Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.eso.org/~hboffin/Astronet/Presentations/ScienceVision_Aspera.pdf Äàòà èçìåíåíèÿ: Wed Jan 31 03:43:07 2007 Äàòà èíäåêñèðîâàíèÿ: Fri Feb 28 15:32:39 2014 Êîäèðîâêà:

Science Vision 2015+ The ASPERA view
Science Vision 2015+ Poitiers, January 23-25 2007 S.Katsanevas CNRS coordinator ASPERA

www.aspera-eu.org


History 1: ApPEC
ApPEC aims (2001)

(Astroparticle Physics European Co-ordination)

­ Promote and facilitate co-operation within the growing European Particle Astrophysics community ­ Develop and promulgate long term strategies for European PA, offering advice to national funding agencies or institutions, ESF, and EC and other ­ Assist in improving links and co-ordination between European PA and the scientific programmes of organisations such as CERN, ESA, and ESO ­ Express their collective views on PA in appropriate international forums, such as EC, OECD, UNESCO etc.

ApPEC membership
­ At the outset it comprised the national funding agencies of France CNRS/CEA, Germany BMBF, Italy INFN, the Netherlands NIKHEF and the UK PPARC. ­ Since then Spain, Belgium, Portugal, Greece, and Switzerland have joined ­ Recently Poland has expressed interest in joining. ­ Eligibility: Funding Agencies (decision making body, having a national coordinating role)


History 2: ApPEC Operation
ApPEC operates ­ strategically through its Steering Committee and operationally with the wider academic community through its Peer Review Committee ­ Observers from ESA, ESF, ESO, CERN Steering Committee (SC)
­ France: M.Spiro, S.Katsanevas, C. Cavata, Germany: T. BerghÆfer, R.KÆpke, H. Bluemer, Netherlands: F. Linde, UK: A. Coates, R. Wade , Italy: R. Petronzio B. Dettore, Spain: D. Espriu, A.Ferrer, Switzerland: M. Bourquin, Belgium: D. Bertrand, C. DeClerq, Portugal K. Gaspar Greece: D. Nanopoulos,

Peer Review Committee (PRC)
­ Frank Avignone, Jose Bernabeu, Pierre Binetruy, Hans Bluemer, Karsten Danzmann, Franz v. Feilitzsch, Enrique Fernandez, Werner Hofmann, John Iliopoulos, Uli Katz, Paolo Lipari, Manel Martinez, Antonio Masiero, Benoit Mours, Francesco Ronga, Andre Rubbia, Subir Sarkar, Guenther Sigl, Gerard Smadja, Nigel Smith, Christian Spiering, Alan Watson ApPEC actions:
­ ­ ­ ­ I3 ILIAS (underground labs and Grav waves, the HE part did not pass the EU procedure) Review by the PRC of 6 major fields of astroparticle, suggestions of merging of projects KM3 (Neutrino telescope in the mediterranean, ESFRI list) ASPERA


Start 1st July 2006 (3y)

ASPERA
17 agencies 12 countries + CERN:
1. 2. 3. 4. 5. 6. 7. 8. 9. Belgium FNRS/FWO Czech Rep. MEYS France CEA/CNRS Germany BMBF/PTDESY Greece DEMOKRITOS Italy INFN Netherlands FOM Portugal FCT Spain MEC/FECYT
QuickTimeTM and a TIFF (LZW) decompressor are needed to see this picture.

10. Sweden VR 11. Switzerland SNF 12. UK PPARC 13. CERN


5 workpackages
WP1 Status in research funding NIKHEF

WP4 Web/Database/Outreach Network Extension BMBF/MEC

WP2 Roadmap PPARC

WP3 European wide procedures INFN

WP5 Management CNRS


Goals of ASPERA
(WP3) Prepare the ground for

(reverse engineering)

­ Common European Funding of at least one large infrastructure ­ A common call on R&D ­ Alignment of procedures of evaluation to fund future common projects

(WP2) In order to do so one needs: ­ A common roadmap (3 phases)
· Phase I list of opportunities: Wshop: Valencia Nov 2006, Pub: March 2007 · Phase II projection of resources, WG meetings, Wshop: September 20-21 Amsterdam, Pub: early 2008 · Phase IIII priority list, end of 2008 - mid 2009 ­ A posteriori linking of existing infrastructures

(WP1) A prerequisite of the above is:
­ Detailed assessment of the resources available
· questionnaires, workshops, national days

