Summary Talk atVI Rencontre du Vietnam

Challenges in ParticleAstroPhysics

Hinrich Meyer

Univ. of Wuppertal

and DESY

Overview of talks

UHECR 7

VHEGR 2

CMB 4

DE, DM 5

GRW 5

Neutrino 14

And 4 parallel sessions on one afternoon 37

Please accept my apologies if you do not find your beautiful and important work properlyrepresented in my talk. There have been about 2000 pictures shownin the talks at this meeting.

And, the results and presentations have been of such high quality that many (most) of uswere keen not to miss one the talks.

In the last 10 years or so there have been several great advances in particle-astrophysics just when a rather complete picture of the Standard Model of particle physics was found.

Keynote talk by John Ellis

The matter particles

The ‘Standard Model’

The fundamental interactions

Gravitation electromagnetism weak nuclear force strong nuclear force

= Cosmic DNA

Some particles have mass, some do not

+1 0 -1

W+ Z 0 W -

Mass 80.419 91.188 80.419

0photon

Mass 0

Where do the masses come from?

Newton:Weight proportional to Mass

Einstein:Energy related to Mass

Neither explained origin of Mass

Are masses due to Higgs boson? (yet another particle)

Neutrino oscillations have been discovered in studies of neutrinos from the SUN, the earth atmosphere,from reactors and particle accelerators.

Extensive studies of the CMB have revealed a flat universe and supported by SN1A observations a content of the universe dominated by dark energy and dark matter, and not by ordinary baryonic matter.

CR-experiments have revealed more than 40 TeV gamma ray sources both of galactic and extragalactic origin of (at least) five different kinds.

Searches for gravitational waves have reached anew quality with 3 LIGO, GEO600 and VIRGOtaking data in a regular search mode.

Searches for diffuse SN Neutrinos and for diffuseinfrared photons have produced interesting limitsalso for astronomers

Further developments in the field is driven by thesesuccesses and most important by very basic questionsand problems formulated long ago by great scientistsof the past. To name a few…..

Max Planck, 1899

Victor Hess, 1912

Albert Einstein, 1916

Wolfgang Pauli, 1930

Fritz Zwicky, 1933

Ettore Majorana,1937

Peter Higgs, 1962

Greisen, Zatsepinand Kuzmin, 1966

Andre Sakharov,1968

Bruno Pontecorvo, 1968

Upper end of the CR-spectrum

Protons?> 50 Mpc isotropically ??

Protons producingPions colliding with the CMB photons

Dip due pair production ?

Is there a cutof in the all-particle CR-spectrum??

Rubakov at Moscow summary

Overview of detection methods for UHE showers

The Pierre Auger Observatory Fluorescence Detectors: 11000 PMTs

Surface Detectors: 1600 Cherenkov tanks (spacing 1.5 km)

3000 km2 covered

The radiowavesgenerated byparticle showersin matter area new and very promisingmeans to detectCosmic Rays

Askarian 1962!!

Geo-synchrotronEffect in earthMag.field

Use Westerbork radio observatory

NuMoon Experiment @ WRST

Using “Askarian” to detect Neutrino-showers emerging

High energy Neutrinos

The South Pole

NSF NSFNSF

NSF

Circum polar flights with balloons (40 days)

Flux of Neutrinosis dropping offfaster than acceptance canbe provided by theexperiments

Dark Matter

Full Macho Halo:

LMC

0.45 10-6

SMC

0.65 10-6

Self lensing:

LMC-LMC

0.005 - 0.05 10-6

SMC-SMC

0.04 10-6

Lensing LMC-Galactic stars:

LMC-gal

0.01 10-6

Lensing Galactic-Galactic stars:

gal-gal

2.0 10-6

Events rate comparison :

(MACHO 0.12 10-6)

_3% at 10-2 M

Final EROS combined limit (1990-2003)

_7% at 0.4 M

_10% at 1 M

LMC data set / No event

LMC + SMC data set with 1 SMC halo candidate

Domain excluded from all EROS data

ZOOMZOOM

LCDM TeVeS-MOND

Stay Tuned!

• Tides/vertical force

• Rot. curves HSB/LSB

• Lensing by Ellip/Cluster

• Hubble Expansion/CMB

Alternative gravitational theories compared to cold dark matter

Dwarf spheroidal galaxies

M/L ranges from 1 to 3000!!

12 have been analysed sofar, 5 more newly discovered

But all seem to have 4x10e7 solar mass DM!!!

