cosmology principles
DESCRIPTION
CosmologyTRANSCRIPT
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CosmologyCosmologyCourseCourse
GustavoNizGustavoNiz
Camille Flammarion L'atmosphre: mtorologie populaire
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Content
Brief history & scales Observations & the CDM Model Understanding the CMB Inflation and the early Universe (EFTs in cosmology & the cosmic accelerator)
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Word of caution
Bayesiananalysis
1
2
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History&
Scales
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Cosmology until the twentieth century
Universe is finite and with the size of our galaxy (the milky way)
How to measure distancesnot well understood
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Cepheids
Discovered by E.Pigott & J. Goodricke, 1784
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Cepheids
Real luminocity depends on period (Henrietta Swan Leavitt, 1908)
Apparent luminocity (the one wemeasured on Earth) tell us what the distance is
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A bigger Universe
Edward Hubble (1924) measured distance to Cepheids and found them in Andromeda's Galaxy
Cepheids = steps on the distance ladder
Mount Wilson Observatory
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Universe is not static
Doppler effect
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Universe is not static
Redshift
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E. Hubble (1929)
Velocity = H * Distance
Universe is not static
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An old Universe
Velocity = Ho * Distance
Now
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Parsecs?
Parsec = 3.08x1016 m
1 AU
1''1 Pc
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Parsecs?Parsec = 3.08x1016 m
= 3.2 light years
Radius of visible Universe (particle horizon) 14.0 Gpc (~ 46 billion light years)
0.78 Mpc (2.5 million light-years)
30 kpc ~ 1,000,000,000,000,000,000 km~ 100,000 light years
Mpcs
~0.0000000001 pc
Andromeda
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Observations&
TheCDMmodel
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Hubble diagram today
Now we know:
0) Empty1) Big2) Expanding
(E. Hubble off by factor ~10)
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The big bang theory
Universe was HOT and DENSE in the past
Pillars0) FRWL metric + perts.1) Hubble diagram2) Nucleosynthesis3) Cosmic Microwave Radiation
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Thermal history
z=0 z=z=1
Half size
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Expansion
Misconceptions
No explosion Not an expansion into something else Expansion may be faster than c
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Thermal history
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Thermal history
300,000 years
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Cosmic Microwave Background (CMB) radiation
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CMB
T=2.7 K
Error 1K
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CMB
Radiation is Isotropic and Homogeneous
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CMB
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CMB
Gaussian~scale invariant
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CMB
Seeds of Large Scale Structure
(LSS)
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Other key observations
Dark Matter
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We do not understand what it is!
Only acts gravitationally and does not emit light
Best candidate: a weakly interacting particle that we have not seen yet
Or have we?
Dark matter
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Some experiments (Dama, CoGeNT, CDMS, etc.) have signals, hard to explain with known physics, but others
(Xenon, LUX) have not seen anything in the same regions.
Dark matter
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Or, could it be a modification of gravity?
Dark matter
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There are other objects (called supernovae IA) which also belong to the distance ladder. The supernovae are big star explosions.
SN 1987ARemanentede SN 1572 SN 1987A
Dark Energy
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Dark Energy
Hubble diagram with supernovas IA:
the Universe presentsaccelerated expansion
(5-sigma detection)
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We understand even less what it is!
Only acts gravitationally, but in a repulsive way
Best candidate: Cosmological Constant
Vacuum energy value?
Dark Energy
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5%
27%
68%
VisibleDark MatterDark Energy
??
Cosmic Pie (energy content)
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Important concepts:Isotropy and homogeneity
Building the theory
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On sufficiently large scales (>200Mpc) the Universe is isotropic and homogeneous
FilamentsVoids
SDSS
Building the theory
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Theory
Cosmological PrincipleAssume an isotropic and homogeneous metricFRWL
Open
Flat
Closed
Scalefactor
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TheoryFriedmann equationsEinstein equations with a perfect fluid reduce to
Open k = -1
Flat k = 0
Closed k = +1
From two aboveOr Bianchi id.
Energy conservation
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Theory
Critical Mass
Define in terms of critical mass
Friedmann eqn reduces to
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TheoryOne matter component (dust p=0)
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Theory
Scale factor evolution
t
MatterRadiation
Dark energy
p=1/3p=0
p=-1
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Theory
Scale factor evolution
t
MatterRadiation
Dark energy
Model fits ALL observations to great accuracy
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Perturbation Theory
But this is only the background!
