20-21 December 2017
Axion physics and dark matter cosmology Workshop
Osaka, Japan

A comprehensive approach to the strong CP-problem
Yannis Semertzidis, IBS/CAPP and KAIST• IBS/CAPP• Status of our axion dark matter experiments• Axion physics, storage ring EDM and future plans1

IBS/CAPP•Was established October 15, 2013
•To put together the best possible axion darkmatter exps and reach all the way down to thetheoretical predictions

Center for Axion and Precision
Physics KAIST, Daejeon, Korea

DaejeonCosmological inventory

Professor Jihn E. Kim!
Father of the Invisible axions

Also, worked tirelessly toestablish IBS/CAPP tomake axions Visible!

Jihn E. Kim and ASK2011

Axion (Higgslet) dark matter: Imprint on thevacuum since soon after the Big-Bang!

Animation by Kristian Themann7Axion dark matter is partially converted to avery weak flickering Electric (E) field in thepresence of a strong magnetic field (B).

Animation by Kristian Themann

J. Hong, J.E. Kim, S. Nam, YkS
8
hep-ph: 1403.1576

P. Sikivie’s method: Axions convert intomicrowave photons in the presence of a
DC magnetic field (Inv. Primakov effect)
aXDetector

9a
The conversion power on resonance  g 2PV
B


Cm

0aa QL  fa 2C 
210 Watt   
 500liter   7Tesla   0.4 22B0V22

a g    ma c 2   QL  0.36   5 1025 gr/cm3   hGHz   105  

The axion to photon conversion power isvery small. Need to do more.
10

IBS/CAPP inauguration: November 2, 2017

IBS/CAPP inauguration: November 2, 2017

IBS/CAPP at Munji Campus, KAIST, January 2017.

Great people. No WIMPS!

Center for Axion and Precision Physics (IBS/CAPP)
14

Director: Yannis K. Semertzidis IBS & KAIST CAPP of Institute for Basic Science (IBS) at KAIST in Korea since October 2013.
 Projects : Axion dark matter, Storage ring proton EDM, Axion mediated long range forcesMembers : 1 Director
 1 Group Leader
 ~20 Research Fellows
 3 Engineers 5 Administrators
 ~20 Graduate Students

Refurbished a state ofthe art lab in anexisting bldg.

State of the art
infra-structure:
7 low vibration
pads for parallel
experiments; 6 cryoor dilution
refrigerators; highB-field magnets:
25T, 18T, 12T

IBS/CAPP-Physics approach
Strong CP problem (Symmetry crisis in strong
forces: hadronic EDM exp. Limits too small!)•Cosmic Frontier (Dark Matter axions): Improve in all
possible fronts: B-field, Volume, Resonator Quality
factor, Physical and Electronic noise. Check dark
matter down to 10% of axion content.
•Storage ring proton EDM (most sensitive hadronic
EDM experiment). Improve theta_QCD sensitivity by
three to four orders of magnitude!
•Together with long-range monopole-dipole (axionmediated) forces probe axion Physics!

- Low vibration pad installation

7 Low Vibration Pads (LVP) will behosting axion related experiments. 5 ofthem are dedicated to axion dark matter
experiments.

LVP facility at IBS/CAPP
Low vibration facility
search haloscope
UpFortoaxion
sevenMore than five large scale axion searchaxionexps in parallel
Search system to be installed and operated

He-3Fridge

CAPP’s lab space at KAIST,
201718

IBS/CAPP Three world-class axion dark matter experiments to reachhadronic axion dark matter sensitivity
 Cryogenics, microwave expertise, quantum limited noise
microwave amplifiers,…
 Develop open resonator exps.
 Significant player for next ten years…
 GNOME (axion dark matter stars over earth), ARIADNE
 Precision Physics in storage rings: muon g-2 and launch thebest hadronic (proton and deuteron) EDM experiment in theworld.

