How do galaxies populate dark matter haloes

By Qi Guo, Simon D. M. White, Cheng Li, M. Boylan-Kolchin. 2009

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For any assumed standard stellar initial mass function, the Sloan Digital Sky Survey (SDSS) gives a precise determination of the abundance of galaxies as a function of their stellar mass over the full stellar mass range 108 M(circle dot) < M(*) < 1012 M(circle dot). Within the concordance Lambda cold dark matter (Lambda CDM) cosmology, the Millennium Simulations give precise halo abundances as a function of mass and redshift for all haloes within which galaxies can form. Under the plausible hypothesis that the stellar mass of a galaxy is an increasing function of the maximum mass ever attained by its halo, these results combine to give halo mass as a function of stellar mass. The result agrees quite well with observational estimates of mean halo mass as a function of stellar mass from stacking analyses of the gravitational lensing signal and the satellite dynamics of SDSS galaxies. For M(*) similar to 5.5 x 1010 M(circle dot), the stellar mass usually assumed for the Milky Way (MW), the implied halo mass is similar to 2 x 1012 M(circle dot), consistent with most recent direct estimates and inferences from the MW/M31 timing argument. The fraction of the baryons associated with each halo which are present as stars in its central galaxy reaches a maximum of 20 per cent at masses somewhat below that of the MW and falls rapidly at both higher and lower masses. These conversion efficiencies are lower than in almost all recent high-resolution simulations of galaxy formation, showing that these are not yet viable models for the formation of typical members of the galaxy population. When inserted in the Millennium-II Simulation, our derived relation between stellar mass and halo mass predicts a stellar mass autocorrelation function in excellent agreement with that measured directly in the SDSS. The implied Tully-Fisher relation also appears consistent with observation, suggesting that galaxy luminosity functions and Tully-Fisher relations can be reproduced simultaneously in a Lambda CDM cosmology.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3beefe2615a90b370ae6bdd2eeae337f87414760

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Citations in the corpus

The APOSTLE simulations: solutions to the Local Group's cosmic puzzles (2015, result): “…model of the EAGLE code, which we have adopted in this work, generally results in slightly low stellar masses in haloes of around 1012 M compared to abundance matching expectations (e.g. Guo et al. 2010), while the MW and M31 both appear to lie above the average stellar-tohalo mass relation.”
Bent by baryons: the low-mass galaxy-halo relation (2014, methodology): “Abundance matching is employed widely to infer quantities such as the stellar-to-total mass relation (e.g. Frenk et al. 1988; Yang et al. 2003; Guo et al. 2010; Moster et al. 2013).”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “Furthermore, η∗ peaks for Milky Way-sized galaxies (Mh ≈ 10 12M⊙), and declines rapidly on either side of the peak (e.g. Figure 2 in Guo et al. 2010).”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “However, negligible differences would have been obtained using e.g. the similar relations derived by Behroozi, Conroy & Wechsler (2010) or Guo et al. (2010).”
A mass-dependent density profile for dark matter haloes including the influence of galaxy formation (2014, positive): “The galaxies that use the ﬁducial parameters from Stinson et al. (2013) match the stellar-halo mass relation at z = 0 (Guo et al.2010; Moster et al.2010) and at higher redshift (Kannan et al. 2014) as well as a range of present observed galaxy properties and scaling relations (Brook et al. 2012b;…”
Self-regulated star formation in galaxies via momentum input from massive stars (2011, background): “…it difficult to drive winds and suppress star formation at the level needed to explain the galaxy mass function (especially at low masses) and observed star formation efficiencies (see e.g. Guo et al. 2010; Powell, Slyz & Devriendt 2011; Brook et al. 2011; Nagamine 2011, and references therein).”
Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, methodology): “Several groups used this abundance matching technique to compare total halo masses with galaxy stellar masses (Conroy & Wechsler 2009; Moster et al. 2010; Guo et al. 2010; Behroozi et al. 2010).”
Idealized models for galactic disc formation and evolution in ‘realistic’ ΛCDM haloes (2012, background): “…these simulations have in general suffered from a range of problems, including angular momentum loss leading to overly small discs (Navarro & Benz 1991), production of overly massive galaxies (Guo et al. 2010), and too much early and too little late star formation (SF; Scannapieco et al. 2009).”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, background): “In the local Universe, abundance-matching studies have shown that at z < 0.1 the stellar-to-halo mass ratio (SHMR, Mstar/Mh) reaches a maximum of a few percent at Mh ∼ 1012 M , much smaller than the universal baryon fraction (Guo et al. 2010).”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, background): “Results of abundance matching of halo mass function to the stellar mass function of galaxies showed that this efficiency peaks at halo masses of M ≈ 1012 M but is quickly decreasing at both smaller and larger masses (e.g., Conroy & Wechsler 2009; Guo et al. 2010).”
THIRD-EPOCH MAGELLANIC CLOUD PROPER MOTIONS. I. HUBBLE SPACE TELESCOPE/WFC3 DATA AND ORBIT IMPLICATIONS (2013, methodology): “The dispersion decreases as the LMC’s mass increases; for high mass LMC models (consistent with ΛCDM expectations, Guo et al. 2010) dynamical friction limits the number of closed orbit solutions within the error space.”
Mass models of the Milky Way (2011, positive): “Guo et al. (2010) found that the ratio of total stellar mass M∗ to halo mass Mv was well fit by M∗ = Mv ×A [ ( Mv M0 )−α + ( Mv M0 )β ]−γ , (5) with an intrinsic scatter of order 0.2 in log10 M∗, where A = 0.129, M0 = 10 11.4 M⊙, α = 0.926, β = 0.261 and γ = 2.440.”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, background): “…mass with an efficiency η(Mh, z) ≡ (M∗/Mh)×(ΩM/Ωb) that depends strongly on halo mass, peaking at Mh ∼ 1012 M and declining toward lower and higher masses at z ∼ 0 (e.g., Mandelbaum et al. 2006b; Conroy & Wechsler 2009; Moster et al. 2010; Behroozi et al. 2010; Guo et al. 2010; More et al. 2010).”
Cusp-core transformations in dwarf galaxies: observational predictions (2012, result): “…formation simulations (Piontek & Steinmetz 2009; Governato et al. 2010; Agertz et al. 2011), when compared to individual galaxies or to an ensemble of galaxies using the abundance matching technique (Guo et al. 2010; Moster et al. 2010), although recently Munshi et al. (2012) argue differently.”
TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS (2012, methodology): “…baryon masses and concentrations of galaxies compared to expected values derived using dark matter halo abundance matching (Conroy & Wechsler 2009; Guo et al. 2010), satellite kinematics (Klypin & Prada 2009; More et al. 2010), and weak lensing (Mandelbaum et al. 2006), see Behroozi et al. (2010)…”