Dark Halo and Disk Galaxy Scaling Laws in Hierarchical Universes

By J. Navarro, Matthias Steinmetz. 2000

337 citations recorded by the source corpus.

We use cosmological N-body/gasdynamical simulations that include star formation and feedback to examine the proposal that scaling laws between the total luminosity, rotation speed, and angular momentum of disk galaxies reflect analogous correlations between the structural parameters of their surrounding dark matter halos. The numerical experiments follow the formation of galaxy-sized halos in two cold dark matter (CDM)-dominated universes: the standard Ω = 1 CDM scenario and the currently popular ΛCDM model. We find that the slope and scatter of the I-band Tully-Fisher relation are well reproduced in the simulations, although not, as proposed in recent work, as a result of the cosmological equivalence between halo mass and circular velocity: large systematic variations in the fraction of baryons that collapse to form galaxies and in the ratio between halo and disk circular velocities are observed in our numerical experiments. The Tully-Fisher slope and scatter are recovered in this model as a direct result of the dynamical response of the halo to the assembly of the luminous component of the galaxy. We conclude that models that neglect the self-gravity of the disk and its influence on the detailed structure of the halo cannot be used to derive meaningful estimates of the scatter or slope of the Tully-Fisher relation. Our models fail, however, to match the zero point of the Tully-Fisher relation, as well as that of the relation linking disk rotation speed and angular momentum. These failures can be traced, respectively, to the excessive central concentration of dark halos formed in the CDM cosmogonies we explore and to the formation of galaxy disks as the final outcome of a sequence of merger events. Disappointingly, our feedback formulation, calibrated to reproduce the empirical correlations linking star formation rate and gas surface density established by Kennicutt, has little influence on these conclusions. Agreement between model and observations appears to demand substantial revision to the CDM scenario or to the manner in which baryons are thought to assemble and evolve into galaxies in hierarchical universes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/24b845d22ce5ca826e061d7725203976943e4325

