The Early and the Late Universe Inflationary Features

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The Early and the Late Universe: Inflationary Features and Implications on Cosmological Parameters Cora

The Early and the Late Universe: Inflationary Features and Implications on Cosmological Parameters Cora Dvorkin Harvard University “B-mode from space” workshop, December 2017, Berkeley 1

Cosmic Microwave Background Planck collaboration 2

Cosmic Microwave Background Planck collaboration 2

CMB Power Spectrum Power spectrum: predicted and measured with great precision. Planck collaboration 3

CMB Power Spectrum Power spectrum: predicted and measured with great precision. Planck collaboration 3

H 0 tension Bernal et al. , JCAP (2016) 4

H 0 tension Bernal et al. , JCAP (2016) 4

Local cosmological inferences depend on the assumptions in the CDM model, in particular the

Local cosmological inferences depend on the assumptions in the CDM model, in particular the form of the inflationary power spectrum. 5

Going Beyond Slow Roll Slow roll is a commonly used approximation for inflationary models

Going Beyond Slow Roll Slow roll is a commonly used approximation for inflationary models where the scalar field potential is sufficiently flat and slowly varying. It leads to curvature power spectra that are featureless and nearly scale invariant. Generalized Slow-Roll approximation: allows for features in the inflationary potential. Here, the curvature power spectrum depends on a single source function (responsible for the observable features): C. Dvorkin, W. Hu, PRD (2009) Simple to relate to the inflaton potential: 6

CMB TEMPERATURE POWER SPECTRUM INFLATIONARY POTENTIAL INITIAL CURVATURE POWER SPECTRUM CMB POLARIZATION POWER SPECTRUM

CMB TEMPERATURE POWER SPECTRUM INFLATIONARY POTENTIAL INITIAL CURVATURE POWER SPECTRUM CMB POLARIZATION POWER SPECTRUM wavenumber k [Mpc-1] 7

CMB TEMPERATURE POWER SPECTRUM INFLATIONARY POTENTIAL INITIAL CURVATURE POWER SPECTRUM l OBSERVABLES CMB POLARIZATION

CMB TEMPERATURE POWER SPECTRUM INFLATIONARY POTENTIAL INITIAL CURVATURE POWER SPECTRUM l OBSERVABLES CMB POLARIZATION POWER SPECTRUM wavenumber k [Mpc-1] 8

Functional reconstruction of Generalized tilt • 2 PCs (out of 20) deviate from zero

Functional reconstruction of Generalized tilt • 2 PCs (out of 20) deviate from zero the 99% CL. • These deviations prefer a sharp suppression in power at k=0. 004 Mpc-1. Planck (2015) data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 9

Initial Curvature Power Spectrum Reconstruction with Planck data Planck (2015) data G. Obied, C.

Initial Curvature Power Spectrum Reconstruction with Planck data Planck (2015) data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 10

Features from Inflation and our inference of the Hubble constant • Local cosmological inferences

Features from Inflation and our inference of the Hubble constant • Local cosmological inferences depend on the assumptions in the CDM model, in particular the form of the inflationary power spectrum. Planck (2015) data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 11

Residuals in the TT data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and

Residuals in the TT data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 12

H 0 and inflationary parameters G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and

H 0 and inflationary parameters G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 13

Response functions 14

Response functions 14

Residuals in the TE data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and

Residuals in the TE data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 15

H 0 and polarization data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and

H 0 and polarization data G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 16

Amplitude of structure G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda,

Amplitude of structure G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, PRD (2017) 17

Constraints on inflationary parameters • nrun, run shows a 1. 9 preference for violation

Constraints on inflationary parameters • nrun, run shows a 1. 9 preference for violation of slow-roll in the r CDM model. 18

Conclusions • Explored the relationship between features from inflation, and shifts in the cosmological

Conclusions • Explored the relationship between features from inflation, and shifts in the cosmological parameters. • Preference for high H 0 and low values in driven by low <40 residuals in the data. from the TT data at <1000 is • However, TT, <1000 does not match the residuals particularly well. Fitting for inflationary features, the low H 0 values favored by the full TT data are compatible with TT, <1000 data. • The SB parameters show 2 PCs that deviate from zero at 99% CL. These deviations prefer a sharp suppression in power at k=0. 004 Mpc-1. • Planck TE data prefers low H 0 values (due to an outlier at the l=165 bin, region particularly sensitive to changes in ). • Future polarization data should provide insight into low- TT residuals. Features from reionization will have to be disentangled from features from inflation (work in progress; see Vinicius Miranda’s talk). 19

Extra Slides 20

Extra Slides 20

Low-l TT residuals G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda,

Low-l TT residuals G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, ar. Xiv: 1706. 09412 (2017) 21

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