What have we learned from observational cosmology? (observer s point of view) Jean-Christophe Hamilton CNRS - IN2P3 - APC - Paris
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1 What have we learned from observational cosmology? (observer s point of view) Jean-Christophe Hamilton CNRS - IN2P3 - APC - Paris
2 Outline!CDM: the concordance model Observational evidences for!cdm! The Cosmic Microwave Background and the early Universe! Dark Matter! Dark Energy! Tests of the cosmological principle! Tests of the Big-Bang paradigm Summary
3 !CDM foundations Assumptions General Relativity + Cosmological Principle Calculations!CDM FLRW Cosmological Model + ~12 Free parameters Many independent Observations + Fitting There is not much room out of this scheme! Recusing the cosmological principle (obs. constraints)! Extensions/modifications to G.R. (obs. constraints)! Modelling of the energy content of the Universe (obs. constraints + particle physics)
4 The!CDM model! FLRW expanding Universe (Hot Big-Bang) - General Relativity + Cosmological Principle - Hubble constant ~ 70 km.s -1.Mpc -1 - CMB blackbody, BigBang Nucleosynthesis! The Universe is ~ flat : "tot 1 - CMB anisotropies + Hubble constant! It contains ~ 22 % of Dark Matter (unknown) - Galaxies rotation curves, Clusters X, weak-lensing, Structure formation, CMB! It contains ~ 74% of Dark Energy (unknown) - SNIa fainter than expected further acceleration - CMB+H, direct measurements of "m, ISW effect
5 The!CDM model! FLRW expanding Universe (Hot Big-Bang) - General Relativity + Cosmological Principle - Hubble constant ~ 70 km.s -1.Mpc -1 - CMB blackbody, BigBang Nucleosynthesis! The Universe is ~ flat : "tot 1 - CMB anisotropies + Hubble constant! It contains ~ 22 % of Dark Matter (unknown) - Galaxies rotation curves, Clusters X, weak-lensing, Structure formation, CMB! It contains ~ 74% of Dark Energy (unknown) - SNIa fainter than expected further acceleration - CMB+H, direct measurements of "m, ISW effect [Kowalski et al. (2008)]
6 The!CDM model! FLRW expanding Universe (Hot Big-Bang) - General Relativity + Cosmological Principle - Hubble constant ~ 70 km.s -1.Mpc -1 - CMB blackbody, BigBang Nucleosynthesis! The Universe is ~ flat : "tot 1 - CMB anisotropies + Hubble constant 22!% Dark Energy Dark Matter Baryons 4!% 74!%! It contains ~ 22 % of Dark Matter (unknown) - Galaxies rotation curves, Clusters X, weak-lensing, Structure formation, CMB! It contains ~ 74% of Dark Energy (unknown) - SNIa fainter than expected further acceleration - CMB+H, direct measurements of "m, ISW effect [Kowalski et al. (2008)]
7 The!CDM model! FLRW expanding Universe (Hot Big-Bang) - General Relativity + Cosmological Principle - Hubble constant ~ 70 km.s -1.Mpc -1 - CMB blackbody, BigBang Nucleosynthesis! The Universe is ~ flat : "tot 1 - CMB anisotropies + Hubble constant Not Understood Dark but Energy well fitted Understood Dark and well Matter fitted Baryons 4!% 22!% 74!% 96!%! It contains ~ 22 % of Dark Matter (unknown) - Galaxies rotation curves, Clusters X, weak-lensing, Structure formation, CMB! It contains ~ 74% of Dark Energy (unknown) - SNIa fainter than expected further acceleration - CMB+H, direct measurements of "m, ISW effect [Kowalski et al. (2008)]
8 The!CDM model! FLRW expanding Universe (Hot Big-Bang) - General Relativity + Cosmological Principle - Hubble constant ~ 70 km.s -1.Mpc -1 - CMB blackbody, BigBang Nucleosynthesis! The Universe is ~ flat : "tot 1 - CMB anisotropies + Hubble constant Not Understood Dark but Energy well fitted Understood Dark and well Matter fitted Baryons 4!% 22!% 74!% 96!%! It contains ~ 22 % of Dark Matter (unknown) - Galaxies rotation curves, Clusters X, weak-lensing, Structure formation, CMB! It contains ~ 74% of Dark Energy (unknown) - SNIa fainter than expected further acceleration - CMB+H, direct measurements of "m, ISW effect [Kowalski et al. (2008)]
9 Cosmic Microwave background
10 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
