Model-independent measurements of cosmic expansion and growth at z = 0.57 using the anisotropic clustering of CMASS galaxies from the Sloan Digital Sky Survey Data Release 9

Wang, Yun

doi:10.1093/mnras/stu1374

Cited by 20 publications

(19 citation statements)

References 39 publications

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“…In addition, using the 2D two point correlation functions of BOSS DR9 samples, Wang Wang (2014) obtained…”

Section: Bao Datamentioning

confidence: 99%

A Comprehensive Investigation on the Slowing Down of Cosmic Acceleration

Wang

et al. 2016

ApJ

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Shafieloo ea al. firstly proposed the possibility that the current cosmic acceleration (CA) is slowing down. However, this is rather counterintuitive because a slowing down CA cannot be accommodated in most mainstream cosmological models. In this work, by exploring the evolutionary trajectories of dark energy equation of state w(z) and deceleration parameter q(z), we present a comprehensive investigation on the slowing down of CA from both the theoretical and the observational sides. For the theoretical side, we study the impact of different w(z) by using six parametrization models, and then discuss the effects of spatial curvature. For the observational side, we investigate the effects of different type Ia supernovae (SNe Ia), different baryon acoustic oscillation (BAO), and different cosmic microwave background (CMB) data, respectively. We find that (1) The evolution of CA are insensitive to the specific form of w(z); in contrast, a non-flat Universe more favors a slowing down CA than a flat Universe. (2) SNLS3 SNe Ia datasets favor a slowing down CA at 1σ confidence level, while JLA SNe Ia samples prefer an eternal CA; in contrast, the effects of different BAO data are negligible.(3) Compared with CMB distance prior data, full CMB data more favor a slowing down CA. (4) Due to the low significance, the slowing down of CA is still a theoretical possibility that cannot be confirmed by the current observations.

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“…In addition, using the 2D two point correlation functions of BOSS DR9 samples, Wang Wang (2014) obtained…”

Section: Bao Datamentioning

confidence: 99%

A Comprehensive Investigation on the Slowing Down of Cosmic Acceleration

Wang

et al. 2016

ApJ

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“…We find that this cut leads to unbiased estimates of x h = H(0.57) rs(z d )/c, x d = DA(0.57)/rs(z d ), and fg(0.57)σ8(0.57). Wang (2014), one can see that our current modeling significantly improves the recovery of the true H(0.57).…”

Section: Validation Using Mocksmentioning

confidence: 68%

“…Our methodology is based on Wang (2014), with the RSD modeling modified per Zheng et al (2013) (based on the work of ):…”

Section: Modeling the Galaxy Correlation Functionmentioning

confidence: 99%

Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity

Wang¹

2016

Mon. Not. R. Astron. Soc.

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We present a new approach to measuring cosmic expansion history and growth rate of large scale structure using the anisotropic two dimensional galaxy correlation function (2DCF) measured from data; it makes use of the empirical modeling of small-scale galaxy clustering derived from numerical simulations by Zheng et al. (2013). We validate this method using mock catalogues, before applying it to the analysis of the CMASS sample from the Sloan Digital Sky Survey Data Release 10 (DR10) of the Baryon Oscillation Spectroscopic Survey (BOSS). We find that this method enables accurate and precise measurements of cosmic expansion history and growth rate of large scale structure. Modeling the 2DCF fully including nonlinear effects and redshift space distortions (RSD) in the scale range of 16 to 144 h −1 Mpc, we find H(0.57)r s (z d )/c = 0.0459 ± 0.0006, D A (0.57)/r s (z d ) = 9.011 ± 0.073, and f g (0.57)σ 8 (0.57) = 0.476 ± 0.050, which correspond to precisions of 1.3%, 0.8%, and 10.5% respectively. We have defined r s (z d ) to be the sound horizon at the drag epoch computed using a simple integral, f g (z) as the growth rate at redshift z, and σ 8 (z) as the matter power spectrum normalization on 8 h −1 Mpc scale at z. We find that neglecting the small-scale information significantly weakens the constraints on H(z) and D A (z), and leads to a biased estimate of f g (z). Our results indicate that we can significantly tighten constraints on dark energy and modified gravity by reliably modeling small-scale galaxy clustering.

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“…Note that our result is consistent with the results of Shariff et al (2015). To make a comparison, in Fig 5 we also plot the 1D marginalized probability distribution of Ωm0 given by a combination of the CMB Ade et al (2015) 2 and the Baryon Acoustic Oscillations (BAO) Hemantha et al (2014); Wang (2014) data. The best-fit value of Ωm0 given by CMB+BAO data is 0.292, which is closer to the best-fit value of the constant β case.…”

Section: Methodsmentioning

confidence: 99%

More Evidence for the Redshift Dependence of Color from the JLA Supernova Sample Using Redshift Tomography

Li,

Wang

et al. 2016

Preprint

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In this work, by applying the redshift tomography method to Joint Light-curve Analysis (JLA) supernova sample, we explore the possible redshift-dependence of stretch-luminosity parameter α and color-luminosity parameter β. The basic idea is to divide the JLA sample into different redshift bins, assuming that α and β are piecewise constants. Then, by constraining the ΛCDM model, we check the consistency of cosmology-fit results given by the SN sample of each redshift bin. We also adopt the same technique to explore the possible evolution of β in various subsamples of JLA. Using the full JLA data, we find that α is always consistent with a constant. In contrast, at high redshift β has a significant trend of decreasing, at ∼ 3.5σ confidence level (CL). Moreover, we find that low-z subsample favors a constant β; in contrast, SDSS and SNLS subsamples favor a decreasing β at 2σ and 3.3σ CL, respectively. Besides, by using a binned parameterization of β, we study the impacts of β's evolution on parameter estimation. We find that compared with a constant β, a varying β yields a larger best-fit value of fractional matter density Ω m0 , which slightly deviates from the best-fit result given by other cosmological observations. However, for both the varying β and the constant β cases, the 1σ regions of Ω m0 are still consistent with the result given by other observations.

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Model-independent measurements of cosmic expansion and growth at z = 0.57 using the anisotropic clustering of CMASS galaxies from the Sloan Digital Sky Survey Data Release 9

Cited by 20 publications

References 39 publications

A Comprehensive Investigation on the Slowing Down of Cosmic Acceleration

A Comprehensive Investigation on the Slowing Down of Cosmic Acceleration

Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity

More Evidence for the Redshift Dependence of Color from the JLA Supernova Sample Using Redshift Tomography

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