The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Gil-Marín, Héctor; Percival, Will J.; Brownstein, Joel R.; Chuang, Chia-Hsun; Grieb, Jan Niklas; Ho, Shirley; Kitaura, Francisco-Shu; Maraston, Claudia; Prada, Francisco; Rodríguez-Torres, Sergio; Ross, Ashley J.; Samushia, Lado; Schlegel, David J.; Thomas, Daniel; Tinker, Jeremy L.; Zhao, Gong-Bo

doi:10.1093/mnras/stw1096

Cited by 172 publications

(257 citation statements)

References 75 publications

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“…[72][73][74][75][76][77]). In this section we will use the galaxy power spectrum to forecast the precision in measurements of the spectral index and its runnings, as defined in Eq.…”

Section: B Galaxy Clusteringmentioning

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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“…[72][73][74][75][76][77]). In this section we will use the galaxy power spectrum to forecast the precision in measurements of the spectral index and its runnings, as defined in Eq.…”

Section: B Galaxy Clusteringmentioning

confidence: 99%

Towards a measurement of the spectral runnings

Muñoz

Kovetz

Raccanelli

et al. 2017

J. Cosmol. Astropart. Phys.

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“…For all the models we use σ 8 (0, k σ8 ) = 0.820 [56] as the present day value of σ 8 . We compare the results obtained with the available observational data [71,[73][74][75][76][77][78][79][80][81][82][83][84][85][86][87] to check whether the predictions of the models are within the observational constraints. Since at the background level these models are very similar to ΛCDM till the present time, we expect that the deviations from ΛCDM in the evolution of the growth rate to be small.…”

Section: B Initial Conditionsmentioning

confidence: 99%

Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Albarran

Bouhmadi-López

Morais

2017

Physics of the Dark Universe

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We carry out an analysis of the cosmological perturbations in general relativity for three different models which are good candidates to describe the current acceleration of the Universe. These three set-ups are described classically by perfect fluids with a phantom nature and represent deviations from the most widely accepted ΛCDM model. In addition, each of the models under study induce different future singularities or abrupt events known as (i) Big Rip, (ii) Little Rip and (iii) Little Sibling of the Big Rip. Only the first one is regarded as a true singularity since it occurs at a finite cosmic time. For this reason, we refer to the others as abrupt events. With the aim to find possible footprints of this scenario in the Universe matter distribution, we not only obtain the evolution of the cosmological scalar perturbations but also calculate the matter power spectrum for each model. We have carried the perturbations in the absence of any anisotropic stress and within a phenomenological approach for the speed of sound. We constrain observationally these models using several measurements of the growth rate function, more precisely f σ8, and compare our results with the observational ones.

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“…Additionally, the local quantities can be obtained from the definition (9). For every shell r = r i , it is possible to implicitly recover the instant t corresponding to the variable ξ(t, r i ) as…”

Section: Dimensionless Dynamical System and Critical Pointsmentioning

confidence: 99%

“…Other sets of data give us information on the inhomogeneous part of the Universe, such as the data of anisotropy of the cosmic microwave background (CMB) and the data from Barionic Acoustic Oscillations [1], the redshift drift [9], evolution of the growth function [10], etc. All the data regarding the inhomogeneous cosmology can give us information on the Universe through the dynamics of the perturbations in Cosmology.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of a spherically symmetric inhomogeneous coupled dark energy model with coupling term proportional to non relatvistic matter

2017

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Abstract. Quasi-local scalar variables approach is applied to a spherically symmetric inhomogeneous Lemaître-Tolman-Bondi metric containing a mixture of non-relativistic cold dark matter and coupled dark energy with constant equation of state. The quasi-local coupling term considered is proportional to the quasi-local cold dark matter energy density and a quasi-local Hubble factor-like scalar via a coupling constant α. The autonomous numerical system obtained from the evolution equations is classified for different choices of the free parameters: the adiabatic constant of the dark energy w and α. The presence of a past attractor in a non-physical region of the energy densities phase-space of the system makes the coupling term non physical when the energy flows from the matter to the dark energy in order to avoid negative values of the dark energy density in the past. On the other hand, if the energy flux goes from dark energy to dark matter, the past attractor lays in a physical region. The system is also numerically solved for some interesting initial profiles leading to different configurations: an ever expanding mixture, a scenario where the dark energy is completely consumed by the nonrelativistic matter by means of the coupling term, a scenario where the dark energy disappears in the inner layers while the outer layers expand as a mixture of both sources, and, finally, a structure formation toy model scenario, where the inner shells containing the mixture collapse while the outer shells expand.PACS numbers: 98.80.-k, 04.20.-q, 95.36.+x, 95.35.+d

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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Cited by 172 publications

References 75 publications

Towards a measurement of the spectral runnings

Towards a measurement of the spectral runnings

Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Dynamics of a spherically symmetric inhomogeneous coupled dark energy model with coupling term proportional to non relatvistic matter

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