Simulations of the formation, evolution and clustering of galaxies and quasars

Springel, Volker; White, Simon D. M.; Jenkins, Adrian; Frenk, Carlos S.; Yoshida, Naoki; Gao, Liang; Navarro, Julio F.; Thacker, Robert J.; Croton, Darren J.; Helly, John; Peacock, J. A.; Cole, Shaun; Thomas, P.; Couchman, H. M. P.; Evrard, A. E.; Colberg, J. M.; Pearce, Frazer R.

doi:10.1038/nature03597

Cited by 4,622 publications

(5,218 citation statements)

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“…Small-scale structure grows non-linearly, peculiar velocities behave differently from their linear prediction, and galaxies trace the dark matter in a complicated manner. We should worry that these effects might modify the location of the BAO feature relative to the prediction of linear theory, thus distorting our standard ruler (Meiksin et al, 1999;Seo and Eisenstein, 2005;Angulo et al, 2005;Springel et al, 2005;Jeong and Komatsu, 2006;Huff et al, 2007;Angulo et al, 2008;Wagner et al, 2008).…”

Section: Non-linear Evolution and Galaxy Clustering Biasmentioning

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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Section: Non-linear Evolution and Galaxy Clustering Biasmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…Their estimated H2 mass does not include the contribution of helium. They considered radiative cooling (Wiersma et al 2009;Schaye et al 2015), photo-heating by cosmic microwave background, UV and X-ray background radiation (Haardt & Madau 2001 (Springel et al 2005b). With the L-GALAXIES, they implemented radiative cooling with the cooling function of Sutherland & Dopita (1993), photoionisation heating (Gnedin 2000;Kravtsov et al 2004), star formation (Kauffmann 1996;Kennicutt 1989), and the feedbacks from SNe and AGN (Croton et al 2006).…”

Section: Galaxy Formation Models In the Literaturesmentioning

confidence: 99%

Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

Morokuma-Matsui¹,

Baba²

2015

Mon. Not. R. Astron. Soc.

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We investigate the redshift evolution of the molecular gas mass fraction (f mol = M mol M⋆+M mol , where M mol is molecular gas mass and M ⋆ is stellar mass) of galaxies in the redshift range of 0 < z < 2 as a function of the stellar mass by combining CO literature data. We observe a stellar-mass dependence of the f mol evolution where massive galaxies have largely depleted their molecular gas at z = 1, whereas the f mol value of less massive galaxies drastically decreases from z = 1. We compare the observed M ⋆ −f mol relation with theoretical predictions from cosmological hydrodynamic simulations and semi-analytical models for galaxy formation. Although the theoretical studies approximately reproduce the observed mass dependence of f mol evolution, they tend to underestimate the f mol values, particularly of less massive (< 10 10 M ⊙ ) and massive galaxies (> 10 11 M ⊙ ) when compared with the observational values. Our result suggests the importance of the feedback models which suppress the star formation while simultaneously preserving the molecular gas in order to reproduce the observed M ⋆ − f mol relation.

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“…(See, for example, Falder et al [2011] and Capak et al [2011], who find two galaxies in the z ¼ 5:3 cluster bright enough to be detected by SERVS at 4.5 μm.) For comparison, the largest structures seen in the Millennium simulation at z ∼ 1 are of the order of 100 Mpc (Springel et al 2005), which subtends 3°at that redshift, so each SERVS field samples a wide range of environments. By combining the five different fields of SERVS, the survey effectively averages over large-scale structure and presents a representative picture of the average properties of galaxies in the high-redshift universe.…”

Section: Introductionmentioning

confidence: 99%