UZ Dark Matter Searches at Canfranc María Luisa Sarsa Universidad de Zaragoza Laboratorio Subterráneo de Canfranc Experimental observations and well founded arguments Hubble Space Telescope Image of Abell 2218 June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The Universe seems to be mostly DARK Experimental observations and well founded arguments Ω~1 Dark energy 73% Baryonic Dark Matter (3.5%) Visible (0.5%) Non-Baryonic Dark Matter 23 % Weakly Interacting Massive Particles WIMPs Direct Detection of WIMPs vmax d σ ρχ dN W,local WIMP 3 elastic = Nn f(v) v d v ∫ vmin dT dt dT mW scattering off target nuclei 2 W Mm 2 T= v (1 - cosθ ) 2 (M + mW ) Nuclear Recoil energy June 24th 2006 M.L. Sarsa 9 Halo model 9 WIMP model 9 Detector properties Canfranc Underground Laboratory Direct Detection of WIMPs χ Energy conversion into visible signal is very different depending on the detection mechanism and particle type CHARGE + + + - + -+ LIGHT HEAT Nuclear Recoil energy June 24th 2006 M.L. Sarsa Conventional vs hybrid detection Canfranc Underground Laboratory Direct Detection of WIMPs ρ W,local dN = Nn dt dT mW ∫ vmax vmin dσ 3 f(v) v d v dT T = E/REF Evts/ keV/ kg/ day/ pb REF for nuclear recoils 9semiconductors REF= 1. ~ 0.25-0.3 REF= 0.25 9scintillators ~ m = 100 GeV 0.05-0.5 Ge 9bolometers ~ 1. Visible energy (keV) (keVee) w June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory General strategy for DD • Very low energy threshold • Very low background – intrinsic and induced radioactivity: very low – environmental: located in underground laboratories, in a radiopure environment: active / passive shieldings – capabilities to discriminate the signal from the background (hybrid detectors) • Large detector mass (to increase the probability of detection) • Good stability and control of systematics June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Discriminating signal from background NUCLEAR VS. ELECTRONIC RECOILS DISCRIMINATION NEUTRONS REMAIN AS THE MAIN BACKGROUND SOURCE And then… –Annual modulation in the signal –Combination of several targets in the same experimental set-up –Tracking the nuclear recoil energy deposition: directionality June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Annual modulation of the signal B + S + S cos[ω(t − t )] α=60° V๏=232 Km/s Sun 0 m 0 Count rate difference from the average (counts per day per kg per keV) Earth 107731 Kg day Vorb=30 Km/s A = (0.0200+/-0.0032) counts per keV/kg/day to= (140+/-22) d T= (1.00+/-0.01) y Time (day) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory General Strategy for DM Direct Detection To combine as much information as available/possible to decouple unknowns/uncertainties – Different targets – Different techniques of detection – Different signatures June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Dark Matter Search Program at CANFRANC 1990-2006 2006June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The Canfranc Underground Laboratory Under the spanish Pyrenees In the old railway Somport Tunnel June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The Canfranc Underground Laboratory Since 1985, research has been carried out about: Direct WIMP search √ Double beta decay √ Other “rare” processes √ Radiopurity measurements √ June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The Canfranc Underground Laboratory 1985 first