No tidal effects apparent, no r-cut found sofar

Very enigmatic MOND etc. fail

Natural WIMP candidate:SUSY LSP neutralino

Stable if SUSY exists and R-parity is conserved

• Direct detection:– WIMP scattering off nuclei

˜ χ 10 =N11

˜ B +N12˜ W 3 +N13

˜ H 10 +N14

˜ H 20

Zg = N11

2+ N12

2gaugino fraction:

PMTsPMTs

PEEK SupportsPEEK Supports

CathodeCathode

GridsGrids

Waveshifter/ReflectorWaveshifter/Reflector

Gravitational Waves

Noise Sources in LIGOGround motion couplesinto motion of mirrors

Counting statistics ofphotons at photodiode

Thermal excitations ofmirror suspensions

10-24

10-23

10-22

10-21

10-20

10-19

10-18

1 10 100 1000 104

h (

Hz-1

/2)

Virgo

LIGO

Resonantantennas

Hz

GEO

Core Collapse@ 10 Mpc

BH-BH MergerOscillations@ 100 Mpc

Pulsars hmax – 1 yr integration

BH-BH Inspiral,z = 0.4

BH-BH Inspiral, 100 Mpc

QNM from BH Collisions, 1000 - 100 Msun, z=1

NS, =10-6 , 10 kpc

QNM from BH Collisions, 100 - 10 Msun, 150 Mpc

NS-NS Inspiral, 300 Mpc

NS-NS MergerOscillations@ 100 Mpc

Credit: P.Rapagnani

Design sensitivity

Measured sensitivity

C7 NS/NS maximum distance ~ 1.5 Mpc

(7 W)(7 W)(7 W)(7 W)(0.7 W)(0.7 W)(0.7 W)

Design NS/NS maximum distance ~ 30 Mpc

Low energy neutrinos

There is a problem of mass

• Neutrinos will have (already) a very complicated phenomenology!!!!

Great attack on theta 13

• 3 twin reactors

• 4 underground

Tunnels

• Large multinational

collaboration

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RecentAdvancesIn BKGReductionFor2beta decayExperimentsAbout factor100000!!

Arrays are the future

Moore’s sensitivity law ?

• Rapid evolution of sensitivity of discriminating experiments(CDMS, EDELWEISS, CRESST, WARP, XENON…)

• But goals are still ≈3 orders of magnitude beyond present best performances

(After Gaitskell)

TeV photons

OG 2.7: New ExperimentsCherenkov TelescopesCherenkov Telescopes

4. HESS-II [Vincent]

• New 28m telescope.• 2048 pixel camera.• Lower energy 40-50

GeV.

5. MAGIC-II [Teshima]

• New 17m telescope.• Possible high-QE

camera.• 2007 schedule.

MAGIC-IMAGIC-I MAGIC-IIMAGIC-II

85m

Future ConceptsLarge Cherenkov Tel. Arrays

HE-ASTRO: 217 Telescopes (ø10m), 80m separation.1.1 km2 collection area & 15o FOV !

Fie

ld o

f vi

ew [

π s

r] Field

of view

[deg

]

Collecting Area [km2]

Also, detailed work in Europe and Japan. Cherenkov Telescope Array (CTA)concept well underway.

Universal Photon Flux

• HESS, Magic

• Result• Using • Distant • BLASARS• At TeV

Early Universe

WMAP satellite

At t = 400 000 yrs, the Universe becomes transparent: photons no longer interact with

matterBIG BANG

Cosmological background T = 3 K = - 270 °C

Looking back to the primordial Universe

4He synthesis

Light element production , the first three minutes

Since the baryon/photon ratio is so well fixed

How about 4He, 3He, 2H, and 7Li ???

Diffusion plus turbulent mixture in old stars may solve the long standing 7Li problem!!

Max Planck

When do graviton decouple?

Interaction rate ~ GN2 T5 ~ ----T5

MPl4

Expansion rate H ~ ----

---- ~ ----

T2

T3

MPl

MPl3

H

Gravitons decouple at the Planck era : fossile radiation

(radiation dominated era)

(Binetruy)

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Natural units

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which independent of specific bodies and substances keep their importance for all times and for all even extra terrestrial and extra human cultures without doubts and which are therefore called natural units

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benötigt.

b = h

f = Gtoday

length

time

mass

7. November 1899

How to go deeper

• A future mission should:– Achieve BLIP– Observe longer (~2)

• ~2 for satellites• John will discuss ground-

based

– Use many more pixels

• To go much deeper, we must use arrays.

An often used phrase at this meeting

A. StarobinskyHigh precision observations are needed for furtherProgress.

K. Heeger:We have a problem of mass

DUSEL

B. Sadoulet, introducing the conceptualDesign of an all encompassing deep Underground laboratory for the US

For native german speakers

What I nice phrase

Jean Tran Thanh Van

Thank you on behalf of all of us

Double beta decay