The Structural Evolution of Substructure

By E. Hayashi, J. Navarro, James E. Taylor, Joachim Stadel, Thomas R. Quinn. 2002

331 citations recorded by the source corpus.

We investigate the evolution of substructure in cold dark matter (CDM) halos using N-body simulations of tidal stripping of substructure halos within a static host potential. We find that halos modeled following the Navarro, Frenk, & White (NFW) mass profile lose mass continuously because of tides from the massive host, leading to the total disruption of satellite halos with small tidal radii. Although mass is predominantly stripped from the outer regions, tidal heating also causes the halo to expand and the central density to decrease after each pericentric passage, when mass loss preferentially occurs. As a result, simple models based on the tidal-limit approximation underestimate significantly the tidal mass loss over several orbits. The equilibrium structure of stripped NFW halos depends mainly on the fraction of mass lost and can be expressed in terms of a simple correction to the original NFW profile. We apply these results to substructure in the Milky Way and conclude that the dark matter halos surrounding its dwarf spheroidal (dSph) satellites have circular velocity curves that peak well beyond the luminous radius at velocities significantly higher than expected from the stellar line-of-sight velocity dispersion. Our modeling suggests that the true tidal radii of dSphs lie well beyond the putative tidal cutoff observed in the surface brightness profile, suggesting that the latter are not really tidal in origin but rather features in the light profile of limited dynamical relevance. For Draco in particular, our modeling implies that its tidal radius is much larger than derived by Irwin & Hatzidimitriou, lending support to the interpretation of recent Sloan Digital Sky Survey data by Odenkirchen et al. Similarly, our model suggests that Carina's halo has a peak circular velocity of order ~55 km s-1, which may help explain how this small galaxy has managed to retain enough gas to undergo several bursts of star formation. Our results imply a close correspondence between the most massive substructure halos expected in a CDM universe and the known satellites of the Milky Way and suggest that only substructure halos with peak circular velocities below 35 km s-1 lack readily detectable luminous counterparts.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e749150ea526c3a8d79a796daf20e4a4c6071cee

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Citations in the corpus

Dark matter in the Milky Way II. The HI gas distribution as a tracer of the gravitational potential (2007, background): “However, a possible scenario could be a ring-like mass concentration caused by a merger event; see Hayashi et al. (2003) and Peñarrubia et al. (2005, 2006).”
Tracing Galaxy Formation with Stellar Halos. I. Methods (2005, background): “(Note that simulations of satellite accretions in static NFW potentials using this code produced results identical to those reported in Hayashi et al. 2003) Using this approach, the satellites are not influenced by each other, other than through the smooth growth of the parent galaxy potential.”
The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, methodology): “In this context, Hayashi et al. (2003) write ‘We apply these results to substructure in the Milky Way and conclude that the darkmatter haloes surrounding its dwarf spheroidal (dSph) satellites have circular velocity curves that peak well beyond the luminous radius at velocities significantly higher…”
Dark Matter Substructure in Numerical Simulations: A Tale of Discreteness Noise, Runaway Instabilities, and Artificial Disruption (2018, methodology): “Overall these results are in good agreement with previous studies (e.g., Hayashi et al. 2003; Peñarrubia et al. 2010).”
Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies (2017, background): “While the smallest subhalos are likely devoid of baryons, they nonetheless should be dynamically influenced by the central galaxy (Taylor & Babul 2001; Hayashi et al. 2003; Berezinsky et al. 2006; Read et al. 2006a,b; Peñarrubia et al. 2010; D’Onghia et al. 2010).”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, methodology): “To determine which gas and dark matter particles are bound to the galaxy in any particular simulation output, we use the iterative method outlined in Tormen et al. (1998) and Hayashi et al. (2003).”
Dark Matter Subhalos and the Dwarf Satellites of the Milky Way (2008, background): “A solution to the substructure problem suggested by Stoehr et al. (2002) and Hayashi et al. (2003) would be to place the luminous dwarfs in the most massive subhalos at the present epoch, suitably adjusting the mass (or peak circular velocity) threshold for efficient galaxy formation.”
A Two Micron All Sky Survey View of the Sagittarius Dwarf Galaxy. I. Morphology of the Sagittarius Core and Tidal Arms (2003, background): “With the suggestion by Hayashi et al. (2003) that such tidal limit approximations tend to overestimate the bound mass in tidally disrupting systems, it becomes possible to contemplate that the even more centrally defined nuclear ‘‘ cusp ’’ might represent the bound Sgr core embedded in an extensive…”
BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “The tidal effects of a disk are expected to be increasingly stronger as the central density profile of satellites becomes shallower (Taylor & Babul 2001; Stoehr et al. 2002; Hayashi et al. 2003; Read et al. 2006a; Peñarrubia et al. 2010).”
The Milky Way’s bright satellites as an apparent failure of ΛCDM (2011, background): “…further split into two broad classes: those that link a satellite’s luminosity to the present day mass of its dark matter halo (Stoehr et al. 2002; Hayashi et al. 2003; Peñarrubia et al. 2008), and those that assume satellites form only in the biggest halos defined at some earlier epoch, e.g.,…”
Redefining the Missing Satellites Problem (2007, background): “One particular solution states that the masses of the dSphs have been systematically underestimated, so that the ∼ 10 brightest satellites reside systematically in the ∼ 10 most massive subhalos (Stoehr et al. 2002; Hayashi et al. 2003).”
Generating Equilibrium Dark Matter Halos: Inadequacies of the Local Maxwellian Approximation (2003, methodology): “Examples include the survival and evolution of substructure within dark matter (DM) halos (Moore, Katz, & Lake 1996; Taffoni et al. 2003; Hayashi et al. 2003), the effects of tidal stripping and dynamical friction on the orbits of satellites (Velázquez & White 1995; van den Bosch et al. 1999;…”
The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies (2010, background): “As shown by Hayashi et al. (2003) and Peñarrubia et al. (2008b), the evolution of the structural parameters of NFW haloes as they are tidally stripped does solely depend on the total amount of mass lost, and not on the details of how the mass is stripped.”
Linking halo mass to galaxy luminosity (2004, background): “…ously, the actual factor for a given subhalo will be highly variable, but for reasons of simplicity and also because it is not well known (see e.g. Hayashi et al. 2003, for a treatment of the profile of stripped subhaloes), we will be treating this as an average applicable to all subhaloes and…”
Too big to fail? The puzzling darkness of massive Milky Way subhaloes (2011, background): “…models of the MW’s satellite population place the most luminous dwarf galaxies in the most massive subhaloes at redshift zero (Stoehr et al. 2002; Hayashi et al. 2003; Peñarrubia et al. 2008), recent kinematic studies of the satellites have shown that this is unlikely to be the case (Walker…”
The mass function and average mass-loss rate of dark matter subhaloes (2004, background): “For detailed numerical simulations of the mass loss of dark matter subhaloes see Hayashi et al. (2003) and Kazantzidis et al. (2004).”
The subhalo populations of ΛCDM dark haloes (2004, background): “…near the centre of their parent tend to be more heavily affected by tidal stripping than more distant objects as demonstrated in Section 5.4; such tidal stripping affects the masses of subhaloes more strongly than their maximum circular velocities (Ghigna et al. 2000; Hayashi et al. 2003).”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “…resolution simulations can lose substantial mass as they are tidally stripped and gravitationally shocked within the potential of their hosts (e.g., Tormen et al. 1998; Klypin et al. 1999; Ghigna et al. 2000; Hayashi et al. 2003; Kravtsov et al. 2004b; Gao et al. 2004; BoylanKolchin et al. 2009).”