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End of Opaque Universe

After recombination universe becomes transparent.

See photons as Cosmic Microwave Background Radiation redshifted by 1000 to 2.7K

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Penzas and Wilson Discovery of Cosmic

Microwave Background

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Cosmic Microwave Background Radiation

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Cosmic Microwave Background Radiation

(degrees)

(degree

s)

30 45 60 75 90 105 120 135

-30

-35

-40

-45

-50

-55

-60

temperature variation

Analyse angular distribution to see typical variation scale

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Measure Scale of CMBR Fluctuations

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CMBR Data Analysis

location of first peak: total~ 1

amplitude of other peaks sensitive to baryon

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Supernova Type 1aImplosiondu noyaud toile

Explosiond toile

Expansion du matireonde de choc ? acclration

Supernova Restes du Supernova

Implosion

of core of

red giant

Expansion of matter

shock wave 0.5 cExplosion of star

Supernova Supernova Remnant

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SuperNovae observed in our galaxy

Date Remnant Observed

352 BC Chinese

185 AD SNR 185 Chinese

369 ? Chinese

386 Chinese

393 SNR 393 Chinese

437 ?

827 ?902 ?

1006 SN1006 Arabic, ...

1054 Crab Chinese,..

1181 3C58 Chinese,..

1203 ?

1230 ?1572 Tycho Tycho Brahe

1604 Kepler Johannes Kepler

1667 Cas A not seen ?

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SuperNovae Remnants

Vela Cas ATycho

Crab

Cygnus Loop

Soleil

Tycho

Crab

Cas A

Vela

Kepler

Cygnus

SN1006

SN1006SN1006SN1054 (Crab)SN1680 (CasA)

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Supernova in Large Magellenic Cloud

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Distant Supernova

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Life of big star ( > 1,4 M )

End in Supernovae of type Ib, Ic et II

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Life of big star ( < 1,4 M )

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La nbuleuse de la Lyre

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Type Ia supernovae

SNe Ia sont which accrete matter from neighbour star in binary system

When the mass achieves the Chandrasekhar mass (~1.4 M) star collapsesto neutron star in supernova explosion.

Always same mass so always same luminosity

Standard Candle for measuring universe expansion

Flow of

matter

Red Giant

White Dwarf

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Reference Image

Subtraction

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Expansion with Supernova Ia

Acceleration ofuniverse expansion

effective

magnitudeb

rig

htnessd

istance

redshift recession velocity

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In 1998, two teams: High-Z Supernovae

and Supernovae Cosmology Project

simultaneously annouce non-zero

cosmological constant:

= 0,72 0,23

M= 0,28 0,09

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So what does it mean?

( due to E. Copeland, a theorist)

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Supernova at z 1.7

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2500 SNe Ia per year with z < 1.7

Study Equation of state w=pw/w

Future Project: SNAP

-

-

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Understanding Nature of Dark Energy

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Evidence for Matter DensityCombined Data

Cosmic Microwave Background Radiation, Supernova 1a, Galaxy clusters and BBN

tot = total/critical

critical density

for flat universecritical= 3H

2/8GN

H = h . 100 km/s/Mpc

M = matter/critical

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Matter/Energy in the Universe

baryons neutrinos cold dark matter

= b + +CDM 0.4

total = + 1

matter dark energy

Baryonic matter : b

0.05 stars, gas, brown dwarfs, white dwarfs

Matter:

Cold Dark Matter :

CDM 0.3

WIMPS/neutralinos, axions

Neutrinos:

0.003

if() 0.1 eV as from oscillations