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GRAVITATIONAL WAVES AND COSMOLOGY [[electronic resource].]. — AMSTERDAM: IOS PRESS, 2020. — 1 online resource — <URL:http://elib.fa.ru/ebsco/2632788.pdf>.Дата создания записи: 26.09.2020 Тематика: Gravitational waves.; Cosmology. Коллекции: EBSCO Разрешенные действия: –
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Оглавление
- Title Page
- Contents
- Preface
- Course group shot
- F. Fidecaro - Principles of gravitational wave detection
- 1. The detection of gravitational waves
- 1.1. Gravitational waves
- 1.2. Effect on a single mass
- 1.3. Effect on a pair of masses
- 1.4. The laboratory frame
- 2. Essential properties
- 2.1. Distance ladder
- 2.2. Expected amplitude
- 2.3. Compact objects
- 2.4. Single compact objects
- 2.5. Supernovae
- 2.6. The indirect evidence for gravitational radiation: PSR 1913+16
- 3. Signals and noise
- 3.1. Noise power spectrum
- 3.2. Power spectra in practice
- 3.3. Power spectrum in digitized signals
- 3.4. Signal and noise
- 3.5. Optimal filtering
- 4. Primary noise sources in gravitational wave interferometers
- 5. Position noise
- 5.1. Seismic noise
- 5.2. Seismic attenuation
- 5.3. The Virgo Superattenuator
- 5.4. Thermal noise
- 5.5. Fluctuation-Dissipation theorem
- 5.6. Thermal noise mitigation
- 5.7. Newtonian noise
- 6. Measurement noise
- 6.1. Michelson-Morley interferometry
- 6.2. Fabry-Perot cavities
- 6.3. Power recycling
- 6.4. Standard quantum limit
- 7. Noise curve
- 8. Ending remarks
- 1. The detection of gravitational waves
- Fulvio Ricci - A primer on a real gravitational wave detector
- 1. Introduction
- 2. The modulation
- 3. The detection of the modulation component
- 4. The readout of the output signal
- 5. The Fabry-Perot cavities as Michelson arms
- 5.1. More about the Fabry-Perot cavities
- 6. How to keep the FP cavities in resonance
- 7. The gravitational wave interferometer
- 8. The interferometer control
- 9. The sensitivity curve
- 10. Thermal noise and cryogenics for future gravitational wave detectors
- 11. Reduction of the readout noise
- 12. Conclusion
- Viviana Fafone - Optical aberrations in gravitational wave detectors and a look at the future
- 1. Introduction
- 2. Optical aberrations and their effects
- 3. Correction of optical aberrations
- 4. Mid and longer term perspective for ground-based detectors
- Michela Mapelli - Astrophysics of stellar black holes
- 1. Lesson learned from the first direct gravitational wave detections
- 2. The formation of compact remnants from stellar evolution and supernova explosions
- 2.1. Stellar winds and stellar evolution
- 2.2. Supernovae (SNe)
- 2.3. The mass of compact remnants
- 3. Binaries of stellar black holes
- 3.1. Mass transfer
- 3.2. Common envelope (CE)
- 3.3. Alternative evolution to CE
- 4. The dynamics of black hole binaries
- 4.1. Dynamically active environments
- 4.2. Three-body encounters
- 4.3. Exchanges
- 4.4. Hardening
- 4.5. Dynamical ejections
- 4.6. Formation of intermediate-mass black holes by runaway collisions
- 4.7. Formation of intermediate-mass black holes by repeated mergers
- 4.8. Kozai-Lidov resonance
- 4.9. Summary of dynamics and open issues
- 5. Black hole binaries in cosmological context
- 5.1. Analytic prescriptions
- 5.2. Cosmological simulations
- 6. Summary and outlook
- Marica Branchesi - GW170817: the dawn of multi-messenger astronomy including gravitational waves
- 1. The first gravitational-wave observation of the coalescence of a binary system of neutron stars
- 2. Discovery of the high-energy counterpart
- 3. The multi-wavelength electromagnetic follow-up campaign
- Douglas Scott - The standard model of cosmology: A skeptic's guide
- 1. What is the standard model of cosmology?
- 2. The parameters and assumptions of the SMC
- 3. The numbers that describe the Universe
- 4. Information in the SMC
- 5. The venerableness of the SMC
- 6. Tensions
- 7. Anomalies
- 8. The nature of skepticism
- 9. Beyond the SMC
- 10. Conclusions
- J. Martin - The theory of inflation
- 1. Introduction
- 2. Why inflation?
