Tomographic analyses of the CMB lensing and galaxy clustering to probe the linear structure growth

Marques, Gabriela A.; Bernui, Armando

doi:10.1088/1475-7516/2020/05/052

Cited by 31 publications

(25 citation statements)

References 90 publications

(121 reference statements)

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“…A Gaussian random realization with the correct noise covariance is generated many times (one for each sample), then this noise realization is added to the measured Ŵ xc,g (χ) and finally a smooth B-spline with positivity constraint and curvature penalty is fit to the resulting W xc,g (χ) sample. This procedure generates (bias-weighted) redshift distributions that are consistent with the data and whose density in the set of possible distributions is proportional to their probability of being the correct one given the data 8 .…”

Section: Parametermentioning

confidence: 99%

“…CMB lensing by itself is sensitive to a wide range of redshifts. When cross-correlating CMB lensing with low-redshift tracers (CMB lensing tomography) such as galaxies, we extract the information over the redshift range of interest (see for example [3][4][5] for some of the early work and [6][7][8][9][10][11][12][13] for more recent analyses). Moreover, because of the different dependence on galaxy bias of the auto and cross-correlations, we can efficiently break the degeneracy between bias and the amplitude of fluctuations at low redshift, providing tight cosmological constraints on the low-redshift Universe.…”

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confidence: 99%

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Cosmological constraints from unWISE and Planck CMB lensing tomography

Krolewski,

Ferraro,

White

2021

Preprint

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A number of recent, low-redshift, lensing measurements hint at a universe in which the amplitude of lensing is lower than that predicted from the ΛCDM model fit to the data of the Planck CMB mission. Here we use the auto-and cross-correlation signal of unWISE galaxies and Planck CMB lensing maps to infer cosmological parameters at low redshift. In particular, we consider three unWISE samples (denoted as "blue", "green" and "red") at median redshifts z ∼ 0.6, 1.1 and 1.5, which fully cover the Dark Energy dominated era. Our cross-correlation measurements, with combined significance S/N ∼ 80, are used to infer the amplitude of low-redshift fluctuations, σ 8 ; the fraction of matter in the Universe, Ω m ; and the combination S 8 ≡ σ 8 (Ω m /0.3) 0.5 to which these low-redshift lensing measurements are most sensitive. The combination of blue and green samples gives a value S 8 = 0.776 ± 0.017, that is fully consistent with other low-redshift lensing measurements and in 2.6σ tension with the CMB predictions from Planck. This is noteworthy, because CMB lensing probes the same physics as previous galaxy lensing measurements, but with very different systematics, thus providing an excellent complement to previous measurements.

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Section: Parametermentioning

confidence: 99%

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confidence: 99%

Cosmological constraints from unWISE and Planck CMB lensing tomography

Krolewski,

Ferraro,

White

2021

Preprint

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“…To achieve these objectives, in this work we use measurements of the transversal BAO scale (θ BAO ), data obtained following an approach that weakly depends on the assumption of a cosmological model, as described in ref. [36] (all these measurements were obtained following the same methodological approach, however, since the clustering analyses were performed with diverse cosmological tracers -blue galaxies, luminous red galaxies, quasars-one should be careful with the systematics of each dataset [for some tests to deal with systematics in data analyses see, e.g.,] [37][38][39]). A distinctive feature of these data is that they were measured without assuming a geometry of the Universe; this is a crucial advantage as compared with data sets obtained under the hypothesis of a flat geometry, an attribute that may bias cosmological parameter analyses.…”

