direct detection of composite dark matter...wimps, hidden sector, asymmetric, etc high number...

D.M. Grabowska BSM Circa 2020 03/01/2019

Direct Detection of Composite Dark Matter

Dorota M Grabowska

UC Berkeley and LBL

Work with: - A. Coskuner, S. Knapen, & K. Zurek arXiv: 1812.07573

- T. Melia and S. RajendranarXiv: 1807.03788

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

Ultra Light DM

Axions, ALPS, etc

Classically coherent fields compensate for weak

coupling

Particle DM

WIMPs, Hidden Sector, Asymmetric,

etc

High number density compensates for small

cross sections

Macroscopic DM

Primordial Black Holes, MACHOS,

etc

High mass compensates for

weakness of gravity

zeV keV PeV 1050 GeV 1060 GeV

2

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

Ultra Light DM

Axions, ALPS, etc

Classically coherent fields compensate for weak

coupling

Particle DM

WIMPs, Hidden Sector, Asymmetric,

etc

High number density compensates for small

cross sections

Macroscopic DM

Primordial Black Holes, MACHOS,

etc

High mass compensates for

weakness of gravity

zeV keV PeV 1050 GeV 1060 GeV

2

(103 M☉)(10 -21 eV)

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

Ultra Light DM

Axions, ALPS, etc

Classically coherent fields compensate for weak

coupling

Particle DM

WIMPs, Hidden Sector, Asymmetric,

etc

High number density compensates for small

cross sections

Macroscopic DM

Primordial Black Holes, MACHOS,

etc

High mass compensates for

weakness of gravity

zeV keV PeV 1050 GeV 1060 GeV

2

(103 M☉)(10 -21 eV)

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

Ultra Light DM

Axions, ALPS, etc

Classically coherent fields compensate for weak

coupling

Particle DM

WIMPs, Hidden Sector, Asymmetric,

etc

High number density compensates for small

cross sections

Macroscopic DM

Primordial Black Holes, MACHOS,

etc

High mass compensates for

weakness of gravity

zeV keV PeV 1050 GeV 1060 GeV

2

(103 M☉)(10 -21 eV)

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

Ultra Light DM

Axions, ALPS, etc

Classically coherent fields compensate for weak

coupling

Particle DM

WIMPs, Hidden Sector, Asymmetric,

etc

High number density compensates for small

cross sections

Macroscopic DM

Primordial Black Holes, MACHOS,

etc

High mass compensates for

weakness of gravity

zeV keV PeV 1050 GeV 1060 GeV

2

(103 M☉)(10 -21 eV)

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

3

zeV keV PeV 1050 GeV 1060 GeV

DM flux at least one per year

Earth

Xenon OneTon

Olympic Swimming Pool

(Distance from Earth to Sun)3

1010 GeV 1042 GeV1033 GeV1019 GeV 1022 GeV

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark Matter Mass LandscapeAllowable mass range covers ~ 90 orders of magnitude

3

zeV keV PeV 1050 GeV 1060 GeV

DM flux at least one per year

Earth

Xenon OneTon

Olympic Swimming Pool

(Distance from Earth to Sun)3

1010 GeV 1042 GeV1033 GeV1019 GeV 1022 GeV

D.M. Grabowska BSM Circa 2020 03/01/2019

1. Dark Matter candidates in this mass regime

1. Take Away: Bound states of strongly interacting dark sectors can span full regime

2. Possible Detection Strategies

1. Take Away: Need multi-prong experimental and observational approach

4

Plan

D.M. Grabowska BSM Circa 2020 03/01/2019

1. Dark Matter candidates in this mass regime

1. Take Away: Bound states of strongly interacting dark sectors can span full regime

2. Possible Detection Strategies

1. Take Away: Need multi-prong experimental and observational approach

4

Plan

Take Away: Need multi-prog experimental and observational approach

Take Away: Bound states in strongly interacting dark sectors have masses that span ~40 orders of magnitude

D.M. Grabowska BSM Circa 2020 03/01/2019

• Relic abundance set by dark baryon asymmetry

Strongly Interacting Dark Sector

5

Example: Dark Nuclear Matter

“Dark Nucleon”

“Dark Nucleus”

General Properties

• Theory confines at energy scale ΛΧ• Spectrum contains massive particle with mx ~ Λx

