Direct Detection of Composite Dark Matter...WIMPs, Hidden Sector, Asymmetric, etc High number...
Transcript of 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
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Dark Nuclear Matter“Dark Nuggets”
*Gresham, Lou and Zurek, 1707.02316
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Detection
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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
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Short Range Mediator
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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
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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