Highlight

on New Views on the

Universe

Vemes Recontres du Hanoy 11/04/08

Vietnam

The Big BangWe live in a

Homogeneous & Isotropic Universe

described by (a Robertson-Walker metric

& Friedmann’s equation derived from)

Einstein’s General Relativity.

It began 13.7 billion years ago,

and is composed of...

Cosmological ContextCosmological Context

« Precision Cosmology Era »

• CMB flattness• SNIa (+CMB) acceleration

=> « Concordance Model »-CDM

• Clusters evolution is a direct, global and independant test of the matter content of the Universe

AE (F)

launched 1989

Precision Cosmology

WMAP

The New SN Ia Hubble Diagram

97ff

(6 of the 7 highest- redshift SNe Ia)

(Riess et al. 2004, ApJ, in press)

97ff

(Riess et al. 2004, ApJ, 607, 665)

(6 of the 7 highest-redshift SNe Ia)

The New SN Ia Hubble Diagram(m

ag)

[Dashed line: best fit, assuming total = 1]

log dL

Redshift (z)

Residual Hubble diagram (Riess et al. 2004, ApJ, 607, 665)

(log dL)

(SN Ia + LSS: M =

0.28, = 0.72, with precision ~ CMB + LSS)

Riess et al. (2004), using all published high-z SN Ia data.

=1 ruled out

at very many !

SnIa

LSS 2dF

WMAP (h fix)

Primordial Nucleosynthesis

in the New Cosmology

Big Bang Nucleosynthesis Theory vs. Observations:

Remarkable agreement over 10 orders of magnitudein abundance variation

Concordance region:b h2 = 0.02For h=0.7, b = 0.04.

Deuterium: strongest constraint

4He

b

Standard BBN

WMAP

Dark Radiation relaxes the tension between the CMB and 4He limits on the baryon/photon

ratio

K. Ichiki, M. Yahiro, T. Kajino, M. Orito, G. J. Mathews PRD (2002), astro-ph/0203352

Official detections by H.E.S.S.

Linton, WatsonFest, Leeds July 2004

• Crab Nebula (2003, 3 Tel.) - 54 sigma• PKS 2155 (2003, 2 Tel.) - 45 sigma• Mrk 421 (2004, 4 Tel.) - 71 sigma• PSR B1259 (2004, 4 Tel.) - 8 sigma• RX J1713 (2003, 2 Tel.) - 20 sigma• Sagittarius A* (2003. 2 Tel.) - 11 sigma

High-Resolution Simulations ofCold Dark Matter (CDM) Halos

Dense flat Universe

Low density Universe -CDM

Basic Idea: Cluster evolution strongly depends on m (and 8, )

Z=3 Z=1

Virgo Consortium

RDCS: 50 deg²fx 3. 10-14 erg/s/cm²

MACS: 22 000 deg²fx 10-12 erg/s/cm²

=0.3, 8~[.75,1], =0.2=[0.8,1.] , 8~.55, =0.12L-T DispersionM-T Dispersion

Ultra-high energy cosmic ray propagation in the Universe

UHECR mystery :origin ?? … nature ?? … energy spectrum ??

What source can accelerate particles to 1020 eV ?Why do we see (do we?) particles with energy 1020 eV ? Why do we not see the source in the arrival directions of UHECRs ?

Martin LemoineInstitut d’Astrophysique de Paris

Propagation effects may be the key to the mystery :

1. Energy losses: GZK cut-off or not ?

2. Effects of magnetic fields

The 9th wonder of the world32

ord

ers

of m

agni

tude

12 orders of magnitude

non thermal!

most interesting for general astrophysics

?

Is there an end?

propagationacceleration

one-century quest!

Fe kneeHe

C,O,…

p

ankle:pair production dip

All particle cosmic ray spectrum(artist’s view !) UHECR:

composition ??spectrum ??broken tibia:

transition to UHECR ?

Nagano & Watson 00

Pierre Auger Project3000 km2 - 1600 water tank array

The night

Image of source is somewere along image of shower axis ...

Use more views tolocate source!

The night

The ground

Imaging Air Cherenkov Telescopes

SourceSource

PSR B1259-63 : H.E.S.S. Observations

Pre-periastron:► 26.2. - 2.3.2004► 3 telescopes only► Zenith angle: 42

deg► Threshold: 360

GeV► Livetime: 7.8 h

Post-periastron:► 19.3. - 29.3.2004► Zenith angle: 44

deg► Threshold: 380

GeV► Livetime: 17.4 h

Still under analysis:► April, May 2004► Livetime: 14 h

M. Beilicke (Gamma 2004)

Significance: 9

.1 σ

6.3 σ

Galactic centre

News on GRB

The great debate (1995) Fluence:10-7 erg cm-2 s-1

Distance: 1 GpcEnergy:1051 erg

Distance: 100 kpcEnergy: 1043 erg

Cosmological - Galactic?Need a new type of observation!

