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Direct Dark Matter Searches

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Presentation on theme: "Direct Dark Matter Searches"— Presentation transcript:

1 Direct Dark Matter Searches
Situation, Future, Strategy from a German perspective

2 Direct Dark Matter Searches
Axion Parameter Space Next Generation HDM CDM Situation, Future, Strategy from a German perspective AXIONs CAST will increase sensitivity it looks for hot DM interesting astroparticle physics this talk concentrates on WIMP DM direct detection CAST

3 Direct DM Searches σWIMP-nucleon / cm2 σWIMP-nucleon / cm2
WIMP mass / GeV σWIMP-nucleon / cm2 Present best sensitivities (for spin independent WIMP scattering) Cryogenic Liquid Xenon + other techniques (doing better for spin dependent WIMP scattering) superheated droplets anorganic scintillators … we have different techniques with promising sensitivity simultaneously LHC is starting and will march upward in mass σWIMP-nucleon / cm2 This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level. WIMP mass / GeV

4 Direct DM Searches σWIMP-nucleon / cm2 σWIMP-nucleon / cm2
WIMP mass / GeV σWIMP-nucleon / cm2 published 2000 σWIMP-nucleon / cm2 Remarkable progress x 100 improvement in sensitivity in 10 yrs a number of experiments are demonstrating sensitivities interesting from SUSY perspective This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level. WIMP mass / GeV

5 Direct DM Searches - Future
WIMP mass / GeV σWIMP-nucleon / cm2 σWIMP-nucleon / cm2 presently: results from a few kg targets coming year(s): projects prepare / run a few 10kg targets where to go: need in future ton scale targets 1 ev / kg / month 1 ev / 10 kg / year This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level. 1 ev / 1000 kg / year WIMP mass / GeV

6 Direct DM Searches - Worldwide
CRYOGENIC LIQUID NOBLE GASES DROPLETS XENON ARGON Super CDMS GeoDM US, Canada, Switzerland all prepare ~ kg, 2010 planning ~ 1000 kg, 2015 CRESST EURECA Germany, UK, Italy EDELWEISS France, Germany, UK, Russia prepare ~ kg, 2010 prepare / run ~ 100 kg, 2010 COUPP USA prepare / run a few kg good SD limits PICASSO Canada, USA, Czeck LUX 10 US institutions, Moscow WARP Italy, US XMASS 10 institutions from Japan DEAP / CLEAN Canada, US run ~30 kg, 2010 planning ~1000 kg, 2013 This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level. ArDM Switzerland, Spain, UK, Poland XENON USA, Switzerl. Italy, Japan, Portugal, Germ. France, China all prepare / plan ~ kg, 2012

7 Direct DM – next years coming year(s): (10-100) kg targets cryogenic
CRESST EDELWEISS SuperCDMS liquid noble gases Liquid Xenon XENON LUX XMASS Liquid Argon WARP droplets COUP PICASSO This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level.

8 Next Years - Germany CRESST phonon-light W, Zn, Ca, O Gran Sasso
MPI Munich, TU Munich, Tübingen Oxford, Gran Sasso phonon-light W, Zn, Ca, O Gran Sasso 2kg fiducial running goal: 15 kg nxt 2-3 yrs with diff.targets in same setup EDELWEISS KIT Karlsruhe Saclay, Orsay, Lyon, Grenoble, Dubna, Oxford phonon-charge Ge LSM 2kg fiducial running goal: 6 kg fid. in 20 kg fid. end 2011 XENON Münster, MPI Heidelberg Columbia, Rice, UCLA, Gran Sasso, Coimbra, Zürich, Subatech, Shanghai charge-light Xe Gran Sasso 50 kg fiducial starting next step will be 1t fid.

9 CDMS result – 2 events ??? .. !!! direct Dark Matter search
always entering new territory stepwise increase of sensitivity typically by x ( 3 – 10) if there have been no counts before 2 events is the best you can expect from a real signal needs confirmation: interesting year 2010 whenever Dark Matter shows up, it will start with just a few counts we will always ask for confirmation

10 Theory, a moving Target Inelastic Dark Matter CRESST most
CDMS and XENON results still leave some room to be compatible with DAMA CRESST most sensitive to inelastic DM CRESST would have ~ 1,5 events / kg day is just collecting a few 100 kg days interesting year 2010 CDMS astro_ph Sensitivity of an experiment depends on what we are looking for (on the model) keep a certain variety of experiments, techniques and targets inelastic Dark Matter (almost)* excluded * only for channeled DAMA * somewhat depending on halo model DAMA evidence CRESST CDMS Hoberg, Winkler astro_ph

11 Future - Germany where to go next five to .. yrs: 1000 kg targets
cryogenic EURECA GeoDM liquid noble gases Liquid Xenon XENON Liquid Argon WARP DEAP/CLEAN ARDM, DARKSIDE This is just a summary of what the various sensitivites mean. There are rather few events to be detected at the 10E-10 pb level.

