Primeval Adiabatic Perturbation in an Expanding Universe

Peebles, P. J. E.; Yu, Jiabin

doi:10.1086/150713

Cited by 1,205 publications

(1,047 citation statements)

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“…This was soon extended to the late-time matter power spectrum by (Sakharov, 1966;Peebles and Yu, 1970;Sunyaev and Zeldovich, 1970); of course, they were considering pure baryon cosmologies, where the effect is very strong. The introduction of adiabatic cold dark matter in the mid-1980's made the predicted late-time acoustic peak very weak (particularly in Figure 8 (Left) The current BAO distance-redshift relation.…”

Section: The Current State Of Playmentioning

confidence: 97%

“…The result is a close coupling between the electrons, nuclei (baryons), and photons for sufficiently long wavelength perturbations in the early universe. The radiation pressure of the photons is large compared to the gravitational forces in the perturbations, with the result that perturbations in the baryon-photon fluid oscillate as sound waves (Peebles and Yu, 1970;Sunyaev and Zeldovich, 1970). Diffusion of photons relative to baryons damps these oscillations on comoving scales smaller than ∼ 8 h −1 Mpc, the phenomenon known as Silk damping (Silk, 1968).…”

Section: Linear Theorymentioning

confidence: 99%

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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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Section: The Current State Of Playmentioning

confidence: 97%

Section: Linear Theorymentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…In the standard CDM cosmological model, with dark energy and cold dark matter, structure formation in our Universe is described as the gravity-induced growth of small perturbations in the matter density field (Peebles & Yu 1970). This field is dominated by dark matter (DM) which outweighs the mass in baryons by a factor of ∼5 (Planck Collaboration XIII 2016).…”

Section: Introductionmentioning

confidence: 99%

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Brouwer¹,

Cacciato²,

Dvornik³

et al. 2016

Mon. Not. R. Astron. Soc.

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Galaxies and their dark matter haloes are part of a complex network of mass structures, collectively called the cosmic web. Using the tidal tensor prescription these structures can be classified into four cosmic environments: voids, sheets, filaments and knots. As the cosmic web may influence the formation and evolution of dark matter haloes and the galaxies they host, we aim to study the effect of these cosmic environments on the average mass of galactic haloes. To this end we measure the galaxy-galaxy lensing profile of 91, 195 galaxies, within 0.039 < z < 0.263, from the spectroscopic Galaxy And Mass Assembly (GAMA) survey, using ∼ 100 deg 2 of overlapping data from the Kilo-Degree Survey (KiDS). In each of the four cosmic environments we model the contributions from group centrals, satellites and neighbouring groups to the stacked galaxy-galaxy lensing profiles. After correcting the lens samples for differences in the stellar mass distribution, we find no dependence of the average halo mass of central galaxies on their cosmic environment. We do find a significant increase in the average contribution of neighbouring groups to the lensing profile in increasingly dense cosmic environments. We show, however, that the observed effect can be entirely attributed to the galaxy density at much smaller scales (within 4 h −1 Mpc), which is correlated with the density of the cosmic environments. Within our current uncertainties we find no direct dependence of galaxy halo mass on their cosmic environment.

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“…The angular power spectrum of cosmic microwave background (CMB) temperature fluctuations is now becoming a powerful cosmological probe [1], both due to our detailed understanding of physics during the recombination era [2] and progress on the experimental front [3]. In addition to the primary anisotropies generated at the last-scattering surface, CMB photons are also affected by large-scale structure at low redshifts.…”

Section: Introductionmentioning

confidence: 99%

Small-scale cosmic microwave background polarization from reionization

2003

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We discuss fluctuations in the cosmic microwave background (CMB) polarization due to scattering from reionized gas at low redshifts. Polarization is produced by re-scattering of the primordial temperature anisotropy quadrupole and of the kinematic quadrupole that arises from gas motion transverse to the line of sight. We show that both effects produce equal E-and B-parity polarization, and are, in general, several orders of magnitude below the dominant polarization contributions at the last scattering surface to E-modes or the gravitational-lensing contribution to B-modes at intermediate redshifts. These effects are also several orders of magnitude below the B polarization due to lensing even after subtraction with higher-order correlations, and are thus too small to constitute a background for searches for the polarization signature of inflationary gravitational waves.

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Primeval Adiabatic Perturbation in an Expanding Universe

Cited by 1,205 publications

References 0 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Small-scale cosmic microwave background polarization from reionization

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Primeval Adiabatic Perturbation in an Expanding Universe

Cited by 1,205 publications

References 0 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg2of KiDS weak lensing data

Small-scale cosmic microwave background polarization from reionization

Contact Info

Product

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Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data