Probing primordial features with future galaxy surveys

Ballardini, M.; Finelli⋆, F.; Fedeli, C.; Moscardini, L.

doi:10.1088/1475-7516/2016/10/041

Cited by 79 publications

(87 citation statements)

References 152 publications

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“…The relative phases of the acoustic and primordial oscillations will thus be different in the baryon acoustic oscillations (BAO) than they are in the CMB. Furthermore, another probe of this model would be to look for correlated features in the primordial spectra [48,[53][54][55][56][57][58][59]. On the other hand, we have shown also that it is difficult that oscillating features in the power spectrum which are linear in k (or almost linear) are generated during inflation from an oscillatory modulation of the background and that could explain the A L anomaly at the same time.…”

Section: Discussionmentioning

confidence: 87%

Lensing anomaly and oscillations in the primordial power spectrum

Domènech

Kamionkowski

2019

J. Cosmol. Astropart. Phys.

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The latest analysis of the cosmic microwave background by the Planck team finds more smoothing of the acoustic peaks in the temperature power spectrum than predicted by ΛCDM. Here we investigate whether this additional smoothing can be mimicked by an oscillatory feature, generated during inflation, that is similar to the acoustic peaks but out of phase. We consider oscillations generated by oscillating modulations of the background-e.g., due to heavy fields or modulated potentials-and by sharp features. We show that it is difficult to induce oscillations that are linear (or almost linear) in k by oscillatory modulations of the background. We find, however, that a sharp bumpy feature in the sound speed of perturbations is able to produce the desired oscillations. The scenario can be tested by combining CMB and BAO data. * domenech@thphys.uni-heidelberg.de † kamion@jhu.edu 1 A L parametrizes a rescaling of the lensing power spectrum such that A L = 1 for ΛCDM [5].

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Section: Discussionmentioning

confidence: 87%

Lensing anomaly and oscillations in the primordial power spectrum

Domènech

Kamionkowski

2019

J. Cosmol. Astropart. Phys.

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“…See for example Ref. [97] for a similar analysis. From Table II it is clear that a wide survey, like DESI, will be more successful at measuring the runnings than a deep one, like WFIRST.…”

Section: Resultsmentioning

confidence: 99%

Towards a measurement of the spectral runnings

Muñoz

Kovetz

Raccanelli

et al. 2017

J. Cosmol. Astropart. Phys.

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Single-field slow-roll inflation predicts a nearly scale-free power spectrum of perturbations, as observed at the scales accessible to current cosmological experiments. This spectrum is slightly red, showing a tilt (1 − ns) ∼ 0.04. A direct consequence of this tilt are nonvanishing runnings αs = dns/d log k, and βs = dαs/d log k, which in the minimal inflationary scenario should reach absolute values of 10 −3 and 10 −5 , respectively. In this work we calculate how well future surveys can measure these two runnings. We consider a Stage-4 (S4) CMB experiment and show that it will be able to detect significant deviations from the inflationary prediction for αs, although not for βs. Adding to the S4 CMB experiment the information from a WFIRST-like or a DESI-like survey improves the sensitivity to the runnings by ∼ 20%, and 30%, respectively. A spectroscopic survey with a billion objects, such as the SKA, will add enough information to the S4 measurements to allow a detection of αs = 10 −3 , required to probe the single-field slow-roll inflationary paradigm. We show that only a very-futuristic interferometer targeting the dark ages will be capable of measuring the minimal inflationary prediction for βs. The results of other probes, such as a stochastic background of gravitational waves observable by LIGO, the Ly-α forest, and spectral distortions, are shown for comparison. Finally, we study the claims that large values of βs, if extrapolated to the smallest scales, can produce primordial black holes of tens of solar masses, which we show to be easily testable by the S4 CMB experiment.

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“…ArXiv ePrint: 1606.03747 In this erratum we correct some of the figures appeared in [1] with the marginalized 2D plots for the extra parameters of the features models. The errors which have a big visible impact on the figures are due to an error in the script used to generate the contour plots affecting both the size of the axes of the ellipses and their orientations.…”

Section: Erratum To: Jcap10(2016)041mentioning

confidence: 99%