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H O W S E N S I T I V E A R E D I R E C T D E T E C T I O N E X - - PowerPoint PPT Presentation

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H O W S E N S I T I V E A R E D I R E C T D E T E C T I O N E X P E R I M E N T S T O S T R O N G LY I N T E R A C T I N G D A R K M AT T E R ? T I M O N E M K E N ( C P - O R I G I N S , O D E N S E ) Based on: [arXiv:1802.04764]*

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SLIDE 1

H O W S E N S I T I V E A R E D I R E C T D E T E C T I O N E X P E R I M E N T S T O S T R O N G LY I N T E R A C T I N G D A R K M AT T E R ?

T I M O N E M K E N ( C P ³ - O R I G I N S , O D E N S E )

Based on: [arXiv:1802.04764]* [arXiv:180?.????]**

* In collaboration with Chris Kouvaris. ** In collaboration with Rouven Essig, Chris Kouvaris, and Mukul Sholapurkar.

01.06.2018 MASS2018: Origin of Mass at the High Energy and Intensity Frontier

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SLIDE 2

Goodman and Witten, Phys.Rev. D31 (1985) 3059 Starkman et al, Phys.Rev. D41 (1990) 3594

  • Constraints from

direct detection are typically upper bounds on the cross section.

  • However, detectors

lose sensitivity to strongly interacting dark matter due to scatterings in the

  • verburden.
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SLIDE 3

Goodman and Witten, Phys.Rev. D31 (1985) 3059 Starkman et al, Phys.Rev. D41 (1990) 3594

  • Constraints from

direct detection are typically upper bounds on the cross section.

  • However, detectors

lose sensitivity to strongly interacting dark matter due to scatterings in the

  • verburden.
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SLIDE 4
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SLIDE 5
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SLIDE 6
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SLIDE 7
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SLIDE 8
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SLIDE 9
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SLIDE 10
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SLIDE 11

O U T L I N E

  • I. Terrestrial DM-nucleus scatterings
  • II. When detectors lose sensitivity
  • Analytic approach
  • Monte Carlo simulations
  • III. DM-electron scattering experiments
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SLIDE 12

T E R R E S T R I A L D M - N U C L E U S S C AT T E R I N G S

Part I

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SLIDE 13

R E L E VA N C E O F E A R T H S C AT T E R I N G S F O R S U B - G E V D M D E T E C T I O N

L ⊃ gX ¯ XγµXA0

µ + εFµνF 0µν + m2 φA0 µA0µ

σχp σχe ' ✓µχp µχe ◆2

  • Look e.g. at models with a heavy dark photon portal
  • Here tested DM-electron cross sections are

accompanied by strong DM-nucleus interactions.

S.K. Lee et al, PRD92 (2015) 083517 TE, C. Kouvaris, I. Shoemaker, PRD96 (2017) no.1, 015018

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SLIDE 14

D A R K M AT T E R S C AT T E R I N G I N S I D E T H E E A R T H

P(L) = 1 − exp  − Z dx MFP(~ x,~ v)

  • Probability to scatter after travelling a distance L:
  • The mean free path is given by
  • Underground DM-nucleus scatterings have two consequences:
  • A. re-distribution of DM particles inside the Earth
  • B. deceleration of the DM particles
  • If DM-nucleus interactions are sufficiently strong, these two effects

could influence the outcome of a DM detection experiment severely. −1

MFP(~

x,~ v) = X

i

fAi(~ x)⇢⊕(~ x) mAi total

χAi (~

v)

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SLIDE 15

W H E N T E R R E S T R I A L D E T E C T O R S L O S E S E N S I T I V I T Y

Part II

Atmosphere Earth crust Lead shielding Detector

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SLIDE 16

A N A LY T I C D E S C R I P T I O N O F D A R K M AT T E R S T O P P I N G P O W E R

  • DM traversing through matter lose energy:
  • Method A: Find cross section, for which the
  • verburden makes even the fastest particles

undetectable.

  • Method B: Compute the change of the DM spectrum

dhEi dx = X

i

ni(x)

Emax

R

Z dER ER dσi dER dR dER = nDMnT

∞

Z

vmin(ER)

dv vf(v) dσi dER

J.H. Davis, Phys.Rev.Lett. 119 (2017) no.21, 211302 B.J. Kavanagh, [arXiv:1712.04901]

  • D. Hooper et al., [arXiv:1802.03025]
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SLIDE 17

A N A LY T I C D E S C R I P T I O N O F D A R K M AT T E R S T O P P I N G P O W E R

  • DM traversing through matter lose energy:
  • Method A: Find cross section, for which the
  • verburden makes even the fastest particles

undetectable.

  • Method B: Compute the change of the DM spectrum

dhEi dx = X

i

ni(x)

Emax

R

Z dER ER dσi dER dR dER = nDMnT

∞

Z

vmin(ER)

dv vf(v) dσi dER

J.H. Davis, Phys.Rev.Lett. 119 (2017) no.21, 211302 B.J. Kavanagh, [arXiv:1712.04901]

  • D. Hooper et al., [arXiv:1802.03025]
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SLIDE 18

M O N T E C A R L O S I M U L AT I O N S

Two problems of the analytic approach:

  • 1. DM particles do not move on straight paths.
  • 2. The stopping equation only describes the average

behavior of DM particles. Particle tracks from the distribution tails can significantly contribute to detection rates.

M.S. Mahdawi, G.R. Farrar, [arXiv:1712:01170]

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SLIDE 19

M O N T E C A R L O S I M U L AT I O N S

Two problems of the analytic approach:

  • 1. DM particles do not move on straight paths.
  • 2. The stopping equation only describes the average

behavior of DM particles. Particle tracks from the distribution tails can significantly contribute to detection rates.