visits to the Somport Tunnel First Canfranc Underground Facility 1989, Mounting ββ/γ June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The Canfranc Underground Laboratory ~100 m2 ~10 m2 2450 m.w.e. June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The NEW Canfranc Underground Laboratory Facilities ≈600 m2 ≈100 m2 June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory The NEW Canfranc Underground Laboratory Facilities June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Site Baksan (Russia) Bern (Switzerland) Boulby (UK) Canfranc (Spain) Frejus (France) Gran Sasso (Italy) Otto-Cosmo (Japan) Rustrel (France) Stanford (USA) Soudan (USA) SNO (Canada) Expe rim ent IGEX ORPHEUS NaI NaIAD ZEPLIN I ZEPLIN II/III ZEPLIN-MAX DRIFT-I DRIFT-10 COSME IGEX ANAIS ROSEBUD Saclay-NaI EDELWEISS I EDELWEISS II Hdlberg/Mscw HDMS Genius DAMA LIBRA Xenon CRESST-I CRESST-II CUORICINO CUORE Elegants V Elegants VI SIMPLE CDMS-1 CDMS-II PICASSO Tec hnique Ionisation SSD Scintillator Scintillator Scintillator Scintillator/Ionisation Scintillator/Ionisation TPC TPC Ionisation Ionisation Scintillator Thermal Scintillation Thermal/Ionisation Thermal/Ionisation Ionisation Ionisation Ionisation Scintillation Scintillation Scintillation Thermal Thermal/Scintillation Thermal Thermal Scintillation Scintillation SDD Thermal/Ionisation Thermal/Ionisation SDD Target 3kg Ge 0.5kg Sn 5kg NaI 50kg NaI 5kg Lxe 30kg/7kg Xe 1000kg Xe 0.2kg CS2 2kg CS2 0.2kg Ge 2.1kg Ge 107kg NaI Al2O3,Ge,CaWO4 10kg NaI 0.07kg Ge 1.3 kg Ge 2.7kg Ge 0.2kg Ge 100kg Ge 100kg NaI 250kg NaI 6kg Xe 1kg Al2O3 10kg CaWO 4 40kg TeO2 760kg TeO2 NaI CaF2 Freon 0.1kg Si, 1kg Ge 0.3ks Si, 0.75kg Ge 1g Freon Stat u s Operational Operational Completed Operational Operational Construction Planned Operational Planned Completed Operational Constrcution Operational Completed Completed Operational Completed Operational Planned Operational Construction Operational Oprational Construction Construction Planned Operational Operational Operational Completed Construction Operational M.L. Sarsa Canfranc Underground Laboratory APPEC Peer Review Committee, C. Spiering June 24th 2006 Ionization COSME, IGEX-DM Ge U. Zaragoza / South Carolina / PNNL / INR / ITEP Collaboration CANFRANC EXPERIMENTS WIMP detection techniques June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory WIMP searches with Ge • Ultrahigh purity material: very low background levels • Low energy threshold • Reasonable quenching factor: Evisible≅0.25 Erecoil • Medium size, A~70 • For spin-independent coupling no enrichment needed June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory COSME Experiment E. García, A. Morales, J. Morales, A. Ortiz de Solórzano, J. Puimedón, C. Sáenz, A. Salinas, M. L. Sarsa, J. A. Villar University of Zaragoza F.T. Avignone III, .I. Collar University of South Caroline, USA R. L. Brodzinski, W.K. Hensley, H.S. Miley, J.H. Reeves Pacific Northwest National Laboratory, USA COSME Counts//keV/kg/day Counts 234 g natural Germanium Search for WIMPs and solar axions Low energy threshold 1,6 keVee June 24th 2006 PNL/ USC/ UZ 1990 - 1992 COSME 92 / COSME 98 130, 7 kgd / 72, 8 kgd Phys. Rev. D 51 (1995) 1458 M.L. Sarsa Canfranc Underground Laboratory IGEX Collaboration S. Cebrián, E. García, D. González, I. G. Irastorza, A. Morales, J. Morales, A. Ortiz de Solórzano, J. Puimedón, A. Salinas, M. L. Sarsa, J. A. Villar