­ Identification of the legal/financial barriers to coordination and a census of possible legal forms of cooperation ­ Census of evaluation procedures (people, projects, laboratories) ­ Common electronic tools (database, web)


Astroparticle Physics, a definition through 6 questions*
From Phase I roadmap
1. 2. 3. 4. 5. 6. What is the Universe made of ? Do protons have a finite life time ? What are the properties of neutrinos ? What is their role in cosmic evolution ? What do neutrinos tell us about the interior of Sun and Earth, and about Supernova explosions ? What is the origin of cosmic rays ? What is the view of the sky at extreme energies ? What is the nature of gravity ? Can we detect gravitational waves ? What will they tell us about violent cosmic processes ?

*"Science is the art of replacing unimportant questions that can be answered by important ones which cannot" Edward B. Ferguson Jr. 1976.


- Dark matter: WIMPS direct and indirect, axions from Sun - Dark energy (not addressed in detail but closely related to dark matter) - Other particles beyond the standard model - Cosmic antimatter Soon: Pamela, later: AMS Soon: Pamela, later: AMS > 2010: > 2010: Two direct-search experiments with Two direct-search experiments with

-10 pb 10-10 pb 10

sensitivity sensitivity


) 6 (CDMS 200
expectation 2008

10

-10

pb


Field/ Experiment Dark Matter Search: Low background experiments with 1-ton mass

cost scale (M) 60-100 M

Desirable start of construction 2011-2013

Remarks

two experiments (different nuclei, different techniques), e.g. 1 bolometric 1 noble liquid more than 2 expt`s worldwide

Background, background, background ! Expect technical proposals ~ 2009/10


Spectrum endpoint and , oscillations at reactors Soon: KATRIN Soon: KATRIN Soon: Double CHOOZ Soon: Double CHOOZ

>2010: ~2 experiments >2010: ~2 experiments with sensitivity to with sensitivity to test inverse hierarchy test inverse hierarchy


Field/ Experiment Properties of neutrinos: Double beta experiments

cost scale (M) 60-80 M

Desirable start of construction 2011-2013

Remarks

1) Explore inverted hierarchy scenario 2) two experiments with different nuclei (techniques) worldwide 1 ton

20-50 meV range requires active mass of order one ton, good resolution, low BG. Need several isotopes.


2015: 2015:

Ultimate price tag 400-800 M

A very large multi-purpose facility A very large multi-purpose facility

Options: Options: Water Megatonne (,,MEMPHYS") --Water Megatonne (,,MEMPHYS") 100 kton Liquid Argon (,,GLACIER") --100 kton Liquid Argon (,,GLACIER") 50 kton scintillaton detector (,,LENA") --50 kton scintillaton detector (,,LENA")


Soon: Borexino Soon: Borexino 2015: 2015:

Ultimate price tag 400-800 M

A very large multi-purpose facility A very large multi-purpose facility

Options: Options: Water Megatonne (,,MEMPHYS") --Water Megatonne (,,MEMPHYS") 100 kton Liquid Argon (,,GLACIER") --100 kton Liquid Argon (,,GLACIER") 50 kton scintillaton detector (,,LENA") --50 kton scintillaton detector (,,LENA")


65m

MEMPHYS: Water Cherenkov, (420 kton -1 Mton) LENA: Liquid Scintillator (30-70 kton)
100m

60m

30m

Muon veto
~

70m 20m

12000 PMT (50cm)

GLACIER: Liquid Argon (50 -100 kton)


Field/ Experiment Proton decay and low energy neutrino astronomy: Large infrastructure for p-decay and astronomy on the 100kt-1 Mton scale

cost scale (M)

Desirable start of construction
-

Remarks

400-800 M

Civil engineering :2012-2013

multi-purpose - 3 technological ..options - needs huge new ..excavation - most of expenditures after ..2015 worldwide sharing

LAGUNA DS


Charged cosmic rays, neutrinos, TeV
Started: Auger Started: Auger >2008: >2008: Auger North Auger North >2015: EUSO ? >2015: EUSO ?

