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Theories of Light Dark Matter and Their Connection to Intensity - - PowerPoint PPT Presentation

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Theories of Light Dark Matter and Their Connection to Intensity Experiments Kathryn M. Zurek University of Michigan Sunday, January 26, 14 Focus on Weak Scale for New Physics Gravitational Interactions LHC Energy Tevatron Sub-weak

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SLIDE 1

Theories of Light Dark Matter and Their Connection to Intensity Experiments

Kathryn M. Zurek University of Michigan

Sunday, January 26, 14

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SLIDE 2

Focus on Weak Scale for New Physics

  • Higgs sector

M S S M p a r t i c l e s LHC Tevatron LEP

Gravitational Interactions Sub-weak Interactions

Mp ∼ 1 GeV

Extra Dimensions Inaccessibility Energy

Sunday, January 26, 14

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SLIDE 3

Paradigm Shift

Standard Model

Dark World Weak Interactions Sub-weak Interactions (DM here.)

LHC

Torres del Paine Hidden Valley Sunday, January 26, 14

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SLIDE 4

Paradigm Shift

Standard Model

?

Mp ∼ 1 GeV

Our thinking has shifted From a single, stable weakly interacting particle ..... (WIMP, axion) ...to a hidden world with multiple states, new interactions

Wednesday, March 20, 13 Sunday, January 26, 14

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SLIDE 5

Hidden Dark Worlds

Standard Model

Mp ∼ 1 GeV

Our thinking has shifted From a single, stable weakly interacting particle ..... (WIMP, axion) ...to a hidden world with multiple states, new interactions

A’ (Heavy Photon Search)

Sunday, January 26, 14

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SLIDE 6
  • Abundance of new stable states set by

interaction rates

Why the (sub-)Weak Scale is Compelling

Γ = nσv = H

Measured by WMAP + LSS

Freeze-out

→ σ ∼ 1 few TeV2

Sunday, January 26, 14

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SLIDE 7

Why the Weak Scale is Compelling

hσvi ' 3 ⇥ 10−26 cm3/s ' 1 (20 TeV)2

Kolb and Turner Meausured by CMB plus large scale structure

Sunday, January 26, 14

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SLIDE 8

Idea Focus: Supersymmetry

  • Provides sharp predictions
  • Must be neutral
  • Sneutrino scatters through Z
  • Neutralino does not because operator

vanishes identically for Majorana fermion

˜ ν

˜ B, ˜ W3, ˜ H

¯ χγµχ ¯ NγµN

Sunday, January 26, 14

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SLIDE 9

Sub-Weakly Interacting Massive Particles

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

  • 45

10

  • 44

10

  • 43

10

  • 42

10

  • 41

10

  • 40

10

  • 39

10

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

  • 45

10

  • 44

10

  • 43

10

  • 42

10

  • 41

10

  • 40

10

  • 39

10

]

2

WIMP Mass [GeV/c

6 7 8 910 20 30 40 50 100 200 300 400 1000

]

2

WIMP-Nucleon Cross Section [cm

  • 45

10

  • 44

10

  • 43

10

  • 42

10

  • 41

10

  • 40

10

  • 39

10

DAMA/I DAMA/Na CoGeNT CDMS (2010/11) EDELWEISS (2011/12) XENON10 (2011) X E N O N 1 ( 2 1 1 ) C O U P P ( 2 1 2 ) SIMPLE (2012) Z E P L I N

  • I

I I ( 2 1 2 ) CRESST-II (2012)

XENON100 (2012)

  • bserved limit (90% CL)

Expected limit of this run: expected σ 2 ± expected σ 1 ±

Scattering through the Z boson: ruled out Next important benchmark: Scattering through the Higgs

σn ∼ 10−39 cm2 σn ∼ 10−45−46 cm2

Sunday, January 26, 14

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SLIDE 10

Are there ways around for the Neutralino?

