The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history at<i>z</i>&lt; 1

Blake, Chris; Brough, Sarah; Colless, Matthew; Contreras, Carlos; Couch, Warrick J.; Croom, S. M.; Croton, Darren J.; Davis, Tamara M.; Drinkwater, Michael J.; Forster, Karl; Gilbank, David; Gladders, M. D.; Glazebrook, Karl; Jelliffe, Ben; Jurek, Russell J.; Li, I-hui; Madore, Barry F.; Martin, Chris; Pimbblet, Kevin A.; Poole, Gregory B.; Pracy, Michael; Sharp, Robert; Wisnioski, Emily; Woods, David; Wyder, Ted K.; Yee, H. K. C.

doi:10.1111/j.1365-2966.2012.21473.x

Cited by 846 publications

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“…Other treatment improvements are described in [23]. To avoid possible correlations and to assure data independence, we also excluded the three data points from [40], at z = 0.44, z = 0.60 and z = 0.68, since the same data is used in our CMB/BAO analysis [15]. In our compilation we have also included two new measurements from cosmic chronometers at redshifts 1.363 and 1.965 from [24].…”

Section: H(z)mentioning

confidence: 99%

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Santos

Reis

Waga

2016

J. Cosmol. Astropart. Phys.

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Abstract. We revisit the kink-like parametrization of the deceleration parameter q(z) [1], which considers a transition, at redshift z t , from cosmic deceleration to acceleration. In this parametrization the initial, at z z t , value of the q-parameter is q i , its final, z = −1, value is q f and the duration of the transition is parametrized by τ . By assuming a flat space geometry we obtain constraints on the free parameters of the model using recent data from type Ia supernovae (SN Ia), baryon acoustic oscillations (BAO), cosmic microwave background (CMB) and the Hubble parameter H(z). The use of H(z) data introduces an explicit dependence of the combined likelihood on the present value of the Hubble parameter H 0 , allowing us to explore the influence of different priors when marginalizing over this parameter. We also study the importance of the CMB information in the results by considering data from WMAP7, WMAP9 (Wilkinson Microwave Anisotropy Probe -7 and 9 years) and Planck 2015. We show that the contours and best fit do not depend much on the different CMB data used and that the considered new BAO data is responsible for most of the improvement in the results. Assuming a flat space geometry, q i = 1/2 and expressing the present value of the deceleration parameter q 0 as a function of the other three free parameters, we obtain z t = 0.67 +0.10 −0.08 , τ = 0.26 +0.14 −0.10 and q 0 = −0.48 +0.11 −0.13 , at 68% of confidence level, with an uniform prior over H 0 . If in addition we fix q f = −1, as in flat ΛCDM, DGP and Chaplygin quartessence that are special models described by our parametrization, we get z t = 0.66 +0.03 −0.04 , τ = 0.33 +0.04 −0.04 and q 0 = −0.54 +0.05 −0.07 , in excellent agreement with flat ΛCDM for which τ = 1/3. We also obtain for flat wCDM, another dark energy model described by our parametrization, the constraint on the equation of state parameter −1.22 < w < −0.78 at more than 99% confidence level.

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Section: H(z)mentioning

confidence: 99%

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Santos

Reis

Waga

2016

J. Cosmol. Astropart. Phys.

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“…Figure 12. Constraints on f σ 8 from several redshift surveys in the base of ΛCDM, with f (z) = Ωm(z) γ : orange circle (6dFGRS by Beutler et al (2012)); gray triangle (SDSS Main Galaxy Sample by Howlett et al (2015)); green inverse triangle (SDSS Luminous Red Galaxies by Oka et al (2014)); cyan diamonds (WiggleZ by Blake et al (2012)); and purple pentagon (VIPERS by de la Torre et al (2013)). In red squares the results from BOSS-DR12 for the LOWZ and CMASS sample according to Table 3.…”

Section: Comparison With Other Galaxy Surveysmentioning

confidence: 99%

“…(iv) The WiggleZ analysis by Blake et al (2012) measures the galaxy correlation function and power spectrum. Considering both RSD and AP effects, they report f σ8 at 3 different redshifts, f (0.44)σ8(0.44) = 0.413 ± 0.080, f (0.6)σ8(0.6) = 0.390±0.063 and f (0.73)σ8(0.73) = 0.437± 0.072.…”

Section: Comparison With Other Galaxy Surveysmentioning

confidence: 99%

“…Key milestones include measurements from the PSCz galaxy survey (Tadros et al 1999), 2-degree Field Galaxy Redshift Survey (Peacock et al 2001;Hawkins et al 2003;Percival et al 2004), WiggleZ (Blake et al 2012), 6-degree Field Galaxy Survey (Beutler et al 2012) and the SDSS-II LRGs (Oka et al 2014). Previous measurements made from BOSS including DR9, when the survey was approximately one third complete (Samushia et al 2013), and most recently from DR10/11 (Chuang et al 2013;Beutler et al 2014;Samushia et al 2014;Sánchez et al 2014;Reid et al 2014;Alam et al 2015b).…”

Section: Introductionmentioning

confidence: 99%

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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

Gil-Marín¹,

Percival²,

Brownstein³

et al. 2016

Mon. Not. R. Astron. Soc.

