Direct detection of Dark Matter with the EDELWEISS experiment J. - - PowerPoint PPT Presentation

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Direct detection of Dark Matter with the EDELWEISS experiment J. - - PowerPoint PPT Presentation

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Direct detection of Dark Matter with the EDELWEISS experiment J. Billard on behalf of the EDELWEISS collaboration Institut de Physique Nuclaire de Lyon / CNRS / Universit Lyon 1 Journe Matire Noire, APC 1er Dcembre, 2016 1 The

slide-1
SLIDE 1
  • J. Billard
  • n behalf of the EDELWEISS collaboration

Institut de Physique Nucléaire de Lyon / CNRS / Université Lyon 1 Journée Matière Noire, APC 1er Décembre, 2016

1

Direct detection of Dark Matter with the EDELWEISS experiment

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SLIDE 2
  • [/]
  • []
  • []

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C D M S I I G e ( 2 9 ) X e n

  • n

1 ( 2 1 2 )

CRESST CoGeNT (2012) CDMS Si (2013) DAMA

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

  • I

I I ( 2 1 2 ) C O U P P ( 2 1 2 ) L U X ( 2 1 3 ) C D M S l i t e ( 2 1 3 ) S u p e r C D M S L T ( 2 1 4 )

8B

Neutrinos Atmospheric and DSNB Neutrinos

7Be

Neutrinos

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C R E S S T ( 2 1 4 ) EDELWEISS (2011) D A M I C ( 2 1 2 )

2

  • J. Billard et al., PRD 89 (2014)

Julien Billard (IPNL) - APC

The neutrino background

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SLIDE 3
  • [/]
  • []
  • []

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C D M S I I G e ( 2 9 ) X e n

  • n

1 ( 2 1 2 )

CRESST CoGeNT (2012) CDMS Si (2013) DAMA

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

  • I

I I ( 2 1 2 ) C O U P P ( 2 1 2 ) L U X ( 2 1 3 ) C D M S l i t e ( 2 1 3 ) S u p e r C D M S L T ( 2 1 4 )

8B

Neutrinos Atmospheric and DSNB Neutrinos

7Be

Neutrinos

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C R E S S T ( 2 1 4 ) EDELWEISS (2011) D A M I C ( 2 1 2 )

2

  • J. Billard et al., PRD 89 (2014)

Julien Billard (IPNL) - APC

Low WIMP mass High WIMP mass

The neutrino background

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SLIDE 4
  • [/]
  • []
  • []

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C D M S I I G e ( 2 9 ) X e n

  • n

1 ( 2 1 2 )

CRESST CoGeNT (2012) CDMS Si (2013) DAMA

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

  • I

I I ( 2 1 2 ) C O U P P ( 2 1 2 ) L U X ( 2 1 3 ) C D M S l i t e ( 2 1 3 ) S u p e r C D M S L T ( 2 1 4 )

8B

Neutrinos Atmospheric and DSNB Neutrinos

7Be

Neutrinos

C O H E RE NT N E U TR IN O S C A TT E RI N G COHERENT NEU TR I NO S C AT T E R I N G C O H E RE N T N EU TRI NO SCATTERING

C R E S S T ( 2 1 4 ) EDELWEISS (2011) D A M I C ( 2 1 2 )

3

  • J. Billard et al., PRD 89 (2014)