11 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K (COBE/DMR homepage) Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
12 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K -1.4 mk (COBE/DMR homepage) +1.4 mk Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
13 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K -1.4 mk (COBE/DMR homepage) +/ / mk µk µk WMAP Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
14 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K -1.4 mk (COBE/DMR homepage) +/ / mk µk µk WMAP Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations Density Ionized Opaque Radiation Matter Neutral Transparent Dark Energy Time
15 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
16 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
17 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
18 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
19 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations
20 CMB Physics Origin! Early Universe - Ionized opaque to photons - thermal equilibrium! T << 13.6 ev - Neutral matter/radiation decoupling - CMB emitted. Blackbody at 3000K (z=1000) - Now blackbody at 3K Shape! Early Universe radiation dominated! at Matter/Radiation equality - Matter collapses in Dark Matter perturbations - Acoustic oscillations start, coherent w.r.t. scale! At Matter/Radiation decoupling - Oscillations frozen - CMB temperature reflects density fluctuations Power Large scales Small scales Angular scale
21 Influence of the cosmological parameters Sound horizon at decoupling Open Closed Flat Open Flat Closed Flat
22 Influence of the cosmological parameters Sound horizon at decoupling Open Closed Flat Actually slightly more complex due to the degeneracy with H et! Open Flat Closed Flat WMAP 7y
23 Influence of the cosmological parameters Sound horizon at decoupling Open Closed Flat Actually slightly more complex due to the degeneracy with H et! Open Flat Closed Flat [Kowalski et al. (2008)] WMAP 7y
24 Influence of the cosmological parameters Sound horizon at decoupling Open Dark Energy Dark Matter Baryons 4!% Closed Flat 22!% Actually slightly more complex due to 74!% the degeneracy with H et! Open Flat Closed Flat [Kowalski et al. (2008)] WMAP 7y
25 Tremendous progress over the last decade South Pole Telescope arxiv: Huge success : thousands of independant points fitted with less than 10 parameters and a # 2 /ndf about 1 Theoretical curve predicted in 1987 [Bond & Efstathiou] without any data...
26 Predicted long ago! electrons/photons scattering before decoupling CMB Polarization Detection 2001! DASI et CBI (interferometers) Later measurements:! WMAP, QUAD, BICEP...! Perfect agreement with temperature measurements Correspondance between TT peaks and EE troughs! Typical of adiabatic primordial fluctuations (generated by inflation for instance...) [QUAD Collaboration: Arxiv: ]
27 Predicted long ago! electrons/photons scattering before decoupling CMB Polarization Detection 2001! DASI et CBI (interferometers) Later measurements:! WMAP, QUAD, BICEP...! Perfect agreement with temperature measurements Correspondance between TT peaks and EE troughs! Typical of adiabatic primordial fluctuations (generated by inflation for instance...) [QUAD Collaboration: Arxiv: ]
28 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves
29 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K Big-Bang confirmed... Where are the anisotropies? 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves
30 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves
31 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured Topological defects excluded Inflation favoured Evidence for flatness 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves
32 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured Topological defects excluded Inflation favoured Evidence for flatness Major prediction confirmed
