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Astrophysical evidence for dark matter Galaxies Universe Theory - - PowerPoint PPT Presentation

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Astrophysical evidence for dark matter Luis Urea Introduction Astrophysical evidence for dark matter Galaxies Universe Theory DPyC-SMF FRWL Gravity BBang CMB Luis Urea BBN DM Dark Matter Pie Instituto de Fsica Dark energy

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SLIDE 1

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Astrophysical evidence for dark matter

DPyC-SMF Luis Ureña

Instituto de Física Universidad de Guanajuato and Instituto Avanzado de Cosmología (IAC) collaboration

21 Jun 2007 / Reunión Anual de la DPyC

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SLIDE 2

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

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SLIDE 3

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

slide-4
SLIDE 4

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

slide-5
SLIDE 5

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

slide-6
SLIDE 6

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 7

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Typical galaxies

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SLIDE 8

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 9

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Clusters of galaxies

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SLIDE 10

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

The whole observable universe

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SLIDE 11

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

CMB anisotropies

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SLIDE 12

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Supernovae type Ia

Observed day from peak Observed day from peak

Knop (2003)

  • et. al.

−40 40 80 120 1997ek z=0.86 −250 0.4 0.8 150 550 −40 40 80 120 −250 0.4 0.8 150 550 −40 40 80 120 1997eq z=0.54 −250 0.4 0.8 150 550 −40 40 80 120 −250 0.4 0.8 150 550 −40 40 80 120 1997ez z=0.78 −250 0.4 0.8 150 550 −40 40 80 120 −250 0.4 0.8 150 550 −40 40 80 120 1998as z=0.35 −250 0.4 0.8 150 350 −40 40 80 120 −250 0.4 0.8 150 550 −40 40 80 120 1998aw z=0.44 −450 0.4 0.8 150 550 −40 40 80 120 −450 0.4 0.8 150 550

normalized flux normalized flux normalized flux normalized flux normalized flux F814W F675W F814W F675W F675W R−band I−band

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 14

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Homogeneity and Isotropy (I)

  • The universe is spatially homogeneous and isotropic
  • We are not priviledged observers (Copernican principle)
  • The universe is isotropic around us (CMB)
  • Friedmann-Robertson-Walker-Lemaître (FRWL) metric

ds2 = −dt2+a2(t)  dψ2 +   sin2 ψ ψ2 sinh2 ψ   dΩ2      k = k = k =

  • Scale factor: a(t); Hubble parameter: H(t) = ˙

a/a

  • (cosmological) Redshift: a(z) = 1/(1 + z)
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Homogeneity and Isotropy (II)

  • Homogeneity: extrapolation from local measurements
  • Isotropy around any point leads to homogeneity
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Homogeneity and Isotropy (II)

  • Homogeneity: extrapolation from local measurements
  • Isotropy around any point leads to homogeneity
  • Sunyaev-Zeldovich effect: CMB scattering by hot gas in

clusters of galaxies

  • Expansion of the universe?
  • Dilation factor from SN Ia: (1 + z)1.07±0.06
  • CMB Temperature: T(z) = 2.73(1 + z) K
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SLIDE 17

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

General Relativity Theory

  • Energy-momentum tensor: T µ

ν = diag(−ρ, p, p, p)

  • Energy density: ρ
  • Isotropic pressure: p
  • Equation of state (EOS): p = ωρ
  • Conservation equation: T µν;ν = 0

˙ ρ + 3H(ρ + p) = 0 , ρ = ρ0a−3(1+ω)

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

General Relativity Theory

  • Energy-momentum tensor: T µ

ν = diag(−ρ, p, p, p)

  • Energy density: ρ
  • Isotropic pressure: p
  • Equation of state (EOS): p = ωρ
  • Conservation equation: T µν;ν = 0

˙ ρ + 3H(ρ + p) = 0 , ρ = ρ0a−3(1+ω)

  • Main matter components
  • Relativistic: ω = 1/3
  • non-Relativistic: ω = 0
  • Cosmological constant: ω = −1
  • Dark energy: ω < −2/3
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

