Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology

By Qi Guo, Simon D. M. White, M. Boylan-Kolchin, G. Lucia, G. Kauffmann, Gerard Lemson, Cheng Li, Volker Springel, Simone M. Weinmann. 2010

949 citations recorded by the source corpus.

We have updated and extended our semi-analytic galaxy formation modelling capabilities and applied them simultaneously to the stored halo/subhalo merger trees of the Millennium and Millennium-II simulations. These differ by a factor of 125 in mass resolution, allowing explicit testing of resolution effects on predicted galaxy properties. We have revised the treatments of the transition between the rapid infall and cooling flow regimes of gas accretion, of the sizes of bulges and of gaseous and stellar disks, of supernova feedback, of the transition between central and satellite status as galaxies fall into larger systems, and of gas and star stripping once they become satellites. Plausible values of efficiency and scaling parameters yield an excellent fit not only to the observed abundance of low-redshift galaxies over 5 orders of magnitude in stellar mass and 9 magnitudes in luminosity, but also to the observed abundance of Milky Way satellites. This suggests that reionisation effects may not be needed to solve the “missing satellite” problem except, perhaps, for the faintest objects. The same model matches the observed large-scale clustering of galaxies as a function of stellar mass and colour. The fit remains excellent down to � 30 kpc for massive galaxies. For M∗ < 6×10 10 M⊙, however, the model overpredicts clustering at scales below � 1 Mpc, suggesting that the assumed fluctuation amplitude, σ8 = 0.9, is too high. The observed difference in clustering between active and passive galaxies is matched quite well for all masses. Galaxy distributions within rich clusters agree between the simulations and match those observed, but only if galaxies without dark matter subhalos (so-called orphans) are included. Even at MS-II resolution, schemes which assign galaxies only to resolved dark matter subhalos cannot match observed clusters. Our model predicts a larger passive fraction among low-mass galaxies than is observed, as well as an overabundance of � 10 10 M⊙ galaxies beyond z � 0.6. (The abundance of � 10 11 M⊙ galaxies is matched out to z � 3.) These discrepancies appear to reflect deficiencies in the way star-formation rates are modelled.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3e1e7b48201976b99d265121f1278eba0aab2be1

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Citations in the corpus

A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “Semi-analytical models (e.g., White & Frenk 1991; Kauffmann et al. 1993; Baugh 2006; Croton et al. 2006; Guo et al. 2011; Benson 2012) account for baryonic physics by adding galaxy formation as a post-processing step on top of the output of N-body simulations or onto Monte-Carlo realisations of…”
Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models (2012, methodology): “We compare our results with a theoretical light-cone based on the latest version of the Munich semi-analytic galaxy formation and evolution model (Guo et al. 2011; Henriques et al. 2012).”
Halo concentrations in the standard LCDM cosmology (2011, background): “The main difference in cosmological parameters between the simulations is that the Millennium simulations adopted a substantially larger amplitude of perturbations σ8 that is nearly 4σ away from recent constraints (e.g., Klypin et al. 2010; Guo et al. 2011).”
The Phoenix Project: the dark side of rich galaxy clusters (2012, positive): “…by tidal stripping and so are poor indicators of galaxy properties, the mass or circular velocity at infall are plausibly much better and give meaningful results when used in subhalo abundance matching analyses (Vale & Ostriker 2004; Conroy et al. 2006; Behroozi et al. 2010; Guo et al. 2010).”
Idealized models for galactic disc formation and evolution in ‘realistic’ ΛCDM haloes (2012, background): “Since detailed population properties are reproduced quite well in the standard cold dark matter ( CDM) paradigm by simple semi-analytic simulations (e.g. Guo et al. 2011), it has been argued that the relevant SF and feedback processes are still inadequately represented in hydrodynamical simulations.”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “A similar recipe is incorporated into the later generations of MPA-SAMs (e.g. Croton et al. 2006, De Lucia & Blaizot 2007, Guo et al. 2011, Henriques et al. 2013).”
Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries (2016, methodology): “…estimates: they used state-of-the-art binary population synthesis models in combination with the global star-formation history and metallicity evolution predicted by the semi-analytic galaxy formation model of Guo et al. (2011), to calculate the energy input from binaries at z ∼> 6-8.”
THE COSMOLOGICAL SIZE AND VELOCITY DISPERSION EVOLUTION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “The early domination of in-situ star formation and the subsequent growth by stellar mergers is in agreement with predictions from semianalytical models (Kauffmann 1996; Khochfar & Silk 2006a; De Lucia et al. 2006; De Lucia & Blaizot 2007; Guo & White 2008; Shankar et al. 2010a,b) and the assembly sc”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “…only simulations of cosmic large-scale structure (e.g. Davis et al. 1985; Springel et al. 2006) and with semi-analytic galaxy formation models (e.g. Guo et al. 2011), making realistic spiral galaxies on the computer has emerged as an unexpectedly difficult endeavor that has withstood countless…”
The missing massive satellites of the Milky Way (2012, background): “…the relatively small number of subhalos massive enough to host luminous galaxies (see, e.g., Kauffmann et al. 1993; Bullock et al. 2000; Benson et al. 2002; Somerville ⋆ Email: jie.wang@durham.ac.uk 2002; Cooper et al. 2010; Li et al. 2010; Macciò et al. 2010; Guo et al. 2011; Font et al. 2011).”
THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES (2012, background): “With new and updated data, we have observed that the 14 For clarity we note that Guo et al. (2011) excluded the square on the normalized velocity term in their eq.”
Star formation in semi-analytic galaxy formation models with multiphase gas (2015, methodology): “…H2 in radial bins in each galaxy, using both the metallicitydependent recipes of Krumholz et al. (2009b) and the pressure-based recipe of Blitz & Rosolowsky (2006), and self-consistently implemented an H2-based star formation recipe, within the semi-analytic modeling framework of Guo et al. (2011).”
How sensitive are predicted galaxy luminosities to the choice of stellar population synthesis model (2013, methodology): “At z =0, the curve is quite close to that calculated by Guo et al. (2011) using a diﬀerent semi-analytical model based on the Millennium N-body simula-Figure tion.”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, methodology): “…reproducing a wide range of the observed galaxy properties (see Oppenheimer & Davé 2008, Khandai et al. 2014, and Vogelsberger et al. 2014 for the latest hydrodynamic simulations and see Guo et al. 2011 for the recent development in SAM), though still with several possible areas of improvement.”
Bulge mass is king: the dominant role of the bulge in determining the fraction of passive galaxies in the Sloan Digital Sky Survey (2014, background): “In most contemporary theoretical frameworks (e.g. Croton et al. 2006, Bower et al. 2008, Guo et al. 2011) it is radio-mode, not quasar-mode, AGN feedback which is expected to have the dominant impact on the star formation history of most masses of galaxies.”
Theoretical Challenges in Galaxy Formation (2016, background): “…attempts to input what are thought to be the most important physical processes in a simple fashion (e.g. Bower et al. 2006; Croton et al. 2006; Guo et al. 2011; Henriques et al. 2015; Kauffmann, White & Guiderdoni 1993; Somerville & Primack 1999) aim at finding that set which best produces…”