33 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured Topological defects excluded Inflation favoured Evidence for flatness Major prediction confirmed Confirmation of adiabatic primordial perturbations Precision cosmology
34 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured Topological defects excluded Inflation favoured Evidence for flatness Major prediction confirmed Confirmation of adiabatic primordial perturbations Precision cosmology Ultimate T and E spectra factor 3 gain on cosmological parameters
35 Major steps for CMB 1965: Dicovery by Penzias & Wilson! Isotropic black-body radiation at T~3K 1992: COBE! Anisotropies discovered DT/T=10-5! Black-body confirmed 1999: Boomerang and Maxima! First acoustic peak discovered 2001: DASI & CBI! Polarization detection 2003: WMAP! Exquisite full-sky measurement of T and E 2013: Planck! Ultimate measurements of T and E 20XX: B-modes experiments! primordial gravitational waves Big-Bang confirmed... Where are the anisotropies? Cold Dark Matter strongly favoured Topological defects excluded Inflation favoured Evidence for flatness Major prediction confirmed Confirmation of adiabatic primordial perturbations Precision cosmology Ultimate T and E spectra factor 3 gain on cosmological parameters Exploration of inflationary physics
36 Primordial fluctuations: where are we standing? Inflation predictions Flatness, Homogeneity Nature of perturbations:! TT peaks at the same location as EE troughs [predicted] " Adiabatic perturbations Spectral index! SPT+WMAP [arxiv: ] n s = ± " Almost scale invariant spectrum [predicted] P (k) k n s 1 Gaussianity! No convincing evidence for non-gaussianity (despite impressive efforts) Tensor perturbations of the metric! No B-mode detection (yet...)!!!!?
37 Primordial fluctuations: where are we standing? Inflation predictions Flatness, Homogeneity Nature of perturbations:! TT peaks at the same location as EE troughs [predicted] " Adiabatic perturbations Spectral index! SPT+WMAP [arxiv: ] n s = ± " Almost scale invariant spectrum [predicted] P (k) k n s 1 Gaussianity! No convincing evidence for non-gaussianity (despite impressive efforts) Tensor perturbations of the metric! No B-mode detection (yet...)!!!!?
38 Dark Matter Bullet Cluster
39 Dark Matter Clusters dynamics:! Zwicky velocity dispersion gives kinetic energy - Distances between galaxies gives potential energy - Virial theorem allows to infer mass times larger than stellar mass Coma cluster (image X: ROSAT)! X emission from hot gaz in clusters - gaz far more extended than galaxies in clusters - BUT: - gaz can account for a factor 2 in mass - gaz needs to be heated to K " ~85% dark matter needed Galaxies rotation curves! Stars velocities too high in outer parts! well explained by a dark matter halo with ~ 200 times the stellar mass
40 Dark Matter Clusters dynamics:! Zwicky velocity dispersion gives kinetic energy - Distances between galaxies gives potential energy - Virial theorem allows to infer mass times larger than stellar mass Coma cluster (image X: ROSAT)! X emission from hot gaz in clusters - gaz far more extended than galaxies in clusters - BUT: - gaz can account for a factor 2 in mass - gaz needs to be heated to K " ~85% dark matter needed Galaxies rotation curves! Stars velocities too high in outer parts! well explained by a dark matter halo with ~ 200 times the stellar mass
41 The Bullet Cluster Visible image (Galaxies)
42 The Bullet Cluster Visible image (Galaxies) X image (gaz) - Chandra
43 The Bullet Cluster Visible image (Galaxies) X image (gaz) + weak lensing contours (mass) X image (gaz) - Chandra
44 The Bullet Cluster Visible image (Galaxies) Visible : Galaxies X : Gaz Lensing : mass X image (gaz) + weak lensing contours (mass) X image (gaz) - Chandra
45 Bullet Cluster Collision of two clusters Galaxies and dark matter are non collisional! They pass without seeing each other Gaz is collisional! it stays at the center and is heated! Shock waves appear Simulation Chandra Visible : Galaxies X : Gaz Lensing : mass Strongest argument for Dark Matter?