  • Make the Neutralino a

pure state -- coupling to Higgs vanishes

  • However, Wino and

Higgsino pure states can be probed by indirect detection

  • W

qL, ℓL, Hu, Hd

  • qL,

ℓL, Hu, Hd

  • B

q, ℓ, Hu, Hd

  • q,

ℓ, Hu, Hd χ χ χ

n

Z Z

Large!

hσvi ⇠ ✓2 TeV mχ ◆2 10−26cm3/s

Sunday, January 26, 14

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SLIDE 11

Are there ways around for the Neutralino?

  • Thermal Wino ruled
  • ut
  • Thermal Higgsino still

allowed, but can be ruled out in the future

(TeV)

χ

m

  • 2

10

  • 1

10 1 10 /s)

3

(95% CL) (cm

γ γ → χ χ

v> σ <

  • 29

10

  • 28

10

  • 27

10

  • 26

10

  • 25

10

HESS Einasto Fermi-LAT Einasto

0.5 1.0 1.5 2.0 2.5 3.0 10-27 10-26 10-25 10-24 10-23 10-22 M2 @TeVD Thermal sgg+

1 2gZ v Acm3ësE

10-26 10-25 10-24 10-23 10-22 10-21 sWW v Acm3ësE

Cohen, Lisanti, Pierce, Slatyer

Sunday, January 26, 14

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SLIDE 12

Are there ways around for the Neutralino?

  • Bino escapes
  • Pay a fine-tuning price

| | m2

Z

= |m2

Hd − m2 Hu|

  • 1 − sin2(2β)

− m2

Hu − m2 Hd − 2|µ|2.

µ M1 ⇠ mwk

Sunday, January 26, 14

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SLIDE 13

Are there ways around for the Neutralino?

  • Tune away the coupling

to the Higgs

  • Smaller cross-sections

correspond to more tuning in the neutralino components

10 20 50 100 200 500 1000 2000 10-48 10-47 10-46 10-45 10-44 10-43 10-42

mc @GeVD sSI @cm2D

SI cross-section for b éêh é

XENON100 LUX XENON1T SuperCDMS m > 0 m < 0 M1 + sin2b m M1 < 0.1

Cheung, Hall, Pinner, Ruderman

mχ condition M1 M1 + µ sin 2β = 0 M2 M2 + µ sin 2β = 0 −µ tan β = 1 M2 M1 = M2

Sunday, January 26, 14

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SLIDE 14

Are there ways around for the Neutralino?

  • Tune away the coupling

to the Higgs

  • Smaller cross-sections

correspond to more tuning in the neutralino components

Cheung, Hall, Pinner, Ruderman

mχ condition M1 M1 + µ sin 2β = 0 M2 M2 + µ sin 2β = 0 −µ tan β = 1 M2 M1 = M2

D

  • 1000
  • 500

500 1000 1 2 5 10 20 40

m @GeVD tan b XENON 1T reach H~2017L

LEP c- c+

  • verclosed
  • verclosed

XENON1T SI XENON1T SD chcc = 0

Sunday, January 26, 14

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SLIDE 15

When Should We Start Looking Elsewhere?

  • Cannot kill neutralino DM, but

paradigm does become increasingly tuned

  • Somewhat below Higgs pole --

Neutrino background?

  • Well-motivated candidates that are

much less costly to probe

  • Light WIMPs

Sunday, January 26, 14

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SLIDE 16

Current Sensitivity Limited

CRESST 2011

DAMA CoGeNT CRESST CDMS-Si

Sunday, January 26, 14

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SLIDE 17

Terra Incognita

1 10 100 1000 104 1050 1049 1048 1047 1046 1045 1044 1043 1042 1041 1040 1039 1014 1013 1012 1011 1010 109 108 107 106 105 104 103 WIMP Mass GeVc2 WIMPnucleon cross section cm2 WIMPnucleon cross section pb