- 2.1. The pre-inflationary standard model
- 2.2. The puzzles of the standard model
- 2.3. Basics of inflation
- 3. Inflationary cosmological perturbations
- 4. Extensions
- 5. Inflation and CMB observations
- 6. Conclusions
- M. Celoria and S. Matarrese - Primordial Non-Gaussianity
- 1. Introduction
- 1.1. Historical outline
- 2. Non-Gaussianity in the initial conditions
- 2.1. Non-Gaussianity and higher-order statistics
- 2.2. Bispectrum of a self-interacting scalar field in de Sitter space
- 2.3. Shapes of non-Gaussianity from inflation
- 2.4. The role of fNL and the detection of primordial non-Gaussianity
- 3. Non-Gaussianity and Cosmic Microwave Background
- 3.1. Planck results on primordial non-Gaussianity
- 3.2. Implications for inflation
- 3.3. Primordial non-Gaussianity with CMB spectral distorsions
- 4. Primordial Non-Gaussianity and the Large-Scale Structure
- 4.1. Non-Gaussianity and halo mass function
- 4.2. Halo bias in NG models
- 4.3. PNG with LSS: the galaxy bispectrum
- 5. Controversial issues on non-Gaussianity
- 5.1. Single-field consistency relation
- 5.2. Non-Gaussian fNL-like terms generated by non-linear general relativistic evolution
- 6. Concluding remarks
- 1. Introduction
- Wayne Hu - CMB polarization theory
- 1. Introduction
- 2. Sources of CMB polarization
- 3. Acoustic source
- 4. Inflation source
- 5. Reionization source
- 6. Lensing distortion
- 7. Discussion
- C. Burigana and T. Trombetti on behalf of the Planck Collaboration - The legacy of Planck
- 1. Introduction
- 2. The Planck mission
- 3. Control of systematic effects
- 4. Astrophysical foregrounds
- 4.1. Catalogs of sources and clusters of galaxies
- 4.2. Galactic diffuse components
- 5. Main implications for cosmology and fundamental physics
- 5.1. Cosmological results
- 5.2. Fundamental physics results
- 5.3. Constraints on primordial B-modes
- 6. Towards future CMB missions
- 6.1. CMB mission proposals at degree resolution
- 6.2. CMB mission proposals at sub-degree resolution
- Jens Chluba - Future steps in cosmology using spectral distortions of the cosmic microwave background
- 1. Overview and motivation
- 1.1. Why are spectral distortions so interesting today
- 1.2. Overview and goal of the lecture
- 2. The physics of CMB spectral distortions
- 2.1. Simple blackbody relations
- 2.2. Photon energy and number density
- 2.3. What we need to do to change the blackbody temperature
- 2.4. What is the thermalization problem all about
- 2.5. General conditions relevant to the thermalization problem
- 2.6. Photon Boltzmann equation for average spectrum
- 2.7. Collision term for Compton scattering
- 2.7.1. Comptonization efficiency
- 2.8. Bremsstrahlung and double Compton emission
- 3. Types of spectral distortions from energy release
- 3.1. Scattering of CMB photons in the limit of small y-parameter
- 3.1.1. Thermal Sunyaev-Zeldovich effect
- 3.2. Chemical potential or mu-distortion
- 3.2.1. Compton equilibrium solution
- 3.2.2. Definition of the mu-distortion
- 3.2.3. But how do we define the distortion?
- 3.3. Simple description of primordial distortions
- 3.3.1. Inclusion of photon production in the mu-era
- 3.3.2. The importance of double Compton emission
- 3.4. Modeling the transition between mu and y
- 3.5. Distortions from photon injection
- 3.1. Scattering of CMB photons in the limit of small y-parameter
- 4. CMB spectral distortion signals from various scenarios
- 4.1. Reionization and structure formation
- 4.2. Damping of primordial small-scale perturbations
- 4.3. Adiabatic cooling for baryons
- 4.4. The cosmological recombination radiation
- 4.5. Dark matter annihilation
- 4.6. Decaying particle scenarios
- 4.7. Anisotropic CMB distortions
- 5. Conclusions
- 1. Overview and motivation
- Will J. Percival - Recent developments in the analysis of galaxy surveys
- 1. Introduction
- 2. The overdensity field
- 3. Line-of-sight assumptions
- 4. Multipole moments
- 5. Correlation function estimators in the local plane-parallel formalism
- 6. Power spectrum estimators in the global plane-parallel formalism
- 7. Power spectrum estimators in the local plane-parallel formalism
- 8. Grid assignment, aliasing and interlacing
- 9. Linking Fourier and Fourier-Bessel bases
- 10. Window convolution of models
- 11. Power spectrum integral constraint
- 12. Covariance matrix under Gaussian assumption
- 13. 1-point systematics
- 14. 2-point systematics
- 15. Binning in redshift and redshift-dependent weighting
- 16. Reconstruction
- 17. Conclusions
- David F. Mota - Nonlinear astrophysical probes of screened modified gravity
- 1. Introduction
- 2. Theoretical models
- 2.1. Chameleon-f(R) gravity
- 2.2. Symmetron
- 3. Efficiency of screening mechanisms
- 3.1. Solar System constraints
- 3.2. Simulations
- 3.3. Results
- 4. Distribution of fifth force in dark matter haloes
- 5. The matter and the velocity power spectra
- 6. The dynamical and lensing masses
- 7. Thermal versus lensing mass measurements
- 7.1. Including the non-thermal pressure component
- 8. Modelling void abundance in modified gravity
- 8.1. Linear power spectrum
- 8.2. Spherical collapse
- 8.2.1. Spherical expansion
- 8.3. Void abundance function
- 8.4. Voids from simulations
- 8.5. Results
- 8.5.1. Fitting beta and D from simulations
- 8.5.2. Constraining modified gravity
- 8.5.3. Voids in galaxy samples
- 9. Conclusions and perspectives
- List of participants
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