

Axions and strong CP (bottom up)

0 ⇡�⇡

time

n

nCoherent oscillations

=Dark Matter Axions

Energy

~ One parameter theory

axion mass✓(t, x) = a(t, x)/fa

ma = 6meV109 GeV

fa

Measured today |✓| < 10�10 (strong CP problem)

- is it a dynamical field? ✓(t,x)generated by QCD!

✓(t) = ✓0 cos(mat)

Axions and strong CP (bottom up)

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

ma ' m⇡f⇡fa

' 6 meV109GeV

fa

Mass

1

faa

1

faa

1

faa WISPs

Axion Mass/couplings

Quarks, Photons

Leptons

- Generic interactions for Pseudo-Goldstone bosons- Stringy ALPs, f scale ~ string scale, mass unrelated

New gauge forces : light hidden photons

- Extra hidden U(1)’s (Stückelberg mass)

- Kinetic mixing with photon

- Building blocks in type IIb string theory

� ⇠ egh16⇡2

� �0LI = �1

2�Fµ⌫B

µ⌫

Predictions ...Goodsell 2011

Mass

Mix

ing

Strin

g sc

ale

Cicoli 2011

Anisotropic predictions ...

Mass

Mix

ing

Relic production

Relic production: realignment

- Thermal relics would be hot DM but never enough (recall m<eV)

- Non-thermal mechanisms: realignment from initial conditions

0.001 0.01 0.1 1 10 100 1000-0.5

0.0

0.5

1.0

⇢ ⇠ ⇢0/R(t)3

DUST-likeLambda-like

ak + 3Hak +m2aak ' 0

⇢ = cons

Evolution of decoupled field (zero mode)

t ⇠ 1

ma

✓(t) =a(t)

aI

Relic production: realignment

- Thermal relics would be hot DM but never enough (recall m<eV)

- Non-thermal mechanisms: realignment

Is Predictivity lost? not completely

⇢CDM ' ⇢DM ⇥r

ma

eV

✓aI

4.8⇥ 1011 GeV

◆2

Axio

n

ma / f�1a

aI = faaI ⌧ fa

�⇡

✓

⇡Relic production: topological defects

- After phase transition- random initial conditions- average is predictive

- but topological defects!

- decay into axions uncertain! - Sikivie, Shellard, ... - Kawasaki & al 2014 - Fleury & Moore 2015

�⇡

✓

⇡Relic production: topological defects

- After phase transition- random initial conditions- average is predictive

- but topological defects!

- decay into axions uncertain! - Sikivie, Shellard, ... - Kawasaki & al 2014 - Fleury & Moore 2015

Relic production: topological defects

- After phase transition- random initial conditions- average is predictive

- but topological defects!

- decay into axions uncertain! - Sikivie, Shellard, ... - Kawasaki & al 2014 - Fleury & Moore 2015

Generalisation for ALPs coupled to photons

g ⇠ ↵

2⇡aI

Arias et al 2012

Average models

modelsaI ⌧ fa

Phot

on co

uplin

g

why-not models

ExcludedLab & Astro

Generalisation for ALPs coupled to photons

g ⇠ ↵

2⇡aI

Arias et al 2012

Average models

modelsaI ⌧ fa

Phot

on co

uplin

g

why-not models

ExcludedLab & Astro Unstable

Generalisation for ALPs coupled to photons

g ⇠ ↵

2⇡aI

Arias et al 2012

Average models

modelsaI ⌧ fa

Phot

on co

uplin

g

why-not models

Observable Decays

ExcludedLab & Astro Unstable

Generalisation for ALPs coupled to photons

g ⇠ ↵

2⇡aI

Arias et al 2012

Average models

modelsaI ⌧ fa

Phot

on co

uplin

g

why-not models

Hidden photons : isocurvature dark matter Graham 2015

- Misalignment sourced by Inflation itself

- Longitudinal mode ~ scalar- Except for extra suppression low modes- Compatible with CMB isocurvature constraints- Not possible for axions & ALPs

small scale extra suppression

h|Al|i ⇠HI

2⇡

Hidden photons : isocurvature dark matter Graham 2015

HI ⇠ 1014GeV

- Prediction?, connection of DM abundance with H-Inflation (measurable from B-modes)

HI < 1014GeV

Excluded for HP dark matter (too interacting)

Ultralight is different- DUST-like period before matter-radiation!- Lower limit to the mass CMB distortions

Hlozek 2015

- Ultralight axions (~10^-22 eV) differences in Structure formation (wave interference)

DM fr

actio

n

Schive 2014

- Lengths ~ 1/m- softer cores- low mass halos suppressed- Sikivie’s condensate...