Axion mass target and technique
CAST

Monopole-Dipole
Interactions, No dark
matter assumed
Openresonators(ARIADNE)

Microwave cavities

20

Woohyun Chung’s slide

Magnet charging (207A, 18T)

Power output

18.7 T @ 207A after 8 hours

Monitoring programMicrostrip SQUID Amplifiers (MSA) for 1.0 – 3.0 GHz
band

Andrei Matlashov’s slide

MSA from KRISS, Korea

CHIP: 3-2 A 19 2.8

F0 = 2396 MHz, ΔF = 100 MHz, Gain = 15 dB

Andrei Matlashov’s slide

Resonant MSAs from IPHT, Jena, Germany

F0 = 1382 MHz, ΔF20dB = 8.3 MHz, ΔF15dB = 14 MHz
Andrei Matlashov’s slide

CAPP8TB
search range  [1.6, 1.7] GHz  [6.6, 7.0]  eV
conventional AMI magnet
cold bore = 165 mm
Bcenter  8 T

Vcavity~3.5 L

BlueFors DL-400
 ~ 0.45 mW cooling power @ 100 mK

2017
HEMT based
SQUID based

2018

2019

Axion haloscopes withthe Oxford-Leiden system
Oxford magnet
cold bore = 320 mm
Bcenter  12 T @ 4.2 K

Vcavity~30 Lcancellation region (<100 G) of 100 mm  100 mm
around the mixing plate of the Leiden dilution fridge

Leiden dilution fridge (magenta region)
1 mW cooling power @ 100 mKcan load up to 200 kg

Axion haloscopes withthe Oxford-Leiden system
2016
Leiden DF
Oxford magnet

2017

2018

2019

2020

2021

2022

2023

2024

25T High Tc magnet from BNL

ByeongRok Ko29

Slide by SungWoo Youn

Multi-cell Cavity: Magnet bore

Single cavity

Multiple cells ina single cavity

Multiple cavities: Cavity

Multiple cellswith a hole

• Superior to conventional multiple-cavity– Larger detection volume• V4-cell ≈ 1.7×V4-cavity=>df/dt4-cell ≈ 2.0×df/dt4-cavity– Simpler receiver chain• Single antenna => No power combiner– Easier phase-matching mechanism

Slide by SungWoo Youn

Multi(Double)-cell Cavity• Opening breaks the frequency
degeneracy– Lowest mode => TM010-like• C=0 for higher mode(s)– Does not interfere with sensitivity• Symmetric field distribution
TM010-like

TM110-like– Condition of phase-matching• E=0 at center for higher mode(s)– Vanishing of higher mode peaks inS parameter => phase-matching• Promising design for higherfrequency regionsCell 1

Cell 2

“Others”

34

HAYSTAC exp. (Yale,…)35

HAYSTAC exp. (Yale,…)36

Axion sensitivity
22æöæöæödf f 1 1 GHz5GHz
40.25
K15=»g10GeV) ç÷ ç÷÷ ç(aggdt Q tyearè f ø è SNR ø è T ø24

æ B ö æ c ö æV ö æ Q ö´ç÷ ç ÷ ç ÷ ç 5÷
è 25T ø è 0.6 ø è 5l ø è 10 ø
42

2Parameter
dependence

ADMX plans

IBS/CAPP &KAIST

Gain factor

B4QT2V2

7.5 – 9T
50-300K
50mKV125 – 35T
107 (106)
50-30mK
1-7 x V1

100-250
3-10
11-50

Up to 5-7 parallel experiments at IBS/CAPP.
Total gain in scanning rate: 300 – 105; gain in gγ: 4 - 18

Ben MacAllister, The ORGAN project

38

MADMAX principle: axion-photonmixing

39

MADMAX projected sensitivity

40

5-10 years away:

41

Storage ring proton EDM and ARIADNE• Proton EDM exp. and ARIADNE together probing axion
physics like no other exps!
• It is hard to look for large axion mass (>20GHz) as dark matterwith existing techniques. For large axion mass ARIADNE has
the best chance of pointing out its mass if a signal is detected.
After that we can design a dedicated axion dark matter
experiment for that mass…
• For example: a proton EDM signal at 10-27e-cm and the absenceof a signal with related ARIADNE sensitivity can exclude
axions from a large parameter space!