Section: Introductionmentioning

confidence: 99%

BAO signatures in the 2-point angular correlations and the Hubble tension

Nunes

Bernui

2020

Eur. Phys. J. C

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An observational tension on estimates of the Hubble parameter, $$H_0$$ H 0 , using early and late Universe information, is being of intense discussion in the literature. Additionally, it is of great importance to measure $$H_0$$ H 0 independently of CMB data and local distance ladder method. In this sense, we analyze 15 measurements of the transversal BAO scale, $$\theta _\mathrm{BAO}$$ θ BAO , obtained in a weakly model-dependent approach, in combination with other data sets obtained in a model-independent way, namely, Big Bang Nucleosynthesis (BBN) information, 6 gravitationally lensed quasars with measured time delays by the H0LiCOW team, and measures of cosmic chronometers (CC). We find $$H_0 = 74.88_{-2.1}^{+1.9}$$ H 0 = 74 . 88 - 2.1 + 1.9 km s$${}^{-1}$$ - 1 Mpc$${}^{-1}$$ - 1 and $$H_0 = 72.06_{-1.3}^{+1.2}$$ H 0 = 72 . 06 - 1.3 + 1.2 km s$${}^{-1}$$ - 1 Mpc$${}^{-1}$$ - 1 from $$\theta _{BAO}$$ θ BAO +BBN+H0LiCOW and $$\theta _{BAO}$$ θ BAO +BBN+CC, respectively, in fully accordance with local measurements. Moreover, we estimate the sound horizon at drag epoch, $$r_\mathrm{d}$$ r d , independent of CMB data, and find $$r_\mathrm{d}=144.1_{-5.5}^{+5.3}$$ r d = 144 . 1 - 5.5 + 5.3 Mpc (from $$\theta _{BAO}$$ θ BAO +BBN+H0LiCOW) and $$r_\mathrm{d} =150.4_{-3.3}^{+2.7}$$ r d = 150 . 4 - 3.3 + 2.7 Mpc (from $$\theta _{BAO}$$ θ BAO +BBN+CC). In a second round of analysis, we test how the presence of a possible spatial curvature, $$\Omega _k$$ Ω k , can influence the main results. We compare our constraints on $$H_0$$ H 0 and $$r_\mathrm{d}$$ r d with other reported values. Our results show that it is possible to use a robust compilation of transversal BAO data, $$\theta _{BAO}$$ θ BAO , jointly with other model-independent measurements, in such a way that the tension on the Hubble parameter can be alleviated.

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“…ξ(s, µ) [31], allows us to measure f σ 8 , where σ 8 is the rootmean-square linear fluctuation of the matter distribution at the scale of 8 Mpc/h (for other approaches to study matter clustering see, e.g., [11,41,26,27]). The literature reports diverse compilations of measurements of [f σ 8 ](z) (see, e.g., [48,5]) which we update here.…”

Section: H(z) Datamentioning

confidence: 99%

Observational constraints on Starobinsky $f(R)$ cosmology from cosmic expansion and structure growth data

Bessa,

Campista,

Bernui

2021

Preprint

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The unknown physical nature of the Dark Energy motivates in cosmology the study of modifications of the gravity theory at large distances. One of these types of modifications are the theories known as f (R) gravity. In this paper we use observational data to both constraint and test the Starobinsky f (R) model [57], using updated measurements from the dynamics of the expansion of the universe, H(z), and the growth rate of cosmic structures, [f σ8](z), where the distinction between the concordance ΛCDM model and modified gravity models, f (R), become clearer. We use MCMC likelihood analyses to explore the parameters space of the f (R) model using H(z) and [f σ8](z) data, both individually and jointly, and further check which of the models better fit the joint data. To further test the Starobinsky model, we use a method proposed by Linder [38], where the data from the observables is jointly binned in redshift space. This allows to further explore the model's parameter that better fits the data in comparison to the ΛCDM model. Our analyses show that the result from the MCMC run using [f σ8](z) data alone fits the analyzed model better than using the joint data. At the end, we reaffirm that this joint analysis is able to break the degenerescence between modified gravity models through the f σ8 observable, as the original author proposed; our results show that the f (R) Starobinsky model although not favored by the available data, cannot be discarded and is a possible alternative to the ΛCDM model.

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Tomographic analyses of the CMB lensing and galaxy clustering to probe the linear structure growth

Cited by 31 publications

References 90 publications

Cosmological constraints from unWISE and Planck CMB lensing tomography

Cosmological constraints from unWISE and Planck CMB lensing tomography

BAO signatures in the 2-point angular correlations and the Hubble tension

Observational constraints on Starobinsky $f(R)$ cosmology from cosmic expansion and structure growth data

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