Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7

Mandelbaum, Rachel; Slosar, Anže; Baldauf, Tobias; Seljak, U.; Hirata, Christopher M.; Nakajima, Reiko; Reyes, Reinabelle; Smith, R. E.

doi:10.1093/mnras/stt572

Cited by 324 publications

(434 citation statements)

References 125 publications

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“…As far as the signal-to-noise ratio of the stacked haloes is concerned, these effects counterbalance each other and lensing results are comparable (Johnston et al 2007;Mandelbaum, Seljak & Hirata 2008;Mandelbaum et al 2013;Brimioulle et al 2013;Hudson et al 2015;Covone et al 2014;Ford et al 2014Ford et al , 2015Velander et al 2014;Oguri 2014). A similar choice of data-sets for a joint analysis of galaxy clustering and galaxy-galaxy lensing was recently made by More et al (2014).…”

Section: Datamentioning

confidence: 91%

“…The main observable quantity for weak lensing is the tangential shear distortion γ+ of the shapes of background galaxies. It is related to the projected surface density Σ(R) around lenses (Mandelbaum et al 2013),…”

Section: Basicsmentioning

confidence: 99%

“…Vertical red lines delimit the radial range considered when fitting the shear profiles. be subject to systematic uncertainties both in terms of theoretical interpretation and observational uncertainties (Mandelbaum et al 2013). We did not try to connect it directly to the halo bias and the cosmological background.…”

Section: Shear Profile Modellingmentioning

confidence: 99%

“…These studies can be optimised to estimate σ8, i.e., the root mean square mass fluctuation amplitude in spheres of size 8h −1 Mpc. Mandelbaum et al (2013) recently constrained cosmology and galaxy bias using measurements of galaxy abundances, galaxy clustering and galaxy-galaxy lensing taken from the Sloan Digital Sky Survey (SDSS) data release 7. In the framework of the cold dark matter model with a cosmological constant (ΛCDM), they found σ8 = 0.76 ± 0.06.…”

Section: Introductionmentioning

confidence: 99%

“…Using non-linear models of the dark-matter power spectrum, Kilbinger et al (2013) estimated σ8 = 0.84±0.03 for a flat ΛCDM model with ΩM = 0.3 from 2D large-scale structure weak gravitational lensing in the CFHTLenS. This method is not affected by halo bias but since it relies on auto-correlations rather than shear cross-correlations, coherent additive errors in galaxy shapes (such as those induced by seeing or distortions in the telescope) may be difficult to remove from the analysis (Mandelbaum et al 2013). Moreover, intrinsic alignments with the local density field anticorrelate with the real gravitational shear and can contaminate cosmic shear measurements (Hirata & Seljak 2004).…”

Section: Introductionmentioning

confidence: 99%

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New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Sereno¹,

Veropalumbo²,

Marulli³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The joint analysis of clustering and stacked gravitational lensing of galaxy clusters in large surveys can constrain the formation and evolution of structures and the cosmological parameters. On scales outside a few virial radii, the halo bias, b, is linear and the lensing signal is dominated by the correlated distribution of matter around galaxy clusters. We discuss a method to measure the power spectrum amplitude σ 8 and b based on a minimal modelling. We considered a sample of ∼ 120000 clusters photometrically selected from the Sloan Digital Sky Survey in the redshift range 0.1 < z < 0.6. The auto-correlation was studied through the two-point function of a subsample of ∼ 70000 clusters; the matter-halo correlation was derived from the weak lensing signal of the subsample of ∼ 1200 clusters with CanadaFrance-Hawaii Lensing Survey data. We obtained a direct measurement of b, which increases with mass in agreement with predictions of the ΛCDM paradigm. Assuming Ω M = 0.3, we found σ 8 = 0.78 ± 0.16. We used the same clusters for measuring both lensing and clustering and the estimate of σ 8 did require neither the mass-richness relation, nor the knowledge of the selection function, nor the modelling of b. With an additional theoretical prior on the bias, we obtained σ 8 = 0.75 ± 0.08.

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Section: Datamentioning

confidence: 91%

Section: Basicsmentioning

confidence: 99%

Section: Shear Profile Modellingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Sereno¹,

Veropalumbo²,

Marulli³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Euler–Heisenberg Black Hole Surrounded by Quintessence in the Background of Perfect Fluid Dark Matter: Thermodynamics, Shadows, and Quasinormal Modes

Hamil,

Lütfüoğlu

2024

Fortschritte der Physik

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Current observations show that a significant fraction of the Universe is composed of dark energy and dark matter. In this paper, the simultaneous effects of these dark sectors on the Euler–Heisenberg black hole are investigated, using the quintessence matter field and perfect fluid to model them. In particular, the black hole's thermodynamics, shadows, and quasinormal modes are studied, and detailed discussions are provided on how these properties change with relatively large or small dark sector components.

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Structure Formation in Modified Gravity Cosmologies

Barreira

2016

Springer Theses

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source• a link is made to the metadata record in Durham E-Theses• the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. AbstractWe study linear and nonlinear structure formation in cosmologies where the accelerated expansion is driven by modifications to general relativity (GR). We focus on Galileon andNonlocal gravity, which are two classes of models that have been attracting much attention.We derive the linearly perturbed model equations and solve them with suitably modified versions of Einstein-Boltzmann codes. We also derive the perturbed equations keeping the relevant nonlinear terms for small scale structure formation, which we solve using Nbody codes and semi-analytical techniques that were developed for these models. Using CMB, SNIa and BAO data we find strong evidence for nonzero active neutrino masses (Σm ν ≈ 0.6 eV) in all three main branches of covariant Galileon cosmologies, known as the Cubic, Quartic and Quintic models. However, in all branches, the lensing potential does not decay at late times on sub-horizon scales, which contradicts the measured positive sign of the ISW effect, thereby ruling out the Galileon model. The Nonlocal model we study should be able to fit the CMB with similar parameter values as ΛCDM. The N-body simulation results show that the covariant Galileon model admits realistic halo occupation distributions of luminous red galaxies, even for model parameters whose linear growth is noticieably enhanced (σ 8 ≈ 1) relative to ΛCDM. In the Cubic Galileon model the screening mechanism is very efficient on scales 1Mpc, but in the Quartic and Quintic sectors, as well as in the Nonlocal model, we identify potential tensions with Solar System bounds.We illustrate that, despite the direct modifications to the lensing potential in the CubicGalileon and Nonlocal models, cluster masses estimated from lensing remain the same as in GR. The lensing effects produced by cosmic voids found in the simulations of the Cubic Galileon are significanly boosted (≈ 100%) compared to GR, which strongly motivates using voids in tests of gravity. The combination of linear and nonlinear theory results presented here for Galileon and Nonlocal gravity is an example of what it could be done for any serious alternative models to ΛCDM, which will be tested by future experiments.

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Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7

Cited by 324 publications

References 125 publications

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Euler–Heisenberg Black Hole Surrounded by Quintessence in the Background of Perfect Fluid Dark Matter: Thermodynamics, Shadows, and Quasinormal Modes

Structure Formation in Modified Gravity Cosmologies

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