General Relativity Theory

  • Einstein’s equations: Rµν − (1/2)gµνR = 8πG Tµν
  • Friedmann equation

H2 = 8πG 3

  • i

ρi − k a2

  • Acceleration equation

¨ a a = −4πG 3

  • i

(ρi + 3pi)

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

General Relativity Theory

  • Einstein’s equations: Rµν − (1/2)gµνR = 8πG Tµν
  • Friedmann equation

H2 = 8πG 3

  • i

ρi − k a2

  • Acceleration equation

¨ a a = −4πG 3

  • i

(ρi + 3pi)

  • Cosmological parameters
  • Density parameters: Ωi = ρi/ρc, Feq: 1 =

i Ωi − Ωk

  • Age of the Universe: ∼ 13.7 Gy

T0 = ∞

z0

dz (1 + z)H(z)

  • Size of the Universe: ∼ 40 Gl-y (∼ 12, 000 Mpc)

L0 = 1 1 + z0 ∞

z0

dz H(z)

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SLIDE 22

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 23

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

CMB anisotropies

  • Acoustic peaks from primordial plasma[1]
  • Origin at z = 1100
  • Measurements:
  • Curvature of the universe: ΩT = 1 − Ωk (flat)
  • Hubble parameter: H0 = 70.4+1.5

−1.6 km Mpc−1 s−1

  • Baryonic component: Ωb,0h2 = 0.02186 ± 00068

(Ωb,0 = 0.044)

  • Dark matter: Ωdm,0 = 0.268 ± 0.018
  • Dark energy: Ωde,0 = 0.732 ± 0.018
  • Inflation parameters: AS, ns
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

CMB anisotropies: Baryons and cold dark matter

2e-10 4e-10 6e-10 8e-10 1e-09 1.2e-09 1.4e-09 200 400 600 800 1000 1200 1400

(δT/T)2

l

l

Ω0b=0.013, Ω0dm=0.257 Ω0b=0.022, Ω0dm=0.248 Ω0b=0.044, Ω0dm=0.226 Ω0b=0.0065, Ω0dm=0.205 Ω0b=0.089, Ω0dm=0.181

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

CMB anisotropies: Anisotropy map

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

CMB anisotropies: WMAP3y

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SLIDE 27

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 28

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Nucleosynthesis, z ∼ 1010

  • Particle Physics in an expanding universe[2, 3]
  • Protons + neutrons + electrons + photons
  • Baryon to photon ratio: η10 = 1010(nb/nγ) = 274Ωbh2
  • Primordial elements: H, D, 3He, 4He, 7Li
  • Dependency on parameters
  • Gravitational constant G
  • Neutron lifetime τn
  • Fine structure constant α
  • Electron mass me
  • Average nucleon mass mN ≡ (mn + mp)/2
  • Neutron-proton mass difference QN ≡ mn − mp
  • Binding energies
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

BBN observations

0.00 0.20 0.40 0.60 0.80 1.00

Y

50 100 150 200 250 300

10 6 O/H

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Nucleosynthesis, z ∼ 1010

  • Particle Physics in an expanding universe[2, 3]
  • Protons + neutrons + electrons + photons
  • Baryon to photon ratio: η10 = 1010(nb/nγ) = 274Ωbh2
  • Primordial elements: H, 3He
  • Baryons: Ωb,0h2 = 0.0224 (WMAP 0.02186 ± 0.00068)

Abundances Observed Predictions

4He/H

0.249 ± 0.009 0.2478 ± 0.0002

3He/H

(1.1 ± 0.2) × 10−5 (1.03 ± 0.03) × 10−5

7Li/H

(1.5 ± 0.5) × 10−10 (4.5 ± 0.4) × 10−10

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SLIDE 31

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 32

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Dark universe!

