shedding light on dark matter from deep underground with xenon

Shedding Light on Dark Matter from Deep Underground with XENON

Kaixuan Ni (Columbia)

University of Maryland, 11-25-2008

A well-known mystery for astronomers

2

Fritz Zwicky, The Astrophysical Journal, 85 (1937) 217

... All curves show a fairly rapid velocity rise to V ~ 125 km s-1 at R ~ 5 kpc, and a slower rise thereafter. Most rotation curves are rising slowly even at the farthest measured point. Neither high nor low luminosity Sc galaxies have falling rotation curves. Sc galaxies of all luminosities must have significant mass located beyond the optical image. ...

3

Modern Precision Cosmology

Dark Matter is a stable, neutral, and heavy particle that interacts very weakly, or only through gravity.

Leading DM candidates, such as neutralinos and axions, are from theories beyond the Standard Model!

Three ways to probe the nature of dark matter

5

Indirectly search for DM annihilation products (gamma rays, neutrinos, electrons, positrons, etc.)

Produce dark matter in the Collider

Directly detect DM interacting with a terrestrial target

A fruitful year for indirect DM searches

6

Observation of an anomalous positron abundance in the cosmic radiation [arXiv:0810.4995]

PAMELA

A fruitful year for indirect DM searches

7

J Chang et al. Nature 456, 362-365 (2008) doi:10.1038/nature07477

ATIC

DM local density 0.43 GeV/cm3

Kaluza-Klein mass 620 GeVAnnihilation rate 10-23 cm3/s

An excess of cosmic electrons.

Dark Matter Equation of State

8

Ωχh2 =mχnχ

ρc=

3 × 10−27 cm3/s〈σAv〉freezout

〈σAv〉freezout = 3 × 10−26 cm3/s

dnχ

dt+ 3Hnχ = −〈σAv〉

[(nχ)2 −

(neq

χ

)2]

A fruitful year for indirect DM searches

9

J Chang et al. Nature 456, 362-365 (2008) doi:10.1038/nature07477

ATIC

Kaluza-Klein mass 620 GeVAnnihilation rate 10-23 cm3/s

A boost factor of ~200 is required

Also a busy year for direct DM searches

in the summer, moving against wind

in the winter, moving away from wind

expect an annual modulation in signal!WIMP “wind”

Also a busy year for direct DM searches

10

in the summer, moving against wind

in the winter, moving away from wind

expect an annual modulation in signal!WIMP “wind”

Also a busy year for direct DM searches

10

DAMA/LIBRA reconfirmed their early observation of annual modulation signal [arXiv:0804.2741]

in the summer, moving against wind

in the winter, moving away from wind

expect an annual modulation in signal!WIMP “wind”

Also a busy year for direct DM searches

11

CDMS further improves Spin-Independent after XENON10 [arXiv:0802.3530]

DAMA allowed

Also a busy year for direct DM searches

12

XENON10 Spin-Dependent pure-neutron coupling [PRL 101, 091301 (2008)]

COUPP further improves Spin-dependent proton coupling

[Science 319:933-936,2008]

arXiv:0810.0713

arXiv:0810.0713

arXiv:0810.0713

Are we at the edge of uncovering the nature of DM?

15

Galactic WIMP Halo

(ρ = 0.3 GeV/cm3)

ElasticScattering

TargetNucleus

<V> = 220 km/s

Recoil Nucleus~10-100 keV or less

χχ

σχ-p can be as low as 10-46 cm2

Direct Dark Matter Detection

Goodman and Witten,coherent scattering for WIMPsPhys Rev D 31, 3059 (1985)

Recoil Energy [keVr]

0 10 20 30 40 50 60 70 80

Rate

[evts

/keV

r/kg

/day]

-710

-610

-510

Xe (A=131)

Ge (A=73)

Ar (A=40)

18 evts/100-kg/year (Eth=5 keVr)

8 evts/100-kg/year (Eth=15 keVr)

WIMP Scattering Rates

The Challenges for Direct DM Detection

large mass (ton scale)

low energy threshold (a few keV)

background suppression

deep underground

passive shield

low intrinsic radioactivity

gamma background discrimination

16

Mχ = 100 GeV,σχ−p = 10−45cm2

R ∼ Mdet

Mχρσ〈v〉

Why do we need go to deep underground?

17

Why do we need go to deep underground?

17

Homestake

muon induced neutron flux

Mei and Hime, PRD (2006)

Why do we need go to deep underground?

17

100 GeV WIMPs, 10-46 cm2

signal/background event rates

Homestake

muon induced neutron flux

Mei and Hime, PRD (2006)

World Wide Dark Matter Searches

18

Gran SassoCRESST

DAMA/LIBRAWARP

XENON

SNOLABDEAP/CLEAN

PICASSO

KamiokaXMASS

YangyangKIMS

SoudanCDMS

HomestakeLUX

BoulbyZEPLINDRIFT

Frejus/Modane

EDELWEISS

Dark Matter physicists

Dark Matter physicists

Cryogenic (CDMS etc.)