7Be

Neutrinos

N EU T R I N O C OH ER EN T S CA T TE R ING NE UT R IN O C O H E R EN T S C A T TERIN G

(Green&ovals)&Asymmetric&DM&& (Violet&oval)&Magne7c&DM& (Blue&oval)&Extra&dimensions&& (Red&circle)&SUSY&MSSM& &&&&&MSSM:&Pure&Higgsino&& &&&&&MSSM:&A&funnel& &&&&&MSSM:&BinoEstop&coannihila7on& &&&&&MSSM:&BinoEsquark&coannihila7on& &

8B

Neutrinos Atmospheric and DSNB Neutrinos CDMS II Ge (2009) Xenon100 (2012)

CRESST CoGeNT (2012) CDMS Si (2013)

EDELWEISS (2011)

DAMA

S I M P L E ( 2 1 2 ) Z E P L I N

  • I

I I ( 2 1 2 ) COUPP (2012)

SuperCDMS Soudan Low Threshold SuperCDMS Soudan CDMS-lite XENON 10 S2 (2013) CDMS-II Ge Low Threshold (2011)

S u p e r C D M S S

  • u

d a n X e n

  • n

1 T LZ L U X D a r k S i d e G 2 D a r k S i d e 5 D E A P 3 6 P I C O 2 5

  • C

F 3 I PICO250-C3F8 S N O L A B SuperCDMS

CF1 Snowmass report, 1310.8327

Sunday, January 26, 14

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SLIDE 18

Cross-Sections May Be Mediated By A’

LUX talk KZ, 0811.4429

σSI ' g2

ng2 χm2 r

πm4

A0

⇠ 10−40 cm2 ⇣gngχ 10−4 ⌘2 ✓8 GeV mA0 ◆4

χ2 χ1 γ, Z

χ χ

A’

e, n e, n

Sunday, January 26, 14

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SLIDE 19

Connection to Dark Forces

  • A’ searches can constrain this parameter space

0.001 0.010 0.100 1.000 mX [GeV] 10-55 10-50 10-45 10-40 10-35 σe [cm2] m

φ

> > m

X

Ge Large width D e c a y b e f

  • r

e B B N 0.001 0.010 0.100 1.000 10-55 10-50 10-45 10-40 10-35

10-3 10-2 10-1 1 10-5 10-4 10-3 10-2 mA' HGeVL e A' Æ Standard Model

APEXêMAMI Test Runs

U70 E141 E774 am, 5 s am,±2 s f a v

  • r

e d

ae

BaBar KLOE WASA

Orsay HPS APEX DarkLight VEPP-3 MESA MAMI

Lin, Yu, KZ 1111.0293 1311.0029

Sunday, January 26, 14

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SLIDE 20

Light WIMPs: Asymmetric Dark Matter

  • Standard picture: freeze-out of

annihilation; baryon and DM number unrelated

  • Accidental, or dynamically

related?

nDM ≈ nb ΩDM ≈ 5Ωb

Experimentally, Mechanism

mDM ≈ 5mp

Sunday, January 26, 14

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SLIDE 21

Chemical Potential Dark Matter

Visible Dark

Matter Anti-matter

Matter Anti-Matter

Sunday, January 26, 14

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SLIDE 22

Baryon and DM Number Related?

  • Standard picture: freeze-out of

annihilation; baryon and DM number unrelated

  • Accidental, or dynamically

related?

nDM ≈ nb ΩDM ≈ 5Ωb

Experimentally, Mechanism

mDM ≈ 5mp

Nussinov, Hall, Gelmini, Barr, Chivukula, Farhi, D.B. Kaplan

Sunday, January 26, 14

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SLIDE 23

Baryon and DM Number Related?

  • Standard picture: freeze-out of

annihilation; baryon and DM number unrelated

  • Accidental, or dynamically

related?