46 but... there exists a counter example... Abell 520 z=0.02 [Mahdavi et al. 2007] Dark Matter core coincides with gaz, not with galaxies... [From F. Combes]
47 Structure formation requires Dark Matter Primordial anisotropies! very weak from CMB: 1/ Gravitational collapse! starts at matter-radiation equality for ordinary matter! Then expansion slows down the contraction! This is not enough to explain observations HDM! More matter is needed! Some matter needs to start collapsing earlier - Needs to be decoupled earlier than baryons...! Needs to be slow enough (heavy) so that small structures form Cold Dark Matter required (CDM) MDM CDM
48 Structure formation requires Dark Matter Primordial anisotropies! very weak from CMB: 1/ Gravitational collapse! starts at matter-radiation equality for ordinary matter! Then expansion slows down the contraction! This is not enough to explain observations HDM! More matter is needed! Some matter needs to start collapsing earlier - Needs to be decoupled earlier than baryons...! Needs to be slow enough (heavy) so that small structures form Cold Dark Matter required (CDM) MDM CDM
49 Baryonic Acoustic Oscillations BAO:! Acoustic Oscillations: - between matter/radiation equality and decoupling - Sound wave propagation - Stops at decoupling " Observed in the CMB! Now: - Each D.M. peak surrounded by a spherical excess " Galaxies prefereably form there - peak in the 2-pts correlation function of matter - Standard ruler for angular distance test! Meaning: - Prediction confirmed! at the right place! - This is among the strongest evidences for "m=0.3 and the presence of Dark Matter! m h 2 = 0.12! m h 2 = 0.13! m h 2 = 0.14 [Eisenstein et al., 2005]
50 Baryonic Acoustic Oscillations BAO:! Acoustic Oscillations: - between matter/radiation equality and decoupling - Sound wave propagation - Stops at decoupling " Observed in the CMB! Now: - Each D.M. peak surrounded by a spherical excess " Galaxies prefereably form there - peak in the 2-pts correlation function of matter - Standard ruler for angular distance test! Meaning: - Prediction confirmed! at the right place! - This is among the strongest evidences for "m=0.3 and the presence of Dark Matter! m h 2 = 0.12! m h 2 = 0.13! m h 2 = 0.14 [Eisenstein et al., 2005]
51 BAO support Dark Matter With Dark Matter (LCDM)! m h 2 = 0.12! m h 2 = 0.13! m h 2 = 0.14 [Eisenstein et al., 2005] Without Dark Matter (LCDM)!CDM No Dark Matter
52 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the late 90s Excluded Particle Physics Modifications of Gravity
53 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the 90s Particle Physics! Supersymetry - minimal models seem disfavored by LHC - Resists direct search (Edelweiss, CDMS, Xenon) - BUT: DAMA, COGENT, CRESST claim for detection! Extra dimensions, Axions LHC feb Modifications of Gravity
54 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the 90s Particle Physics! Supersymetry - minimal models seem disfavored by LHC - Resists direct search (Edelweiss, CDMS, Xenon) - BUT: DAMA, COGENT, CRESST claim for detection! Extra dimensions, Axions LHC feb Modifications of Gravity Early 90s SuSy evolution Today
55 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the 90s Particle Physics! Supersymetry - minimal models seem disfavored by LHC - Resists direct search (Edelweiss, CDMS, Xenon) - BUT: DAMA, COGENT, CRESST claim for detection! Extra dimensions, Axions LHC feb [CRESST arxiv: ] Modifications of Gravity
56 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the 90s Particle Physics! Supersymetry - minimal models seem disfavored by LHC - Resists direct search (Edelweiss, CDMS, Xenon) - BUT: DAMA, COGENT, CRESST claim for detection! Extra dimensions, Axions Modifications of Gravity! D.M. is only seen through gravitationnal effects! MOND/TeVeS
57 MOND new fundamental principle of dynamics: F = m a 2 a 0 si a<a 0 ma si a>a 0 Newton force: F = GMm r 2 Circular orbit: a = v2 r MOND Newton Dynamics: GM r 2 = a2 a 0 a = GMa 0 r v2 r = GMa 0 r v =(GMa 0 ) 1/4 L M v 4 Flat rotation curves Tully-Fisher relation x x v2 GM r 2 = a r = GMr 2 GM v = r L M rv 2 Impressive but MOND fails on everything else...
