A combined analysis of 3D weak lensing, Lyman-α forest and WMAP year three data

Lesgourgues, Julien; Viel, Matteo; Haehnelt, Martin G.; Massey, Richard

doi:10.1088/1475-7516/2007/11/008

Cited by 63 publications

(65 citation statements)

References 32 publications

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“…For instance, it is well known that EdS based models fail to reproduce the BAO peak [15,40,41]. At first sight the value for σ 8 = 0.92 seems too high, which may be inconsistent with measurements of the Lyman-α forest [42]. Finally, we may not also be able to fit the turnaround point of the galaxy power spectrum, which is mostly controlled by the product Ω m h, and as compared to the standard value of Ω m h ≈ 0.21, this is too high in our model, although the analysis of [15,16] shows that the addition of a hot component (neutrinos) helps to fit the galaxy power spectrum (SDSS data main sample).…”

Section: Jcap09(2009)025mentioning

confidence: 99%

Local void vs dark energy: confrontation with WMAP and type Ia supernovae

Alexander

Biswas

Notari

et al. 2009

J. Cosmol. Astropart. Phys.

126

193

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Abstract. It is now a known fact that if we happen to be living in the middle of a large underdense region, then we will observe an "apparent acceleration", even when any form of dark energy is absent. In this paper, we present a "Minimal Void" scenario, i.e. a "void" with minimal underdensity contrast (of about −0.4) and radius (∼ 200 − 250 Mpc/h) that can, not only explain the supernovae data, but also be consistent with the 3-yr WMAP data. We also discuss consistency of our model with various other measurements, and in particular consistency with local measurements of the Hubble parameter. We also point out possible observable signatures.

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Section: Jcap09(2009)025mentioning

confidence: 99%

Local void vs dark energy: confrontation with WMAP and type Ia supernovae

Alexander

Biswas

Notari

et al. 2009

J. Cosmol. Astropart. Phys.

126

193

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“…The initial conditions have been generated using the CAMB 3 software (Lewis et al 2000). A concordance flat ΛCDM model is used, in agreement with recent observations of the cosmic microwave background radiation, weak gravitational lensing, Lyman-α forest and galaxy cluster mass function evolution (e.g., Lesgourgues et al 2007;Vikhlinin et al 2009;Komatsu et al 2011). The seven new runs use the following parameters: ΩM,0 = 0.24, ΩΛ,0 = 0.76, ΩB,0 = 0.04, H0 = 72 km s −1 Mpc −1 .…”

Section: Simulationsmentioning

confidence: 99%

Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

Barai

Monaco

Murante

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We measure and quantify properties of galactic outflows and diffuse gas at z 1 in cosmological hydrodynamical simulations performed using the GADGET-3 code containing novel baryonic feedback models. Our sub-resolution model, MUPPI, implements supernova feedback using fully local gas properties, where the wind velocity and mass loading are not given as input. We find the following trends at z = 2 by analysing central galaxies having a stellar mass higher than 10 9 M ⊙ . The outflow velocity and mass outflow rate (Ṁ out ) exhibit positive correlations with galaxy mass and with the star formation rate (SFR). However, most of the relations present a large scatter. The outflow mass loading factor (η) is between 0.2 − 10, with an average η ∼ 1. The comparison Effective model generates a constant outflow velocity as expected from the input fixed wind kick speed, and a negative correlation of η with halo mass as opposed to the fixed input η. The shape of the outflows is bi-polar in 95% of the MUPPI galaxies. The MUPPI model produces colder galaxy cores and flatter gas metallicity radial profiles than the Effective model. The number fraction of galaxies where outflow is detected decreases at lower redshifts, but remains more than 80% over z = 1 − 5. High SF activity at z ∼ 2 − 4 drives strong outflows, causing the positive and steep correlations of velocity andṀ out with SFR. The outflow velocity correlation with SFR becomes flatter at z = 1, and η displays a negative correlation with halo mass in massive galaxies. Our study demonstrates that both the MUPPI and Effective models produce significant outflows at ∼ 1/10 of the virial radius; at the same time shows that the properties of outflows generated can be different from the input speed and mass loading in the Effective model. Our MUPPI model, using local properties of gas in the sub-resolution recipe, is able to develop galactic outflows whose properties correlate with global galaxy properties, and consistent with observations.

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“…al. [68] to incorporate the shear cross correlations as seen in, for example, [63] and the MG parameters.…”

Section: B Weak-lensing Implementationmentioning

confidence: 99%

Testing general relativity at cosmological scales: Implementation and parameter correlations

2011

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The testing of general relativity at cosmological scales has become a possible and timely endeavor that is not only motivated by the pressing question of cosmic acceleration but also by the proposals of some extensions to general relativity that would manifest themselves at large scales of distance. We analyze here correlations between modified gravity growth parameters and some core cosmological parameters using the latest cosmological data sets including the refined Cosmic Evolution Survey 3D weak lensing. We provide the parametrized modified growth equations and their evolution. We implement known functional and binning approaches, and propose a new hybrid approach to evolve the modified gravity parameters in redshift (time) and scale. The hybrid parametrization combines a binned redshift dependence and a smooth evolution in scale avoiding a jump in the matter power spectrum. The formalism developed to test the consistency of current and future data with general relativity is implemented in a package that we make publicly available and call ISiTGR (Integrated Software in Testing General Relativity), an integrated set of modified modules for the publicly available packages CosmoMC and CAMB, including a modified version of the integrated SachsWolfe-galaxy cross correlation module of Ho et al and a new weak-lensing likelihood module for the refined Hubble Space Telescope Cosmic Evolution Survey weak gravitational lensing tomography data. We obtain parameter constraints and correlation coefficients finding that modified gravity parameters are significantly correlated with σ8 and mildly correlated with Ωm, for all evolution methods. The degeneracies between σ8 and modified gravity parameters are found to be substantial for the functional form and also for some specific bins in the hybrid and binned methods indicating that these degeneracies will need to be taken into consideration when using future high precision data.PACS numbers: 95.36.+x,98.80.Es,98.62.Sb

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A combined analysis of 3D weak lensing, Lyman-α forest and WMAP year three data

Cited by 63 publications

References 32 publications

Local void vs dark energy: confrontation with WMAP and type Ia supernovae

Local void vs dark energy: confrontation with WMAP and type Ia supernovae

Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

Testing general relativity at cosmological scales: Implementation and parameter correlations

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