Prospects for Cosmic Axion Detection with ABRACADABRA · Jesse Thaler — Prospects for Cosmic Axion Detection with ABRACADABRA 5 Initial Target: ABRACADABRA–10cm Axion Coupling

Jesse Thaler — Prospects for Cosmic Axion Detection with ABRACADABRA 1

Jesse Thaler

GPMFC Workshop on Ultralight Dark Matter, Washington, DC — January 27, 2017

Prospects for

Cosmic Axion Detection

with ABRACADABRA


From Theory… …to Experiment

a

h

R

B0

r

A Broadband/Resonant Approach toCosmic Axion Detection with an

Amplifying B-field Ring Apparatus

[Kahn, Safdi, JDT, 1602.01086] [development at MIT under NSF EAGER with PI Winslow,Conrad, Formaggio, Heine, Kahn, Minervini, Ouellet,

Perez, Radovinsky, Safdi, JDT, Winklehner]

ABRA–10cm


Ultimate Goal: ABRACADABRA–1m (or 10m)

GUT-scale QCD Axion Dark Matter

[2016 PDG Axion Review]

Axion Mass mA (eV)

fA (GeV)

10-11

10-10

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

103

104

105

106

100

101

102

103

104

105

106

107

108

109

1010

1011

1012

1013

1014

1015

1016

1017

ADMX G2 ADMX IAXO CASPEr CAST

WDLF (gAee DFSZ) WDLF Hint

HB Stars in GCs (gAγγ DFSZ)

KS

VZ

HB Hint

RGs in GCs (gAee DFSZ) RG Hint

SN1987A (gApp KSVZ) Burst Duration Counts in SuperK

Telescope/EBL

Hot-DM / CMB / BBN

Beam Dump

XENON100 (gAee, DFSZ)

NS in Cas A Hint (gAnn DFSZ)

Dark Matter (post-inflation PQ phase transition)

Dark Matter (pre-inflation PQ phase transition)

Black Holes

10–22 T signal @ 250 kHz

t

aHtL

initial misalignment

3H = ma

a ∝ T 3/2 cos(mat)

θi = ai/fa

Strong CP solution atwell-motivated mass scale…

…and right DM abundance with 1% tuning in initial

misalignment angle.

Jesse Thaler — Prospects for Cosmic Axion Detection with ABRACADABRA

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Initial Target: ABRACADABRA–10cm

Axio

n C

ouplin

g |G

Aγγ

| (

GeV

-1)

Axion Mass mA (eV)

10-16

10-14

10-12

10-10

10-8

10-6

10-10

10-8

10-6

10-4

10-2

100

LSW(OSQAR)

Helioscopes(CAST)

Haloscopes(ADMX)

Tele

scopes

Horizontal Branch Stars

KSVZ

DFSZ

VMB(PVLAS)

SN 1987A HESS

IAXO

AD

MX

CAST

ABRA–10cmbroadband

ABRA–10cmresonant

Axion-like DM coupled to Electromagnetism

Substantial discovery potential for small scale prototype

QCD A

xion

Band

L ⊃ gaγγ aE ·B


Initial Target: ABRACADABRA–10cm

Axio

n C

ouplin

g |G

Aγγ

| (

GeV

-1)

Axion Mass mA (eV)

10-16

10-14

10-12

10-10

10-8

10-6

10-10

10-8

10-6

10-4

10-2

100

LSW(OSQAR)

Helioscopes(CAST)

Haloscopes(ADMX)

Tele

scopes

Horizontal Branch Stars

KSVZ

DFSZ

VMB(PVLAS)

SN 1987A HESS

IAXO

AD

MX

CAST

ABRA–10cmbroadband

ABRA–10cmresonant

Axion-like DM coupled to Electromagnetism

Substantial discovery potential for small scale prototype

QCD A

xion

Band

L ⊃ −1

4gaγγaFµν

eFµν10-5

10-4

10-3

10-2

10-1

1/2 1

/

10-14

10-12

10-10

10-8

10-6

10-4

10-2

100

10-20

10-18

10-16

10-14

10-12

10-10

10-8

10-6

108

1010

1012

1014

1016

1018

1020

ma (eV)

ga

(GeV-1)

fa (GeV)

KSVZ

N-M=2

N-M=26

IAXO

ADMX

ABRA-Res

ABRA-Broad

CASPEr-II

Solve Strong CP with Exponentially Large E&M Coupling?

[Farina, Pappadopulo, Rompineve, Tesi, 1611.09855][based on Choi, Im, 1511.00132; Kaplan, Rattazzi, 1511.01827; Giudice, McCullough, 1610.07962]

[appears to evade misalignment bounds from Ariasa, Cadamuro, Goodsell, Jaeckel, Redondo, Ringwald, 1201.5902]

ψE,Ec ψD,Dc

π0 π1 πM πNπN−1

A “Clockwork” Axion:

Further motivation to cover full axion parameter space


ABRACADABRA: Cosmic Axion Detection

Cold Axion DM ≈ Classical Field Oscillations

Local DM Velocity Spatial Coherence Temporal Coherence

(motivates Q~106 resonators)

e.g.