B, L X LEP and Precision EW tend to result in problematic models Use:

Sunday, January 26, 14

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SLIDE 24

Asymmetric DM

“Integrate out” heavy state Higher dimension operators:

Standard Model

Dark Matter (Hidden Valley)

Mp ∼ 1 GeV N

X X

Inaccessibility Energy

Xucdcdc

Luty, Kaplan, KZ 0901.4117 Sunday, January 26, 14

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SLIDE 25

Asymmetric DM

OB−LOX,

OB−L = LHu, LLEc, QLDc, U cDcDc,

OX = X, X2

Standard Model

Dark Matter

Mp ∼ 1 GeV

Inaccessibility Energy

Luty, Kaplan, KZ 0901.4117 Sunday, January 26, 14

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SLIDE 26

What Does an ADM Model Do?

  • 1. Share an asymmetry between the visible

and dark sectors

  • 2. Decouple transfer mechanism to

separately freeze-in the asymmetries in both sectors

  • 3. Annihilate the symmetric abundance

nX n ¯

X ⇠ nb n¯ b,

suggests mX ⇠ 5mp ' 5 GeV.

KZ, 1308.0338 Sunday, January 26, 14

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SLIDE 27
  • 3. Annihilating
  • While it doesn’t directly probe the

asymmetry mechanism, it is more likely this physics is at a low scale which we can probe.

Visible Dark

Anti-matter Matter

Matter Anti-Matter

Sunday, January 26, 14

slide-28
SLIDE 28
  • 3. Annihilating
  • While it doesn’t directly probe the

asymmetry mechanism, it is more likely this physics is at a low scale which we can probe.

Visible Dark

Anti-matter Matter

Matter Anti-Matter

Sunday, January 26, 14

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SLIDE 29
  • 3. Annihilating
  • While it doesn’t directly probe the

asymmetry mechanism, it is more likely this physics is at a low scale which we can probe.

Visible Dark

Anti-matter Matter

Matter Anti-Matter

?

Sunday, January 26, 14

slide-30
SLIDE 30

Annihilating through weak scale states ...

  • doesn’t really work ....

Ov

f: 1 L2 f†∂m f q gm q

1 10 100 1000 104 1 10 100 1000 104 mDM HGeVL L HGeVL

March-Russell et al 1203.4854 Sunday, January 26, 14

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SLIDE 31

Dark Forces and DM Interactions

  • Dark Forces Very Important for

Asymmetric Dark Matter!

  • May also be important for structure of

DM halos

  • May be important for DM direct

detection and collider searches

χ1 χ1 χ2 γ, Z γ, Z χ2 χ1 γ, Z f ¯ fχ

χ χ χ χ χ χ

χ2 χ1 γ, Z

χ χ

A’ A’ A’ A’

e, n e, n

Sunday, January 26, 14

slide-32
SLIDE 32

Low Energy Accelerator Constraints

e e Z A0 γ

A B C D E

0.01 0.1 1 10-8 10-7 10-6 10-5 10-4 10-3 0.01 0.01 0.1 1 10-8 10-7 10-6 10-5 10-4 10-3 0.01 mA'êGeV e

Bjorken, Essig, Schuster, Toro

✏

Sunday, January 26, 14

slide-33
SLIDE 33

Translate to Direct Detection

e e Z A0 γ

A B C D E

0.01 0.1 1 10-8 10-7 10-6 10-5 10-4 10-3 0.01 0.01 0.1 1 10-8 10-7 10-6 10-5 10-4 10-3 0.01 mA'êGeV e

Bjorken, Essig, Schuster, Toro

✏

χ χ

Sunday, January 26, 14

slide-34
SLIDE 34

Translate to Direct Detection

e e Z A0 γ

✏

χ χ

Ingredients:

mχ, mA0, ge, gχ

Constrained by HPS

Other complementary searches for other two parameters?

Sunday, January 26, 14

slide-35
SLIDE 35

Translate to Direct Detection

e e Z A0 γ

✏

χ χ mχ, mA0, ge, gχ

χ1 χ1 χ2 γ, Z γ, Z χ2 χ1 γ, Z f ¯ f

φ φ φ χ χ χ χ χ χ χ

DM Relic Abundance DM self-scattering

Can we connect dark photon searches to direct detection and other astrophysical observables?