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

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Degeneracy: Believe it or not! (All together)[2]

w = w0+2w’(1-a) 0.2 0.3 0.4

  • 0.05

0.0 0.05

ΩK ΩM

w = -1

  • 0.05

0.0 0.05

ΩK

Ned Wright - 22 Feb 07

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

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SLIDE 35

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

20

  • 21
  • 22
  • 23
  • 24
  • 25
  • 0.01
  • 0.02
  • 0.04
  • 0.1
  • 14
  • 16
  • 18
  • 20
  • 22
  • 24
  • 26
  • 0.4
  • 0.2
  • 0.6
  • 1.0
  • 0.4
  • 0.2
  • 0.6
  • 1.0
  • Magnitude
  • Redshift
  • Type Ia Supernovae
  • ΛCDM
  • OCDM
  • SCDM
  • r TCDM
  • Calan/Tololo

Supernova Survey

  • Supernova

Cosmology Project

  • fainter
  • Decelerating

Universe

  • Accelerating

Universe

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

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SLIDE 37

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

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SLIDE 38

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Cosmological constant

  • Origin: by hand T Λ

µν = (Λ/κ2)gµν

  • Nernst 1916; Lemaître 1934; Zel’dovich 1967
  • Ideas:
  • Adjustments mechanisms
  • Anthropic considerations
  • Changing gravity
  • Quantum gravity
  • Supergravity
  • Degenerate vacua
  • Higher dimensional gravity
  • Space-time foam
  • Vacuum fluctuations
  • String landscape
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Cosmological constant

  • Origin: by hand T Λ

µν = (Λ/κ2)gµν

  • Nernst 1916; Lemaître 1934; Zel’dovich 1967
  • Ideas:
  • Adjustments mechanisms
  • Anthropic considerations
  • Changing gravity
  • Quantum gravity
  • Supergravity
  • Degenerate vacua
  • Higher dimensional gravity
  • Space-time foam
  • Vacuum fluctuations
  • String landscape
  • Laboratory test of Newton’s Gravitational

Inverse-Square Law [4]

  • Valid for distances λ > 56µm
  • Size of extra dimensions: R < 44µm
  • Fundamental scale: M2

Pl = Mn+2Rn[5]

slide-40
SLIDE 40

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

slide-41
SLIDE 41

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Rotation curves [6]

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Modified Newtonian Dynamics: What if ..?[7]

  • Universal acceleration limit a0 ≃ 10−10 m/s2

F = ma ×

  • 1

a ≫ a0 µ(a/a0) a ≪ a0

  • Predicts Tully-Fischer relation
  • No-dark matter at all!
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Modified Newtonian Dynamics: What if ..?[7]

  • Universal acceleration limit a0 ≃ 10−10 m/s2

F = ma ×

  • 1

a ≫ a0 µ(a/a0) a ≪ a0

  • Predicts Tully-Fischer relation
  • No-dark matter at all!
  • Laboratory test of Newton’s Second Law
  • Valid for a > 5 × 10−14 m/s2
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Weak gravitational lensing (Bullet cluster 1E 0657-56)[8]

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Weak gravitational lensing (Bullet cluster 1E 0657-56)

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Weak gravitational lensing (CL0024+17)[9]

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Weak gravitational lensing (CL0024+17)[9]

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

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FRWL Gravity

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Structure formation

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

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Dark Matter Pie Dark energy Dark matter Strange models

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Weakly self-interacting dark matter

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SLIDE 50

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Weakly self-interacting dark matter

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SLIDE 51

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Outline

1

Introduction What are galaxies made of? What is the universe made of?

2

Theoretical Cosmology Homogeneity and Isotropy Cosmological dynamics

3

Big Bang Physics CMB anisotropies Nucleosynthesis

4

Dark Matters Brief summary of matter contents Dark energy Cold dark matter Candidates

slide-52
SLIDE 52

Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

WIMP’s

  • Boltzmann equation and freeze out
  • Neutral particle
  • Stable particle (lightest!)
  • Standard result

ΩXh2 ≃ 0.310−39cm2 σv

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

WIMP’s

  • Boltzmann equation and freeze out
  • Neutral particle
  • Stable particle (lightest!)
  • Standard result

ΩXh2 ≃ 0.310−39cm2 σv

  • Neutralino, gravitino, etc.
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

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Dark Matter Pie Dark energy Dark matter Strange models

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Wikipedia candidates

  • Scalar Field Dark Matter (SFDM, Matos, Guzmán &

Ureña-López)[10]