58 Candidates for Dark Matter Compact objects - Black holes, brown dwarfs - Essentially excluded in the 90s Particle Physics! Supersymetry - minimal models seem disfavored by LHC - Resists direct search (Edelweiss, CDMS, Xenon) - BUT: DAMA, COGENT, CRESST claim for detection! Extra dimensions, Axions Modifications of Gravity! D.M. is only seen through gravitationnal effects! MOND/TeVeS: appealing but... - still requires a lot of neutrinos to explain galaxy rotation curves and clusters and CMB - CMB hard to fit now, obvious disagreement with BAO observed in distribution of galaxies - Does it really seem more sensible than D.M.? F = MOND+$ [Skordis et al. 2006] m a 2!CDM a 0 si a<a 0 ma si a>a 0
59 Dark Energy
60 SNIa: accelerated expansion (1998) Standard candles! bright (more that host galaxy)! standardizable (within ~ 0.15 mag) Luminosity distance Vs. z! SNIa fainter than expected! Possible systematics well controlled B Band as measured M B 5 log(h/65) Calan/Tololo SNe Ia days Kim (1996)
61 SNIa: accelerated expansion (1998) Standard candles! bright (more that host galaxy)! standardizable (within ~ 0.15 mag) Luminosity distance Vs. z! SNIa fainter than expected! Possible systematics well controlled M B B 5 5 log(h/65) B Band light-curve timescale as measured stretch-factor corrected Calan/Tololo SNe Ia days Kim (1996)
62 SNIa: accelerated expansion (1998) Standard candles! bright (more that host galaxy)! standardizable (within ~ 0.15 mag) Luminosity distance Vs. z! SNIa fainter than expected! Possible systematics well controlled M B B 5 5 log(h/65) B Band light-curve timescale as measured stretch-factor corrected Calan/Tololo SNe Ia days Kim (1996)
63 SNIa: accelerated expansion (1998) Standard candles! bright (more that host galaxy)! standardizable (within ~ 0.15 mag) Luminosity distance Vs. z! SNIa fainter than expected! Possible systematics well controlled M B B 5 5 log(h/65) B Band light-curve timescale as measured stretch-factor corrected Calan/Tololo SNe Ia days Kim (1996)
64 SNIa: accelerated expansion (1998) Standard candles! bright (more that host galaxy)! standardizable (within ~ 0.15 mag) Luminosity distance Vs. z! SNIa fainter than expected! Possible systematics well controlled M B B 5 5 log(h/65) B Band light-curve timescale as measured stretch-factor corrected Present results Calan/Tololo SNe Ia days Kim (1996)
65 Actually, the idea was around...
66 Actually, the idea was around...
67 Cosmic substraction: 1-0.3=0.7 "m ~ 0.3 From R. Kolb
68 evidence for D.E. from CMB alone WMAP 7y WMAP 7y + ACT (no H0) [Sherwin et al. 2011]
69 ISW effect: independent probe Integrated Sachs-Wolfe effect! Photons gain energy falling into clusters potential wells! They loose energy escaping! In the presence of Dark Energy the net result is not zero " Correlation between CMB hot/cold spot expected with foreground clusters/voids CMB map with positions of known foreground clusters and voids Stacking [Granett et al. 2008] " 4% level detection by various teams " N.B. expected effect is zero if no D.E. (or more generally if no acceleration) [Granett et al. 2008]
70 Finally, with latest data Dark Energy Equation of state: p = wρ! w=-1 pure cosmological constant (or scalar field)
71 Bug or reality? So the Universe really seems to be accelerating...! «we are in a void» explanation excluded by lack of ksz effect [Zhang and Stebbins 2011] " D.E.~0.7 with and equation of state w~-1! It really looks like a cosmological constant! or maybe a scalar field depending on which side in Einstein s Equation R µν 1 2 g µνr Λg µν = 8πG c 4 T µν or R µν 1 2 g µνr = 8πG c 4 T µν + Λg µν Now... is it really serious?! No scalar field has ever been observed! Strong disagreement with particle physics vacuum - From H0 and "! :!~10-52 m -2 - From Planck scale physics:!~10 70 m-2! Something deep is obviously not understood...
