Cold dark matter variant cosmological models — I. Simulations and preliminary comparisons

Groß, Michael; Somerville, Rachel S.; Primack, Joel R.; Holtzman, Jon; Klypin, Anatoly

doi:10.1046/j.1365-8711.1998.01998.x

Cited by 108 publications

(107 citation statements)

References 57 publications

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“…The PS mass function is not compared because, as is well known, while qualitatively correct, it disagrees with the results of N-body simulations: the PS formula overestimates the abundance of halos near the characteristic mass M Ã and underestimates the abundance in the high-mass tail ( Efstathiou et al 1988;Lacey & Cole 1994;Tozzi & Governato 1998;Gross et al 1998;Governato et al 1999). The J01 result is also not plotted since that mass function fits much of R03 data well at z ¼ 0 but diverges from R03 simulation results once well below the limit of its empirical fit of ln À1 ¼ À1:2, which corresponds to '4 ; 10 11 h À1 M with 8 ¼ 1:0.…”

Section: Resultsmentioning

confidence: 97%

Evolution of the Cosmological Mass Function in a Moving Barrier Model

Popolo

2006

Astron J

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I calculate the mass function evolution in a ÃCDM model by means of the excursion set model and an improved version of the barrier shape obtained by Del Popolo & Gambera, which implicitly takes account of the total angular momentum acquired by the protostructure during evolution and of a nonzero cosmological constant. I compare the result with that of Reed et al., who used a high-resolution ÃCDM numerical simulation to calculate the mass function of dark matter halos down to the scale of dwarf galaxies, back to a redshift of 15. I show that the mass function obtained in the present paper gives similar predictions to the Sheth & Tormen mass function but does not share its overprediction of extremely rare objects. The results confirm previous findings that the simulated halo mass function can be described solely by the variance of the mass distribution, and thus has no explicit redshift dependence.

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Section: Resultsmentioning

confidence: 97%

Evolution of the Cosmological Mass Function in a Moving Barrier Model

Popolo

2006

Astron J

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“…By the mid-1990s, many cosmological simulation studies included both open-CDM models and Λ-CDM models, along with Ω m = 1 models incorporating tilted inflationary spectra, nonstandard radiation components, or massive neutrino components (e.g., Ostriker and Cen 1996;Cole et al 1997;Gross et al 1998;Jenkins et al 1998). Once normalized to the observed level of CMB anisotropies, the large-scale structure predictions of open and flat-Λ models differed at the tens-of-percent level, with flat models generally yielding a more natural fit to the observations (e.g., Cole et al 1997).…”

Section: Historymentioning

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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“…The number of galaxies in each pixel is divided by its selection function; we then consider the galaxy overdensity per pixel: δ g = (N −N)/N . These data are then compared to N-body simulations by Gross et al [8] of four cosmological models:…”

Section: How Probable Are the Spikes?mentioning

confidence: 99%

Cosmological implications of Lyman-break galaxy clustering

Groß¹,

Primack²,

Blumenthal³

et al. 1999

The 9th Astrophysics Conference: After the Dark Ages, When Galaxies Were Young (The Universe at 2Self Cite

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Abstract. We review our analysis of the clustering properties of "Lyman-break" galaxies (LBGs) at redshift z ∼ 3, previously discussed in Wechsler et al. [1]. We examine the likelihood of spikes found by Steidel et al. [2] in the redshift distribution of LBGs, within a suite of models for the evolution of structure in the Universe. Using highresolution dissipationless N-body simulations, we analyze deep pencil-beam surveys from these models in the same way that they are actually observed, identifying LBGs with the most massive dark matter halos. We find that all the models (with SCDM as a marginal exception) have a substantial probability of producing spikes similar to those observed, because the massive halos are much more clumped than the underlying matter -i.e., they are biased. Therefore, the likelihood of such a spike is not a good discriminator among these models. The LBG correlation functions are less steep than galaxies today (γ ∼ 1.4), but show similar or slightly longer correlation lengths. We have extened this analysis and include a preliminary comparison to the new data presented in Adelberger et al. [3]. We also discuss work in progress, in which we use semi-analytic models to identify Lyman-break galaxies within dark-matter halos.

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Cold dark matter variant cosmological models — I. Simulations and preliminary comparisons

Cited by 108 publications

References 57 publications

Evolution of the Cosmological Mass Function in a Moving Barrier Model

Evolution of the Cosmological Mass Function in a Moving Barrier Model

Observational probes of cosmic acceleration

Cosmological implications of Lyman-break galaxy clustering

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