Dark Matter physicists

Cryogenic (CDMS etc.)

Noble Liquids (XENON etc.)

The Merits of Noble Liquids for Dark Matter Detection

20

Xe*

+Xe

Xe2*

Triplet27ns

Singlet3ns

2Xe2Xe

175nm175nm

Xe** + Xe

Xe2+

+e-

(recombination)

Xe+

+XeIonisation

Excitation

Electron/nuclear recoil

time constants depend on gase.g. Xe 3/27nsAr 10/1500ns

wavelengthdepends on gase.g. Xe 175nmAr 128nm

Nigel Smith, RAL

Recombination depends on type of recoils (stronger for nuclear recoils)

scalability : relatively cheap and “easy” cryogenics at 170 K (LXe), 87 K (LAr)

bkg reduction: via self-shielding

low threshold : high scintillation yield

gamma rejection: electron and nuclear recoil discrimination

The Noble Liquid Revolution

21

• Noble liquids (LAr, LXe) are relatively inexpensive, easy to scale up

• Self-shielding reduce external background

• Excellent gamma background rejection (pulse-shape, or ionization/scintillation)

Single Phase(XMASS, CLEAN/DEAP)

Two Phase(XENON,LUX,ZEPLIN II/III,WARP,ArDM.)

XMASS 800-kg WARP

Two-phase Xenon Detectors for Dark Matter Detection

22

WIMPs/Neutrons

nuclear recoil

electron recoil

Gammas

Top PMT Array

Signals from XENON10

23

S1 S2

S1

S2

The Phased XENON Program

24

XENON10(2006-2007) XENON100

(2007-2012)

XENON R&D (2001-2005)

XENON1T(2012)

136 kg-days Exposure= 58.6 live days x 5.4 kg x 0.86 (ε) x 0.50 (50% NR)

(data collected between Oct.2006 and Feb.2007)

4.5 –27 keVr

25

XENON10 WIMP Search Data

~1800 events

WIMP Search Windownoise event

Statistical leakage from

electron recoil band

Anomalous events due to non-active Xe

XENON10 WIMP-Nucleon Cross-Section Upper Limits

26

XENON10

CDMS II

(NO BKG SUBTRACTION)

8.8 x 10-44 cm2 at 100 GeV

4.5 x 10-44 cm2 at 30 GeV

Constrained Minimal

Supersymmetric Model

Spin-independent

Phys. Rev. Lett. 100, 021303 (2008)

Spin-dependent

Phys. Rev. Lett. 101, 091301 (2008)

XENON10

CDMS ZEPLIN-II

(NO BKG SUBTRACTION)

6 x 10-39 cm2 at 30 GeV

Can XENON10 anomalous events be explained by “iDM”?

27

δ ≤ 12µβ2c2 ≈ 100 keV

µ =MχMN

Mχ + MN

No longer elastic scattering.If dark matter can only scatter off of a nucleus

by transitioning to an excited state, the kinematics are changed dramatically

inelastic Dark Matter (iDM)

N. Weiner

Spencer Chang, Graham D. Kribs, David Tucker-Smith, Neal Weiner [arXiv:0807.2250]

visible to DAMA and XENON

visible to CDMS and

WARPf(v)

must have enough kinetic energy to scatter

modulation is also significantly enhanced

N. Weiner

Spectrum is dramatically modifiedStandard WIMPs have a spectrum that

peaks at low energies

Mχ=100 GeV, δ = 120 keV,normalized to DAMA 2-6 keV

XENON10 “background” data adjusted for efficiencies (taking unpublished acceptance x efficiency = 0.3, error bars estimated)

Mχ=100 GeV, δ=0 keV,normalized to inelastic XENON10 signal

Status of XENON100: the TPC Assembly

3112

the

170 kg LXe(70 kg target)

XENON100: The TPC Assembly

XENON100 Collaboration

32

An international collaboration of 46 physicists from 9 institutions

Laboratori Nazionali del Gran Sasso, Italy

XENON100

LVDICARUS

OPERA

LNGS 1400 m Rock (3100 w.m.e)

34

LNGS: 1.4km rock (3100 mwe)

XENON100

inside shield

XENON10

XENON100

outside shield

XENON100

XENON10

XENON100 Underground at the Laboratori Nazionali del Gran Sasso

3516

• 242 PMTs (Hamamatsu R8520-06-Al )

• 1 “ square metal channel developed for XENON

• Low radioactivity (<1 mBq U/Th per PMT)

• 80 PMTs for bottom array (33% QE)

• 98 PMTs for top array (23% QE)

• 64 PMTs for top/bottom/side Veto (23% QE)

XENON100: The PMTs Bottom Array

Top Array PMTs for Side & Bottom Shield

PMT Base

Ultra-low radioactive material selection

36

All materials used in XENON100 detector were selected based on low radioactivity

Background simulation

37

• 0.15 mBq/PMT x 242 PMTs gives 3000 238U decays/day• Each 238U decay produces 15 gammas and 9 alphas• 16M gamma/year• (alpha,n) reaction results 7 neutron/year

A realistic model based on Geant4 was constructed to propagate all the gammas/neutrons to simulate the

background rate.

