Effects of Baryons and Dissipation on the Matter Power Spectrum

Rudd, Douglas H.; Zentner, Andrew R.; Kravtsov, Andrey V.

doi:10.1086/523836

Cited by 414 publications

(560 citation statements)

References 106 publications

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“…Jing et al (2006), Rudd et al (2008), Guillet et al (2010), Casarini et al (2012) all confirmed the significance of baryonic feedback at k > 1h Mpc −1 by comparing hydrodynamical simulations to pure N-body dark matter ones. Schaye et al (2010) .…”

Section: Baryonic Feedbackmentioning

confidence: 57%

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

MacCrann

Zuntz

Bridle

et al. 2015

Monthly Notices of the Royal Astronomical Society

177

192

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We examine the level of agreement between low redshift weak lensing data and the CMB using measurements from the CFHTLenS and Planck+WMAP polarization. We perform an independent analysis of the CFHTLenS six bin tomography results of Heymans et al. (2013). We extend their systematics treatment and find the cosmological constraints to be relatively robust to the choice of non-linear modeling, extension to the intrinsic alignment model and inclusion of baryons. We find that when marginalised in the Ω m -σ 8 plane, the 95% confidence contours of CFHTLenS and Planck+WP only just touch, but the discrepancy is less significant in the full 6-dimensional parameter space of ΛCDM. Allowing a massive active neutrino or tensor modes does not significantly resolve the tension in the full n-dimensional parameter space. Our results differ from some in the literature because we use the full tomographic information in the weak lensing data and marginalize over systematics. We note that adding a sterile neutrino to ΛCDM brings the 2d marginalised contours into greater overlap, mainly due to the extra effective number of neutrino species, which we find to be 0.88 ± 0.43 (68%) greater than standard on combining the datasets. We discuss why this is not a completely satisfactory resolution, leaving open the possibility of other new physics or observational systematics as contributing factors. We provide updated cosmology fitting functions for the CFHTLenS constraints and discuss the differences from ones used in the literature.

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Section: Baryonic Feedbackmentioning

confidence: 57%

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

MacCrann

Zuntz

Bridle

et al. 2015

Monthly Notices of the Royal Astronomical Society

177

192

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“…The power spectrum can then be calculated by providing the mass of the central galaxy (through abundancematching), its size, the total gas mass as a fraction of the total halo mass, and an adiabatic contraction for the cold dark matter. This model has been developed over a number of years [303,304,305,306,307,308,309], and has been found to agree well with zooming hydrodynamical simulations [310]. One can then use such models to marginalize over baryonic effects in surveys, e.g.…”

Section: Simulating the Universementioning

confidence: 90%

BeyondΛCDM: Problems, solutions, and the road ahead

Bull

Akrami

Adamek

et al. 2016

Physics of the Dark Universe

460

210

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Despite its continued observational successes, there is a persistent (and growing) interest in extending cosmology beyond the standard model, ΛCDM. This is motivated by a range of apparently serious theoretical issues, involving such questions as the cosmological constant problem, the particle nature of dark matter, the validity of general relativity on large scales, the existence of anomalies in the CMB and on small scales, and the predictivity and testability of the inflationary paradigm. In this paper, we summarize the current status of ΛCDM as a physical theory, and review investigations into possible alternatives along a number of different lines, with a particular focus on highlighting the most promising directions. While the fundamental problems are proving reluctant to yield, the study of alternative cosmologies has led to considerable progress, with much more to come if hopes about forthcoming high-precision observations and new theoretical ideas are fulfilled.Keywords: cosmology -dark energy -cosmological constant problem -modified gravitydark matter -early universe Cosmology has been both blessed and cursed by the establishment of a standard model: ΛCDM. On the one hand, the model has turned out to be extremely predictive, explanatory, and observationally robust, providing us with a substantial understanding of the formation of large-scale structure, the state of the early Universe, and the cosmic abundance of different types of matter and energy. It has also survived an impressive battery of precision observational tests -anomalies are few and far between, and their significance is contentious where they do arise -and its predictions are continually being vindicated through the discovery of new effects (B-mode polarization [1] and lensing [2,3] of the cosmic microwave background (CMB), and the kinetic Sunyaev-Zel'dovich effect [4] being some recent examples). These are the hallmarks of a good and valuable physical theory.On the other hand, the model suffers from profound theoretical difficulties. The two largest contributions to the energy content at late times -cold dark matter (CDM) and the cosmological constant (Λ) -have entirely mysterious physical origins. CDM has so far evaded direct detection by laboratory experiments, and so the particle field responsible for it -presumably a manifestation of "beyond the standard model" particle physics -is unknown. Curious discrepancies also appear to exist between the predicted clustering properties of CDM on small scales and observations. The cosmological constant is even more puzzling, giving rise to quite simply the biggest problem in all of fundamental physics: the question of why Λ appears to take such an unnatural value [5,6,7]. Inflation, the theory of the very early Universe, has also been criticized for being fine-tuned and under-predictive [8], and appears to leave many problems either unsolved or fundamentally unresolvable. These problems are indicative of a crisis.From January 14th-17th 2015, we held a conference in Oslo, Norway to surve...

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“…Therefore one should worry that the removal of baryonic physics-induced bias seen by Semboloni et al (2011) might not be realized in practice, if the simulation captures the qualitative features of AGN feedback but does not quantitatively reproduce the correct functional form. Zentner et al (2012) avoid this issue by fitting cosmic shear power spectra based on the van simulations using a mitigation procedure tuned to the Rudd et al (2008) simulations. However they find that this procedure, while successful on simulated Stage III (DES) survey data, is not adequate for the more ambitious task of Stage IV data analysis.…”

Section: Intrinsic Alignments*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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Effects of Baryons and Dissipation on the Matter Power Spectrum

Cited by 414 publications

References 106 publications

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

BeyondΛCDM: Problems, solutions, and the road ahead

Observational probes of cosmic acceleration

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