169

247

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We measure and analyse the clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) relative to the line-of-sight (LOS), for LOWZ and CMASS galaxy samples drawn from the final Data Release 12 (DR12). The LOWZ sample contains 361 762 galaxies with an effective redshift of z lowz = 0.32, and the CMASS sample 777 202 galaxies with an effective redshift of z cmass = 0.57. From the power spectrum monopole and quadrupole moments around the LOS, we measure the growth of structure parameter f times the amplitude of dark matter density fluctuations σ 8 by modeling the Redshift-Space Distortion signal. When the geometrical Alcock-Paczynski effect is also constrained from the same data, we find joint constraints on f σ 8 , the product of the Hubble constant and the comoving sound horizon at the baryon drag epoch H(z)r s (z d ), and the angular distance parameter divided by the sound horizon D A (z)/r s (z d ). We find f (z lowz )σ 8 (z lowz ) = 0.394 ± 0.062, D A (z lowz )/r s (z d ) = 6.35 ± 0.19, H(z lowz )r s (z d ) = (11.41 ± 0.56) 10 3 kms −1 for the LOWZ sample, and f (z cmass )σ 8 (z cmass ) = 0.444 ± 0.038, D A (z cmass )/r s (z d ) = 9.42 ± 0.15, H(z cmass )r s (z d ) = (13.92 ± 0.44) 10 3 kms −1 for the CMASS sample. We find general agreement with previous BOSS DR11 measurements. Assuming the Hubble parameter and angular distance parameter are fixed at fiducial ΛCDM values, we find f (z lowz )σ 8 (z lowz ) = 0.485 ± 0.044 and f (z cmass )σ 8 (z cmass ) = 0.436 ± 0.022 for the LOWZ and CMASS samples, respectively.

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“…With this type of work, one typically compiles a unified sample of H(z) versus redshift measurements based on various approaches, including the determination of differential ages using cosmic chronometers (Moresco et al 2016b) and the inference of a characteristic distance scale revealed in baryon acoustic oscillations (BAOs; see, e.g. Blake et al 2012).However, it is inadvisable to make combined use of BAO measurements with other data. The BAO approach results in certain systematic effects that are difficult to quantify, certainly without the pre-assumption of a particular model.…”

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confidence: 99%

Analysing H(z) data using two-point diagnostics

Leaf

Melia

2017

Monthly Notices of the Royal Astronomical Society

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Measurements of the Hubble constant H(z) are increasingly being used to test the expansion rate predicted by various cosmological models. But the recent application of two-point diagnostics, such as Om(z i , z j ) and Omh 2 (z i , z j ), has produced considerable tension between CDM's predictions and several observations, with other models faring even worse. Part of this problem is attributable to the continued mixing of truly model-independent measurements using the cosmic-chronometer approach, and model-dependent data extracted from baryon acoustic oscillations. In this paper, we advance the use of two-point diagnostics beyond their current status, and introduce new variations, which we call h(z i , z j ), that are more useful for model comparisons. But we restrict our analysis exclusively to cosmic-chronometer data, which are truly model independent. Even for these measurements, however, we confirm the conclusions drawn by earlier workers that the data have strongly non-Gaussian uncertainties, requiring the use of both 'median' and 'mean' statistical approaches. Our results reveal that previous analyses using two-point diagnostics greatly underestimated the errors, thereby misinterpreting the level of tension between theoretical predictions and H(z) data. Instead, we demonstrate that as of today, only Einstein-de Sitter is ruled out by the two-point diagnostics at a level of significance exceeding ∼3σ . The R h = ct universe is slightly favoured over the remaining models, including Lambda cold dark matter and Chevalier-Polarski-Linder, though all of them (other than Einstein-de Sitter) are consistent to within 1σ with the measured mean of the h(z i , z j ) diagnostics.Key words: galaxies: distances and redshifts -galaxies: evolution -large-scale structure of Universe -cosmology: observations -cosmology: theory. I N T RO D U C T I O NLambda cold dark matter ( CDM) has done reasonably well accounting for a broad range of data and is therefore correctly viewed as the current standard model of cosmology (see, e.g. Planck Collaboration XXIII 2014). But recent analyses of the two-point correlation function of the cosmic microwave background (Melia 2014;Copi et al. 2015), as well as the Om(z i , z j ) and Omh 2 (z i , z j ) diagnostics applied to measurements of the Hubble expansion rate H(z) (Shafieloo, Sahni & Starobinsky 2012; Sahni, Shafieloo & Starobinsky 2014), appear to have revealed significant tension between its predictions and recent measurements (see, e.g. Zheng et al. 2016).In this paper, we directly address the problems highlighted by the various analyses carried out with the H(z) data, which apparently do not confirm the anticipated transition from early deceleration E-mail: kyleaf@email.arizona.edu (KL); melia@physics.arizona.eduto more recent acceleration in the cosmic expansion rate (Jimenez & Loeb 2002;Moresco et al. 2016a). With this type of work, one typically compiles a unified sample of H(z) versus redshift measurements based on various approaches, including the determination of differ...

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The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history atz< 1

Cited by 846 publications

References 62 publications

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

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

Analysing H(z) data using two-point diagnostics

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