• Massive particles form bound states with Mx ~ Nx Λx

D.M. Grabowska BSM Circa 2020 03/01/2019

• Relic abundance set by dark baryon asymmetry

Strongly Interacting Dark Sector

5

Example: Dark Nuclear Matter

“Dark Nucleon”

“Dark Nucleus”

General Properties

• Theory confines at energy scale ΛΧ• Spectrum contains massive particle with mx ~ Λx

• Massive particles form bound states with Mx ~ Nx Λx

D.M. Grabowska BSM Circa 2020 03/01/2019

Treat dark nucleus as drop of liquid to determine how binding energy depends on number of constituents

Maximum Size of Dark Nucleus

6

Semi-empirical mass formula

• Assume no long range force to destabilize dark nuclei

Binding energy unbounded from above!

D.M. Grabowska BSM Circa 2020 03/01/2019

Treat dark nucleus as drop of liquid to determine how binding energy depends on number of constituents

Maximum Size of Dark Nucleus

6

Semi-empirical mass formula

Short Range Strong Interaction

Surface Correction

Long Range Weak Interaction

• Assume no long range force to destabilize dark nuclei

Binding energy unbounded from above!

D.M. Grabowska BSM Circa 2020 03/01/2019

Treat dark nucleus as drop of liquid to determine how binding energy depends on number of constituents

Maximum Size of Dark Nucleus

6

Semi-empirical mass formula

Short Range Strong Interaction

Surface Correction

Long Range Weak Interaction

• Assume no long range force to destabilize dark nuclei

Binding energy unbounded from above!

D.M. Grabowska BSM Circa 2020 03/01/2019 7

Early Universe FormationBig Bang Dark Nucleosynthesis

Dark nuclei form via fusion processes in the Early Universe

“Nuclear Physics”

* Krnjaic & Sigurdson, ’14, Hardy et al, ’14, Gresham, Lou & Zurek, ’17

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark nuclei size is limited by how long fusion lasts during early Universe

• Compare Fusion rate to Hubble rate for rough estimate

• Generically find exponentially large states

Dark BBN

8

Fusion in Early Universe

D.M. Grabowska BSM Circa 2020 03/01/2019

Dark nuclei size is limited by how long fusion lasts during early Universe

• Compare Fusion rate to Hubble rate for rough estimate

• Generically find exponentially large states

Dark BBN

8

Fusion in Early Universe

D.M. Grabowska BSM Circa 2020 03/01/2019 9

Dark Nuclear Matter“Dark Nuggets”

*Gresham, Lou and Zurek, 1707.02316

D.M. Grabowska BSM Circa 2020 03/01/2019 10

Detection

D.M. Grabowska BSM Circa 2020 03/01/2019 11

Dark Matter Direct DetectionDM Scattering

General Idea: DM passes through detector, resulting in either nuclei/electron recoil or collective mode excitation

DM

SM Detector

pi pf

Differential Scattering Rate per Unit Target Mass

D.M. Grabowska BSM Circa 2020 03/01/2019 11

Dark Matter Direct DetectionDM Scattering

General Idea: DM passes through detector, resulting in either nuclei/electron recoil or collective mode excitation

DM

SM Detector

pi pf

Differential Scattering Rate per Unit Target Mass

Target and DM Dependent!

D.M. Grabowska BSM Circa 2020 03/01/2019 12

Dynamic Structure FunctionParameterizes Target Response

General Idea: Structure Function S(q, ω) quantifies response of target to injection of momentum, q, and energy, ω

D.M. Grabowska BSM Circa 2020 03/01/2019 12

Dynamic Structure FunctionParameterizes Target Response

General Idea: Structure Function S(q, ω) quantifies response of target to injection of momentum, q, and energy, ω

DM Velocity Dist.

Target ResponseDM Form Factor

Mediator “Form Factor”

DM Number Density

D.M. Grabowska BSM Circa 2020 03/01/2019 13

Standard Model CouplingsNucleon Coupling

General Idea: Dark Matter couples to Standard Model nucleons via mediator of mass mφ

Results in spin-independent four fermion interaction with specific mediator “form factor”

D.M. Grabowska BSM Circa 2020 03/01/2019 14

DM Form FactorFinite Size effects

10-2 10-1 100 101 102

10-6

10-3

100

q (1/RX)

|FX(q)2

Coherent Incoherent

General Idea: Form factors “encode” the deviation of scattering amplitudes from the point particle limit