What happens to perturbations?
Linear scales Vs Non-linear scales
Initial conditions? (later)
Density perturbations
Vectorperturbations
Tensorperturbations
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Perturbation Theory
But this is only the background!
What happens to perturbations?
Linear scales Vs Non-linear scales
Initial conditions? (later)
Density perturbations
Vectorperturbations
Tensorperturbations
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Linear theory
Othereffects
Non-linear theory
Relativistic effects
Strongly coupled NL theory
r=Ho^(-1) r=2GM
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Assume a perfect fluid, use the Newtonian limit
And that
Expanding on and solving iteratively
Density perturbations
Perturbation Theory
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Correlation function
In Fourier spacepower spectrum
Perturbation Theory
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Tegmark, M. et al. 2004
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Linear theory
r=Ho^(-1) r=GM
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UnderstandingtheCMB
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CMBConvenient to expand CMB anisotropies in spherical harmonics
The power spectrum is defined as
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CMB
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CMB
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~.25
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CMBWhat are these oscillations?
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CMBWhat are these oscillations?
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CMB
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UNIVERSE IS FLAT(error < 0.1%)
Planck, 2013
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~.25
Other peaks account for Visible Matter, Dark
Matter and Dark Energy
Planck, 20135%
27%
68%
VisibleDark MatterDark Energy
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Other effects in the CMB
Gravitaional lensing
Planck2015
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E & B modes
PolarisationEquivalent to Electric and
Magnetic fields
E B
Divergence Curl
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E & B modesRECALL
Surface
Unpolarised light
Linear polarisation
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E & B modes
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E & B modes
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E & B modes
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E and B
Zaldarriaga and Seljak, 1997
Spin raising andLowering operators
Non-localrelations
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E & B modesUsing spin two spherical harmonics (like usual spherical harmonics with additional U(1))
Stokes parametersZaldarriaga and Seljak, 1997
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E & B modesSpin raising/ lowering
Zaldarriaga and Seljak, 1997
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EE
BB
SMALL SIGNAL!
E & B modes
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Modos E y B
EE
BB
Amplitude depends on primordial fraction of gravitational waves
TT
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EE
BB
r=0
r=0.3
SMALL SIGNAL!
E & B modes
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Before BICEP2Foregrounds
B modes only
E & B modes
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BICEP 2
E & B modes
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BICEP2 bites the dust...
Planck dust 2014
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BICEP's Talk (John Kovac)
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B modes
TO QUANTUM GRAVITY
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TheearlyUniverse(inflation)
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Problems of the Big Bang Theory
1) Magnetic monopoles With many phase transitions why there are not any topological relics?2) Horizon problem Why disconnected region of space have same CMB temperature3) Size
4) Flatness
Expansion13.7 Gyrs
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Problems1) Magnetic monopoles With many phase transitions why there are any topological relics?2) Horizon problem Why disconnected region of space have same CMB temperature3) Size
4) Flatness
Expansion13.7 Gyrs
5) The initial (big bang) singularity
Problems of the Big Bang Theory
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Inflationary mechanism
Phase of exponential acceleration
t=10 s-35
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Inflationary mechanism
Simplest realisation: canonical scalar field slowly rolling down a potential
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InflationFriedmann equations read
If slow-roll is assumed (potential energy dominates over kinetic), then
which imply the following solution
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Inflation
Solves the Problems1) Magnetic monopoles Dilutes them2) Horizon problem A small patch was enlarged beyond the Hubble horizon 3) Size4) Flatness
5) Singularity problem remains
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InflationIn order to solve problems inflation should last
N =50 - 60 e-foldings
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Inflation
Slow-roll paramters
Should be roughly
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Inflation
Quantum fluctuations - BONUS
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Inflation
Quantum fluctuations - Evolution
k
R=1/(aH)
Baumann notes
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Inflation
Scalar perturbations
Changing variables
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Inflation
In slow-roll
It is a harmonic oscillator! Can quantise provided a vacuum (e.g. Bunch-Davis)
The two-point correlation function is
Where is the curvature perturbations
and k is wavenumber.
