Features of heavy physics in the CMB Biases in our priors? Outline - PowerPoint PPT Presentation

Features of heavy physics in the CMB Subodh P. Patil Introductory remarks Priors and degeneracies Features of heavy physics in the CMB Biases in our priors? Outline When UV physics does not decouple Our highest energy Subodh P. Patil probe? Probing compactifications? Inflation with a CPhT, Ecole Polytechnique & mass hierarchy LPTENS, Ecole Normale Sup´ erieure Bends in field space Features in the power spectrum UOC, Iraklion, March 30 th 2011

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? Outline When UV physics does not decouple Our highest energy probe? Probing compactifications? Inflation with a mass hierarchy Bends in field space Features in the power spectrum

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? ◮ It’s anisotropies ( δ T / T ∼ 10 − 5 ) provide us with a Outline When UV physics topographic map of the gravitational potential field at does not decouple Our highest energy the time of last scattering T ∼ 13 . 6 eV . probe? Probing compactifications? Inflation with a mass hierarchy Bends in field space Features in the power spectrum

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? ◮ It’s anisotropies ( δ T / T ∼ 10 − 5 ) provide us with a Outline When UV physics topographic map of the gravitational potential field at does not decouple Our highest energy the time of last scattering T ∼ 13 . 6 eV . probe? Probing compactifications? ◮ δ T / T = v E − φ + δ T / T rad : Inflation with a mass hierarchy Bends in field space Features in the power spectrum

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? ◮ It’s anisotropies ( δ T / T ∼ 10 − 5 ) provide us with a Outline When UV physics topographic map of the gravitational potential field at does not decouple Our highest energy the time of last scattering T ∼ 13 . 6 eV . probe? Probing compactifications? ◮ δ T / T = v E − φ + δ T / T rad : Inflation with a mass hierarchy ◮ v E is the dipole motion of us through the CMB rest Bends in field space Features in the power frame, spectrum

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? ◮ It’s anisotropies ( δ T / T ∼ 10 − 5 ) provide us with a Outline When UV physics topographic map of the gravitational potential field at does not decouple Our highest energy the time of last scattering T ∼ 13 . 6 eV . probe? Probing compactifications? ◮ δ T / T = v E − φ + δ T / T rad : Inflation with a mass hierarchy ◮ v E is the dipole motion of us through the CMB rest Bends in field space Features in the power frame, spectrum ◮ φ is the so-called integrated SW contribution, from climbing out of the potential generated by the perturbed line element: ds 2 = (1 − 2 φ ) dt 2 + (1 + 2 φ ) a 2 ( t ) dx i dx i ,

Features of heavy What is the CMB telling us? physics in the CMB Big bang cosmology predicts a relic background of photons Subodh P. Patil with a perfect blackbody spectrum. Introductory ◮ It’s overall isotropy (+ homogeneity) confirms the large remarks Priors and scale homogeneity + isotropy of our Hubble patch. degeneracies Biases in our priors? ◮ It’s anisotropies ( δ T / T ∼ 10 − 5 ) provide us with a Outline When UV physics topographic map of the gravitational potential field at does not decouple Our highest energy the time of last scattering T ∼ 13 . 6 eV . probe? Probing compactifications? ◮ δ T / T = v E − φ + δ T / T rad : Inflation with a mass hierarchy ◮ v E is the dipole motion of us through the CMB rest Bends in field space Features in the power frame, spectrum ◮ φ is the so-called integrated SW contribution, from climbing out of the potential generated by the perturbed line element: ds 2 = (1 − 2 φ ) dt 2 + (1 + 2 φ ) a 2 ( t ) dx i dx i , ◮ δ T / T rad is the intrinsic photon gas temperature variation (adiabatic / isocurvature).

Features of heavy What is the CMB telling us? physics in the CMB The standard gravitational Jeans instability is not effective Subodh P. Patil enough to generate the implied δρ/ρ ∼ 10 − 5 instabilities Introductory since the onset of the hot big bang– there must be a remarks primordial seed spectrum. Priors and degeneracies Biases in our priors? ◮ On top of ‘naturally’ providing the initial conditions for Outline the hot big bang, inflation provides such a seed When UV physics does not decouple spectrum that is (in its simplest realizations) scale Our highest energy probe? invariant (Harrison- Zel’dovich), adiabatic and phase Probing compactifications? coherent– δ T / T ( k ) = Ω( k ) P φ ( k ) Inflation with a mass hierarchy Bends in field space Features in the power spectrum

Features of heavy What is the CMB telling us? physics in the CMB The standard gravitational Jeans instability is not effective Subodh P. Patil enough to generate the implied δρ/ρ ∼ 10 − 5 instabilities Introductory since the onset of the hot big bang– there must be a remarks primordial seed spectrum. Priors and degeneracies Biases in our priors? ◮ On top of ‘naturally’ providing the initial conditions for Outline the hot big bang, inflation provides such a seed When UV physics does not decouple spectrum that is (in its simplest realizations) scale Our highest energy probe? invariant (Harrison- Zel’dovich), adiabatic and phase Probing compactifications? coherent– δ T / T ( k ) = Ω( k ) P φ ( k ) Inflation with a mass hierarchy ◮ Ω( k ) is the so-called transfer function ≈ 1 at the largest Bends in field space Features in the power scales and encodes all the astrophysical processing since spectrum last scattering,

Features of heavy What is the CMB telling us? physics in the CMB The standard gravitational Jeans instability is not effective Subodh P. Patil enough to generate the implied δρ/ρ ∼ 10 − 5 instabilities Introductory since the onset of the hot big bang– there must be a remarks primordial seed spectrum. Priors and degeneracies Biases in our priors? ◮ On top of ‘naturally’ providing the initial conditions for Outline the hot big bang, inflation provides such a seed When UV physics does not decouple spectrum that is (in its simplest realizations) scale Our highest energy probe? invariant (Harrison- Zel’dovich), adiabatic and phase Probing compactifications? coherent– δ T / T ( k ) = Ω( k ) P φ ( k ) Inflation with a mass hierarchy ◮ Ω( k ) is the so-called transfer function ≈ 1 at the largest Bends in field space Features in the power scales and encodes all the astrophysical processing since spectrum last scattering, ◮ P φ ( k ) = k 3 �| φ ( k ) | 2 � ∼ k n s − 1 , with the so-called spectral index n s ≈ 1 in simple toy models of inflation.

Features of heavy What is the CMB telling us? physics in the CMB The standard gravitational Jeans instability is not effective Subodh P. Patil enough to generate the implied δρ/ρ ∼ 10 − 5 instabilities Introductory since the onset of the hot big bang– there must be a remarks primordial seed spectrum. Priors and degeneracies Biases in our priors? ◮ On top of ‘naturally’ providing the initial conditions for Outline the hot big bang, inflation provides such a seed When UV physics does not decouple spectrum that is (in its simplest realizations) scale Our highest energy probe? invariant (Harrison- Zel’dovich), adiabatic and phase Probing compactifications? coherent– δ T / T ( k ) = Ω( k ) P φ ( k ) Inflation with a mass hierarchy ◮ Ω( k ) is the so-called transfer function ≈ 1 at the largest Bends in field space Features in the power scales and encodes all the astrophysical processing since spectrum last scattering, ◮ P φ ( k ) = k 3 �| φ ( k ) | 2 � ∼ k n s − 1 , with the so-called spectral index n s ≈ 1 in simple toy models of inflation. ◮ It is a combination of an input seed spectrum + knowledge of physics since last scattering that we fit to the data, which allows us to infer cosmological parameters.