D.M. Grabowska BSM Circa 2020 03/01/2019 15

Short Range Mediator

D.M. Grabowska BSM Circa 2020 03/01/2019 16

Nuclear RecoilTraditional WIMP Search

General Idea: Dark Matter scatters of single nucleus, which then recoils

Effect of DM’s finite radius on detectability depends on how much of scattering phase space is suppressed by form factor

D.M. Grabowska BSM Circa 2020 03/01/2019 16

Nuclear RecoilTraditional WIMP Search

General Idea: Dark Matter scatters of single nucleus, which then recoils

On-Shell recoilForm Factor of Nucleus

Effect of DM’s finite radius on detectability depends on how much of scattering phase space is suppressed by form factor

D.M. Grabowska BSM Circa 2020 03/01/2019

Form Factor Effects

General Idea: Effect of form factor depends on how DM radius compares to qmax and qmin

• ss: : Cross section for point-like DM scattering off nucleon

Massive Mediator

Maximizing target’s atomic number is key

17

D.M. Grabowska BSM Circa 2020 03/01/2019

Form Factor Effects

General Idea: Effect of form factor depends on how DM radius compares to qmax and qmin

• ss: : Cross section for point-like DM scattering off nucleon

Massive Mediator

Maximizing target’s atomic number is key

17

D.M. Grabowska BSM Circa 2020 03/01/2019 18

Short Range Mediator10 GeV

103 106 109 1012 1015 101810-48

10-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

10-48

10-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

MX (GeV)

σ Xn(cm2 )

mχ=10 GeV, Fmed = 1

LiquidXe, 1.5*104 kg

year, E

thres=5keV

XENON1T,

98 kgyear,

Ethres=5 ke

V

He (Nuclea

r Recoil), k

g year, Ethre

s=1meV

Geometric Cro

ss Section

Overburden

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 19

Short Range Mediator10 GeV

Collider Constraints

103 106 109 1012 1015 101810-48

10-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

MX (GeV)

σ Xn(cm2 )

mχ=10 GeV, Fmed = 1LiquidXe, 1.5*104 kg

year, E

thres=5keV

XENON1T,

98 kgyear,

Ethres=5 ke

V

Semicond

uctor(Ge),

100 kg yea

r, Ethres=50

eV

CDMSLite

, 0.2kg ye

ar, Ethres=0

.5 keV

Semicondu

ctor (Si), kg

year,Ethres

=10 meV

He (Nuclea

r Recoil), k

g year, Ethre

s=1 meV

Geometric Cros

s Section

Overburden

10-9

10-6

0.001

1

1000

106

gXgnMXμ XN/(M

Nm

ϕ2 )

(1/GeV

)

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 20

Short Range Mediator10 MeV

100 103 106 109 1012 101510-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

10-15

10-12

10-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

10-15

10-12

MX (GeV)

σ Xn(cm2 )

mχ=10 MeV, Fmed = 1, 1% subcomp. DM

LiquidXe, 1.5*104kgyear, E

thres=5keV

XENON1T,98kgyear, E

thres=5keV

He(NuclearRecoil),kgyear, E

thres=1meV

Geometric Cro

ss Section

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 21

Short Range Mediator10 MeV

Collider Constraints

100 103 106 109 1012 101510-42

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

10-15

10-12

MX (GeV)

σ Xn(cm2 )

mχ=10 MeV, Fmed = 1, 1% subcomp. DM

LiquidXe, 1.5*104kgyear, E

thres=5keV

XENON1T,98kgyear, E

thres=5keV

Semiconductor(Ge

), 100kgyear, E

thres=50

eV

CDMSLite, 0.2 kg year, E t

hres=0.5keV

Semicon

ductor

(Si), kg

year, E t

hres=10 meV

He(NuclearRecoil), kg year, E t

hres=1 meV

Geometric Cros

s Section

10-9

10-6

0.001

1

1000

106

gXgnMXμ XN/(M

Nm

ϕ2 )

(1/GeV

)