The neutrino background

liquid noble gases

cryogenic crystals

Julien Billard (IPNL) - APC

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SLIDE 5

4

http://edelweiss.in2p3.fr

10 institutions

CEA/IRFU CEA/IRAMIS IKP EKP IPE JINR DUBNA

  • Univ. OXFORD

Univ. SHEFFIELD CNRS/INP CNRS/IN2P3 CNRS/IN2P3 CNRS

The EDELWEISS-III Experiment

Julien Billard (IPNL) - APC

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SLIDE 6

5

Cryogenic semiconductor detectors looking for WIMPs WIMP

Julien Billard (IPNL) - APC

The EDELWEISS-III Experiment

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SLIDE 7

6

WIMP WIMP E field

Charge/Phonon sensors Charge/Phonon sensors

Julien Billard (IPNL) - APC

The EDELWEISS-III Experiment

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SLIDE 8

7

e- e- h+

E field

prompt phonons

Charge/Phonon sensors Charge/Phonon sensors

Julien Billard (IPNL) - APC

The EDELWEISS-III Experiment

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SLIDE 9

8

e- e- h+

E field

prompt phonons

Charge/Phonon sensors Charge/Phonon sensors

Etotal = Erecoil + Eluke = Erecoil + EQΔV

1 3 eV Julien Billard (IPNL) - APC

The EDELWEISS-III Experiment

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SLIDE 10

9

  • Clean room
  • Radon-free air around the detectors
  • To reduce surface contamination

with radioactive contaminants

  • Two layers of lead shield
  • To stop the gammas
  • Standard (far from detectors)
  • Ancient (near the detectors)
  • Inner and outer polyethylene shield
  • To stop the neutrons
  • Muon veto
  • To suppress muon induced

neutrons in surrounding materials EDELWEISS setup

The EDELWEISS-III Experiment

Julien Billard (IPNL) - APC

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SLIDE 11

10

The EDELWEISS-III Experiment

  • Upgrade from EDELWEISS-II:
  • Extra 10 cm internal PE shield
  • New electronics
  • Cryogenics (Vibrations)

Julien Billard (IPNL) - APC

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SLIDE 12

10

The EDELWEISS-III Experiment

  • Upgrade from EDELWEISS-II:
  • Extra 10 cm internal PE shield
  • New electronics
  • Cryogenics (Vibrations)
  • New FID800 (850g) germanium detectors

measure both ionization and heat

Julien Billard (IPNL) - APC

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SLIDE 13

10

The EDELWEISS-III Experiment

  • Upgrade from EDELWEISS-II:
  • Extra 10 cm internal PE shield
  • New electronics
  • Cryogenics (Vibrations)
  • New FID800 (850g) germanium detectors

measure both ionization and heat

C1 +4 V V1 -1.5 V

NTD NTD

V2 +1.5 V C2 -4 V

  • Interdigitized electrodes for surface event

rejection from both top/bottom surfaces and sidewall (600g of fiducial mass)

Julien Billard (IPNL) - APC

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SLIDE 14

10

The EDELWEISS-III Experiment

  • Upgrade from EDELWEISS-II:
  • Extra 10 cm internal PE shield
  • New electronics
  • Cryogenics (Vibrations)
  • New FID800 (850g) germanium detectors

measure both ionization and heat

  • Interdigitized electrodes for surface event

rejection from both top/bottom surfaces and sidewall (600g of fiducial mass)

  • Nuclear/Electron recoil discrimination from

simultaneous heat and ionization measurements

Julien Billard (IPNL) - APC

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SLIDE 15

10

The EDELWEISS-III Experiment

  • Upgrade from EDELWEISS-II:
  • Extra 10 cm internal PE shield
  • New electronics
  • Cryogenics (Vibrations)
  • New FID800 (850g) germanium detectors

measure both ionization and heat

  • Interdigitized electrodes for surface event

rejection from both top/bottom surfaces and sidewall (600g of fiducial mass)

  • Nuclear/Electron recoil discrimination from

simultaneous heat and ionization measurements Technical paper: EDELWEISS Coll., to be submitted soon

  • Original design (ANR FIDSUSY 2010):
  • 20 kg of Ge target, 161 days of DM data
  • Largest bolometer array for direct detection
  • Initial physics goal: WIMP masses > 20 GeV, σ ~ 10-9 pb, ~3000 kg.day

Julien Billard (IPNL) - APC

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SLIDE 16

Strategies for Light WIMP Searches

11

Recoil energy [keV] 2 4 6 8 10 12 ]

  • 1

Event rate [(ton.year.keV)

  • 1

10 1 10

2

10

5 GeV WIMP 7 GeV WIMP 10 GeV WIMP

Lowering the energy threshold is the key for light WIMP searches

  • 1. Low Threshold analysis: Improve exposure and extend background ID to low energy