  • Strongly Interacting Massive Particle (SIMP)
  • Light Dark Matter
  • Self-interacting dark matter
  • Mirror matter
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Astrophysical evidence for dark matter Luis Ureña Introduction

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Summary

  • Pillars of BBC: GR (1915), BBN (1950’s), CMB (1992),

SN Ia (1998), BAO (2005)

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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Summary

  • Pillars of BBC: GR (1915), BBN (1950’s), CMB (1992),

SN Ia (1998), BAO (2005)

  • Non-exciting physics?: BBN (1950’s), CMB (1992), SN

Ia (1998), BAO (2005)

  • (Best) (Consistent) (Concordance) model: Flat ΛCDM
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Summary

  • Pillars of BBC: GR (1915), BBN (1950’s), CMB (1992),

SN Ia (1998), BAO (2005)

  • Non-exciting physics?: BBN (1950’s), CMB (1992), SN

Ia (1998), BAO (2005)

  • (Best) (Consistent) (Concordance) model: Flat ΛCDM
  • Outlook: New observations!
  • Gravitational waves (LISA)
  • Direct detection of dark matter (?)
  • Physics of the XXI’st century (?)
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Astrophysical evidence for dark matter Luis Ureña Introduction

Galaxies Universe

Theory

FRWL Gravity

BBang

CMB BBN

DM

Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

Summary

  • Pillars of BBC: GR (1915), BBN (1950’s), CMB (1992),

SN Ia (1998), BAO (2005)

  • Non-exciting physics?: BBN (1950’s), CMB (1992), SN

Ia (1998), BAO (2005)

  • (Best) (Consistent) (Concordance) model: Flat ΛCDM
  • Outlook: New observations!
  • Gravitational waves (LISA)
  • Direct detection of dark matter (?)
  • Physics of the XXI’st century (?)

How odd it is that anyone should not see that all

  • bservation must be for or against some view if it is

to be of any service! Charles Darwin (George Smoot, private communication)

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Galaxies Universe

Theory

FRWL Gravity

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CMB BBN

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Dark Matter Pie Dark energy Dark matter Strange models

Summary Bibliography

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Galaxies Universe

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FRWL Gravity

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Summary Bibliography

For further reading WMAP Collaboration, D. N. Spergel et al., “Wilkinson microwave anisotropy probe (wmap) three year results: Implications for cosmology,” astro-ph/0603449.

  • E. L. Wright, “Constraints on dark energy from

supernovae, gamma ray bursts, acoustic oscillations, nucleosynthesis and large scale structure and the hubble constant,” astro-ph/0701584.

  • T. Dent, S. Stern, and C. Wetterich, “Primordial

nucleosynthesis as a probe of fundamental physics parameters,” arXiv:0705.0696 [astro-ph].

  • D. J. Kapner et al., “Tests of the gravitational

inverse-square law below the dark-energy length scale,”

  • Phys. Rev. Lett. 98 (2007) 021101, hep-ph/0611184.
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  • A. Perez-Lorenzana, “An introduction to extra

dimensions,” J. Phys. Conf. Ser. 18 (2005) 224–269, hep-ph/0503177.

  • V. C. Rubin, N. Thonnard, and J. Ford, W. K.,

“Rotational properties of 21 sc galaxies with a large range of luminosities and radii, from ngc 4605 /r = 4kpc/ to ugc 2885 /r = 122 kpc/,” Astrophys. J. 238 (1980) 471.

  • M. Milgrom, “Mond–a pedagogical review,” Acta Phys.
  • Polon. B32 (2001) 3613, astro-ph/0112069.
  • D. Clowe, A. Gonzalez, and M. Markevitch, “Weak

lensing mass reconstruction of the interacting cluster 1e0657-558: Direct evidence for the existence of dark matter,” Astrophys. J. 604 (2004) 596–603, astro-ph/0312273.

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Summary Bibliography

  • M. J. Jee et al., “Discovery of a ringlike dark matter

structure in the core of the galaxy cluster cl 0024+17,” arXiv:0705.2171 [astro-ph].

  • T. Matos and L. A. Urena-Lopez, “On the nature of dark

matter,” Int. J. Mod. Phys. D13 (2004) 2287–2292, astro-ph/0406194.