Sunday, January 26, 14

slide-36
SLIDE 36

Dark Matter Self- Scattering

  • Dark matter self-coupling changes the

shape of a dark matter halo (such as the milky way halo) - we can extract constraints on coupling gχ

σχχ ≈ g4

χm2 χ

4πm4

A0 . 4.4 × 10−27 cm2 ⇣

mχ 1 GeV ⌘

Lin, Yu, KZ 1111.0293

Sunday, January 26, 14

slide-37
SLIDE 37

Connection to Direct Detection

  • Can now take

constraints from heavy photon searches + halo shapes to map to direct detection experiments

σn ≈ g2

χg2 nµ2 n

πm4

A0

σe ≈ g2

χg2 eµ2 e

πm4

A0

χ

N χ()

Constrained by halo shapes Constrained by heavy photon search

χ2 χ1 γ, Z

χ χ

e−, n e+, ¯ n

A’

Sunday, January 26, 14

slide-38
SLIDE 38

Map into Direct Detection Plane

0.001 0.010 0.100 1.000 mX [GeV] 10-55 10-50 10-45 10-40 10-35 σe [cm2] mφ >> mX Ge Large width Decay before BBN 0.001 0.010 0.100 1.000 10-55 10-50 10-45 10-40 10-35

Lin, Yu, KZ 1111.0293

0.001 0.010 0.100 1.000 mφ [GeV] 10-9 10-8 10-7 10-6 10-5 10-4 10-3 10-2 ge 0.001 0.010 0.100 1.000 10-9 10-8 10-7 10-6 10-5 10-4 10-3 10-2

Projected maximum sensitivity of direct detection experiment Cut-out gives combined constraints of beam dump + supernova + g-2

Sunday, January 26, 14

slide-39
SLIDE 39

Map into Direct Detection Plane

0.001 0.010 0.100 1.000 mX [GeV] 10-55 10-50 10-45 10-40 10-35 σe [cm2] mφ >> mX Ge Large width Decay before BBN 0.001 0.010 0.100 1.000 10-55 10-50 10-45 10-40 10-35

Lin, Yu, KZ 1111.0293

Require A’ to decay before BBN

Note that the lower bound

  • f the theory parameter

space is totally out of reach

  • f any experiment! Can we

do better?

ge & 5 × 10−11p 10 MeV/mA0

Sunday, January 26, 14

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SLIDE 40

Particular Models Can be MUCH More Predictive!

  • Goal: explain why GeV? Dynamically

generate DM mass

Dark Visible

SUSY Breaking

Electroweak scale

Smaller than electroweak scale

mX ∼ √✏mSUSY

Sunday, January 26, 14

slide-41
SLIDE 41

Particular Models Can be MUCH More Predictive!

  • Goal: explain why GeV? Dynamically

generate DM mass

Dark Visible

SUSY Breaking

X X f ¯ f ˜ f U U U U X X

Yukawa Gauge

m2

X g2 visg2 Xm2 SUSY

16π2

m2

X y2m2 SUSY

16π2

σv g2

visg2 X

16πm2

X

Hooper, KZ ’08, Feng, Kumar ’08, Arkani-Hamed, Finkbeiner, Slatyer, Weiner ’08 Nelson, Weiner ’04, KZ ’08

Sunday, January 26, 14

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SLIDE 42

Particular Models Can be MUCH More Predictive!

  • Predict DD cross-section for

Asymmetric Dark Matter!

χ2 χ1 γ, Z

χ χ

e−, n e+, ¯ n

Coupling predicted by setting mass scale in DM sector!