Julien Billard (IPNL) - APC

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SLIDE 17

12

  • Use 8 detectors with lowest trigger thresholds (4 @ 2.4 keVnr and 4 @ 3.6 keVnr)
  • 582 kg-d of fiducial exposure (August. 2014 - March 2015)
  • 2 analyses in parallel optimized for exclusion: BDT and Likelihood

Lowering the analysis thresholds down to the experiment’s trigger thresholds

Low Threshold analysis

Sidebands Background model BDT/Likelihood Data Upper limit WIMP model

Julien Billard (IPNL) - APC

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SLIDE 18

Et = Er + EL Er = Et - EQ(Et)ΔV

1 3 eV

  • Since signal-to-noise is poor, consider mean

ionization energy for nuclear recoils

  • Nuclear recoil calibration better fitted to a power

law

  • Consistent with Lindhard’s prediction with less

ionization at low energy and more at high energy

13

Low Threshold analysis

8V

Julien Billard (IPNL) - APC

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SLIDE 19

for illustration (FID837 subset)

14

EDELWEISS-III backgrounds

Low Threshold analysis

For all backgrounds : data-driven model from sideband data No fiducial cut

Julien Billard (IPNL) - APC

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SLIDE 20

15

Low Threshold analysis

Gamma + activation lines

  • Internal radioactivity from

shielding and cryostat

  • Cosmogenic activation lines: K/

L-shell capture from 68,71Ge,

65Zn, 68Ga

For all backgrounds : data-driven model from sideband data

for illustration (FID837 subset)

No fiducial cut B u l k Surface

Julien Billard (IPNL) - APC

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SLIDE 21

for illustration (FID837 subset)

16

210Pb “surface events”

Low Threshold analysis

  • betas and 206Pb nuclei from

210Pb decay chain

  • events are located on detector

face and sidewall surfaces from

222Rn contamination

For all backgrounds : data-driven model from sideband data No fiducial cut

210Pb 210Po 206Pb 210Bi

22.3 y 5.01 d 138.4 d

80%: β 17.0 keV 20%: β 63.5 keV 100%: β 1161.5 keV 100%: α 5.3 MeV 13.7%: conv. e 42.5 keV + Auger e 3.5%: conv. e 45.6 keV + Auger e 4.3%: γ 46.5 keV 103 keV 58.1%:

  • conv. e 30.2 keV + Auger e’s

+ 22.0%: x-rays 9.4-15.7 keV

Julien Billard (IPNL) - APC

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SLIDE 22

17

Low Threshold analysis

Neutron

  • Radiogenic origin only for the

neutron background

  • Estimated from coincident

Nuclear Recoils scaled by the single-to-multiple ratio derived from Geant4 simulations For all backgrounds : data-driven model from sideband data

for illustration (FID837 subset)

No fiducial cut

Julien Billard (IPNL) - APC

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SLIDE 23

18

Low Threshold analysis

Heat only

  • Dominating background at

low-energy

  • Estimated from Eion<0

sideband data (no WIMP expected)

  • Origin under investigation

highest priority of the EDELWEISS collaboration For all backgrounds : data-driven model from sideband data

for illustration (FID837 subset)

No fiducial cut

Julien Billard (IPNL) - APC

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SLIDE 24

19

  • No statistically significant excess
  • Dominant backgrounds:
  • 5 GeV: Heat Only
  • 20 GeV: Radiogenic neutrons
  • 2D fit E_ion Vs E_heat
  • Joint fit over the 8 selected detectors
  • x7 better at low mass w.r.t BDT
  • Method of choice for the future

BDT Likelihood

EDELWEISS Coll., EPJ C (2016) 76:548 EDELWEISS Coll., JCAP 05 (2016) 019

Low Threshold analysis

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SLIDE 25

]

2

WIMP Mass [GeV/c 4 5 6 7 8 9 10 20 30 ]

2

WIMP-nucleon cross section [cm

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

CRESST 2015 C R E S S T 2 1 2 EDWIII-BDT CDMSLITE LUX CoGeNT 2012 DAMA CDMSII-Si SCDMS-LT E D E L W E I S S I I I L i k e l i h