12 Future - Germany CRESST XENON charge-light EDELWEISS EURECA
MPI Munich, TU Munich, Tübingen Oxford phonon-light W, Zn, Ca, O LSM 2kg fiducial running goal: 15 kg nxt 2-3 yrs XENON Münster, MPI Heidelberg Columbia, Rice, UCLA, Gran Sasso, Coimbra, Zürich, Subatech, Shanghai charge-light Xe Gran Sasso 50 kg fiducial starting goal: 100kg /12 EDELWEISS KIT Karlsruhe Saclay, Orsay, Lyon, Grenoble, Dubna, Oxford EURECA MPI Munich, TU Munich, KIT Karlsruhe, Uni Tübingen, Oxford, Sheffield, Saclay, Orsay, Grenoble, Lyon, Dubna, Kiev, Zaragoza phonon-charge/light Ge, W, Zn, Ca, O LSM goal: 1000kg XENON Münster, MPI Heidelberg Columbia, Rice, UCLA, Gran Sasso, Coimbra, Zürich, Subatech, Shanghai phonon-charge Ge LSM 2kg fiducial running goal: 9kg in 2010 charge-light Xe Gran Sasso goal: start 1000kg 2013

13 Xenon XENON 100 + at Gran Sasso 50 kg fiducial / 170 kg total funded
USA, Switzerland, Italy, Portugal, Germany, France, Japan, China XENON 100 + at Gran Sasso 50 kg fiducial / 170 kg total funded starting end of 2009 projected 2010: ~ 2 x cm2 projected 2012: ~ 2 x cm2 XENON 1t projected 2013: 1000 kg target < cm2 at Gran Sasso or LSM

14 Possible EURECA Facility Layout
Germany, France, UK, Spain, Russia, Ukraine combines all European cryogenic DM efforts: R&D cooperation with CDMS/GeoDM Existing laboratory 2009/10: design study => TDR 2011/12: LSM excavation + construction EURECA components ~ 100 kg fiducal target at present sites, ~ cm2 2013/14: construction at LSM 2015: begin data taking at LSM 2015 – 2018: continuous upgrade to 1t target ~ cm2 New LSM extension Possible EURECA Facility Layout

15 Strategy – Direct DM Search
large potential in the coming years SuSy DM might be discovered soon even if not, experiments will strongly restrict SuSy models pursuing the two promising techniques liquid nobel gas and cryogenic to establish a signal with confidence to show consistency between different nuclei and techniques Germany is very well placed activities in both liquid nobel gas and cryogencis expertise in essential issues: cryodetectors, (gas)purity

16 Strategy – Direct DM Search
Germany is very well placed activities in both liquid nobel gas and cryogencis expertise in essential issues: cryodetectors, (gas)purity cooperation within the whole community e.g. cooperation cryogenics liquid noble gas planned in the continuation of DFG-TR27 ‘Neutrinos and Beyond‘ projects will need invest when starting in coming years

17 ASPERA Common Call common call of European funding agencies
for Gamma Astronomy and Dark Matter Searches German groups are partners in two Dark Matter proposals liquid noble gases DARWIN Heidelberg Karlsruhe Münster cryogenics EURECA Munich Karlsruhe Tübingen both studies funded, without Germany now design study activties without German participation is this the signal Germany wants to give ?

18 Strategy – Direct DM Search
pursuing the two promising techniques liquid nobel gas and cryogenic to establish a signal with confidence to show consistency between different nuclei and techniques Germany is very well placed activities in both liquid nobel gas and cryogencis expertise in essential issues: cryodetectors, (gas)purity never give up a competetive level of R & D be prepared to fight new backgrounds you might find new territory eventually we need directional detectors, to observe diurnal modulation in 10 years, we probably know what Dark Matter is (direct, indirect, LHC)

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