Cohen, Phalen, Pierce, KZ 1005.1655

A’

Sunday, January 26, 14

slide-43
SLIDE 43

Also Probed by Intensity Experiments

BBN Li B Factories PEW

3 GeV 7 GeV 14 GeV

102 102 101 101 104 104 103 103 102 102

gd ⇥

0.001 0.01 0.1 1 10 10-5 10-4 10-3 10-2 mA' @GeVD ∂ Hidden Photon Æ invisible HmA' > 2 mcL

a

m , 5 s

a

m , ± 2 s

f a v

  • r

e d ae BaBar BaBar

Improved

Belle II

Standard

Belle II

Converted Mono-photon Ha,bL

Belle II

Low-Eg

DarkLight

ô

VEPP-3 ô KÆpA'

E787, E949

ô

ô

KÆpA'

ORKA

LSND

aD=0.1

Cohen, Phalen, Pierce, KZ 1005.1655 Essig, Mardon, Papucci, Volansky, Zhong 1309.5084

e− e+

b

¯ b

Υ(3S)

γ χ

¯ χ

A0(⇤)

e− e+

γ χ

¯ χ

A0(⇤)

Sunday, January 26, 14

slide-44
SLIDE 44

Low Energy Accelerator Constraints

e− e+

b

¯ b

Υ(3S)

γ χ

¯ χ

A0(⇤)

e− e+

γ χ

¯ χ

A0(⇤)

0.001 0.01 0.1 1 10 10-5 10-4 10-3 10-2 mA' @GeVD ∂ Hidden Photon Æ invisible HmA' > 2 mcL

a

m , 5 s

a

m , ± 2 s

f a v

  • r

e d ae BaBar BaBar

Improved

Belle II

Standard

Belle II

Converted Mono-photon Ha,bL

Belle II

Low-Eg

DarkLight

ô

VEPP-3 ô KÆpA'

E787, E949

ô

ô

KÆpA'

ORKA

LSND

aD=0.1

A0 Z e e χ χ p, n A0 Z χ χ

Essig, Mardon, Papucci, Volansky, Zhong Izaguirre, Krnjaic, Schuster, Toro 1307.6554

mc = 10 MeV, aD = 0.1

e+e- Æ g + inv. Hg- 2Le Hg- 2Lm

K+ Æ p+ + inv.

e- Beam Jêy Æ inv. ILC

0.01 0.1 1 10-8 10-7 10-6 10-5 10-4 mA' HGeVL e2

Sunday, January 26, 14

slide-45
SLIDE 45

Intensity Experiments Complement ....

0.001 0.010 0.100 1.000 mX [GeV] 10-55 10-50 10-45 10-40 10-35 σe [cm2] mφ >> mX Ge Large width Decay before BBN 0.001 0.010 0.100 1.000 10-55 10-50 10-45 10-40 10-35

XENON 10 Æ Æ Æ Æ Æ Model Point: mA' = 500 MeV, aD = 1

e- Beam

Hg-2Lm e+e- Æ g + inv.

ILC

0.01 0.02 0.05 0.10 0.20 0.50 1.00 10-40 10-39 10-38 10-37 mc HGeVL sce @cm2D

Izaguirre, Krnjaic, Schuster, Toro 1307.6554

Lin, Yu, KZ 1111.0293

Sunday, January 26, 14

slide-46
SLIDE 46

These Dark Forces May Solve ...

  • the core/cusp

problem of dark matter halos (newer incarnation: “too big to fail” problem)

Moore, Quinn, Governato, Stadel, Lake Boylan-Kolchin et al, 1103.0007 Sunday, January 26, 14

slide-47
SLIDE 47

DM Interactions and DM Halos

  • Dark matter self-interactions

randomize momenta and isotropize halos

  • Lead to lower density dark

matter halo cores

  • Dark matter halos (including

baryon poor dwarf galaxies) seem to have cores rather than cusps (still controversy as to cause)

Dave, Spergel, Steinhardt, Wandelt Sunday, January 26, 14

slide-48
SLIDE 48

Implies Dark Forces!