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One obtains
Which is complete agreement with the CMB
Planck (2013)
Remember scalar perturbations only produce E modes (Zaldarriaga & Seljak, 1997)
Inflation
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Tensor perturbations = gravity waves
Inflation
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Tensor perturbations = gravity waves
Also obtain a harmonic oscillator, and their power spectrum would be given by
We can define
These tensor modes produce both E and B modes (Zaldarriaga y Seljak, 1997)
Inflacin
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Tensor perturbations = gravity waves
Another way to write the potential is
r=0.01 results in GUT scale for inflation.
Inflation
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Tensor perturbations = gravity waves
Generically, one gets a bound (Lyth)
If r ~ 0.01 the field moves more than a Planck unit (large field models)
Perturbation theory stops being validand
One needs to understand quantum gravity corrections
Inflation
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Tensor perturbations = gravity waves
Inflation
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Inflation. Problems
But introduces new (or keeps) problems:
No explanation of amplitude in the CMB anisotropies
What is the inflaton (inflation's scalar field)?
Why did we start at the top of the potential?
Initial conditions (homogeneity and isotropy, the singularity)?
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Alternatives to inflation
1. Horava's gravity Speed of light is infinite in the UV, thus leading to scale invariance.
2. Cyclic models The contraction phase (if fast) can generate scale invariant fluctuations
3. EFT ( Effective field theories of inflation) Write down all possible relevant operators in the quantum gravity scale which are consistent with the symmetries (cf. SM).
Among others...
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TheCosmicAccelerator(EFTofLSS)
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EFTofLSSProgram
Inflation
Matter
Tracers
RedshiftPajer's talk, 2015
Dark EnergyDark MatterNon-GaussianityModified Gravity
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Non-linear theory
r=Ho^(-1) r=GM
EFT of LSS
All possible operators to describe non-linear perturbations in LSS
Capture small-large scale interactions (breaks perfect fluid approximation!)
Fix parameters with sims or data
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Cosmic accelerator
1) Most efforts in studying the propagator or two point correlation function (power spectrum)
2) What about higher correlation functions?
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Higher correlation functions
1) More data to break degeneracies between theories, calculate errors, etc.
2) Direct understanding of the theory behind our Universe (RG, inflacin, etc.)
3) Check small deviations from Gaussian (initial) conditions (f_NL).
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Higher correlation functions
4) Consistency relations
*Invariant under renormalization and baryon physics*Equivalence principle violations?
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UNIVERSIDADGUANAJUATODE
Grupode
GRAVITACINYFSICAMATEMTICA
8 Profesores3 Postdocs
15+ Estudiantes de Posgrado
Temas
CosmologaGravedad cunticaTeoras alternasGravedad modificadaTeora de cuerdas(astropartculas y partculas)
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UNIVERSIDADGUANAJUATODE
Postdocs: PROMEP CONACyT
Posgrados: MAESTRIA DOCTORADO
(Competencia Internacional CONACYT)
Website fisica.ugto.mx/~gfmContacto Gustavo Niz (responsable) [email protected]
Temas
CosmologaGravedad cunticaTeoras alternasGravedad modificadaTeora de cuerdas(astropartculas)
Grupode
GRAVITACINYFSICAMATEMTICA
8 Profesores3 Postdocs
15+ Estudiantes de Posgrado
Oportunidades
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Singularity theorems
Initial data (assuming some energy conditions) can lead, unavoidable, to geodesically incomplete space-times.
Global statement.
What about the analytical structure of fields near the singularity?
Penrose, Hawking (60-70's)
Extra slides: The singularity in GR
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Belinski, Khalatnikov and Lifshitz (BKL)
Assumed ultralocality :
spatial gradients are not as important as time derivatives!
Big Bang
System reduces to 1d, but may have strong dependence on the initial conditions!
Chaos
(e.g. Mixmaster)
Extra slides: The singularity in GR
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All depends on matter content: *scalar fields tend to remove chaos *gauge fields (p-forms) may restore it
Cosmological billiards
Damour et al '03Hamiltonian:
Near t=0,
Extra slides: The singularity in GR
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Away from walls:
Kasner metric
Extra slides: The singularity in GR
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*GeneralRelativity(d
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Note that there are potentials for the scalar fields which can overtake this oscillating behaviour, providing a deterministic evolution of the Universe.
However, for generic cases, we found a unpredictable behaviour of the metric near the spacetime singularity. We can even forget a description of the singularity itself.
Extra slides: The singularity in GR
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