Algorithm for the direct reconstruction of the dark matter correlation function from weak lensing and galaxy clustering

Baldauf, Tobias; Smith, R. E.; Seljak, Uroš; Mandelbaum, Rachel

doi:10.1103/physrevd.81.063531

Cited by 135 publications

(204 citation statements)

References 93 publications

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“…8. Beyond linear galaxy bias, r can deviate from 1 and acquire scale dependences, and it must be properly modeled to constrain cosmology with combined galaxy clustering and galaxy-galaxy lensing (e.g., [54]). We constrain r i at fixed cosmology using the Y1COSMO covariance, which includes the covariance between the two probes.…”

Section: Results: Galaxy Bias and Stochasticitymentioning

confidence: 99%

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Elvin-Poole¹,

Crocce²,

Ross³

et al. 2018

Phys. Rev. D

163

235

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We measure the clustering of DES year 1 galaxies that are intended to be combined with weak lensing samples in order to produce precise cosmological constraints from the joint analysis of large-scale structure and lensing correlations. Two-point correlation functions are measured for a sample of 6.6 × 10 5 luminous red galaxies selected using the REDMAGIC algorithm over an area of 1321 square degrees, in the redshift range 0.15 < z < 0.9, split into five tomographic redshift bins. The sample has a mean redshift uncertainty of σ z =ð1 þ zÞ ¼ 0.017. We quantify and correct spurious correlations induced by spatially variable survey properties, testing their impact on the clustering measurements and covariance. We demonstrate the sample's robustness by testing for stellar contamination, for potential biases that could arise from the systematic correction, and for the consistency between the two-point auto-and cross-correlation functions. We show that the corrections we apply have a significant impact on the resultant measurement of cosmological parameters, but that the results are robust against arbitrary choices in the correction method. We find the linear galaxy bias in each redshift bin in a fiducial cosmology to be bðσ 8 =0.81Þj z¼0.24 ¼ 1.40 AE 0.07, bðσ 8 =0.81Þj z¼0.38 ¼ 1.60 AE 0.05, bðσ 8 =0.81Þj z¼0.53 ¼ 1.60 AE 0.04 for galaxies with luminosities L=L Ã > 0.5, bðσ 8 =0.81Þj z¼0.68 ¼ 1.93 AE 0.04 for L=L Ã > 1 and bðσ 8 =0.81Þj z¼0.83 ¼ 1.98 AE 0.07 for L=L Ã > 1.5, broadly consistent with expectations for the redshift and luminosity dependence of the bias of red galaxies. We show these measurements to be consistent with the linear bias obtained from tangential shear measurements.

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Section: Results: Galaxy Bias and Stochasticitymentioning

confidence: 99%

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Elvin-Poole¹,

Crocce²,

Ross³

et al. 2018

Phys. Rev. D

163

235

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“…This type of analysis is also best done in real space rather than Fourier space so that the 1-halo contributions (see §2.3) to both clustering and lensing can be eliminated. A specific outline for how to do this, including the next-order perturbation theory corrections to r = 1 and comparison to simulations, is presented by Baldauf et al (2010).…”

Section: Methods Ii: Power Spectrum Tomography*mentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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“…Methods to combine galaxy clustering and weak lensing data have been studied extensively in the recent literature (e.g., [60][61][62][63][64][65][66]), suggesting high improvements for precision cosmology. Unfortunately, obtaining the dark matter density field in 3D from observations is a highly nontrivial problem and is subject of active research.…”

Section: Multitracer Fitmentioning

confidence: 99%

Optimal weighting in galaxy surveys: Application to redshift-space distortions

2012

Self Cite

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Using multiple tracers of large-scale structure allows to evade the limitations imposed by sampling variance for some parameters of interest in cosmology. We demonstrate the optimal way of carrying out a multitracer analysis in a galaxy redshift survey by considering the principal components of the shot noise matrix from two-point clustering statistics. We show how to construct two tracers that maximize the benefits of sampling variance and shot noise cancellation using optimal weights. On the basis of high-resolution N -body simulations of dark matter halos we apply this technique to the analysis of redshift-space distortions and demonstrate how constraints on the growth rate of structure formation can be substantially improved. The primary limitations are nonlinear effects, which cause significant biases in the method already at scales of k < 0.1hMpc −1 , suggesting the need to develop nonlinear models of redshift-space distortions in order to extract the maximum information from future redshift surveys. Nonetheless we find gains of a factor of a few in constraints on the growth rate achievable when merely the linear regime of a galaxy survey like EUCLID is considered.PACS numbers: 98.80.-k, 98.62.-g, 98.65.-r

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Algorithm for the direct reconstruction of the dark matter correlation function from weak lensing and galaxy clustering

Cited by 135 publications

References 93 publications

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Observational probes of cosmic acceleration

Optimal weighting in galaxy surveys: Application to redshift-space distortions

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