Expected Background and Sensitivity Reach

38

R (cm)0 2 4 6 8 10 12 14

Z (c

m)

-30

-25

-20

-15

-10

-5

0 )ee

(dru

-510

-410

-310

-210

-110

50 kg30 kg

Current XENON100: gamma bkgdruee = evts/keVee/kg/day

e assume cross section 10-44 cm2

XENON100: Data Acqusition System

20

Requirements:

digitize full waveform (320!s) of 242 PMTs

with no deadtime and with high rate capability for calibration

CAEN V1724 Flash ADC: 14bit, 100MHz

circular buffer: no deadtime

on board FPGA: Zero Length Encoding only relevant signal portion transferred from ADCto DAQ computer to allow faster event transfer rates >60 Hz in calibration mode

39

First signals from XENON100

40

0 5000 10000 15000 20000 25000 300000

1

2

3

4

5

6

7

8

13900 14000 14100 14200 143000

0.1

0.2

0.3

0.4

0.5

0.6

0.7

14400 14600 14800 15000 152000

1

2

3

4

5

6

7

8

Gamma Event Digitized

S1 S2

Gamma Event Localized

1

2

3

4

5 6

7 8 9 10 11

12

13

14

15

16

17

18

19

20 21

22 23 24 25 26

27

28

29

30

31

32

33

34 35

36 37 38 39

40

41

42

43

44

45

46 47

48 49 50 51

52

53

54

55

56

57

58 59 60 61

62

63

64

65

66

67

68 69 70 71

72

73

74

75

76

77 78 79

80

81

82

83

84 85 86

87

88

89

90 91

92

93

94 95

96

97 98179

180

181

182

183

184185

186 187 188189

190

191

192

193

194

195

196

197

198

199

200201

202203204205

206

207

208

209

210

Top Array

1

2

3

4

5 6

7 8 9 10 11

12

13

14

15

16

17

18

19

20 21

22 23 24 25 26

27

28

29

30

31

32

33

34 35

36 37 38 39

40

41

42

43

44

45

46 47

48 49 50 51

52

53

54

55

56

57

58 59 60 61

62

63

64

65

66

67

68 69 70 71

72

73

74

75

76

77 78 79

80

81

82

83

84 85 86

87

88

89

90 91

92

93

94 95

96

97 98179

180

181

182

183

184185

186 187 188189

190

191

192

193

194

195

196

197

198

199

200201

202203204205

206

207

208

209

210

E [keV]

0 500 1000 1500 2000 2500 3000

Ra

te [

ev

ts/k

g/d

ay

/ke

V]

-310

-210

-110

1

XENON100 MC Background

XENON100 background run

41

S1 [keVee]

0 500 1000 1500 2000 2500 3000

Evts/keVee/kg/day

-310

-210

-110

1

xe100_080620_2018xe100_080620_2018

data Simulation

Detector has been fully filled with liquid xenon.First Measured background Spectrum in good agreement with MC prediction!

WIMP search run is planned to start in April 2009.

all single/multiple scattering events

all single/multiple scattering events

single scatter only with ~46 kg fiducial mass cut

edge events with poor light collection, will be removed by radial position cut

A proposal to upgrade XENON100 (2009-2012)

42

Sensitivity Reach of the XENON100 Program

43

Exposure Time with Zero Bkg [month]

0 5 10 15 20 25 30 35 40

]2

(90%

C.L

. u

pp

er

lim

it)

[cm

-p!"

-4610

-4510

-4410

-4310

)2

cm

-44

= 1

0-p!"

Exp

ecte

d #

of

WIM

P E

ven

ts (

-110

1

10

210

XENON Sensitivity Projection - 100 GeV WIMPs

2009 2011-2012

Current Best Sensitivity

Multi-ton scale XENON Detector for DUSEL (beyond 2012)

• Explore the full region/accumulate WIMP statistics

• New design with full coverage of ultra-low background photodetectors and cryostat

• Larger International Collaboration

• Total project cost: $50M-$100M

• neutrinoless double beta decay

• pp solar neutrinos

44