University of Zaragoza C. Aalseth, F.T. Avignone III, .I. Collar University of South Caroline, USA R. L. Brodzinski, W.K. Hensley, H.S. Miley, J.H. Reeves Pacific Northwest National Laboratory, USA A.A. Klimenko, S.B. Osetrov, A.A. Smolnikov, A.A. Vasenko, S.I. Vasiliev Institute for Nuclear Research, INR, Baksan I.V. Kirpichnikov Institute for Theoretical and Experimental Physics, ITEP, Moscow V.S. Pogosov, A.S. Starostin, A.G. Tamanyan, Yerevan Physics Institute IGEX ββ IGEX Collaboration searched for 76Ge double beta decay with enriched detectors (86%) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory IGEX-DM ƒ IGEX-DM used one detector (2.1 kg) ƒ An improved neutron shielding allowed a significant reduction of background at low energies archaeological lead side 60 cm 2.5 tons Low activity lead side 100 cm 10 tons Plastic scintillator PVC bags with N2 Cadmium layer 2 mm Polyethylene / borated water June 24th 2006 M.L. Sarsa RG-II detector Canfranc Underground Laboratory IGEX-DM 1.0 0.9 0.8 counts/keV/kg/day 194 kg-days with 40 cm neutron shielding BACKGROUND 4-10 keV background: 0.22 c/keV/kg/day 10-20 keV background: 0.10 c/keV/kg/day 25-40 keV background: 0.04 c/keV/kg/day 82 kg-days with 80 cm neutron shielding 0.7 0.6 0.5 4 keVee threshold 0.4 -6 10 0.3 IGEX-DM (2000) 0.1 0.0 0 10 20 30 Energy (keV) 40 50 σn (nbarn) 0.2 -7 10 IGEX-DM IGEX-DM (2001&2002) 2001-2002 - -8 10 Astrop. Phys. 20 (2003) 247 Astrop. Phys. 21 (2004) 523 -9 Phys. Lett. B 532 (2002) 8 10 1 10 100 1000 Phys. Lett. B 489 (2000) 268 M (GeV) M.L. Sarsa Canfranc Underground Laboratory June 24 2006 W th Light Ionization COSME, IGEX-DM Ge U. Zaragoza / South Carolina / PNNL / INR / ITEP Collaboration DM32, ANAIS NaI U. Zaragoza CANFRANC EXPERIMENTS WIMP detection techniques June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory WIMP searches with NaI scintillators • 100% nuclei with non-zero spin: 23Na (J=3/2) 127I (J=5/2) • Heavy+light nuclei, A=127 & 23 • Easy scale up to large mass • Pulse shape discrimination (PSD) capability • Small quenching factor (Q<10%) for I, and medium for Na (Q~30-40%) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory NaI Scintillators at Canfranc 14 detectors, used in previous experiments, underground since 1988 PMT EMI9765 quartz window stainless steel vessel 0.5 mm 1.27 cm 7.62 cm 23.3 cm crystal 10.7 kg NaI (Tl) June 24th 2006 M.L. Sarsa 20.32 cm Canfranc Underground Laboratory NaI32 Experiment E. García, A. Morales, J. Morales, A. Ortiz de Solórzano, J. Puimedón, C. Sáenz, A. Salinas, M. L. Sarsa, J. A. Villar University of Zaragoza NaI32 (3x10,7 kg NaI, LSC) looking for the modulation effect annual carried out in the Canfranc Underground Laboratory from 1993 to 1995 Mt=4614 kg.day Phys. Lett. B 386 (1996) 458 Phys. Rev. D 56 (1997) 1856 June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory ANAIS experiment J. Amaré, B. Beltrán, J. M. Carmona, S. Cebrián, E. García, H. Gómez, I. G. Irastorza, G. Luzón, M. Martínez, J. Morales, A. Ortiz de Solórzano, C. Pobes, J. Puimedón, A. Rodríguez, J. Ruz, M. L. Sarsa, L. Torres, J. A. Villar University of Zaragoza ANAIS PROJECT 10 x 10.7 kg NaI dark matter search experiment looking for annual 40 cm neutron shielding modulation Active vetos To be installed at the new Canfranc Underground Laboratory 20 cm lead PVC box 2 mm Cd 10 cm Roman lead