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Astroparticle Physics

Astroparticle Physics. The European Strategy. Christian Spiering, DESY XIII Workshop Neutrino Telescopes Venice, March 11, 2009. ApPEC and ASPERA. ApPEC. Founded 2001. Steering Committee and Physics Review Committee Promote cooperation within European APP community

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Astroparticle Physics

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  1. Astroparticle Physics The European Strategy Christian Spiering, DESY XIII Workshop Neutrino Telescopes Venice, March 11, 2009

  2. ApPEC and ASPERA ApPEC Founded 2001 • Steering Committee and Physics Review Committee • Promote cooperationwithin European APP community • Develop long term strategies for European APP, offering advice to national funding agencies and EU • Improve links and coordination between European APP and the scientific programmes of organisations like CERN, ESA, and ESO • Express views on APP in international forums, such as OECD, UNESCO etc. ASPERA Launched 2006 • The ERA-Net of Astroparticle Physics • Funded by EU FP6 (2.5 M€/3yr from July 2006) • Phase 2 recently approved (July 2009 – 2012) • Coordination with ASTRONET (the ERA-Net of astronomers) and also CERN strategy bodies • Roadmap for APP in Europe 14 countries +CERN 14 countries +CERN

  3. Phases of Roadmapping 1 • science case • status: overview • recommendations for convergence 2 • Critical assessment of plans • Calendar for milestones and decisions • Input for ESFRI Roadmap • Coordinated with ASTRONET (Long write-up with detailed data and arguments in work)

  4. ASPERA Roadmap Long Write-Up Deliverables and Plans to be completed ASPERA Common Call 2009: CTA & Dark Matter Experiments

  5. The Magnificient Seven Einstein Telescope (LISA) Megaton Ton-scale Double Beta Auger-Nord Ton-scale Dark Matter KM3NeT CTA

  6. Dark Matter and Dark Energy Searches

  7. Dark Matter Searches 10-4 10-6 Cross section (pb) 10-8 - Background - Funding / Infrastructure 10-10 1985 1990 1995 2000 2005 2010 2015

  8. 10-4 10-6 We are now here Cross section (pb) • - Background • Funding • Infrastructure 10-8 10-10 1980 1985 1990 1995 2000 2005 2010 2015

  9. Dark Matter Searches Towards 2 ton-scale zero-background detectors Now: 10 kg scale 2009/11: 100 kg scale 2011-17: constr. ton scale CRESST EURECA @ ton scale EURECA-100 Edelweiss modular expansion LXe XENON/LUX, WARP LXe ELIXIR, .. Xe-100 Noble liquid @ ton scale LAr Ar-100 LAr a possible convergence scenario, slide CS from 1½ year ago. …

  10. 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Dark Matter Searches now 100 kg scale ton scale operation ZEPLIN-II operation ZEPLIN-III construction operation CUORE LUX/ZEPLIN construction operation XENON liquid xenon operation XENON-100 construction operation XENON-1Ton CUORE construction operation WARP operation WARP-140 construction liquid argon Tests ArDM Noble liquid detectors with European participation

  11. Dark Matter Searches • Support current round of experiments at high priority, also technology development towards their next-generation versions • A recommendation on which of the technologies should first move to a next stage can only be made after first results from present experiments with 10-100 kg target mass become available and after noise rejection and sensitivity/cost ratio for ton-scale detectors can be judged on a more realistic basis. • This milestone can be reached by 2010 or 2011. • As soon as one of the technologies turns out to be clearly superior insensitivity, cost, and timing  Promote it with priority! At the same time, a second technology must be systematically prepared since a possible positive observation by the first method would call for a prompt, independent confirmation. • In an ideal scenario, LHC observations of new particles at the weak scale could place these observations in a well-confined particle physics context. Also, direct detection would be supported by indirect signatures. In case of a discovery, “smoking-gun signatures” of direct detection such as directionality and annual variations would be measured in detail.

  12. Dark Energy • Particle physicists engaged since the beginning. • Construction of future instruments depends on choices beyond the single authority of the agencies charting this roadmap. ASTRONET Roadmap. • Examples (> 2013): • Implications for fundamental physics are profound. Therefore, strongest support for DE missions from APP community. EUCLID LSST

  13. Properties of Neutrinos

  14. Properties of Neutrinos • Direct Mass Measurements • KATRIN, start 2012, down to 0.2 eV • Troitzk (Russia) start 2009, down to 0.8 eV • Double Beta Decay Experiments • Cuoricino, Nemo-3 • Gerda, Cuore, Super-Nemo • EXO, SNO+ • Cobra, NEXT, …. • Mixing Parameters • Double CHOOZ • T2K • experiments with CERN beam (Opera, ICARUS, .MODULAR, .. )

  15. KKGH claim GERDA, EXO200, SNO+ CUORE, SuperNEMO Ton-scale Double Beta Decay Price tag for ton-scale 50-200 M€.

  16. now 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Double Beta Decay operation bolometric 41 kg 130Te CUORICINO operation construction CUORE bolometric 740 kg 130Te operation tracking 8 kg 130Mo/82Se NEMO-3 operation Super-NEMO design study construction tracking 100 kg 150Nd/82Se operation construction GERDA 18  40 kg 76Ge operation EXO (USA) 200 kg 130Xe design study construction (Projects running, under construction or with substantial R&D funding)