72 Tests of the Cosmological principle Miko"aj Kopernik
73 Cosmological Principle tests At first a simplifying hypothesis Isotropy tested with increasing success (here z~1) 470 Millions objects, 1.5 million on the way of being spectred
74 Cosmological Principle tests At first a simplifying hypothesis Isotropy tested with increasing success (here z~1000) (COBE/DMR homepage) corps noir à 3 K
75 Cosmological Principle tests At first a simplifying hypothesis Isotropy tested with increasing success (here z~1000) (COBE/DMR homepage) +/- 30 µk corps noir &T/T=10 à 3 K -5 WMAP
76 Cosmological Principle tests At first a simplifying hypothesis Isotropy tested with increasing success If Copernican principle is assumed! Every observer would see similar matter/cmb distribution " homogeneity follows [Maartens, 2011]! But no strong observational basis for Copernican principle... Testing the Copernican Principle! Spectral distorsions on the CMB - Black-Body nature [Caldwell and Stebbins, 2008] - lack of kinetic-sz effect on small scales [Zhang and Stebbins, 2010]! future: time drifts of cosmological redshifts [Uzan et al, 2008] Basically it seems fine...
77 Tests of the Hot Big- Bang paradigm
78 Hubble s law Long debate on H0 value Now stabilized: H0 = 72 ± 3(stat) ± 7(syst)! main systematics: - Cepheids metallicity - Distance to LMC Hubble s original data Freedman et al. (2001) 1927 : H0 ~ 500 km/s/mpc 2001: H0 = 72 km/s/mpc
![Age of stars supports!cdm Oldest stars in Milky Way globular clusters:! age > 11.2 Gyr (95% C.L.) [Krauss & Chaboyer, 2003] 1.0 Age of the Universe (Gyr) 15 0.](/docs-images/85/92619824/images/79-3.jpg "8 14 Time since Big-Bang depends on content in FLRW! in open \"m=0.3 : 11.3 Gyr! in flat \"m=1 : 9.2 Gyr! in!cdm : 13.7 Gyr Ω Λ 0.6 0.4 0.2 ΛCDM Oldest stars : 11.")
79 Age of stars supports!cdm Oldest stars in Milky Way globular clusters:! age > 11.2 Gyr (95% C.L.) [Krauss & Chaboyer, 2003] 1.0 Age of the Universe (Gyr) Time since Big-Bang depends on content in FLRW! in open "m=0.3 : 11.3 Gyr! in flat "m=1 : 9.2 Gyr! in!cdm : 13.7 Gyr Ω Λ ΛCDM Oldest stars : 11.2 Gyr But: SDSS J ! Ridiculously low metals, no Li, age~13 Gyr? Ω m
80 Black Body spectrum of the CMB Thermal equilibrium in the past! photons: small mean free path in the hot plasma! decoupled when Universe becomes neutral! Black Body observed today Tests of T CMB as a function of z! Low-z: S-Z effect in clusters (scattering of CMB photons on the hot gas)! High-z: rotational excitation of the CO molecules in QSOs absorption systemas Mather et al. In perfect agreement with!cdm Noterdaeme et al., 2010
81 Primordial nucleosynthesis Gamow 1948:! Earlier (high T) nuclei were broken - in early times: ',p,n - form nuclei when T is low enough - Nuclear reactions stop when T too low! Abundances calculated from theory! free parameter: fraction of baryons "b Difficult measurements:! Fusion in stars modify the picture - Metal poor stars, Ly-( forest of QSOs Excellent agreement! Matches CMB "b! possible problem: 7 Li - Maybe... but measurement is extremely difficult (could be burnt in stars)! N.B.: "bh 2 ~0.02 is small... " open Universe or dark stuff?