June 24th 2006 M.L. Sarsa Vibration isolator Canfranc Underground Laboratory PROTOTYPE I 10.7 kg NaI PSD discrimination to reject PMT noise: lowering threshold 2069.85 kg day Nucl. Phys. B (PS) 114 (2003) 111 IMPROVED PROTOTYPE I Understanding and improvement of background June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Counts/keV/kg/day IMPROVED PROTOTYPE I Background from PMT PMT9302 PMT9765 OpticGuide 1460keV 10 2614keV 1 0.1 0 400 800 1200 1600 2000 2400 2800 Energy (keV) EMI9302 210Pb Counts/keV/kg/day EMI9765 + x-Rays Pb 10 PMT9302 PMT9765 OpticGuide 1 0 100 200 300 400 500 Energy (keV) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory IMPROVED PROTOTYPE I 210Pb + x-Rays Pb β 210Bi (Qβ=1161.5keV) + β 40K (Qβ=1312.1keV) Counts/keV/kg/day 10 40K 208Tl + α’s 1 0.1 0 400 800 1200 1600 2000 2400 2800 Energy/keV June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II (2003-) • Removal of the old PMT and steel vessel • Coupling to 2 ultra-low background PMT + light guides Nake crystal – Anticoincidence – Light collection efficiency – Background improvement • Selection of high purity materials in Canfranc using a Ge detector – Background improvement June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II NaI Light guides 10.7 kg NaI Flexible set-up Test reflector/diffusor materials and thickness Optimal light guides length June 24th 2006 M.L. Sarsa PMTs Teflon bank Canfranc Underground Laboratory Light collection results 30 % collection variation 25 20 1 cm teflon 9 Teflon thickness slightly increases light collection 15 1.5 cm teflon 10 5 2 cm teflon 0 1 cm teflon+ external reflectant -5 -10 reflectant -15 -20 0 2 4 6 8 10 12 14 16 18 20 22 Distance LED-PMT (cm) 9 Reflectant improves light collection ~20% 9 Reflectant decreases positional dependency of light collection Teflon Reflectant 2200 2000 Collected light (a.u.) 1800 1600 9 We lose ~10% light every 5 cm optical guide 1400 1200 1000 800 600 400 200 0 0 5 10 Guide Length (cm) June 24th 2006 M.L. Sarsa 15 20 Canfranc Underground Laboratory STRIPPING THE CRYSTAL COUPLING PROTOTYPE II June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II: Canfranc measurements 10 cm archeological lead Anti-radon PVC box 10 cm lead June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II: Canfranc measurements 232Th contamination! 238.6 keV 338.3 keV Counts/keV/kg/day 10 583keV Improved Prototype I Prototype II 2614keV Identified at the weldings of the copper box GTAW 911keV 1 0.1 0 400 800 1200 1600 2000 2400 2800 3200 Energy/keV June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II: Noise rejection Trigger at photoelectron level implies noise in coincidence Cuts applied down to 2 keV 57Co calibration Background PROTOTYPE II: Canfranc measurements 2 cm Copper Inner Cu shielding Noise rejection MLS Diapositiva 45 MLS7 Comparar el fondo con Cobre con el fondo antes de colocar el cobre María Luisa Sarsa; 08/ 06/ 2006 PROTOTYPE II: PSD for α discrimination α β+γ V (t ) = ( − QR −t /τ s − e −t / τ r e τ r −τ s June 24th 2006 ) M.L. Sarsa Canfranc Underground Laboratory PROTOTYPE II: PSD for α discrimination PROTOTYPE II: PSD for α discrimination Contamination (mBq/kg) Parent Isotope PII EP-058 238U 0,017 ± 0,007 - 226Ra 0,14 ± 0,01 0,22 ± 0,05 210Pb 1,2 ± 0,1 0,54 ± 0,12 232Th 0,027 ± 0,007 - 228Ra 0,07 ± 0,02 0,021 ± 0,006 PROTOTYPE II: PSD for α discrimination