  17. 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Double Beta Decay now operation bolometric 41 kg 130Te CUORICINO operation CUORE construction bolometric 740 kg 130Te operation tracking 8 kg 130Mo/82Se NEMO-3 oper Super-NEMO design study construction tracking 100 kg 150Nd/82Se operation GERDA construction 18  40 kg 76Ge operation EXO (USA) 200 kg 130Xe design study Construct. (Projects running, under construction or with substantial R&D funding)

  18. now 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Double Beta Decay operation + R&D Cobra, NEXT, ,… CUORICINO operation CUORE construction operation NEMO-3 oper Super-NEMO design study construction operation GERDA construction operation EXO (USA) design study Construct. operation SNO+ (Canada)

  19. Double Beta Decay • Priority to experiments starting operation within 5 years • GERDA (phase I and II) • CUORE • Super-NEMO • Complementary nuclei/methods essential to judge any positive claim or upper limit. • Will scrutinize the claimed evidence in 76Ge, will touch the “inverted hierarchy” mass range and keep European leadership. • Other methods may become competitive in the future. • At the same time, envisage an experiment on the 1-ton-isotope scale, which will peer deep into the inverted hierarchy range. Two options discussed, both with worldwide cost sharing: • GERDA III as merger of GERDA with Majorana (USA) • CUORE with enriched tellurium, USA participation. • Milestone: Decision on the isotopes/ techniques 2012/13.

  20. Low Energy Neutrino Astronomy and Proton Decay

  21. Neutrino Astrophysics & p-decay • Super-Kamiokande KAMLand • Borexino, LVD • SAGE, Baksan • ICARUS,SNO+, …. • 10-kt scale (non-H2O) • Modular + other osc.- motivated detectors • Baksan scintill. • Megaton scale • Europe • USA • East Asia

  22. LAGUNA FP7 design study MEMPHYS 700 kton water LENA 50 kt scintillator 50 m GLACIER 100 kton liquid argon

  23. Science at the Megaton scale • Proton decay: improve sensitivity by > factor 10 and test a new class of Supersymmetry models • Galactic Supernova: 104- 105 events Incredibly detailed information on the early SN phase • Diffuse flux from past SN: probe cosmological star formation rate • Solar neutrinos: details of the Standard Solar Model determined with percent accuracy • Atmospheric neutrinos: high statistics would improve knowledge neutrino mixing and provide unique information on the neutrino mass hierarchy • Geo-neutrinos: improve understanding of the Earth interior • Indirect WIMP search • Neutrinos accelerators over a long baseline (also with dedicated smaller detectors): neutrino properties

  24. Neutrino Astrophysics & p-decay • LAGUNA: assess discovery potential of different options and sites and then converge to a common proposal in ~ 2010. • Neccessity of a coherent approach with efforts in the USA and Japan is obvious. Worldwide coordination and cost sharing (in total 250-800 M€ per detector) • Recommendation: We recommend supporting the work towards a large infrastructure for proton decay and low energy neutrino astronomy, possibly also accelerator neutrinos in long baseline experiments, in a worldwide context. Results of the LAGUNA FP7 design study are expected around 2010 and should be followed by work towards a technical design report. Depending on technology, site and worldwide cost sharing, construction could start between 2012 and 2015. • Input from BOREXINO (liquid scintillator) and ICARUS-T600 (liquid argon), DoubleChooz and T2K. Proposals for dedicated liquid argon detectors, e.g. MODULAR at Gran Sasso.

  25. The High Energy Universe

  26. Charged Cosmic Rays

  27. Charged Cosmic Rays antimatter, dark matter, mass composition primary mass composition galactic sources mass composition galactic  extragalactic CR astronomy, GZK physics, HE neutrinos, …

  28. 107 Exposure (km² sr year) JEM-EUSO (space) Auger-N 106 similar: TUS 105 Auger-S HiRes 104 AGASa Telescope Array Fly‘s eye 103 102 1985 1990 1995 2000 2005 2010 2015 2020 2025 2030 year Charged Cosmic Rays AGASA Auger North TA Auger South

  29. Charged Cosmic Rays • The case for “Auger-North” is strong: high statistics astronomy with reasonably fast data collection calls for a substantially larger array than Auger South, full sky coverage calls for a Northern site. A larger array would also allow a more detailed inspection of the high energy cut-off of the particle spectrum, which recently has been firmly established by Auger-South. • Recommendation:The priority project for high energy cosmic ray physics is Auger. We encourage the agencies in different continents to work towards a common path for Auger-North. We recommend the construction of such a large array as soon as worldwide agreements allow.