82 Primordial nucleosynthesis Gamow 1948:! Earlier (high T) nuclei were broken - in early times: ',p,n - form nuclei when T is low enough - Nuclear reactions stop when T too low! Abundances calculated from theory! free parameter: fraction of baryons "b Difficult measurements:! Fusion in stars modify the picture - Metal poor stars, Ly-( forest of QSOs Excellent agreement! Matches CMB "b! possible problem: 7 Li - Maybe... but measurement is extremely difficult (could be burnt in stars)! N.B.: "bh 2 ~0.02 is small... " open Universe or dark stuff?
83 Primordial nucleosynthesis Gamow 1948:! Earlier (high T) nuclei were broken - in early times: ',p,n - form nuclei when T is low enough - Nuclear reactions stop when T too low! Abundances calculated from theory! free parameter: fraction of baryons "b Difficult measurements:! Fusion in stars modify the picture - Metal poor stars, Ly-( forest of QSOs Excellent agreement! Matches CMB "b! possible problem: 7 Li - Maybe... but measurement is extremely difficult (could be burnt in stars)! N.B.: "bh 2 ~0.02 is small... " open Universe or dark stuff?
84 Primordial nucleosynthesis Gamow 1948:! Earlier (high T) nuclei were broken - in early times: ',p,n - form nuclei when T is low enough - Nuclear reactions stop when T too low! Abundances calculated from theory! free parameter: fraction of baryons "b Theory Data Difficult measurements:! Fusion in stars modify the picture - Metal poor stars, Ly-( forest of QSOs Excellent agreement! Matches CMB "b! possible problem: 7 Li - Maybe... but measurement is extremely difficult (could be burnt in stars)! N.B.: "bh 2 ~0.02 is small... " open Universe or dark stuff?
85 Primordial nucleosynthesis Gamow 1948:! Earlier (high T) nuclei were broken - in early times: ',p,n - form nuclei when T is low enough - Nuclear reactions stop when T too low! Abundances calculated from theory! free parameter: fraction of baryons "b Theory Data Difficult measurements:! Fusion in stars modify the picture - Metal poor stars, Ly-( forest of QSOs Excellent agreement! Matches CMB "b! possible problem: 7 Li - Maybe... but measurement is extremely difficult (could be burnt in stars)! N.B.: "bh 2 ~0.02 is small... " open Universe or dark stuff?
86 Reionization Dark ages & reionization! Neutral medium after CMB realease - UV light is absorbed by neutral H - Universe opaque to starlight! First stars & QSOs produce UV - Universe starts to reionize - UV absorption less efficient - Reionization complete at z~6 - Universe transparent to UV Test: Gunn-Peterson effect! Light from 1st quasars should be completely absorbed up to H-alpha line! In more recent quasars one should see partial absorption only (Ly-( forest)! Predicted long before observation Reionization epoch dating matches CMB inferred one
87 !CDM Problems
88 Dark Matter Dark Energy BBN Lithium problem! + star SDSS J ?!CDM Issues Galactic-scale dynamics: - Even with D.M., the «bullet cluster» is weird: - Gaz shock seems to involve huge velocities that are not expected in!cdm - not enough satellites w.r.t. simulations - Tully Fisher relation is empirical in!cdm but explained in MOND - cusps at center of galaxies unobserved " Most of this could be explained by lack of realism or resolution of simulations... CMB low multipoles/axis of evil " not serious (just my two cents) Bullet Cluster like simulations [Lee and Komatsu, 2010] [Kravstsov et al. 2004] Bullet Cluster
89 Conclusions (as an observer)!cdm has firm theoretical and observational basis! Confirmed by independent probes! Successfully predictive - CMB fluctuations/polarization, odd/even peaks, scalar index slightly below 1 - BAO - Gunn-Peterson effect Requires large amounts of unobserved/unexplained stuff! Dark Matter! Dark Energy " Both very convincing from the observational point of view Also requires complex analysis of complex data! In most cases analyses are well tested for robustness w.r.t. assumptions! Complexity doesn t make it wrong Cosmology is obviously not finished, maybe just starting...! «C est à la fin du bal qu on paie les musiciens...»
90
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