Baryon acoustic oscillations signature in the three-point angular correlation function from the SDSS-DR12 quasar survey

Carvalho, E. de; Bernui, Armando; Xavier, H. S.; Novaes, Camila P.

doi:10.1093/mnras/staa119

Cited by 31 publications

(18 citation statements)

References 92 publications

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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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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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“…To estimate the error bars of the 2PACF and the statistical significance of our results, we used the covariance matrix built from full-sky log-normal simulations that we produced with the FLASK code 1 (Xavier et al 2016;de Carvalho et al 2020). We generated a set of 1, 000 simulations for which we assume the Lambda cold dark matter (ΛCDM) cosmological parameters measured by the Planck Collaboration (2020), including all effects available such as lensing, redshift space distortions (RSD), and nonlinear clustering to compute with the code CAMBsources 2 (Challinor & Lewis 2011) the fiducial angular power spectrum C that was used as input.…”

Section: Log-normal Simulationsmentioning

confidence: 99%

“…Although we study spectroscopic data, for which this uncertainty is smaller, it is important to quantify this source of error in the final BAO measurement. To do this, we constructed 300 spec-z simulations for which we considered the measured z of each blue galaxy as the true one plus a random error obtained from a Gaussian distribution of zero mean and standard deviation given by its measured uncertainty that is available in the data catalog (see de Carvalho et al 2020).…”

Section: Spectroscopic-z Errormentioning

confidence: 99%

BAO angular scale at z_eff = 0.11 with the SDSS blue galaxies

de Carvalho,

Bernui,

Avila

et al. 2021

Preprint

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Aims. We measure the transverse baryon acoustic oscillations (BAO) signal in the local Universe using a sample of blue galaxies from the Sloan Digital Sky Survey (SDSS) survey as a cosmological tracer. Methods. The method is weakly dependent on a cosmological model and is suitable for 2D analyses in thin redshift bins to investigate the SDSS data in the interval z ∈ [0.105, 0.115].Results. We detect the transverse BAO signal θ bao = 19.8 • ± 1.05 • at z eff = 0.11, with a statistical significance of 2.2 σ. Additionally, we perform tests that confirm the robustness of this angular BAO signature. Supported by a large set of log-normal simulations, our error analyses include statistical and systematic contributions. In addition, considering the sound horizon scale calculated by the Planck Collaboration, r Planck s , and the θ bao value obtained here, we obtain a measurement of the angular diameter distance D A (0.11) = 258.31±13.71 h −1 Mpc. Moreover, combining this θ bao measurement at low redshift with other BAO angular scale data reported in the literature, we perform statistical analyses for the cosmological parameters of some Lambda cold dark matter (ΛCDM) type models.

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“…The first detection of the BAO peak in the 3PCF is provided by Gaztañaga et al (2009) from the analysis of Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) Luminous Red Galaxies. More recently, Slepian et al (2017a,b) obtained a clear detection of the BAO feature in the 3PCF of SDSS-DR12 CMASS sample, while de Carvalho et al (2020) measured the BAO feature in the angular 3PCF of SDSS-DR12 quasars.…”

Section: Introductionmentioning

confidence: 98%

C$^3$-Cluster Clustering Cosmology II. First detection of the BAO peak in the three-point correlation function of galaxy clusters

Moresco,

Veropalumbo,

Marulli

et al. 2020

Preprint

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Third-order statistics of the cosmic density field provides a powerful cosmological probe containing synergistic information to the more commonly explored second-order statistics. Here, we exploit a spectroscopic catalog of 72,563 clusters of galaxies extracted from the Sloan Digital Sky Survey, providing the first detection of the baryon acoustic oscillations (BAO) peak in the three-point correlation function (3PCF) of galaxy clusters. We measure and analyze both the connected and the reduced 3PCF of SDSS clusters from intermediate (r ∼ 10 Mpc/h) up to large (r ∼ 140 Mpc/h) scales, exploring a variety of different configurations. From the analysis of reduced 3PCF at intermediate scales, in combination with the analysis of the two-point correlation function, we constrain both the cluster linear and non-linear bias parameters, b 1 = 2.75 ± 0.03 and b 2 = 1.2 ± 0.5. We analyze the measurements of the 3PCF at larger scales, comparing them with theoretical models. The data show clear evidence of the BAO peak in different configurations, which appears more visible in the reduced 3PCF rather than in the connected one. From the comparison between theoretical models considering or not the BAO peak, we obtain a quantitative estimate of this evidence, with a ∆χ 2 between 2 and 75, depending on the considered configuration. Finally, we set up a generic framework to estimate the expected signal-to-noise ratio of the BAO peak in the 3PCF exploring different possible definitions, that can be used to forecast the most favorable configurations to be explored also in different future surveys, and applied it to the case of the Euclid mission.

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Baryon acoustic oscillations signature in the three-point angular correlation function from the SDSS-DR12 quasar survey

Cited by 31 publications

References 92 publications

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

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

BAO angular scale at z_eff = 0.11 with the SDSS blue galaxies

C$^3$-Cluster Clustering Cosmology II. First detection of the BAO peak in the three-point correlation function of galaxy clusters

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