  30. High Energy Gamma Rays • Enormous progress over last 15 years • Mostly by Imaging Atmospheric Cherenkov Telescopes (IACT) • Whipple • HEGRA, CAT, Cangaroo • HESS, MAGIC, VERITAS • Wide Angle Devices • MILAGRO  HAWC • Argo/YBJ • GAW (R&D) • Future • Fermi + IACTs + WADs

  31. now 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Existing Air Cherenkov Telescopes operation H.E.S.S. four 11-m telescopes operation + one 25-m telescope H.E.S.S.- II construction operation MAGIC-I one 17-m telescope operation 2nd 17-m telescope MAGIC- II construction operation Cangaroo 4 telescopes, Australia operation Whipple 1 telescope, monitoring regime operation Veritas four 12 m telescopes constr

  32. now 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 Future Air Cherenkov Telescopes operation India 4200 m altitude > 20 GeV construction MACE-1 21 m telescope (10 M$, funded) operation construction MACE-2 2nd 21 m operation „Gamma Air Watch“ Wide angle, Fresnel lense (IT, PT, ES) GAW R&D, prototype, constr. Oper. design, prototypes construction + operation CTA Europe, Japan, … 2 arrays, 1 South 1 North Joining !? Plus possible small „monitoring“ telescopes wordwide. AGIS USA

  33. High Energy Gamma Rays • HESS/VERITAS, MAGIC, Whipple, CTA sensitivity in 50 hours, (~0.2 sr/year) • GLAST sensitivity in 1 year (4 sr) • HAWC sensitivity in 1(5) years shown as solid (dashed) line (2 sr)

  34. Startup meeting FP7 proposal Array layout Consortium Components Telescopes Array construction Science operation VERITAS Fermi H.E.S.S. II Japan will join CTA Close collaboration with AGIS (USA) MAGIC II

  35. High Energy Gamma Rays • From “experiment” to “observatory” • 10-fold improvement of sensitivity, extension of energy range, significant improvement in resolution • Expect ~ 1000 sources, explore spatial structure and energy spectra. • Ultimately, a Northern and a Southern CTA instrument, operated under a common framework, should provide full-sky coverage. • Overlap with Fermi provides seamless coverage of 20 octaves • Coordination with AGIS (USA) underway. CTA on the ESFRI list . Also listed as a priority entry in the ASTRONET infrastructure roadmap. • Recommendation:The priority project of VHE gamma astrophysics is CTA. We recommend design and prototyping of CTA and selection of site(s), and proceeding decidedly towards start of deployment in 2012.

  36. 1450m 2450m High Energy Neutrinos A fantastic year 2008 7 year skymap AMANDA IceCube 3/4 complete ANTARES fully operational High-statistics sky-map IceCube High statistics of neutrinos in ANTARES

  37. 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 High Energy Neutrinos now operation AMANDA operation IceCube oonstruction + operation operation NT200, NT200+ GVD operat construction + operation design study operation ANTARES constrn. c + o R&D KM3 NESTOR, NEMO KM3NeT operat construction + operation FP6 Design Study/Fp7 Prep. Phase

  38. KM3NeT - ESFRI list - ASTRONET list FP6 FP7

  39. High Energy Neutrinos • Commissioning of ANTARES defines a milestone towards KM3NeT. • Fully exploit potential of IceCube ! Important input for KM3NeT. • Recommendation:The priority project for high energy neutrino astronomy is KM3NeT. Encouraged by the significant technical progress of recent years, the support for working towards KM3NeT is confirmed. Resources for a Mediterranean detector should be pooled into a single optimised design for a large research infrastructure, with installation starting in 2012. The sensitivity of KM3NeT must substantially exceed that of all existing neutrino detectors including IceCube.

  40. High Energy Neutrinos Point sources: Tremendous progress in sensitivity over last decade factor 1000 in 15 years ! KM3NeT target 3 years

  41. Gravitational Waves

  42. Gravitational Waves /VIRGO

  43. Adv Virgo/ Adv LIGO Virgo/LIGO Gravitational Waves Several to several hundred sources per year

  44. Gravitational Waves FP7 design study 103 to 105 sources per year

  45. Now Gravitational Waves Time Chart Virgo+ Advanced Virgo GEO HF Hanford Advanced LIGO LIGO+ Livingston Launch Transfer data Construct. Commiss. Data DS PCP 1st Generation 2nd Generation 3rd Gen.

  46. Gravitational Waves • E.T. is the long-term future project of ground-based gravitational wave astronomy in Europe. • European GW community has world-leading role in planning. • Similar studies in Japan. • First technical design and associated costing expected in 2011, followed by a ‘Preparatory Phase’. • A decision on funding for the construction of E.T. will earliest after first detections with enhanced LIGO/Virgo but is most likely after collecting about a year of data with advanced LIGO/Virgo in approximately 2014/15. Targeted start of E.T. construction ~ 2017. • At low frequencies: LISA (LISA-Pathfinder 2010)

  47. Infrastructures • R&D • Theory

  48. Infrastructure • Underground Laboratories • Observatories, Satellites

  49. Summary

  50. The factor-2 scenario Investment and maintenance (no personnel) Increase in personnel cost will be smaller !

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