Highlight

on New Views on the UniverseVemes Recontres du Hanoy 11/04/08 Vietnam

The Big BangWe live in a

Homogeneous & Isotropic Universe

described by (a Robertson-Walker metric

& Friedmanns equation derived from)

Einsteins General Relativity.

It began 13.7 billion years ago,

and is composed of...

Cosmological Context

Precision Cosmology Era

CMB flattnessSNIa (+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 CosmologyWMAP

The New SN Ia Hubble Diagram97ff(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(mag)[Dashed line: best fit, assuming W total = 1] log dL

Redshift (z)Residual Hubble diagram (Riess et al. 2004, ApJ, 607, 665) (log dL)

(SN Ia + LSS: WM = 0.28, WL = 0.72, with precision ~ CMB + LSS)Riess et al. (2004), using all published high-z SN Ia data. WM=1 ruled out at very many !

SnIaLSS 2dFWMAP (h fix)

Primordial Nucleosynthesisin 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 4Heb

Standard BBNWMAPDark 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 2004Crab Nebula (2003, 3 Tel.) - 54 sigmaPKS 2155 (2003, 2 Tel.) - 45 sigmaMrk 421 (2004, 4 Tel.) - 71 sigmaPSR B1259 (2004, 4 Tel.) - 8 sigmaRX J1713 (2003, 2 Tel.) - 20 sigmaSagittarius A* (2003. 2 Tel.) - 11 sigma

High-Resolution Simulations ofCold Dark Matter (CDM) Halos

Dense flat UniverseLow density Universe -CDMBasic Idea: Cluster evolution strongly depends on m (and 8, )Z=3Z=1Virgo Consortium

RDCS: 50 degfx 3. 10-14 erg/s/cmMACS: 22 000 degfx 10-12 erg/s/cm

Ultra-high energy cosmic ray propagation in the UniverseUHECR 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 dAstrophysique de ParisPropagation 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 worldone-century quest!

Fe kneeHeC,O,pankle:pair production dipAll particle cosmic ray spectrum(artists view !)UHECR:composition ??spectrum ??broken tibia:transition to UHECR ?Nagano & Watson 00

Pierre Auger Project3000 km2 - 1600 water tank array

The nightImage of source is somewere along image of shower axis ...Use more views tolocate source!The nightThe groundImaging Air Cherenkov Telescopes

PSR B1259-63 : H.E.S.S. ObservationsPre-periastron:26.2. - 2.3.20043 telescopes onlyZenith angle:42 degThreshold:360 GeVLivetime: 7.8 h

Post-periastron:19.3. - 29.3.2004Zenith angle:44 degThreshold:380 GeVLivetime: 17.4 hStill under analysis:April, May 2004Livetime: 14 hSignificance: 9.1 6.3

Galactic centre

News on GRB

GRB: where are they?The great debate (1995)Fluence:10-7 erg cm-2 s-1Distance: 1 GpcEnergy:1051 erg

Distance: 100 kpcEnergy: 1043 ergCosmological - Galactic?Need a new type of observation!

BeppoSAX and the AfterglowsCosta et al. (1997)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 2003dh6 articles in Nature !

Z = 0.17 EGRB = 2 1052 erg

Matheson et al. 2003

Afterglow ObservationsHarrison et al (1999)Achromatic BreakWoosley (2001)

Jet and Energy RequirementsBloom et al. (2003)

Unifying relations ?

GRB for CosmologyAmati et al. (2002)Ghirlanda et al. (2004)

Cosmology with GRBGRB 000131z = 4.5Andersen et al. (2000)

GRB for CosmologyDai, Liang & Xu (2004)

GRB for CosmologyLuminositydistanceRedshiftPreliminary

Cosmic historyRedshiftAge0~ 3-7 ?~ 10-301000013,7 Gyr~ 1-2 Gyr~ 250 Myr~ 500 000 yr

NeutrinoDetectors

Amanda technology80 strings / 60 OMs 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

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

Search forDark Matter

Direct detection techniquesWIMPElastic nuclear scattering few% detected energy usually fast no surface effects? 20% energy100% detected energy relatively slow requires cryogenic detectors

A first WIMP candidate: DAMAData taking completed in July 2002Total exposure of 107,731 kg.dSee annual modulation at 6.3sClaim model-independent evidence for WIMPs in the galactic haloWIMP candidate under standard halo parameters: Mc = (52 +10) GeV and sc-N = (7.2 +0.4) .10-6 pb

Rather opaque analysis (raw spectrum, cuts, calibration)Nevertheless, checking this result remains important2nd 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 predictionsL. Rozkowski et al., hep-ph/0208069CDMS-II, CRESST-II, EDELWEISS-II, XENON, XMASS sensitivity goals1 Ton sensitivity goal (optimistic)CDMS, CRESST EDELWEISS-I present

GravitationalWaves

PSR 1913+16: the prototype gw sourcePrototype NS -NS: binary radio pulsar PSR B1913+16Chirp WaveformGW emission causes orbital shrinkage leading to higher GW frequency and amplitudeorbitaldecayPSR B1913+16Weisberg &Taylor 03

NAUTILUS na= 935 Hznew antenna suspension cablenew 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

First let me remind you about the type of supernova we are looking for and why they areImportant. Type Ia supernovae are the end states of low mass stars.Here is how we think nature produces a SN IaThis model has many attractive featuresAs you can see we have approximately doubled the well-observed redshift range of the Hubble diagram.6 of the 7 highest redshift known

For any material, however, the principles behind direct detection are always the same. It all comes down to measuring the energy deposited by a WIMP interaction expected to be in the keV to tens of keV range. There are basically three ways of measuring this energy, which can eventually be combined. Each leads to a choice of target material.The fastest but less efficient way in terms of collected energy is to look for a light signal produced by a scintillation process. This is the way used in Sodium Iodide or Xenon scintillators.One can also look for a ionization signal: free charge carriers produced by the nuclear recoil can be collected using a drifting electrical field. Depending on the material used and operating conditions, the efficiency of this technique can be significantly higher than that of scintillation.Lastly, a slower heat signal can be detected, assuming that all energy deposited will eventually turn into heat. This technique usually ensures a higher energy collection efficiency, to the cost of a slower signal and tougher operating conditions namely ultra-low cryogenics.The data taking was completed in July 2002, with a total exposure of over 100,000 kg.d accumulated over 5 years.The published results show a modulation confirmed at 6.3 sigma significance using the 2 to 6 keV energy range data, which has lead the DAMA collaboration to claim a model-independent evidence for the presence of WIMPs in the galactic halo. Under standard halo parameters, this translates to a WIMP candidate of mass around 52 GeV and cross-section 7.2 10 to the minus 6 picobarn.As well see in the following, this result has been controversial since quite some time now. To this day, confronting this result to their own data remains for a lot of experiments, if not a goal, at least an important milestone.And now lets talk about spheresHelium forced flow