  • d

DAMIC

20

Low Threshold analysis

EDELWEISS Coll., JCAP 05 (2016) 019 EDELWEISS Coll., EPJ C (2016) 76:548 Julien Billard (IPNL) - APC

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SLIDE 26

21

Let’s take a closer look at the ER band…

Low Threshold analysis

  • Cosmogenically produced tritium will become
  • ne of the major background component for

next generation Ge experiments

  • Thanks to its impressively low gamma

background (<0.1 DRU) and exquisite ionization energy resolution (200 eV RMS)

  • EDELWEISS-III is the first Ge experiment to
  • bserve this ultimate background and to have

measured its production rate which is of first importance for next generation experiments !

Julien Billard (IPNL) - APC EDELWEISS Coll., arXiv:1607.04560

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SLIDE 27

Strategies for Light WIMP Searches

22

Recoil energy [keV] 2 4 6 8 10 12 ]

  • 1

Event rate [(ton.year.keV)

  • 1

10 1 10

2

10

5 GeV WIMP 7 GeV WIMP 10 GeV WIMP

Lowering the energy threshold is the key for light WIMP searches

An intense R&D program to lead the low mass WIMP search at the horizon 2017…

1. High Voltage

Amplify heat signal to reduce threshold 8 V —> 100 V

2. Lower the intrinsic heat threshold

Improved heat sensors 500 eV (RMS) —> 100 eV (RMS)

3. Extended background ID to lower energy

Improved ionization sensors 200 eV (RMS) —> 100/50 eV (RMS)

4. Reduce irreducible backgrounds

/100 heat only rate 100 eVnr 2.4 keVnr

Julien Billard (IPNL) - APC

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SLIDE 28

23

Goal #1: High Voltage

  • First Dark Matter run with HV detectors ongoing
  • Successfully reached 100 V leading to a boost factor of ~35

with Lowest threshold achieved of 60 eVee

  • Even in HV mode, we can still readout both ionization and

heat signals contrarily to SuperCDMS

  • However, loss of particle ID at high voltage —> Exclusion

strategy dedicated to the lowest WIMP masses reachable

Et = Er + EQΔV

1 3 eV

Ba calibration 356 keV line

Julien Billard (IPNL) - APC

slide-29
SLIDE 29

23

Goal #1: High Voltage

  • First Dark Matter run with HV detectors ongoing
  • Successfully reached 100 V leading to a boost factor of ~35

with Lowest threshold achieved of 60 eVee

  • Even in HV mode, we can still readout both ionization and

heat signals contrarily to SuperCDMS

  • However, loss of particle ID at high voltage —> Exclusion

strategy dedicated to the lowest WIMP masses reachable

Et = Er + EQΔV

1 3 eV

Ba calibration 356 keV line

Julien Billard (IPNL) - APC

slide-30
SLIDE 30

24

  • We developed a detailed model of our heat signals that fits very well observed pulses
  • Sensitivity to ballistic phonons
  • Presence of a parasitic heat capacity
  • We should be able to further optimize our heat sensors and gain a factor of 5 is sensitivity

PJA PapA Pax PapB PJB Pab IpA IpB GepA GapA GapB GepB Gab Gax NTD-A NTD-B Parasitic Cryostat Crystal Tb TeA, CeA, R0A, T0A TpA, CpA Ta, Ca TpB, CpB Tx, Cx TeB, CeB, R0B, T0B

!x !B !A

Time [s] 1 1.5 2 Voltage [V]

8 −

10

7 −

10

6 −

10

5 −

10

Data: NTD-A Data: NTD-B Model: NTD-A Model: NTD-B

Ba events: FID 837 @ 18 mK - MCMC3

  • J. Billard et al., J. Low Temp. Phys. (2016)

Goal #2: Improved heat sensors

Julien Billard (IPNL) - APC

slide-31
SLIDE 31

25

Goal #2: Improved heat sensors

Averaged 1 keV template Best fit 95% C.L. band

  • A dedicated R&D to optimize the heat sensors has started mid-2016:
  • no loss in sensitivity: no evidence of parasitic heat capacity
  • Perfect agreement with thermal model predictions: possibility to optimize via simulations
  • We observed a sensitivity of 200 nV/keV compared to 30 nV/keV with FID installed in Modane
  • Extrapolating to the noise level observed in Modane —> heat resolution of 50 eV (RMS) !!!
slide-32
SLIDE 32