> 2009: KM3Net > 2009: KM3Net
under construction: under construction:

IceCube IceCube

H.E.S.S., Magic H.E.S.S., Magic

Very Large Array(s) Very Large Array(s) (,,CTA", > 2009) (,,CTA", > 2009)
also: Argo/YBJ also: Argo/YBJ


High Energy Photon Sky: Source Count vs. Year
10
4

X rays
10
3

10

2

2015 MeV-GeV

10

1

0.1-100 TeV
1960 1965 1970 1975 1980 1985 1990 1995 2000 2005

(modified from M. De Naurois, astro-ph/0409361)


Field/ Experiment High Energy Univ. Gamma Rays Cherenkov Telescope Array CTA Charged Cosmic Rays Auger North Neutrinos KM3NeT

cost scale (M)

Desirable start of construction

Remarks

100 M South 50 M North 85 M

First site 2010 2009

Physics potential well defined by rich physics from present exp`s Confirmation of physics potential from Auger South expected in 2007 FP6 design study Confirm. of physics potential from IceCube and gamma telescopes expected in 2008-10

2011 300 M


Price tags LIGO: 260 M (US costing)
only US

Adv.Ligo: +210 M (dito)

Now: Now: --GEO-600, GEO-600, --VIRGO (( VIRGO+, advVIRGO), VIRGO VIRGO+, advVIRGO), > 2010: 3rd Generation Facility > 2010: -- 3rd Generation Facility

30 M$ Germ. + UK

VIRGO: 85 M (cap.invest) 3rd Gen Fac.: 200 M (?)


Field/ Experiment

cost scale (M)

Desirable start of construction

Remarks

Gravitational waves: Third generation interferometer

250-300 M

Civil engineering 2012

Conceived as underground laboratory

Recoomendations: Welcome LISA which complements Earth bound detectors towards sub-Hz range and enables observation of a wealth of sources.


Phase I Assessing the opportunities of the field
·Examination of the subfields by the ApPEC/PRC in thematic workshops (20032005) · A preliminary census of 66 astroparticle projects (2005-2006) · Draft proposal ready . Feedback by agencies, projects leaders , experts etc. ·Valencia workshop 6/7 November 2006: Public presentation of the proposal and first discussion by 7 thematic groups:

1. 2. 3. 4. 5. 6. 7.

High Energy Rays M. Martinez, G. Herman Mass F. Piquemal , A. Giuliani High Energy Cosmic Rays H. Bluemer High Energy U. Katz, P. Lipari Dark Matter direct detection N. Smith, G. Gerbier Gravitational Waves H. Lueck Low Energy and Proton decay A. Rubbia,


Phases II and III
· Phase II: intra-thematic prioritisation, resource projection

· ·
·

Internal meetings of the 7 working groups (November 2006-April 2007) Final thematic mini-workshops, with the participation of the PRC to examine, uniformize the criteria of the 7 thematic propositions (May 2007-July 2007)
The a. b. c. d. thematic propositions must contain beyond what is present in phase I: Detailed calendar (phasing, milestones, review points) Detailed multi-annual projection of budget and human resources Detailed exposition of enabling R&D Maximal possible prioritization within the thematic.

·
·

Final synthesis: Amsterdam 20-21 September 2007

· Phase II Roadmap January 2008 Phase III: Inter-thematic prioritisation · Selected hearings by the PRC of experts on thematic groups · Discussions in ApPEC and agencies · Deliverables July 2008 · Roadmap with selected priorities (action plan) · Definition of areas where common R&D calls can be launched · Preparation of agreements for next phase large infrastructures


DM: Eureca 100% + Noble gas 100% : Gerda+Majorana 50% + "X" 100% One large detector for low en nu and proton decay (35% before 2016) Cost for one large TeV gamma array KM3Net Auger North (33%) Gravitational Waves (EGO) Smaller projects, R&D Sum 300 M per year (now 135 M) manpower not always included

150 M 100 M 250 100 300 30 250 200 M M M M M M

1400 M

factor 2


Conclusion
ASTROPARTICLE LARGE INFRASTRUCTURES ARE NOW AT THE LEVEL OF FUNDING OF PARTICLE PHYSICS NUCLEAR PHYSICS AND LARGE ASTROPHYSICS INFRASTRUCTURES. SHOULD BE READY TO PARTICIPATE AT THE TIME OF THE WORLD DISTRIBUTION OF LARGE INFRASTRUCTURES (ca 2010-2012) ASPERA's AMBITION IS TO BE THE INSTRUMENT OF THE PREPARATION (IN COLLABORATION WITH ASTRONET ON THE REGIONS OF OVERLAP) FOR EUROPE AND COORDINATION WITH THE OTHER REGIONS OF THE WORLD