Leadership at CAPP:
Yun Chang Shin

Axions with ARIADNE:
Axion Resonant InterAction
DetectioN Experiment
A. Arvanitaki and A. Geraci
PRL 113, 161801 (2014)

ARIADNE PI: A. Geraci

43

ARIADNE’s axion mass range reach

IBS/CAPP

44

Teamleader: Yun-chang Shin
45

Axion mediated long range forces
6meV

600μeV

EW CPV phase, ϑ~10-1660μeV

6μeV

axionmassFundamental particle EDM:
study of CP-violation beyond theStandard Model

-29Proton EDM proposal: d=10 ecm

• High sensitivity experiment:• Blowing up the proton to become as large as thesun, the sensitivity to charge separation along
N-S would be r < 0.1 μm!
Sunproton

Why is there so much matter after the BigBang:We see:nB» (6.08 ± 0.14 ) ´ 10 -10ng

From the SM:nB» 10 -18ng

The proton EDM electric ring, 500m circ.
Current goal 10-29e-cm; upgraded: 10-30e-cm.
New Physics reach >103TeV and improve present
theta_QCD limits by >three orders of magnitude
It has been approved as a PBC candidate project at CERN.
A comprehensive study is underway with the conclusions
to be presented at the European Strategy meeting inVenice 2019.

srEDM Collaboration Meeting at KAIST, KAIST, 21 April, 2016.

CPV new physics induces a non-zerotheta_QCD, probing the axion mechanism!

5SUSY-like physics induces a non-zerotheta_QCD probing the axion mechanism!
6meV

600μeV

60μeVpEDM final sensitivity
at 10-30e-cm.

6μeVaxion
mass

Current nEDMlimit

53

EW CPV phase, ϑ~10-16

Search for axion dark matter instorage rings

54

Indirect Muon EDM limit from the g-2 Experimentz


ωaB






edmsβx



e
m

y



   a   edm
edm
tan  aRon McNabb’s Thesis 2003:

19

 2.7  10Yannis Semertzidise  cm 95% C.L.

Axion dark matter search in storage rings• A modified storage ring EDM method can search forthe oscillating theta term.
• Oscillating axion field in resonance with the g-2frequency.

• Frequency range: 100MHz all the way down to submicro-Hz.
• Great physics output, simpler systematic errors

Search for axion dark matter instorage rings• The axion field (dark matter) induces an oscillating EDM innucleons P. Graham and S. Rajendran PRD 84, 055013, 2011
and PRD 88, 035023, 2013.
• A combination of the storage ring EDM method plus the g-2
principle we can search for axion dark matter!
• Large effective E-field• High statistical power• Large axion frequency coverage• Can take advantage of large axion coherence time since thestability of the g-2 tune is shown to be at the 10-10 per 100s
level! (Work at COSY)

57

Search for axion dark matter instorage rings (1710.05271)

58

Search for axion dark matter instorage rings (1710.05271)

59

PhysRevX.7.041034

StorageRingEDM
potential(preliminary)Summary• Dark matter is a great mystery and challenge• IBS/CAPP goal is to make a significant progress answering
whether or not axions are the dark matter of our universe.
• New powerful magnets/new techniques in the axion dark mattersearch• Very soon we will be reaching the theoretical axion parametersin the mass range possible by microwave cavities.
• Next: Open resonators• Proton EDM exp. and ARIADNE combined probe axion Physics
in a way that no other experiments can• Storage ring EDM in search of low frequency axion dark matter!
62

Extra Slides

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