⇒vDM ' 10

−3

a(t) =

√

2ρDM

ma

sin(mat)

complementary to cavities like ADMX

Key Experimental Feature:

ma ∼ 10−9

eV

λComp ∼ 1 km

τComp ∼ few µs

λdeB '

λComp

vDM

τdeB '

τComp

v2DM

λComp ! Rexp


r ·E = −gaγγra ·B

r⇥E = −∂B

∂t

r ·B = 0

r⇥B = gaγγ∂a

∂tB+ gaγγra⇥E+

∂E

∂t

7

Review of Axion Electrodynamics

ModifiedMaxwell

Equations:

[see, e.g., Sikivie, 1983; Wilczek, 1987]

L ⊃ gaγγ aE ·B



r⇥E = −∂B

∂t

r ·B = 0

r⇥B = gaγγ∂a


∂E

∂t

8


ModifiedMaxwell

Equations:


Gradients suppressed by vDM ~ 10–3

∂E/∂t suppressed for λComp ≫ Rexp

(MQS = magnetoquasistatic limit)

L ⊃ gaγγ aE ·B



r⇥E = −∂B

∂t

r ·B = 0

r⇥B = gaγγ∂a


∂E

∂t

9


ModifiedMaxwell

Equations:


Gradients suppressed by vDM ~ 10–3

Axion-InducedEffective Current:

Static External Field

∂E/∂t suppressed for λComp ≫ Rexp

(MQS = magnetoquasistatic limit)

Parallel to external field

Jeff = gaγγp

2ρDM cos(mat)B0

L ⊃ gaγγ aE ·B

r⇥Bresponse


ABRACADABRA: Amplifying B-field Ring Apparatus

[Kahn, Safdi, JDT, 1602.01086][for a related solenoidal design, see Thomas, Cabrera, 2010; Sikivie, Sullivan, Tanner, 1310.8545]

B0B0

Jeff

Bresponse

B0

! ! !

! ! !

! ! !

! !

! !

⊗ ⊗

⊗ ⊗

Icoil


ABRACADABRA: Amplifying B-field Ring Apparatus

[Kahn, Safdi, JDT, 1602.01086][for a related solenoidal design, see Thomas, Cabrera, 2010; Sikivie, Sullivan, Tanner, 1310.8545]

B0B0

Jeff

Bresponse

B0

Φa(t) = gaγγp

2ρDM cos(mat)× (BmaxVtoroid Gtoroid)

geometric factor,typically O(10%)

Detecting AC fieldwhere DC field is zero(essential for vibrationalnoise suppression)

Small gap to avoidMeissner screening

(superconducting coils)

! ! !

! ! !

! ! !

! !

! !

⊗ ⊗

⊗ ⊗

Icoil


ABRA–10cm: Prototype Toroid Design

Bmax = 1 T Icoil = 120 A Vtoroid = 1020 cm3 Gtoroid = 0.057

12 cm

Counter-wound NbTisuperconducting coils(minimize fringe fields)!

Wire spacing sufficientfor Meissner gap!

Not shown: shunt toallow injection ofpersistent current

6 cm3 cm

B0



Wire to injecttest “signal”

Support donut(perhaps 3D printed)

6 cm3 cm

Bmax = 1 T Icoil = 120 A Vtoroid = 1020 cm3 Gtoroid = 0.057



Superconductingpickup cylinder

!

Minimize inductancewith tall cylinder

(advice from K. Irwin)

Gap to forcepickup currentthrough SQUID

To readout circuit

6 cm3 cm

SQUID pickup + amplifier(shown: Magnicon amplifier array)


Cryogenics & Shielding

Dilution Refrigerator:Oxford Instruments Triton 400 700 mK

50 mK

10 mK

25 cm

12 L working volumeCryogen-free

Can run for weeks unattended

Day job: CUORE 0νββ R&D

Magnetic Shielding:

Ideally superconductingMultilayer NbTi/Nb/Cu sheet?

Alternatively, In/Cu?


ABRACADABRA: A Broadband/Resonant Approach

Minimize circuit noise for given axion mass

[figure adapted from Myers, et al., Journal of Magnetic Resonance, 2007;see related discussion in Jaeckel, Redondo, 1308.1103]

