Highlight on New Views on the Universe

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Highlight on New Views on the Universe
Vemes Recontres du
Hanoy 11/04/08
Vietnam
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The Big Bang
We 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...
Celebrate Einstein Centennial!
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Cosmological Context Precision Cosmology Era

• CMB ? flattness
• SNIa (CMB) ? acceleration
• gt Concordance Model
• ?-CDM
• Clusters evolution is a direct, global and
  independant test of the matter content of the
  Universe

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Cosmology
General Relativity
AE (F)
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launched 1989
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Precision Cosmology
WMAP
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(No Transcript)
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The New SN Ia Hubble Diagram
The New SN Ia Hubble Diagram
Dashed line best fit, assuming W total 1
97ff
97ff
(mag)
(6 of the 7 highest- redshift SNe Ia)
(6 of the 7 highest-redshift SNe Ia)
? log dL
(Riess et al. 2004, ApJ, 607, 665)
(Riess et al. 2004, ApJ, in press)
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Residual Hubble diagram (Riess et al. 2004, ApJ,
607, 665)

• ? ? (log dL)

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

• (SN Ia LSS WM 0.28, WL 0.72, with
  precision CMB LSS)

WM1 ruled out at very many ?!

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SnIa
WMAP (h fix)
LSS 2dF
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Primordial Nucleosynthesisin the New Cosmology
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?b
Big Bang Nucleosynthesis Theory vs.
Observations Remarkable agreement over 10
orders of magnitude in abundance
variation Concordance region ?b h2 0.02 For
h0.7, ?b 0.04. Deuterium strongest
constraint
4He
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Standard BBN
WMAP
K. Ichiki, M. Yahiro, T. Kajino, M. Orito, G. J.
Mathews PRD (2002), astro-ph/0203352
Dark Radiation relaxes the tension between the
CMB and 4He limits on the baryon/photon ratio
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Official detections by H.E.S.S.

• 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

Linton, WatsonFest, Leeds July 2004
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High-Resolution Simulations of Cold Dark Matter
(CDM) Halos
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Low density Universe ?-CDM
Basic Idea Cluster evolution strongly depends
on ?m (and ?8, ?)
Z3
Z1
Dense flat Universe
Virgo Consortium
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RDCS 50 deg² fx ? 3. 10-14 erg/s/cm²
MACS 22 000 deg² fx ?? 10-12 erg/s/cm²
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Ultra-high energy cosmic ray propagation in the
Universe
Martin Lemoine Institut dAstrophysique de Paris
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 ?
Propagation effects may be the key to the mystery

1. Energy losses GZK cut-off or not ?
2. Effects of magnetic fields
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The 9th wonder of the world
one-century quest!
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All particle cosmic ray spectrum (artists view !)
UHECR composition ?? spectrum ??
broken tibia transition to UHECR ?
C,O,
He
Fe knee
p
ankle pair production dip
Nagano Watson 00
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Pierre Auger Project
3000 km2 - 1600 water tank array
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Imaging Air Cherenkov Telescopes
The night
The night
The ground
Image of source is somewere along image of shower
axis ...
Use more views to locate source!
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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

Significance 9.1 s
6.3 s

• Still under analysis
• April, May 2004
• Livetime 14 h

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Galactic centre
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News on GRB
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GRB where are they?
The great debate (1995)
Fluence10-7 erg cm-2 s-1 Distance 1
Gpc Energy1051 erg Distance 100 kpc Energy
1043 erg
Need a new type of observation!
Cosmological - Galactic?
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BeppoSAX and the Afterglows

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

Costa et al. (1997)

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

Kippen et al. (1998)
Djorgoski et al. (2000)
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GRB 030329 SN 2003dh

• 6 articles in Nature !
• Z 0.17 EGRB 2 1052 erg

Matheson et al. 2003
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Afterglow Observations
Harrison et al (1999)
Achromatic Break
Woosley (2001)
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Jet and Energy Requirements
Bloom et al. (2003)
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Unifying relations ?
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GRB for Cosmology
Amati et al. (2002) Ghirlanda et al. (2004)
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Cosmology with GRB
GRB 000131 z 4.5
Andersen et al. (2000)
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GRB for Cosmology
Dai, Liang Xu (2004)
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GRB for Cosmology
Luminosity distance
Preliminary
Redshift
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Cosmic history
?
0
3-7 ?
10-30
1000
Redshift
Age
0
1-2 Gyr
250 Myr
500 000 yr
13,7 Gyr
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NeutrinoDetectors
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• Amanda technology
• 80 strings / 60 OMs each
• 17 m OM spacing
• 125 m between strings
• 1 km2 hexagonal pattern
• Surface array
• 2 OMs each string top
• calibrate angular response
• 100 tagged TeV ? /day
• installation, operation
• 2005-2010

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

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Search forDark Matter
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Direct detection techniques
WIMP
Elastic nuclear scattering
20  energy
  100 detected energy relatively slow
requires cryogenic detectors
  few  detected energy usually fast no
surface effects ?
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A first WIMP candidate DAMA

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

• WIMP 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
  important
• 2nd phase 250 kg LIBRA running...

-8
-0.9
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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
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Experimental status and theoretical predictions
CDMS, CRESSTEDELWEISS-I present
CDMS-II, CRESST-II, EDELWEISS-II,XENON, XMASS
sensitivity goals
1 Ton sensitivity goal (optimistic)
L. Rozkowski et al., hep-ph/0208069
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GravitationalWaves
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PSR 191316 the prototype gw source
Chirp Waveform
Prototype NS -NS binary radio pulsar PSR
B191316
orbital decay
GW emission causes orbital shrinkage leading to
higher GW frequency and amplitude
PSR B191316
Weisberg Taylor 03
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NAUTILUS

• na 935 Hz
• new antenna suspension cable
• new capacitive transducer
• Quantum Design dc SQUID

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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.

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TAMA
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VIRGO
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LIGO
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FutureProspects
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• 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