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CRESST to EURECA – Progress with cryogenic dark matter searches

CRESST to EURECA – Progress with cryogenic dark matter searches. Sam Henry University of Oxford. Dark matter - Evidence. CMBR WMAP + HST:. Galactic dark matter Rotation curves of spiral galaxies Galaxy velocities within clusters. Dark matter - candidates. Neutrinos Axions

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CRESST to EURECA – Progress with cryogenic dark matter searches

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  1. CRESST to EURECA – Progress with cryogenic dark matter searches Sam Henry University of Oxford

  2. Dark matter - Evidence • CMBR • WMAP + HST: • Galactic dark matter • Rotation curves of spiral galaxies • Galaxy velocities within clusters

  3. Dark matter - candidates • Neutrinos • Axions • Gravitinos, axinos • WIMPs - Weakly Interacting Massive Particles • Supersymmetric neutralinos • Kaluza Klein particles • Alternative gravity • MOND - TeVeS Ruiz de Austri, Trotta & Roszkowski

  4. CRESST – Detectors normal-conducting Resistance [m] R T super-conducting heat bath thermal link thermometer(W-film) absorbercrystal Width of transition: ~1mKSignals: few  KStablity: ~  K Particle interaction in absorber creates a temperature rise in thermometer which is proportional to energy deposition in absorber Temperature pulse (~6keV)

  5. Phonon – Scintillation separate calorimeter as light detector W-SPT 300 g CaWO4 W-SPT light reflector Discrimination of nuclear recoils from radioactive backgrounds (electron recoils) by simultaneous measurement of phonons and scintillation light high rejection:99.7% > 15 keV99.9% > 20 keV Energy in light channel keVee] Energy in phonon channel

  6. CRESST II – Results2004 1.5 1.0 0.5 0.0 90% O-Recoils -0.5 0 50 100 150 Run28, 2004, 10.5 kg d Light/Phonon energy 90% W-Recoils Energy in Phonon Channel / keV

  7. CRESST – Results2007 Next step – install and run 17 detector modules

  8. CRESST / EDELWEISS – Results Upper Limit for Spin-independent WIMP Nucleon Cross section for cryogenic detector experiments (Preliminary)

  9. EuropeanUndergroundRareEventCalorimeterArray • Search to σ~10-10pb • (~1 event/tonne/year) • CRESST and EDELWEISS, • with additional groups joining. • Target: Ge, CaWO4, ZnWO4…. • (A dependence) • Mass: above 100 kg towards 1 tonne • Modane Laboratory

  10. EURECA challenges • Detectors • Large volume – 1000kg • Multiple target materials – Ge + scintillators • Radiopurity • Maintain background discrimination • Cryostat • Cool ~1000kg to ~10mK • Allow easy removal / insertion of detectors • Readout • 1000+ channels • Radiation shielding • Neutrons

  11. EURECA Collaboration CRESST + EDELWEISS + ROSEBUD + … France CEA/DAPNIA Saclay CEA/DRECAM Saclay CNRS/CRTBT Grenoble CNRS/CSNSM Orsay CNRS/IPNL Lyon CNRS/IAP Paris Spain Zaragoza CERN United Kingdom Oxford (H Kraus, coordinator) Germany MPI für Physik, Munich Technische Universität München Universität Tübingen Universität Karlsruhe Forschungszentrum Karlsruhe Russia DNLP Dubna Ukraine INR Kiev

  12. Dark matter detection

  13. Why use cryodetectors? Initial recoil energy Displace- ments, Vibrations Athermal phonons Ionization (~10 %) Scintillation (~1 %) Thermal phonons (Heat) Energy to extract electron in PM tube:~300eV Energy to ionize gas molecule:~30eV Energy to produce electronhole pair:3.6eV Energy to break superconducting electron pair:~meV !

  14. EDELWEISS – Detectors Target: Cyl. Ge crystal, 320 g Ø 70 mm, h = 20 mm Phonon - signal: NTD-Ge (~ 20 mK) Ionisation - signal: Inner disc / outer guard ring

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