QUANTUM MATERIALS & DARK MATTER DETECTION MOTIVATION NEW - - PowerPoint PPT Presentation
K. ZUREK Leveraging the many faces (and phases) of matter QUANTUM MATERIALS & DARK MATTER DETECTION MOTIVATION NEW DIRECTIONS IN DARK MATTER THEORY Old paradigm: weak scale dark matter (with relic density fixed by freeze-out)
QUANTUM MATERIALS & DARK MATTER DETECTION
NEW DIRECTIONS IN DARK MATTER THEORY
▸ Old paradigm: weak scale dark matter (with relic density fixed by freeze-out) DM DM time abundance Kolb and Turner nhσvi = H(Tfo) = ) hσvi ' 1 (20 TeV)2 ' g4 wk 4π(2 TeV)2 DIRECT DETECTION GOLD STANDARD
▸ Nuclear recoil experiments; basis of enormous progress in direct detection µN ≡ mNmX mX + mN v ∼ 300 km/s ∼ 10−3c for 50 GeV target v ∼ 10−3c = ⇒ 2µNv = qmax = p 2mNED = ⇒ ED ∼ 100 keV q, ED DARK MATTER MOORE’S LAW
1985 1990 1995 2000 2005 2010 2015 2020 10 −47 10 −46 10 −45 10 −44 10 −43 10 −42 10 −41 10 −40 Homestake Oroville H−M ’94 H−M ’98 IGEX UKDMC DAMA ’98 DAMA ’00 LIBRA ’08 Edelweiss ’98 CDMS I SUF ’99 CDMS I SUF ’02 Edelweiss ’01 Edelweiss ’03 CDMSII Soudan ’04 CDMSII Soudan ’10 Edelweiss ’09 Edelweiss ’11 CRESST ’11 SuperCDMS Soudan ’14 ZEPLIN I ZEPLIN II ZEPLIN III WARP ’07 XENON100 ’10 XENON100 ’11 XENON100 ’12 XENON10 LUX 300kg XMASS 800kg ~ 1 event kg−1 day−1 ~ 1 event 100 kg−1 yr−1 Dark Matter Searches: Past, Present & Future Limit Scalar Cross−section cm2 [60 GeV WIMP] Year Ge NaI Cryodet THEORY TARGETS
Physics Viewpoint, Raphael Lang EARLY EFFORT : DAMIC CCD AT FNAL
▸ Detecting DM Whispers dependent on dark counts and read-out noise ▸ 40 eV threshold, nuclear recoils WIMP Mass [GeV/c2] Crosssection [cm2] (normalised to nucleon) 120329092801 http://dmtools.brown.edu/ Gaitskell,Mandic,Filippini 10 10 1 10 2 10 42 10 40 10 38 10 36 DAMIC collaboration, 1105.5191 DIRECT DETECTION GOLD STANDARD
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TOWARDS LIGHT DARK MATTER
Dark Matter May Reside in a Hidden Sector Dark Matter Standard Model Connector π+ v π− v → π0 vπ0 v π0 v → b¯ b, γγ e.g. a stable dark pion no weak force NUCLEAR RECOILS
▸ Kinematic penalty when DM mass drops below nucleus mass qmax = 2mXv ED & eV ↔ mX = 300 MeV Ekin & 300 eV even though ED = q2 2mN NEXT UP: ELECTRON
▸ More bang for the buck if DM lighter than 1 GeV ▸ Allows to extract all of DM kinetic energy for DM MeV and heavier qmax = 2mXv ED & eV ↔ mX = 1 MeV ED = q2 2me ELECTRONS IN MATERIALS
Rate 1 10 100 103 10-39 10-38 10-37 10-36 10-35 10-34 Dark Matter Mass @MeVD se @cm2D Excluded by XENON10 data 1 electron 2 electrons 3 electrons Hidden- Photon models SENSEI AND SKIPPER CCD’S
▸ DAMIC utilized sensitivity to charge to place constraints on DM ▸ Fundamentally limited by noise ▸ More noise = less sensitivity to DM Whispers ▸ Improved Read-out 1 2 Charge [e−] 500 1000 1500 2000 Entries SENSEI, 1706.00028 RMS = 0.068 e/pix LDRD led by Javier Tiffenberg SENSEI AND SKIPPER CCD’S
QUANTUM DEVICE R&D
▸ In addition to suitable target (quantum phases of matter), need quantum devices capable of measuring small energy deposits ▸ Superconducting devices that measure single quanta ▸ Single infrared or microwave photon detectors, e.g. Aaron Chou LDRD R T Transition Edge Sensor calorimeter Microwave Kinetic Inductance Device See W. Wester talk DARK MATTER LANDSCAPE