  • Very big scattering cross-sections
  • Fits well with our new models of DM!
  • Range of dynamics much bigger than

previously thought

  • Particle imprints on DM halos

σT ⇡ 5 ⇥ 10−23 cm2 ⇣ αX 0.01 ⌘2 ⇣ mX 10 GeV ⌘2 ✓10 MeV mφ ◆4 (1)

σ/mX ⇠ 0.1 cm2/g ' 0.2 ⇥ 10−24 cm2/ GeV

(σweak ∼ 10−39 cm2)

Sunday, January 26, 14

slide-49
SLIDE 49

Resonances are Generic for Thermal DM!

hσviann ⇡ πα2

X/m2 X

dw 0.1 dw 1 dw 10 M W . 1 MW 1 c l . 1 c l 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Symmetric dark matter

dw 0.1 dw 1 dw 10 MW 0.1 MW 1 cl 0.1 cl 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Asymmetric dark matter HaX=10-2L

Tulin, Yu, KZ Sunday, January 26, 14

slide-50
SLIDE 50

Resonances are Generic for Thermal DM!

hσviann ⇡ πα2

X/m2 X

dw 0.1 dw 1 dw 10 M W . 1 MW 1 c l . 1 c l 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Symmetric dark matter

dw 0.1 dw 1 dw 10 MW 0.1 MW 1 cl 0.1 cl 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Asymmetric dark matter HaX=10-2L

Tulin, Yu, KZ

Regions to solve dwarf structure

Sunday, January 26, 14

slide-51
SLIDE 51

Resonances are Generic for Thermal DM!

hσviann ⇡ πα2

X/m2 X

dw 0.1 dw 1 dw 10 M W . 1 MW 1 c l . 1 c l 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Symmetric dark matter

dw 0.1 dw 1 dw 10 MW 0.1 MW 1 cl 0.1 cl 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Asymmetric dark matter HaX=10-2L

Tulin, Yu, KZ

Regions to solve dwarf structure Constraints from MW and clusters

Sunday, January 26, 14

slide-52
SLIDE 52

Implications for Direct Detection

Reachable scattering cross-sections!

m HGeVL

d w . 1 d w 1 d w 1 MW 0.1 MW 1 cl 0.1 cl 1

10-4 0.001 0.01 0.1 1 0.1 1 10 100 1000 104 mf HGeVL mX HGeVL Repulsive force HaX=10-2L

Tulin, Yu, KZ Kaplinghat, Tulin, Yu

✏ = 10−10

which requires that the lifetime gq 1.6 × 10−11 1 GeV/mφ

Lin, Yu, KZ

from BBN

XENON1T

S I D M i n d w a r f s . 1

  • 1

c m2 ê g

H a l

  • s

h a p e s 1 c m2 ê g

CMB excluded

1 10 100 103 104 10-4 10-3 0.01 0.1 1 mX @GeVD mf @GeVD Symmetric SIDM H∂=10-10L

Sunday, January 26, 14

slide-53
SLIDE 53

Astrophysical Implications

  • DM does not annihilate
  • It can accumulate in the

center of stars

  • Notable case: neutron stars
  • Elastically scatter, come to

rest in core

  • High density!

−0.1 0.1 0.2 0.3 0.4 3.75 3.755 3.76 3.765 3.77 3.775 3.78 3.785 3.79 log [L/L] log [Teff/K] no ADM ρχ = 102 GeV/cm3 mχ = 5 GeV ρχ = 103 GeV/cm3 mχ = 10 GeV ρχ = 104 GeV/cm3 mχ = 10 GeV ρχ = 105 GeV/cm3 mχ = 10 GeV ρχ = 106 GeV/cm3 mχ = 10 GeV

Iocco, Taoso, Leclerq, Meynet ’12 Review: KZ, 1308.0338 McDermott, Yu, KZ ’11

Sunday, January 26, 14

slide-54
SLIDE 54

Summary

  • In the last 7-10 years, particle theory has

undergone a paradigm shift from sole focus on weak scale processes

  • A key aspect of this paradigm shift is

towards searching for light hidden sectors

  • This light hidden sector may play a key

role in the dynamics of the DM

Sunday, January 26, 14

slide-55
SLIDE 55

Summary

  • Well-motivated models -- Asymmetric

Dark Matter in particular

  • Intensity experiments such as the heavy

photon search are complementary to direct detection and astrophysical probes

  • Bright future!

Sunday, January 26, 14