Broadband

Resonant

Dominated by SQUID noise

Dominated by thermal noise

Example fromlow-field MRI

Temperature-dependentcrossover


Complementary Readout Strategies

Lp

Li

L

M

LLpLi

M

C

R

Δω

Lower Frequencies: Broadband

Higher Frequencies: Resonant

Superconducting circuit ⇒ SQUID noise dominates

Pickup RLC circuit ⇒ inevitable dissipation

S1/2Φ,0 ∼ 10

−6Φ0/

√Hz

Close to shot noise limit1/f noise present at lower frequencies

Q-enhancement of signal……but thermal noise dominates at 100 mK up to Q = 108

Q = ω0 Lcircuit/Rcircuit

PickupLoop

PickupLoop

SQUID

SQUID

[also good for transients, see Zioutas @ Axion DM 2016]


gmin

aγγ ∝

⇣ ma

ttotal

⌘1/4√Lcircuit

BmaxVtoroidGtoroid

1√ρDM

S1/2Φ,0

gmin

aγγ ∝

⇣

1

mate-fold

⌘1/4√Lcircuit

BmaxVtoroidGtoroid

1√ρDM

s

T

Q

lower mass ⇒longer coherence time

minimize inductance with “tall” geometry;optimal sensitivity scales like (Rexp)-5/2

depends on resonantscanning strategy

want low Tand high Q

Complementary Readout Strategies

Lower Frequencies: Broadband

Higher Frequencies: Resonant


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= == == =

= == == =

ABRACADABRA: Potential Future Reach

Broadband

T < 60 mK1/f knee @ 50 Hz!

Resonant

T = 100 mKQ = 106

MQS approximation breaks down(precisely where ADMX begins)

1 year sensitivitySNR ≈ 1VB = Vtoroid Gtoroid

IAXO

AD

MX

GUT-scale


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ABRA–10 cm: Potential Reach in 2017

1 month sensitivitySNR ≈ 1

IAXO

AD

MX

CAST

QCD A

xion

Band

BroadbandResonant

Assumes SQUIDor thermal noisedominates

Not bad for aone liter frozen donut


The ABRACADABRA Collaboration @ MIT

Janet Conrad, Joe Formaggio, Sarah Heine, Yoni Kahn (Princeton),Joe Minervini, Jonathan Ouellet, Kerstin Perez, Alexey Radovinsky, Ben Safdi,

JDT, Daniel Winklehner, Lindley Winslow (NSF EAGER PI)

Anticipated timeline for ABRA–10cm:Magnet installation by May for Summer 2017 data taking

SUPERCONDUCTING SYSTMIT Plasma Science & Fusion CenterMIT Laboratory for Nuclear Science Superconducting Systems, Inc.

LNSLaboratory for Nuclear Science

Seeking broader collaboration for ABRA–1m!


Key Challenges for ABRA–10cm: Noise, Noise, Noise

SQUID Target: S1/2B ' 10

−2f T/

pHz @ 250 kHz

Vibrational Noise?

fringe field

S1/2B ' (10−6Bmax)S

1/2displacement/Rexp

☆already close to target

Essential that pickup cylinder is in zero-field region

(see backup slide forenvironmental

magnetic noise)


Future Challenges for ABRA–1m

Cool a meter-sized experiment?

Yes*: CUORE = 1.5 ton @ 10 mKBut maybe pickup @10 mK, but toroid @ 1 K?

Optimize pickup geometry?

+ =

“Pickup SnakeSwallowing Its Tail”

Cryogenic CurrentComparators

Dark Matter Radio[1411.7382, 1610.09344]

Yes*:

“The Coldest Cubic Meterin the Known Universe”

Achieve vibrational isolation?

Yes*: Use LIGO-grade technology for ≈106 gain




Toroidal geometrywith zero-field pickup

Lp

Li

L

M

LLpLi

M

C

R

Δω

Complementaryreadout strategies

Anticipated results fromABRA–10cm in 2017

Ultimate Goal: Probe GUT-scale QCD Axion Dark Matter




Hot-DM ê CMB ê BBN

Telescope ê EBL

SN1987ABurst Duration SK

Globular Clusters HgagLHgaeL

White Dwarfs HgaeLWD cooling hint

Solar Neutrino flux HgagLHgaeL

IAXO Helioscopes Beam DumpADMX-IIADMX

Cold DM

post-inflation PQ transition

pre-inflation PQ transition

Hnatural valuesL

10-710-610-510-410-310-210-1 1 10 10

2103104105106107

-0.5

0.0

0.5

1.0

1.5

2.0

10141013101210111010

109108107106105104103102101

1

ma@eVD

fa@GeVD

1019

10−12

10−9

AD

10-

0.5

AD

10-

0.5

AD

10-

0.5

AD

10-

0.5

AD

10-

0.5

AD

10-

0.5

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10 1016

ADMX

Cold

tion PQ tra

pre inflatio

na

10-710

0.5

0.0

0.5

1.0

1.5

2.0

10 10

CASPEr

ABRA-

CADABRA

[adapted from Essig et al., 1311.0029]

BH

super-

radianceARIADNE

Multiple Promising Strategies to Fully Explore QCD Axion


Backup Slides


EnvironmentalMagnetic Noise?

☆With dedicated effort,

target seems achievable

SQUID Target: S1/2B ' 10

−2f T/

pHz @ 250 kHz

Key Challenges for ABRA–10cm: Noise, Noise, Noise

x103

If you don’t shield fully:

Documents

Prospects for Cosmic Axion Detection with ABRACADABRA · Jesse Thaler — Prospects for Cosmic Axion Detection with ABRACADABRA 5 Initial Target: ABRACADABRA–10cm Axion Coupling