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Toward First-Principle Simulations of Galaxy Formation: I. How Should We Choose Star-Formation Criteria in High-Resolution Simulations of Disk Galaxies? (2008, background): “Choosing C∗ ∼ 0.01 reproduces the SchmidtKennicutt relation in the local universe (e.g., Navarro & Steinmetz 2000).”
The formation of disc galaxies in a ΛCDM universe (2010, methodology): “…well with observational constraints on disc characteristics (Courteau 1997; Gnedin et al. 2007), as well as the angular momentum content of disc galaxies (Navarro & Steinmetz 2000), the Tully-Fisher relationship (Pizagno et al. 2007) and the ΣSFR-Σgas relation (Kennicutt 1998; Bigiel et al. 2008).”
The Angular Momentum of Gas in Protogalaxies. I. Implications for the Formation of Disk Galaxies (2002, background): “21 detailed hydrodynamic simulations of disk formation in a cold dark matter (CDM) universe yield disks that are an order of magnitude too small (Navarro & Benz 1991; Navarro & White 1994; Steinmetz & Navarro 1999; Navarro & Steinmetz 2000).”
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, methodology): “…of satellite galaxies around a typical Milky Way sized galaxy (e.g., Moore et al. 1999; Klypin et al. 1999; but see Stoehr et al. 2002) and to problems with the formation of disk galaxies (White & Navarro 1993; Navarro & Steinmetz 1999, 2000; Mo & Mao 2000; van den Bosch, Burkert & Swaters 2001).”
A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts (2003, background): “…gas suggest that a significant fraction of the angular momentum of the baryons is redistributed to the dark matter by dynamical friction (see e.g. Navarro & Steinmetz 2000), although the heating of the gas in sub-galactic halos may increase the tidal stripping and the angular momentum of the gas…”
Triaxial orbit based galaxy models with an application to the (apparent) decoupled core galaxy NGC 4365 (2007, background): “Another area of interest is the validation of predictions on the halo shapes from galaxy merger (e.g. Wechsler et al. 2002) and CDM cosmology simulations (e.g. Navarro & Steinmetz 2000).”
The Dynamics of Sinking Satellites around Disk Galaxies: A Poor Man’s Alternative to High-Resolution Numerical Simulations (2000, background): “This excess structure may be implicated in several other problems, including the small disk sizes produced in hydrodynamic simulations (e.g. Navarro & Steinmetz 2000), and the question of disk survival against heating in minor mergers (Tóth & Ostriker 1992; Kauffmann & White 1993; Lacey & Cole…”
Hierarchical formation of bulgeless galaxies – II. Redistribution of angular momentum via galactic fountains (2011, background): “This resulted in galaxies dominated by spheroidal components which were deficient in angular momentum when compared to their observed counter- parts (Navarro & Steinmetz 2000).”
Simulations of Galaxy Formation in a Λ Cold Dark Matter Universe. I. Dynamical and Photometric Properties of a Simulated Disk Galaxy (2002, background): “The version used here includes the self-gravity of gas, stars, and dark matter, hydrodynamical pressure and shocks, Compton and radiative cooling, as well as the heating effects of a photoionizing UV background (see Navarro & Steinmetz 1997, 2000b for more details).”
Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles (2010, background): “Typically, however, when simulations include baryons, either explicitly or through adiabatic contraction models, the haloes will have a maximum velocity that is a factor of two higher than the halo virial velocity (e.g. Navarro & Steinmetz 2000; Dutton et al. 2007; Pedrosa et al. 2010).”
HALO EXPANSION IN COSMOLOGICAL HYDRO SIMULATIONS: TOWARD A BARYONIC SOLUTION OF THE CUSP/CORE PROBLEM IN MASSIVE SPIRALS (2011, methodology): “…cosmological hydro-dynamical simulations have been extensively used to directly address the question of galaxy properties in the CDM scenario (e.g. Navarro & Steinmetz 2000, Abadi et al. 2003, Brook et al. 2004, Robertson et al. 2004, Okamoto et al. 2005, Macciò et al. 2006, Governato et al.…”
THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, background): “Previous numerical simulations have in fact shown that when only cooling processes are included, the infalling gas loses too much angular momentum, resulting in disks that are much smaller than the observed ones (Navarro & White 1994, Navarro & Steinmetz 2000).”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, background): “…by virtue of the virial theorem, it immediately follows that the halo mass must be proportional to the third power of the virial velocity, but unfortunately the constant of proportionality depends on the adopted cosmology and may vary with time (e.g., Bryan & Norman 1998; Navarro & Steinmetz 2000).”
A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion (2006, methodology): “Models that fail to take these effects into account can therefore not be used for a meaningful comparison with the data (see also Navarro & Steinmetz 2000; van den Bosch 2000).”
Stellar Mass-to-Light Ratios and the Tully-Fisher Relation (2000, methodology): “We dis- agree with their result for the slope by around 2σ (even including systematic error): adopting our slope of 3.5± 0.2 (random)± 0.2 (systematic), the case against the basic relationship m∝ V3halo predicted by simple CDM models is much weaker (e.g. van den Bosch 2000; Navarro & Steinmetz 2000b”
A Merger-driven Scenario for Cosmological Disk Galaxy Formation (2005, background): “…with similar physics produce galaxies that are too centrally concentrated, form toomany stars, contain overly dominant bulges, and lack angular momentum compared with nearby spirals (Katz & Gunn 1991; Katz et al. 1992; Navarro &White 1994; Steinmetz &Muller 1995; Navarro & Steinmetz 2000).”
DO HOT HALOS AROUND GALAXIES CONTAIN THE MISSING BARYONS? (2010, background): “An alternative explanation of the lack of BTF correlation with galaxy type or gas fraction can be inferred from the result of Navarro & Steinmetz (2000).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, background): “…from ‘overcooling’ and from a dearth of angular momentum due to the transfer of angular momentum from the baryonic component to the dark matter during the many merger events that characterize hierarchical assembly (Navarro & Benz 1991; Sommer-Larsen, Gelato & Vedel 1999; Navarro & Steinmetz 2000).”