m2npac AdvancedCosmology201502 1ercours 2 obs hdole · AC Advanced Cosmology - Dole/Joyce/Langer 13...

Feb-2015 Hervé Dole, IAS - M

2NPAC Advanced Cosmology - Dole/Joyce/Langer

1 1

Hervé Dole Institut d’Astrophysique Spatiale, O

rsay Université Paris-Sud 11 et CNRS Institut Universitaire de France http://w

ww.ias.u-psud.fr/dole/m

2.php

why is the night sky dark ? 1.

why galaxy form

ation is a problem ? 2.

how to adress these problem

s ? 3. overview

of observation facts 4. overview

of structure and galaxy formation 5.

introduction to statistical tools: towards the pow

er spectrum 6.

introduction to the

structured universe

1. why is the night sky dark ?



2

exercice 1

2. why galaxy form

ation is a(n interesting) problem

?



3

exercices 3 and 4

3. how to adress these problem

s ?

! 3.1 theory (lectures 5, 6, 7) ! how

the sctructures can grow in an expanding Universe ?

! example

! 3.2 comparisons data vs m

odels ! exam

ple: CMB

! example: statistical tools

! observations



4

3.1 need for theory



5

growth of perturbations



6

From N. Bavouzet’s PhD Thesis, http://tel.archives-ouvertes.fr/tel-00363975 ;

from M

. Langer & H. Dole NPAC lectures, c2008

-> see M

ichael’s lectures for the dem

onstration

3.2 from m

aps to cosmological param

eters

7 Feb-2015

theory allow predictions and are

compared to observations

Hervé Dole, IAS - M2NPAC Advanced Cosm

ology - Dole/Joyce/Langer

3.2 between last scattering surfaces

Feb-2015 8

F. Noel – AAV 2010

Planck - thecmb.org

Planck+13

Ludwig+09

need for statistical

tools

Hervé Dole, IAS - M2NPAC Advanced Cosm

ology - Dole/Joyce/Langer

3.3 history of the universe



9

Hu & White, 2004

? ? structure form

ation, galaxy evolution

redshifts of interest: 1090 to 0

but more im

portantly 10 to 0

Planck 15 mois

Planck Collaboration, 2013

4. overview of observation facts



10

! 4.1 CMB

4.2 extragalactic background light



11

EBL (Extragalactic Background Light) tells us about

the processes

involved in

galaxy form

ation & evolution (budget for radiation em

ission by nucleosynthesis & gravitation, presence of dust, …

). All fundamental forces

are at play.

CIB

(Cosm

ic In

frare

d B

ackg

round

) leve

l and

stru

ctu

re

dep

en

d

on

his

tory

of

en

erg

y p

rod

uc

tion

in

the

po

st-re

co

mb

ina

tion

Unive

rse [Kashlinsky, 2005]

cosmological backgrounds



12 D

ole et al., 2006 ; Dole 2010 H

DR

D

ole & B

éthermin in prep

4.3 overview of observation facts

! spectrum of the CM

B ! large scale isotropy of the CM

B temperature

! small anisotropies of the CM

B temperature and polarization

! large-scale distribution of galaxies ! correlations (e.g. BAO

), redshifts, flux distribution etc.. ! galaxy clusters ! SN ! lensing on various tracors (CM

B, clusters, galaxies) ! quasars and absorption lines ! ...



13

scales of mass, dim

ension, d contrast



14

Yannick Mellier, IAP, 2002

Mass in Solar m

asses

Density contrast dρ/ρ"

photometric survey APM

, 1990



15

photometric near-infrared survey: 2M

ASS



16

2MASS + redshifts: structures



17

spectroscopic surveys



18

Peacock, 2002




19

Peacock, 2002




20

adapted from Springel, 2006, YM

spectroscopic survey VVDS



21

scales probed by SDSS



22 SDSS, D. Hogg

SDSS: - 8000 Sq. Deg. - 215e6 objets - 1e6 spectres - 15Tb de données en ligne

http://ww

w.sdss.org/dr8

strong & weak lensing



23

weak lensing -> DM

distribution



24

simulations



25

z=6

z=2

z=0 V. Springel http://w

ww.m

pa-garching.mpg.de/galform

/data_vis/

100 h-1 M

pc

simulations



26

V. Springel - Code: Hydra http://www.mpa-garching.mpg.de/galform/data_vis/

matter pow

er spectrum P(k)



27

other facts and tracors ! ellipticals vs disk galaxies:

physics of cooling ! G

alaxy clusters ! high-z galaxies

! infrared & submillim

eter ! Lym

an-a related sources ! forest ! em

itters ! break ! ERO

, LRGs

! gamm

a ray bursts ! supernovae ! background em

issions

! Baryonic Acoustic O

scillations ! other statistical properties

of galaxies ! lum

inosity function, number

counts, colors, n(z)



28

5. overview of structure and galaxy form

ation



29

structure and galaxy formation



30

Mo, van den Bosch, White fig 1.1

structure formation

galaxy form

ation

linear regime

non-linear regime

some tim

escales



31

Mo, van den Bosch, White sect 1.3

some tim

escales



32

Mo, van den Bosch, White sect 1.3

mass-radius relationship



33

Padmanabhan, 1993, fig1.1

tcool=tgrav line

tcool = cooling time

tgrav = timescale for

gravitational collapse

GMmp/R: potential well m

ass-radius relationship

hierarchical formation



34

Mo, van den Bosch, White fig 1.3

6. introduction to statistical tools: towards

the power spectrum



35

what is a pow

er spectrum ?



36

Fourier analysis

Courtesy Marc-Antoine Miville-Deschênes

Espace direct: tim

e

Espace conjugué: fréquence tem

porelle



37


1 sine centered

2 sine centered



38


n sinus décentrés

n sinus centrés



39


n sine not

centred

autosimilar

form

(fractal)



40


n sine not

centered

WM

AP 1 yr

multipoles applied to the CM

B



41

Hinshaw et al., 2007, W

MAP3

Ylm courtesy Benoit M

osser, LESIA

l=2

l=3

l=4

l=5

l=6

m2npac AdvancedCosmology201502 1ercours 2 obs hdole · AC Advanced Cosmology - Dole/Joyce/Langer 13...

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