New developments in dark matter direct detection experiments

Transcription

1 New developments in dark matter direct detection experiments Christopher M c Cabe SLAP!, Kasteel Woerden 11th October 2017

2 Outline Why direct detection? New developments with Large detectors Small detectors

3 Why direct detection? Up to a point the stories of cosmology and particle physics can be told separately. In the end though, they will come together. Steven Weinberg Cosmology Particle Physics L = L SM DM h 2 = ± m q 3 qq + Suggests DM matter interactions should be present & informs and limits the possible interactions

4 Classic example: SUSY WIMPs Thermal freezeout gives the abundance & Z 0 h We know the interactions q q q q + nucleus (many quarks)

5 Classic example: SUSY WIMPs Thermal freezeout gives the abundance & We know the interactions 0 q Z q q h 0 q + E vis measure recoil energy of the nucleus

6 Where are we? PandaXII 2016 ) 2 SI WIMPnucleon cross section (cm LUX 2016 CDMSLite 2015 CRESSTII XENON1T + PandaXII (update) Post LHC1 msusy constraint 49 Neutrino coherent scattering 50 1 WIMP mass (GeV/c 2 2 ) 3 What next? Keep pushing down and look for other things!

7 New signals in Large Detectors *Large = {multitonne, established technology} XENON1T XENONnT, LZ, PandaXIII: 5t DARWIN, PandaXIV: 50t DEAP3600 DarkSide20t ARGO: 300t Today

8 1. Excite and decay Idea of inelastic scattering has been around for some time TuckerSmith, Weiner, arxiv:01138 NR Can upscatter so long as m m. 200 kev (and you have a model for it)

9 1. Excite and decay New: can look for decays with large detectors ER e.g. magnetic dipole interaction NR L µ µ F µ µs 30cm First search by XE0 (no signal) arxiv: XE0 30cm; XE1T 0cm; LZ 150cm Bonus: directional detection with headtail information Lin, Finkbeiner, arxiv:

10 2. Shake the atom + xenon atom (ground state)

11 2. Shake the atom + nucleus gets a nudge E recoil. 0.1 kev

12 2. Shake the atom a. γ Polarised atom emits a photon Suppression factor ~ 8 + Kouvaris & Pradler arxiv: CM arxiv: b. + e Atom emits an electron (Migdal effect) it takes some time for the electrons to catch up, which causes ionisation of the atom Suppression factor ~ 5 Ibe et al arxiv:

13 2. Shake the atom a. γ Large detectors overcome suppression Photon & electrons easy to detect! 30 + e LZ (g 1 =0.1, 2 phd) b. 36 CRESSTII 37 0 σ SI [cm 2 ] LUX WS2013+ WS201416(PLR) m DM [GeV] + A new probe of subgev DM

14 3. Supernova neutrino detection Energy: ~ 53 erg released ~99% is emitted by all neutrino flavours Neutrino energy ~ 15 MeV Time: Neutrino emission lasts ~ s When/where: ~13 SN/century in our galaxy distance ~ kpc

15 3. Supernova neutrino detection x x Z 0 Xe Xe Now observed by COHERENT Lang, CM, Reichard, Selvi, Tamborra: arxiv: = different SN simulations () /() ()

16 Small Detectors US Cosmic Visions: New Ideas in Dark Matter 2017 : Community Report arxiv: v1 *Small = {< kg, new technology}

17 Why go small? Cosmology DM h 2 = ± Particle L = L SM + m q 3 qq + ev MeV GeV TeV PeV 30M WIMPs Many other DM production mechanisms how can we probe them? Hidden Sector Dark Ma5er Hidden Thermal Relics / WIMPless DM Asymmetric DM FreezeIn DM SIMPs / ELDERS Black Holes

18 Lots of activity (all in USA?) Main Science Goal Experiment Target Readout Estimated Timeline 18 proposed experiments results in 2yrs? US Cosmic Visions: New Ideas in Dark Matter 2017 : Community Report arxiv: v1 SubGeV Dark Matter (Electron Interactions) SubGeV Dark Matter (Nucleon Interactions) Searches down to Neutrino Floor for O(GeV) Dark Matter SENSEI Si charge ready to start project (2 yr to deploy 0g) DAMIC1K Si charge ongoing R&D 2018 ready to start project (2 yr to deploy 1 kg) UA 0 (1) liquid Xe TPC Xe charge ready to start project (2 yr to deploy kg) Scintillator w/ GaAs(Si,B) light 2 yr R&D TES readout 2020 in scdms cryostat NICE; NaI/CsI NaI light 3 yr R&D cooled crystals CsI 2020 ready to start project Ge Detector w/ Ge charge 3 yr R&D Avalanche Ionization 1 yr kg detector Amplification 1 yr 0kg detector PTOLEMYG3, 2d graphene graphene charge directionality 1 yr fab prototype 1 yr data supercond. Al cube Al heat + yr program Superfluid helium He heat, light 1 yr R&D; 2018 ready to with TES readout start project; 2022 run Evaporation & superfluid helium, heat 3 yr R&D; 2020 ready to detection of Heatoms crystals with long start project R&D by field phonon mean free ionization path (e.g. Si, Ge) color centers crystals (CaF) light R&D e ort ongoing Magnetic bubble Single molecule Spinavalanche R&D e ort ongoing chamber magnet crystals (Magnetic flux) SuperCDMSG2+ Ge heat, ionization 3 yr R&D; 1 yr fabrication; 2022 start running NEWSG H, He charge 140cm sphere installed at SNOLAB in 2018 NEWSdm Si, Br, I, C, O, N, charge R&D phase complete. emulsions H, S directionality Now technical test CYGNUS HD SF 6, He charge 1 yr R&D; 1 yr 1 m 3 ; flexible directionality 2 yr m 3 Scintillating bubble Xe, Ar light 2 yr program; test kg Xe chamber C 6 F 6,H 2 0 heat(bubble) chamber with CENNS SpinDependent (Proton) Interactions PICO bubble chambers wide range heat(bubble) 40 l chamber now PICO 500 l next