GEANT-4 Simulation of internal U-Th-Pb-K 40K has been assumed to be completely of internal origen Background Understanding Low Energy calibration 137Cs 55Fe 57Co Low Energy calibration Aprox. linear behaviour down to 14.4 keV 6 keV line from 55Fe at lower energies than extrapolation Superficial effects can be responsible New NaI(Tl) 9,6 kg crystal Last week mounting in Canfra June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Design of a new encapsulation OFHC copper tighly sealed Teflon diffusive layer Quartz optical windows June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Exclusion plots in different scenarios without modulation search (90%CL) 2-8 keV energy window 5x107 kg.yr exposure 1 c/keV/kg/d 5x107 kg.yr exposure Expected sensitivity for a dark matter modulated signal in different scenarios (δ2=5.6, Astrop. Phys. 14 (2001) 339) 2-8 keV energy window 5x107 kg.yr 1 c/keV/kg/d 5x107 kg.yr ANAIS PROSPECTS -New copper encapsulation in preparation - 9,6 kg radiopure crystal to be tested in the PROTOTYPE II set up (taking data) - PMT tests (background and response) -Alpha PSD measurements to select the best crystals among available -Main limitation seem to come from internal contaminants: 40K requires more study -2 keVee threshold achieved (further calibration) - Optimized shielding conditions in the new LSC for Prototype III Light Ionization COSME, IGEX-DM Ge U. Zaragoza / South Carolina / PNNL / INR / ITEP Collaboration DM32, ANAIS NaI U. Zaragoza CANFRANC EXPERIMENTS WIMP detection techniques Al2O3 Ge U. Zaragoza / IAS Orsay Collaboration June 24th 2006 M.L. Sarsa Light+Heat Heat ROSEBUD-I / II TPC MICROMEGAS ROSEBUD-II / III CaWO4 BGO Al2O3 U. Zaragoza / IAS Orsay Collaboration Canfranc Underground Laboratory Bolometric detection Thermal Bath Thermal coupling Thermometer WIMP Phonons ΔE=Trecoil ΔE ΔT ≅ C June 24th 2006 ⎧⎪ C = α T3 ⎨ ⎪⎩C = α T3 + β T M.L. Sarsa Resistencia ( mΩ) Absorber ΔR 10 μK/ keV estabilidad ~ 1μK ΔT Temperatura (mK) Canfranc Underground Laboratory WIMP searches with bolometers • Wide absorber choice • Quenching factors seem to be compatible with 1 • Very low energy thresholds • Discrimination capabilities event by event increase dramatically sensitivity: – CHARGE VS HEAT / LIGHT VS HEAT • Large mass experiments in preparation: feasible June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory ROSEBUD Collaboration Rare Objects SEarch with Bolometers UnDerground J. Amaré, B. Beltrán, J. M. Carmona, S. Cebrián, E. García, H. Gómez, I. G. Irastorza, G. Luzón, M. Martínez, J. Morales, A. Ortiz de Solórzano, C. Pobes, J. Puimedón, A. Rodríguez, J. Ruz, M. L. Sarsa, L. Torres, J. A. Villar University of Zaragoza N. Coron, G. Dambier, J. Leblanc, P. de Marcillac, T. Redon Institute d’Astrophysique Spatiale, ORSAY ROSEBUD Since 1997 Devoted to the search for galactic halo WIMPs at LSC with bolometric techniques 20mK •Phase I (1999-2000): Al2O3 (25 g and 50g) 3Understanding and reduction of the background Astrop. Phys. 15 (2001) 79 June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory ROSEBUD Phase II (since 2000): Al2O3 (50 g), Ge (67 g), CaWO4 (54 g) + Ge (optical bolometer) in the same experimental setup 3First light vs heat discrimination technique implemented deep underground Phys. Lett. B 563 (2003) 48 3First low background experiment using 3 different absorbers in the same