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Summary Talk at VI 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. - PowerPoint PPT Presentation
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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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benötigt.
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