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 22

Long Range Mediator

D.M. Grabowska BSM Circa 2020 03/01/2019 23

Collective ExcitationsPolar Crystals

General Idea: Low momentum transfer excites phonon modes in crystal lattice

*Griffin et al, 1807.1029

D.M. Grabowska BSM Circa 2020 03/01/2019 24

Nuclear Recoil Long RangeEnhancement at Low Momentum

Recall: Scattering due to light mediator is enhanced at low momentum by 1/q4

D.M. Grabowska BSM Circa 2020 03/01/2019 24

Nuclear Recoil Long RangeEnhancement at Low Momentum

Recall: Scattering due to light mediator is enhanced at low momentum by 1/q4

Minimizing detector’s energy threshold is key

D.M. Grabowska BSM Circa 2020 03/01/2019 25

Long Range Mediator10 GeV

103 106 109 1012 101510-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

10-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

MX (GeV)

σ Xn(cm2 )

mχ=10 GeV, Fmed = q02/q2

LiquidXe, 1.5*10

4 kgyear,E thres=5keV

XENON1

T, 98 kg

year, E th

res=5 k

eV

GaAs (A

coustic

Mode), k

g year, E

thres=1

meV

Perturbativity

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 26

Long Range Mediator10 GeV

SIDM constraint

Perturbativity

In-medium effects

103 106 109 1012 101510-45

10-42

10-39

10-36

10-33

10-30

10-27

10-24

MX (GeV)

σ Xn(cm2 )

mχ=10 GeV, Fmed = q02/q2

LiquidXe, 1.5*10

4 kgyear,E thres=5 keV

XENON1

T, 98 kg

year, E thr

es=5keV

Semicon

ductor (G

e), 100 k

g year, E

thres=50 eV

CDMSLit

e, 0.2 kg

year, E thr

es=0.5 ke

V

Semicon

ductor (S

i), kgyear

, E thres=10 me

V He (Nuc

learRec

oil),kg y

ear,E thre

s=1meV

GaAs (A

coustic M

ode), kg

year, E thr

es=1meV

He (Pho

nons), kg

year, E thr

es=1meV

Perturbativity

10-12

10-9

10-6

gXgnMXμ XN/M

N(GeV

)

*Coskuner, DMG, Knapen & Zurek ‘18

D.M. Grabowska BSM Circa 2020 03/01/2019 27

Extremely Long Range Mediator

D.M. Grabowska BSM Circa 2020 03/01/2019

Mediator Coupling ConstraintsDark Sector Constraints

* Akin to gravitational collapse

Scalar Coupling gx Bound: Stability of Dark Nuclei

• Fermi degeneracy pressure must balance self-energy due to long range attractive interaction*

• Additional repulsive interactions does not help as blobs become unbound

28

D.M. Grabowska BSM Circa 2020 03/01/2019

Mediator Coupling ConstraintsDark Sector Constraints

* Akin to gravitational collapse

Scalar Coupling gx Bound: Stability of Dark Nuclei

• Fermi degeneracy pressure must balance self-energy due to long range attractive interaction*

• Additional repulsive interactions does not help as blobs become unbound

28

D.M. Grabowska BSM Circa 2020 03/01/2019 29

Λx = MeV, λ = 200 km

DMG, Melia and Rajendran ‘18

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Extremely Long Range Mediator

D.M. Grabowska BSM Circa 2020 03/01/2019

General Idea: Passing DM induces motion in test mass

Acceleration

30

Free hanging test mass

DM

Test Mass

D.M. Grabowska BSM Circa 2020 03/01/2019

General Idea: Passing DM induces motion in test mass

Acceleration

30

Free hanging test mass

DMTest Mass

b

θ

D.M. Grabowska BSM Circa 2020 03/01/2019

General Idea: Passing DM induces motion in test mass

Acceleration

30

Free hanging test mass

DMTest Mass

b

θ

D.M. Grabowska BSM Circa 2020 03/01/2019

General Idea: Passing DM induces motion in test mass

Acceleration

30

Free hanging test mass

• Example: LIGO sensitive to Δx ~ 0.1 fm/Hz1/2

DMTest Mass

b

θ

D.M. Grabowska BSM Circa 2020 03/01/2019 31

Tank: (500 m)3

Λx = MeV, λ = 200 km

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DMG, Melia and Rajendran ‘18

Extremely Long Range Mediator

D.M. Grabowska BSM Circa 2020 03/01/2019 32

ConclusionsFocus: Detecting composite dark matter

Take Away: Strongly interacting dark sector can give DM whose mass ranges over 40 orders of magnitude

• Dark Nuclear Matter

• Dark Quark Matter (Not discussed here)

Take Away: Need multi-prong approach to span the full parameter space of masses and confinement scales

• Both existing and near future direct detection experiments are important