25

Goal #2: Improved heat sensors

Averaged 1 keV template Best fit 95% C.L. band

  • A dedicated R&D to optimize the heat sensors has started mid-2016:
  • no loss in sensitivity: no evidence of parasitic heat capacity
  • Perfect agreement with thermal model predictions: possibility to optimize via simulations
  • We observed a sensitivity of 200 nV/keV compared to 30 nV/keV with FID installed in Modane
  • Extrapolating to the noise level observed in Modane —> heat resolution of 50 eV (RMS) !!!
slide-33
SLIDE 33

26

  • Transitioning from JFET to HEMT:
  • Lower intrinsic noise, low heat load
  • Can work at 4K: shorter cabling length reduces capacitance and improves resolution
  • Considered by EDW/HARD (resolution) [XB+AB NIMA 787 (2015) 51]
  • and SuperCDMS (heat load) [A. Phipps et al., JLTP 176 (2014) 466 and 911]
  • A successful HEMT amplifier has been designed in collaboration between SuperCDMS and EDELWEISS

with sub-100 eV (RMS) ionization resolution

  • Next step #1: Upgrade our ionization electronics following this newly designed amplifier
  • Next step #2: New electrode design (already successfully tested!) to reach 50 eV (RMS)
  • A. Phipps et al., arXiv:1611.09712

Goal #3: Improved ionization sensors

Am-241 calibration Noise blob 91 eV (RMS)

slide-34
SLIDE 34

26

  • Transitioning from JFET to HEMT:
  • Lower intrinsic noise, low heat load
  • Can work at 4K: shorter cabling length reduces capacitance and improves resolution
  • Considered by EDW/HARD (resolution) [XB+AB NIMA 787 (2015) 51]
  • and SuperCDMS (heat load) [A. Phipps et al., JLTP 176 (2014) 466 and 911]
  • A successful HEMT amplifier has been designed in collaboration between SuperCDMS and EDELWEISS

with sub-100 eV (RMS) ionization resolution

  • Next step #1: Upgrade our ionization electronics following this newly designed amplifier
  • Next step #2: New electrode design (already successfully tested!) to reach 50 eV (RMS)
  • A. Phipps et al., arXiv:1611.09712

Goal #3: Improved ionization sensors

Am-241 calibration Noise blob 91 eV (RMS)

slide-35
SLIDE 35

27

Goal #4: Reduce heat only rate

  • Heat only events are our dominating background for low-mass WIMP searches
  • The idea is to remove any glue from the crystal as it may generates « cracks »
  • Two ways out:
  • Using 2 deported NTDs, we have demonstrated the ability to reject « glue events »
  • Using a totally new sensor technology based on high impedance NbSi TES that are

photo-lithographied on the Ge surface (no glue) and sensitive to athermal phonons

  • To be confirmed with our 7 dedicated detectors being cooled down in Modane

2 deported NTDs NbSi TES

slide-36
SLIDE 36

27

Goal #4: Reduce heat only rate

  • Heat only events are our dominating background for low-mass WIMP searches
  • The idea is to remove any glue from the crystal as it may generates « cracks »
  • Two ways out:
  • Using 2 deported NTDs, we have demonstrated the ability to reject « glue events »
  • Using a totally new sensor technology based on high impedance NbSi TES that are

photo-lithographied on the Ge surface (no glue) and sensitive to athermal phonons

  • To be confirmed with our 7 dedicated detectors being cooled down in Modane

2 deported NTDs NbSi TES

slide-37
SLIDE 37

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)

DAMIC DAMA CDMSII-Si CRESST 2015 CRESST 2012 EDELWEISS-III SCDMS C D M S L I T E LUX CoGeNT 2012

28

The EDELWEISS-III Physics goals

Goal for 2017 reachable from EDELWEISS-III setup:

  • Q. Arnaud et al., J. Low Temp. Phys. (2016)