Monte Carlo simulations

M.S. Mahdawi, G.R. Farrar, [arXiv:1712:01170]

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SLIDE 20

D M S H I E L D I N G B Y T H E E A R T H C R U S T

0.1 0.5 1 10-46 10-44 10-42 10-40 10-38 10-36 10-34 10-32 10-30 10-1 102 105 108 1011 1014

M.S. Mahdawi, G.R. Farrar, JCAP 1712 (2017) 004 TE,C. Kouvaris, [arXiv:1802:04764]

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SLIDE 21

D M - N U C L E U S C O N S T R A I N T S

0.1 0.5 1 5 10 10-47 10-42 10-37 10-32 10-27 10-22

CRESST 2017 surface CRESST III C R E S S T I I DAMIC(2011) XQC CMB XENON1T n e u t r i n

  • b

a c k g r

  • u

n d

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SLIDE 22

D M - E L E C T R O N S C AT T E R I N G E X P E R I M E N T S

Part IV

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SLIDE 23

D M E L E C T R O N E X P E R I M E N T S

What’s next?

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SLIDE 24

D M E L E C T R O N E X P E R I M E N T S

  • Implement the full computation of event rates for liquid

noble gas experiments and semiconductor targets (ionization and crystal form factors).

What’s next?

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SLIDE 25

D M E L E C T R O N E X P E R I M E N T S

  • Implement the full computation of event rates for liquid

noble gas experiments and semiconductor targets (ionization and crystal form factors).

  • R. Essig et al., JHEP 1605 (2016) 046
  • R. Essig et al., Phys.Rev. D96 (2017) no.4, 043017

DarkSide collaboration, [arXiv:1802:06998]

What’s next?

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SLIDE 26

D M E L E C T R O N E X P E R I M E N T S

  • Implement the full computation of event rates for liquid

noble gas experiments and semiconductor targets (ionization and crystal form factors).

  • Main focus lies on light mediators
  • R. Essig et al., JHEP 1605 (2016) 046
  • R. Essig et al., Phys.Rev. D96 (2017) no.4, 043017

DarkSide collaboration, [arXiv:1802:06998]

What’s next?

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SLIDE 27

D M E L E C T R O N E X P E R I M E N T S

  • Implement the full computation of event rates for liquid

noble gas experiments and semiconductor targets (ionization and crystal form factors).

  • Main focus lies on light mediators

➡ new q-dependence in the cross section alter the scattering kinematics and stopping power of the

  • verburden
  • R. Essig et al., JHEP 1605 (2016) 046
  • R. Essig et al., Phys.Rev. D96 (2017) no.4, 043017

DarkSide collaboration, [arXiv:1802:06998]

What’s next?

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SLIDE 28

D M E L E C T R O N E X P E R I M E N T S

  • Implement the full computation of event rates for liquid

noble gas experiments and semiconductor targets (ionization and crystal form factors).

  • Main focus lies on light mediators

➡ new q-dependence in the cross section alter the scattering kinematics and stopping power of the

  • verburden
  • Use both analytic and MC methods.
  • R. Essig et al., JHEP 1605 (2016) 046
  • R. Essig et al., Phys.Rev. D96 (2017) no.4, 043017

DarkSide collaboration, [arXiv:1802:06998]

What’s next?

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SLIDE 29

S C AT T E R I N G D Y N A M I C S W I T H L I G H T M E D I AT O R S

  • 1.0
  • 0.5

0.0 0.5 1.0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4

cos α fN(cos α) FDM=1

  • 1.0
  • 0.5

0.0 0.5 1.0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4

cos α fN(cos α) FDM~ 1

q

  • 1.0
  • 0.5

0.0 0.5 1.0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4

cos α fN(cos α) FDM~ 1

q2

v=50 km

sec

v=300 km

sec

v=vesc+v⊕

mDM = 1 MeV mDM = 10 MeV mDM = 100 MeV mDM = 1000 MeV

FA(q) = a2q2 1 + a2q2

D M F O R M FA C T O R V S C H A R G E S C R E E N I N G

FDM(q) = 8 > > < > > : 1 , for heavy mediator ,

qref q ,

for ED interaction , ⇣

qref q

⌘2 , for light mediator .

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SLIDE 30

P R E L I M I N A RY R E S U LT S

100 101 102 103 10-39 10-38 10-37 10-36 10-35 10-34 10-33 10-32 10-31 10-30 10-29 10-28 10-27 10-26 10-25 10-24 10-23

mχ[MeV] σe[cm2] FDM=1

100 101 102 103 104 10-37 10-36 10-35 10-34 10-33 10-32 10-31 10-30 10-29 10-28 10-27 10-26 10-25 10-24

mχ[MeV] σe[cm2] FDM=αme/q

100 101 102 103 10-37 10-36 10-35 10-34 10-33 10-32 10-31 10-30 10-29 10-28 10-27 10-26 10-25 10-24 10-23 10-22

mχ[MeV] σe[cm2] FDM=(αme/q)2 XENON10 XENON100 SENSEI DarkSide-50 SuperCDMS(2018)

P R E L I M I N A R Y P R E L I M I N A R Y

Further experiments: DarkSide-50 & SuperCDMS Projections for e.g. high-altitude experiments. better understanding on electronic stopping power

To Do

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SLIDE 31

D A M A S C U S

D a r k M a t t e r S i m u l a t i o n C o d e f o r U n d e rg ro u n d S c a t t e r i n g s

The code is public:

http://github.com/temken/

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SLIDE 32

Thank you!