DM Direct detection

10-7 10-6 10-5 10-4 10-310-1

1

10

102

10310-1 1 10 102

10-1

1

10

102

103

c�KSVZ

DFSZ

ADMX

RBF

UF

ADMX AD

MX2 AD

MX-HF

CAR

RACK?

ma[µeV]

⌫[GHz]

IAXO

Cavity experiments

- Dark matter, classical field- Axions, ALPs HPs couple to photons - Modified Electrodynamics (example axions)

r ·D = ⇢f

r⇥H� @D

@t= Jf � c�

↵

2⇡B@✓

@tr ·B = 0

@B

@t+r⇥E = 0

In a magnetised medium

✓(t),�(t), ~A0(t) / cos(mt)

Ea(t) =c�↵✓0B

2⇡✏cos(mat)

|Ea| ⇠ 0.6c� ⇥ 10�30 V

m

- Amplify signal in a MW resonant cavity (Sikivie ‘83)

- Tunable cavity- High B field- Low Temperature (<K)- Low noise pre-amp (<K)

Low signalHigh noise

Cavity experimentsAD

MX

ADM

X-HF

ADM

X-Fe

rmila

b

CULT

ASK

- CAP

P -Ko

rea

CAST

-CAP

P

CARR

ACK

(disc

ontin

ued)

RADE

S

P ⇠ Q|Ea|2(V ma)G

P ⇠ |Ea|2A

Q ⇠ 104 ⇠ Am2acomparable if

Dish antenna

E-fie

ld ex

cites

mirr

or to

emit

phot

ons

Dish antenna for Hidden PhotonsTo

kyo

Expe

rimen

tsKa

rsruh

e FUN

K

visible

MW

Enhanced mirror with dielectric layers

E-fie

ld ex

cites

mirr

or to

emit

phot

ons P ⇠ |Ea|2A⇥ � boost

- Just a mirror is not good enough for axions ...- Use many (mirror configuration, cavity configuration)

Oscillating electric dipole moment (axion DM)

dn ⇠ 10

�35cos(mat)e cm

- Mainz (D. Budker’s group) & Berkeley- B-field, coherence time, sensitivity to m < neV- Phase I starts in 2016, Phase II physics results

EDM + Large E-fields in PbTiO3

Stars as Laboratories

⌫, ⌫ �

WISPs ?

Stellar cooling Numerical simulations vs. Observations

- Strong constraints (Sun, SN1987A, WDs, RG, HB ...)- But slight preferences for meV-mass axions (electron/neutron coupling) Luminosity of brightest Red Giant White dwarf luminosity F CAS A cooling

Viaux 2013 Bertolami 2014 Stetson 2014

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : Axions

Solar Axions 5th forces Photon regeneration

IAXO CDR 2014 Arvanitaki Geraci PRL 2014 ALPS-II TDR 2013

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Laboratory searches : HPs

Coulomb’s law Photon regeneration

SHIPS, DM detectors XENON10 Williams ... 1971 ALPS-II, MW cavities

Solar HPs

Indirect detection

- Axions, ALPs, HPs are not stable

- Decay lifetime very long (sub-eV)- Annihilation negligible

- But inhomogeneous DM, axion miniclusters, HP clumps- Annihilation in a neutron star ... Fast Radio Bursts?

a ! �� , �0 ! ���

Zurek et al 07, See also Kolb & Tkachev 94

Iwazaki; Tkachev , 2014

Conclusions

- Axions, Axion-likes, Hidden Photons make good dark matter

- Bottom-up and Top-bottom motivation

- Relic abundance : realignment and topological defects

- Ultralight is different : hyperlow mass effects in structure formation

- Direct Detection: key target areas not completely covered

- Laboratory searches,

- Indirect Detection ... not much

Axion DM : A developing picture

osc. EDM

IAXO DM

IAXO DM

Dish Antenna?

CAPP

5th forces?

ADMXADMX-HF