set-up (to explore target dependence of the DM signal) Astrop. Phys. 21 (2004) 23 June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Background discrimination: light vs heat 1400 Light Gamma event 1200 1000 800 600 400 200 0 -200 -400 0 500 1000 1500 2000 2500 3000 3500 4000 4500 5000 Neutron Neutron event event 4000 3000 2000 1000 0 -1000 0 500 1000 1500 2000 2500 3000 3500 4000 4500 Heat June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory ROSEBUD phase II: CaWO4 Elight (keV) 252Cf calibration @ IAS Orsay β+γ neutrons β+γ Eheat (keV) Background @ Canfranc T=24,2h M=54g Counts/(keV kg day) 1000 100 n/ recoils 10 1 50 100 150 200 250 Energy (keV) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Results and Prospects A. Morales et al. , Phys. Lett. B 556 (2003) 14 D. Abrams, et al. , Phys. Rev. D 66 (2002) 122003 A. Benoit et al. , Phys. Lett. B 545 (2002) 43 10 kg.day CaWO4 10 keV threshold zero nuclear-recoil events June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory On the search for new scintillating materials (IAS) Scintillation at 20 mK detected for: – Crystals: YAP:Ce, GSO:Ce, CaF2:Eu, Al2O3:Ti – Bolometers: CaWO4, BGO, LiF, TeO2, Al2O3 , SrF2, SiO2 Al O bolometers (25, 50 g) 2 3 BGO – (91 g) and Ge light detector (Ø= 25 mm) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Next DM run at LSC: BGO and Al2O3 Sapphire (Al3O2) promising candidate to explore low WIMP masses Eth for particle discrimination C.L (1 tailed) 90 % 95 % 99 % 99.9 % 99.99 % June 24th 2006 M.L. Sarsa E (keV) 8.7 10.0 13.0 17.1 21.3 Canfranc Underground Laboratory Light signal amplitude (mV) Light yield of undoped sapphire at 20 mK 57Co + 241Am Applied Physics Letters 87 (2005) Heat signal amplitude (mV) Absolute mean light yield estimate of sapphire June 24th 2006 β/γ 0.127 ± 0.010 α n 0.012 ± 0.005 M.L. Sarsa 0.0073 ± 0.0010 Canfranc Underground Laboratory Heat signal REF in sapphire External 210Po source emitting α particles and 206Pb recoils 206Pb PRELIMINARY June 24th 2006 M.L. Sarsa recoil REF (γ : 206Pb recoils) 1.0 Canfranc Underground Laboratory Superficial effects in sapphire 109Cd+57Co Ee = 62.5 keV Ee = 84 keV Ee = 87 keV 60 keV 81.7 keV Self-degradation in the source (unclean) is discarded by calibration on Cu bolometer June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Next DM run at LSC: BGO and Al2O3 BGO (Bi4Ge3O12): Interest for WIMP searches: 209Bi ↑A ⇒ ↑σSI ; J = 9/2 ⇒ ↑σSD • Relative light output factor : Q (recoils : α : γ / β ) = 1 : 2.6 : 15 • Particle discrimination threshold: ƒ90% CL at E > 23 keV ƒ99.99% CL at E > 51 keV June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Prospects • Dark matter run at LSC using BGO and sapphire bolometers as absorbers. Goal 15 keV for BGO and 10 keV for sapphire recoil discrimination energy threshold. • Collaboration with the University of Lisbon for using a dilution unit able to house larger mass bolometers (terms being discussed) • Incorporation to the Cryogenic Dark Matter Search European Project EURECA (application under study) June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory Summary • Searches for Dark Matter at the Canfranc Underground Laboratory are going on since 1990 – Different techniques and targets • ANAIS and ROSEBUD experiments will be installed at the new Canfranc facilites June 24th 2006 M.L. Sarsa Canfranc Underground Laboratory