mass 100 GeV 1 GeV 1 MeV 1 keV 1 eV 1 meV Traditional WIMP XENON1T LZ Semiconductors SuperCDMS Absorption Coherent Mode Production Graphene Super- conductors Superfluid Helium ~eV energy resolution ~keV energy resolution ~meV energy resolution QCD axion, “ultralight frontier” DAMIC, SENSEI ADMX E.G. SUPERCONDUCTORS
∆ ' 0.3 meV ▸ Free electrons succumb to collective dynamics ▸ Typical gap ABSORPTION — SUPERCONDUCTORS
H = Z d3yph ¯ = 1 √ V X ~ k X ~ k0 Cph| ~ Q| √⇢ 1 p 2EQ (c ~ Q + c† − ~ Q)a~ k0a~ k X Φ e e q Q k k0 X Φ e e q Q k k0 ABSORPTION — SUPERCONDUCTORS
10−4 10−3 10−2 10−1 100 101 102 mV [eV] 10−16 10−14 10−12 10−10 10−8 κ Stellar constraints (Stuckelberg case) HB stars (Higgs case, e=0.1) Resonant LC Xenon10 1 kg-day 1 kg-yr Hochberg, Lin, KZ 1604.06800 Dark Photon X Φ e e q Q k k0 x κ ABSORPTION — SEMICONDUCTORS
X Φ e e q Q k k0 10−2 10−1 100 101 102 103 104 mV [eV] 10−18 10−16 10−14 10−12 10−10 κ Stellar constraints Xenon A l , 1 k g HELIUM
▸ Superfluids are naturally insensitive to noise. A good light DM detector? In the context of ordinary nuclear recoils, yes, see e.g. 1605.00694 ▸ To detect lighter DM, couple to phonon modes. ▸ Viable? At first glance — no ▸ Next glance -- yes! ED ∼ vXq ED ∼ csq cs ⌧ vX vs HELIUM
▸ Superfluids are naturally insensitive to noise. A good light DM detector? In the context of ordinary nuclear recoils, yes, see e.g. 1605.00694 ▸ To detect lighter DM, couple to phonon modes. ▸ Viable? At first glance — no ▸ Next glance -- yes! ED ∼ vXq ED ∼ csq cs ⌧ vX vs Beauvois et al 1605.02638 MULTI-EXCITATIONS
▸ Calculated and observed for cold neutrons ▸ However, this is in a very different kinematic regime ▸ No existing calculations in regimeJ2-
'[,t;r/J"
+
i'0;p. MULTI-EXCITATIONS
▸ emit back-to-back excitations to bleed off energy while conserving momentum ▸ Quantize the fluid Hamiltonian, like SHO RESULTS
Great potential! Schutz, KZ 1604.08206 Analytic Numeric 0.01 0.1 1 10 10-44 10-43 10-42 10-41 10-40 10-39 10-38 10-37 10-36 10-35 mc @MeVêc2D sp @cm2D Sensitivity to DM via a Massive Mediator m f =1 MeV, a p =10 DARK MATTER LANDSCAPE
mass 100 GeV 1 GeV 1 MeV 1 keV 1 eV 1 meV Traditional WIMP XENON1T LZ Semiconductors SuperCDMS Absorption Coherent Mode Production Graphene Super- conductors Superfluid Helium ~eV energy resolution ~keV energy resolution ~meV energy resolution QCD axion, “ultralight frontier” DAMIC, SENSEI ADMX COMPLEMENTARITY
ROAD FORWARD
▸ Large part depends on better energy resolution sensors (TESs or KIDs); TESs or KIDs are portable to multiple targets Athermal*Phonon*Se Superconducting Substrate (Al) Insulating layer TES and QP collection antennas (W) SuperConducting Bias Rails (Al) Semiconductors SuperCDMS Current energy resolution: ~300 eV Goal: ~1 eV Superconductors Goal: ~1 meV Superfluid Helium Goal: ~1 meV ROAD FORWARD
▸ New ideas for dark matter detection! ▸ Moving beyond nuclear recoils into phases of matter crucial to access broader areas of DM parameter space ▸ Target diversity essential. graphene, superconductors, semiconductors, helium ….. Weyl semi-metal ▸ Leverage progress is materials and condensed matter physics ▸ Realizing experimental program is 5-10+ years into future ▸ Nine orders of magnitude increased sensitivity in mass ▸ Long view necessary!