Galaxy formation in WMAP1 and WMAP7 cosmologies

By Qi Guo, Simon D. M. White, R. Angulo, B. Henriques, Gerard Lemson, M. Boylan-Kolchin, P. Thomas, C. Short. 2012

261 citations recorded by the source corpus.

Using the technique of Angulo & White (2010) we scale the Millennium and Millennium-II simulations of structure growth in aCDM universe from the cosmo- logical parameters with which they were carried out (based on first-year results from the Wilkinson Microwave Anisotropy Probe, WMAP1) to parameters consistent with the seven-year WMAP data (WMAP7). We implement semi-analytic galaxy formation modelling on both simulations in both cosmologies to investigate how the formation, evolution and clustering of galaxies are predicted to vary with cosmological parame- ters. The increased matter density m and decreased linear fluctuation amplitude σ8 in WMAP7 have compensating effects, so that the abundance and clustering of dark halos are predicted to be very similar to those in WMAP1 for z 6 3. As a result, local galaxy properties can be reproduced equally well in the two cosmologies by slightly altering galaxy formation parameters. The evolution of the galaxy populations is then also similar. In WMAP7, structure forms slightly later. This shifts the peak in cosmic star formation rate to lower redshift, resulting in slightly bluer galaxies at z = 0. Nev- ertheless, the model still predicts more passive low-mass galaxies than are observed. For rp 1 galaxies are predicted to be more strongly clustered for WMAP7. Differences in galaxy properties, including, clustering, in these two cosmologies are rather small out to z � 3. Given that there are still considerable residual uncertainties in galaxy formation models, it is very difficult to distinguish WMAP1 from WMAP7 through observations of galaxy properties or their evolution.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8a8048e2d75861dbaf87e7808eeb43147a730a9e

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Citations in the corpus

The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “Both semi-analytical and hydrodynamical simulations are often (but not always, see e.g. Dubois et al. 2014) calibrated against the local SMF (e.g. Guo et al. 2011, 2013; Genel et al. 2014; Schaye et al. 2016); measurements at z > 0 are then used to test theoretical predictions (Torrey et al. 2014;…”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, methodology): “With the aid of a semi-analytic galaxy formation model (Guo et al. 2011, 2013) they demonstrated that these selection criteria are quite good at minimizing the contamination due to satellite (sub)haloes.”
ANCIENT LIGHT FROM YOUNG COSMIC CITIES: PHYSICAL AND OBSERVATIONAL SIGNATURES OF GALAXY PROTO-CLUSTERS (2013, background): “Recently, aWMAP7 version was released (Guo et al. 2013).”
Galaxy Protoclusters as Drivers of Cosmic Star Formation History in the First 2 Gyr (2017, methodology): “We also use the SAM of Guo et al. (2013) (hereafter G13), which was constrained only using the local galaxy stellar mass function.”
Simulations of the galaxy population constrained by observations from z = 3 to the present day: implications for galactic winds and the fate of their ejecta (2012, methodology): “The latest version of the Munich semi-analytic model (Guo et al. 2011, 2013, hereafter G11-WMAP1, G11-WMAP7, respectively) was tested and its parameter values adjusted by comparison with low-redshift galaxy data, namely, stellar mass and optical luminosity functions, gas fractions, colours,…”
Co-orbiting satellite galaxy structures are still in conflict with the distribution of primordial dwarf galaxies (2014, methodology): “The other obvious difference between the samples is that we use the Millennium II simulation scaled to cosmological parameters from WMAP7 (instead of WMAP1), while the semi-analytic modelling is almost identical (Guo et al. 2013).”
A unified multiwavelength model of galaxy formation (2015, methodology): “3 This is the simulation referred to as MS-W7 in Guo et al. (2013) and Gonzalez-Perez et al. (2014) and as MW7 in Jenkins (2013).”
How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, background): “Similarly, SAMs must include strong outflows to match observational constraints such as the galaxy stellar mass function (e.g.Somerville & Primack 1999; Somerville et al. 2008; Benson et al. 2003; Benson 2014; Croton et al. 2006; Guo et al. 2011, 2013; Lu et al. 2014).”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “— Fraction of massive galaxies (M > 1010 M⊙) that are quiescent in the SAM of Guo et al. (2013), as a function of total stellar mass, stellar mass in the bulge and disk separately, and as a function of halo and black hole mass.”