19 Technique 1: ionise electrons + atom (ground state)

20 Ionise electrons ionised electron + atom (ionised)

21 Ionise electrons ionised electron 1 2 m DMv 2 ' E binding + Atoms: Ebinding ~ ev m DM & MeV atom (ionised)

22 Ionise electrons ionised electron m DMv 2 ' E binding Atoms: Ebinding ~ ev m DM & MeV semiconductor (overlapping electrons) Semiconductors: Ebinding ~ 1 ev m DM & 1 MeV

23 Proofofconcept See talk by Nicola Canci on DarkSide Dualphase detectors Ionised noble atomliquid search performed χ = χ = liquid xenon % liquid xenon e e e ee e S1 / χ = χ = % photosensors S2 sensitive to single electrons et 1 al: 70 3 S2 ) ( time 22 / e * Also CLEAN detector (LAr or LNe) at SNOL ig ss Photo S1 Photosensors sensors Essig / hne i Two phase TPC Depleted argon Currently comm )! first light and ( Physics run exp 9.00 E XENON0 and XENON1T at LNGS, DEAP Dark matter Experiment with LUX at SURF, PandaX at CJPL discrimination = and Pulse shape DarkSide50 at LNGS, kg LAr in single phase at SNO Aim to use depleted argon ArDM at Canfranc Status: int aconstruction l: 170 E Dark Side50 at L gas xenon liquid xenon σ [ ] S2 / / 3 gas xenon gas xenon Bolometer Next LAr dete Photo sensors σ [ ] Rate modulation Photo sensors photosensors hne i with XE,0 data Introduction χ [] FIG % C.L. limit on the DMelectron scattering cross section from XENON data (blue) and XENON0 data

24 Room for improvement e.g. DAMIC DAMIC Program Charge coupled device z 35 y Pixel array 36 DMe Scattering via Ultralight Hidden Photon ± Ionizing CDMSLite(2015) particle 70 kgd Fully depleted substrate DAMIC1K(2020) 1 kgy 0.1 dru, 2 e thres ) 2 ( C DAMI kgd ) 2 ( 0 C DAMI 3 kgd 1 Free charge carriers 41 x CRESST(2015) 52 kgd 39 µm 675 µm z ] 38 σxy ~ z σxy [ σn [cm2crosssection ] WIMPnucleon / cm 2 DMnucleus SI coherent scattering y x x IC M A 0 S er p kip 1 K kg 1 0. y 2 ( gy 0 02 ) k D Device is charge 1 exposed, collecting C MI A D readout. until user commands CDMSIISi JHEP05(2016)046 Readout can be slow / nondestructive : (2013) LUX(2015) ). threshold 2 e very low noise (few e m χ [GeV] Silicon bandgap:[ 1.2] ev. Mean energy for 1 eh pair: 3.8 ev. Also best limits for absorption of hidden photon dark matter (Skipper = lower noise design)

25 Many proposals Motivated parameter space ctions for the DMelectron scattering cross section e. The left (right) pendent (dependent) interaction, FDM = 1 (FDM = ( me /q)2 ). Existing ENON0) [90, 91] are shown in the blue (red) shaded regions. Projections

26 Other ideas covered these processes q Q e k k 0 e absorption absorption & phonons scatter & phonons + more

27 Conclusions We should search for dark matter along every feasible avenue Large detectors x s t n e m i r e xp p u e scal x Z0 e g n i t s i x e Xe Xe new signals are possible Small detectors many novel experiments FIG. 6: Constraints and projections for the DMelectron scattering cross section e. The left (right) vast regions of unexplored parameter space plots assume a momentumindependent (dependent) interaction, FDM = 1 (FDM = ( me /q)2 ). Existing constraints from XENON (XENON0) [90, 91] are shown in the blue (red) shaded regions. Projections show 3 events for a 1year exposure [50, 90, 94, 95, 98, 99]; the label includes the threshold (in terms of number of electrons, photons, or the electron recoil energy) and target mass. Solid/dashed/dotted lines indicate an estimate of the time to start taking data, corresponding roughly to a short/medium/long timescale, respectively. A solid line indicates a mature technology: data taking can begin in. 2 years and a zero background (radioactivity or dark currents) is reasonable for the indicated thresholds. A dashed line indicates more R&D is required and, if successful, data taking could start in 2 5 years; the projected sensitivity assumes that backgrounds can be controlled. A dotted line indicates longerterm R&D e orts. Bottom left plot assumes DM scatters through an A0 with ma0 = 3m. Five theory targets are shown as explained in

28 Thanks