Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure

By J. Diemand, Michael Kuhlen, P. Madau. 2007

511 citations recorded by the source corpus.

We use the "Via Lactea" simulation to study the co-evolution of a Milky Way-sized ΛCDM halo and its subhalo population. While most of the host halo mass is accreted over the first 6 Gyr in a series of major mergers, the physical mass distribution [not Mvir(z)] remains practically constant since z = 1. The same is true in a large sample of ΛCDM galaxy halos. Subhalo mass loss peaks between the turnaround and virialization epochs of a given mass shell, and the abundance of substructure within the shell freezes afterward. Of the z = 1 subhalos, 97% have a surviving bound remnant at the present epoch. The retained mass fraction is larger for initially lighter subhalos: today satellites with maximum circular velocities Vmax = 10 km s-1 at z = 1 have about 40% of the mass they had back then. At the first pericenter passage a larger average mass fraction is lost than during each following orbit. Tides remove mass in the substructure from the outside in, leading to higher concentrations compared to field halos of the same mass. This effect, combined with the earlier formation epoch of the inner satellites, results in strongly increasing subhalo concentrations toward the Galactic center. We present individual evolutionary tracks and present-day properties of the likely hosts of the dwarf satellites around the Milky Way. The formation histories of "field halos" that lie beyond the Via Lactea host today are found to strongly depend on the density of their environment. This is caused by tidal mass loss that affects many field halos on eccentric orbits.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f3edca562adf1a671aa7428a26609365e81c42c9

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Citations in the corpus

Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, methodology): “Tidal stripping removes mass from the outer parts of subhalos and, as a result, subhalos are truncated at smaller radii compared to field halos of the same mass (Ghigna et al. 1998; Taylor & Babul 2001; Kravtsov et al. 2004; Diemand et al. 2007a,b).”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, methodology): “For comparison, Diemand et al. (2007) find that the mass evolution of subhaloes in their ‘Via Lactea’ simulation is best modeled using Eq.”
H i IN LOCAL GROUP DWARF GALAXIES AND STRIPPING BY THE GALACTIC HALO (2009, methodology): “…et al. (2008) predicted the total number of Milky Way satellite galaxies within various radii assuming that the Via Lactea N-body simulation (Diemand et al. 2007) is a good representation of the spatial distribution of Milky Way satellites and also by using the SDSS detection efficiencies…”
The dark side of galaxy colour (2013, background): “…but are not limited to, mass loss due to outside-in stripping (see Watson et al. 2012, and references therein), “strangulation” (Larson et al. 1980; Diemand et al. 2007; Kawata & Mulchaey 2008), ram-pressure stripping (Gunn & Gott 1972; Abadi et al. 1999; McCarthy et al. 2008), “harassment”…”
ELVIS: Exploring the Local Volume in Simulations (2013, methodology): “The correlation between apeak and Vmax is a combination of the apeak − Vpeak correlation and the effects of orbital evolution on subhalo density structure (for discussions on these expected trends see, e.g., Zentner & Bullock 2003; Kazantzidis et al. 2004; Diemand et al. 2007b).”
DEPENDENCE OF THE OUTER DENSITY PROFILES OF HALOS ON THEIR MASS ACCRETION RATE (2014, background): “In fact, the lowest ν bin appears to experience no average infall in any radial shell (see also Diemand et al. 2007; Cuesta et al. 2008).”
Structure finding in cosmological simulations: the state of affairs (2013, background): “…relation (Bullock et al. 2001a; Wechsler et al. 2002), mass accretion histories (Wechsler et al. 2002; De Lucia et al. 2004; De Lucia & Blaizot 2007; Diemand et al. 2007; Behroozi, Wechsler & Conroy 2013c), shape distributions (Dubinski & Carlberg 1991; Kauffmann et al. 1999; Bullock et al.…”
Bayesian strong gravitational-lens modelling on adaptive grids: objective detection of mass substructure in Galaxies (2008, methodology): “Nevertheless subsequent studiesof similar gravitationally lensed systems have shown that therequired mass fraction in substructure is higher than what is obtained numerical simulations (Mao et al. 2004; Macciò & Miranda 2006; Diemand et al. 2007a).”
Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “After a satellite falls into a host halo, the strong gravitational tidal forces prevent the satellite’s (sub)halo from accreting dark matter and also strip mass from the subhalo from the outside-in (e.g., Dekel et al. 2003; Diemand et al. 2007).”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “A number of recent studies (Prada et al. 2006; Diemand et al. 2007; Cuesta et al. 2008; Diemer et al. 2013; Diemer & Kravtsov 2014; Zemp 2014; Correa et al. 2015) have pointed out that the inner density profiles of low-mass, galaxy-sized halos evolve very little at z 1 .”
CHEMICAL EVOLUTION IN HIERARCHICAL MODELS OF COSMIC STRUCTURE. II. THE FORMATION OF THE MILKY WAY STELLAR HALO AND THE DISTRIBUTION OF THE OLDEST STARS (2009, background): “Darkmatter only numerical simulations (White & Springel 2000; Scannapieco et al. 2006; Diemand et al. 2007) have already demonstrated that Milky-Way sized DM halos should contain significant structures that originated before z > 6 (roughly the current observational frontier).”