GRB: where are they?

Costa et al. (1997)

BeppoSAX and the Afterglows

Kippen et al. (1998) Djorgoski et al. (2000)

• Good Angular resolution (< arcmin)• Observation of the X-Afterglow

• Optical Afterglow (HST, Keck)• Direct observation of the host galaxies• Distance determination

GRB 030329 & SN 2003dh

6 articles in Nature !

Z = 0.17 EGRB = 2 1052 erg

Matheson et al. 2003

Afterglow ObservationsHarrison et al (1999)

Achromatic Break

Woosley (2001)

Jet and Energy Requirements

Bloom et al. (2003)

Unifying relations ?

Lamb et al. 2004Berger et al. 2003

GRB for Cosmology

Amati et al. (2002)Ghirlanda et al. (2004)

Cosmology with GRB

GRB 000131z = 4.5

Andersen et al. (2000)

GRB for Cosmology

Dai, Liang & Xu (2004)

GRB for Cosmology

Luminositydistance

Redshift

Preliminary

Redshift

Age

0 ~ 3-7 ? ~ 10-30 1000

013,7 Gyr

~ 1-2 Gyr

~ 250 Myr ~ 500 000 yr

Now

Observable

universe with

present day

telescopes

Reionisation(s)(first stars ?)

Galaxy formation?

Universe not yet directly

observed

Recombination

CMB« Dark ages »

Big BangInflation

BBN

Cosmic history

NeutrinoDetectors

Amanda technology80 strings / 60 OM’s each17 m OM spacing125 m between strings1 km2 hexagonal pattern

Surface array: 2 OMs each string topcalibrate angular response 100 tagged TeV /day

installation, operation 2005-2010

master local control module

LED beacon local control module

string control module andstring power module

interlink cable withwet-mateable connector

acoustic beacon

acoustic receiver

3 optical modules

acoustic receiver

12m

100m

acousticreleases

Antares preproduction prototype (2002-3)...redeploy in October

Search forDark Matter

Direct detection techniquesWIMP

Heat

Ionization

Light

Ge

Liquid Xe

NaI, Xe

Ge, Si

CaWO4, BGO

Al2O3, LiF

Elastic nuclear scattering

• ≈ few % detected energy• usually fast• no surface effects ?

≈ 20 % energy

• ≈ 100% detected energy• relatively slow• requires cryogenic detectors

A first WIMP candidate: DAMA

• Data taking completed in July 2002• Total exposure of 107,731 kg.d• See annual modulation at 6.3• Claim model-independent evidence

for WIMPs in the galactic halo

• WIMP candidate under standard halo parameters: M = (52 +10) GeV and = (7.2 +0.4) .10-6 pb

• Rather opaque analysis (raw spectrum, cuts, calibration)• Nevertheless, checking this result remains important• 2nd phase 250 kg LIBRA running...

-8 -0.9

Direct detection summary

• Background discrimination is now essential• Sensitivity of CDMS, EDELWEISS and CRESST one order of magnitude better than present competitors• Optimistic SUSY models are now tested

Experimental status and theoretical predictions

L. Rozkowski et al., hep-ph/0208069

CDMS-II, CRESST-II, EDELWEISS-II,XENON, XMASS … sensitivity goals

1 Ton sensitivity goal (optimistic)

CDMS, CRESSTEDELWEISS-I present

GravitationalWaves

PSR 1913+16: the prototype gw source

Prototype NS -NS: binary radio pulsar PSR B1913+16

Chirp Waveform

GW emission causes orbital shrinkage leading to higher GW frequency and amplitude

orbitaldecay

PSR B1913+16

Weisberg &Taylor 03

NAUTILUS

• a= 935 Hz

•new antenna suspension cable•new capacitive transducer •Quantum Design dc SQUID

Present SphericalDetectors Properties

Mass 1150 kg CuAl alloy, 65cm diameter

Sound velocity v = 4000 m/s

Resonant freq. f = 3160 Hz

Rapid cool down to mK temperatures.

TAMA

VIRGO

LIGO

FutureProspects

• CMB W-map release 2004.

• GRB Swift launch 2004.

Will GRB become a calibrated source?

• SN 1A few more high-z explosions?

• Cosmic Ray Auger first results 2005.

• Dark Matter many detectors in preparation.

• Many other different fields are growing very fast