Julien Billard (IPNL) - APC EDW-III backgrounds, 350 kg-day

E D E L W E I S S

  • I

I I 2 1 7

slide-38
SLIDE 38

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)

DAMIC DAMA CDMSII-Si CRESST 2015 CRESST 2012 E D E L W E I S S

  • I

I I SCDMS C D M S L I T E LUX CoGeNT 2012

29

2 k g

  • s

c a l e c r y

  • g

e n i c e x p e r i m e n t s

Goal beyond 2017 from the SuperCDMS-EDELWEISS collaboration @ SNOLab

Beyond EDELWEISS-III

Julien Billard (IPNL) - APC

  • Q. Arnaud et al., J. Low Temp. Phys. (2016)

improved backgrounds, 35000 kg-day

E D E L W E I S S

  • I

I I 2 1 7

slide-39
SLIDE 39

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)

DAMIC DAMA CDMSII-Si CRESST 2015 CRESST 2012 E D E L W E I S S

  • I

I I SCDMS C D M S L I T E LUX CoGeNT 2012

29

2 k g

  • s

c a l e c r y

  • g

e n i c e x p e r i m e n t s

Goal beyond 2017 from the SuperCDMS-EDELWEISS collaboration @ SNOLab

Beyond EDELWEISS-III

50 eV (RMS) ionization « 8B neutrino observatory »

Julien Billard (IPNL) - APC

  • Q. Arnaud et al., J. Low Temp. Phys. (2016)

improved backgrounds, 35000 kg-day

E D E L W E I S S

  • I

I I 2 1 7

slide-40
SLIDE 40

30

Beyond EDELWEISS-III

BDT output 1 ! 0.5 ! 0.5 1 Number of events

1 !

10 1 10

2

10

3

10

4

10

5

10

Tritium Neutrons Heat Only Lead Beta

  • Cosmo. lines

Compton Neutrinos Data

sion = 200 eV sion = 50 eV

Heat (keVee) Heat (keVee)

  • Ion. (keVee)

8B

  • Comparison in separation power between

the 8B neutrino signal and the remaining backgrounds for 200 eV and 50 eV ionization resolutions (RMS)

  • We expect about 10% nuclear recoil energy

resolution @ 1 keVee leading to great spectral measurement

  • A BDT analysis of 1 ton-year of simulated

data show about 78 « background free » neutrino events (out of 300)

  • Unique possibility to study in great detail the

still unobserved Coherent Elastic Neutrino- Nucleus Scattering process offering new probes for physics beyond the SM !!

Julien Billard (IPNL) - APC

slide-41
SLIDE 41

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

31

Conclusions

Julien Billard (IPNL) - APC

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)
slide-42
SLIDE 42

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

31

Conclusions

EDELWEISS-III LT analysis

JCAP , EPJC Julien Billard (IPNL) - APC

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)
slide-43
SLIDE 43

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

31

Conclusions

EDELWEISS-III LT analysis

JCAP , EPJC

EDELWEISS-III goals for 2017

intense R&D efforts ongoing Julien Billard (IPNL) - APC

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)
slide-44
SLIDE 44

]

2

WIMP Mass [GeV/c

1 −

10 × 7 1 2 3 4 5 6 7 8 9 10 20 ]

2

WIMP-nucleon cross section [cm

46 −

10

45 −

10

44 −

10

43 −

10

42 −

10

41 −

10

40 −

10

39 −

10

38 −

10

31

Conclusions

EDELWEISS-III LT analysis

JCAP , EPJC

EDELWEISS-III goals for 2017

intense R&D efforts ongoing

Going beyond (200kg-scale)

EDELWEISS-EURECA-SuperCDMS Julien Billard (IPNL) - APC

Neutrino background

  • J. Billard et al., Phys. Rev. D (2014)
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SLIDE 45

Low WIMP mass region (1 GeV - 10 GeV)

EDELWEISS-III results 2016 EDW-III goals 2017 35 ton-days

CRESST-3 phase 1 CRESST-3 phase 2 SuperCDMS@SNOLAB Julien Billard (IPNL) - APC