The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies

By J. Peñarrubia, A. Benson, M. Walker, G. Gilmore, A. McConnachie, Lucio Mayer. 2010

212 citations recorded by the source corpus.

We use N-body simulations to study the eects that a divergent (i.e. \cuspy") dark and disc masses. We nd that tidal encounters with discs tend to decrease the average mass of satellite galaxies at all galactocentric radii. Of all satellites, those accreted before re-ionization (z > 6), which may be singled out by anomalous metallicity patterns, provide the strongest constraints on the inner prole of dark haloes. These galaxies move on orbits that penetrate the disc repeatedly and survive to the present day only if haloes have an inner density cusp. We show that the size-mass relationship established from Milky Way (MW) dwarfs strongly supports the presence of cusps in the majority of these systems, as cored models systematically underestimate the masses of the known Ultra- Faint dSphs. Our models also indicate that a massive M31 disc may explain why many of its dSphs with suitable kinematic data fall below the size-mass relationship derived from MW dSphs. We also examine whether our modelling can constrain the mass threshold below which star formation is suppressed in dark matter haloes. We nd that luminous satellites must be accreted with masses above 10 8 {10 9 M in order to

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ad1231a269915db491d88a001f9ae361d4b7c61f

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Citations in the corpus

The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, background): “…of dwarfs from discs to spheroids (Mayer et al. 2001a; Lokas et al. 2012; Kazantzidis et al. 2013); and physically reshapes the dark matter halo mass function within groups (Peñarrubia et al. 2010; Zolotov et al. 2012; Brooks et al. 2013; Wetzel et al. 2016, and see the discussion in R16a).”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, background): “It has been argued that the observed population of faint galaxy satellites should be hosted inside cuspy halos, as small, cored halos would easily be destroyed by the Milky Way tidal field (Peñarrubia et al. 2010).”
FORTY-SEVEN MILKY WAY-SIZED, EXTREMELY DIFFUSE GALAXIES IN THE COMA CLUSTER (2014, background): “…and stellar masses as UDGs but stellar densities that are a factor of∼ 107 higher.6 We note, however, that the morphological evolution of infalling galaxies is difficult to predict, as it probably depends sensitively on the shape of the inner dark matter profile (e.g., Peñarrubia et al. 2010).”
The Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations (2018, background): “…core formation; for example, subhaloes cored by internal processes are then more susceptible to further mass-loss from external interactions (e.g. Peñarrubia et al. 2010; Brooks & Zolotov 2014, but also see Garrison-Kimmel et al. 2017, who showed that much of the differences in subhalo counts…”
Small scale problems of the $\Lambda$CDM model: a short review (2016, methodology): “Equation (8) of [77] fit for slope γ = 1.”
Gravitational probes of dark matter physics (2017, background): “lower central density of subhalos in hydrodynamic simulations makes satellite galaxies more vulnerable to tidal heating or disruption [385, 372, 225, 143, 386].”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “The flatter density profiles make them more vulnerable to tidal effects of the baryonic disk (see also Taylor & Babul 2001; Read et al. 2006a; Choi et al. 2009; Wetzel & White 2010; Romano-Dı́az et al. 2010a; D’Onghia et al. 2010a; Peñarrubia et al. 2010).”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, methodology): “As we demonstrate in those papers, physical disruption in CDM-based dark-matter-only simulations is extremely rare (see also Diemand et al. 2007; Peñarrubia et al. 2010).”
The influence of Sagittarius and the Large Magellanic Cloud on the stellar disc of the Milky Way Galaxy (2017, background): “The density profile determines how rapidly the satellite disrupts owing to tidal forces (Peñarrubia et al. 2010) and hence has significant influence on the mass remaining bound to the satellite during final infall.”
Dark Matter Substructure in Numerical Simulations: A Tale of Discreteness Noise, Runaway Instabilities, and Artificial Disruption (2018, background): “Overall these results are in good agreement with previous studies (e.g., Hayashi et al. 2003; Peñarrubia et al. 2010).”
A METHOD FOR MEASURING (SLOPES OF) THE MASS PROFILES OF DWARF SPHEROIDAL GALAXIES (2011, background): “N-body simulations by Peñarrubia et al. (2009) and Peñarrubia et al. (2010) demonstrate that for satellite halos that follow the generic density profile given by Equation 16, the instantaneous tidal radius at pericenter is rt ≈ rp[Mdsph(≤ rt )/(3MMW(≤ rp)]1/3, whereMdsph(rt) is the dSph mass…”
The upper bound on the lowest mass halo (2016, background): “This is unfortunate as the disk has been shown to play an important role in sculpting the properties of the Galactic satellites (e.g. Peñarrubia et al. 2002, 2010; D’Onghia et al. 2010; Errani et al. 2017).”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, background): “This tidal effect is particularly strong for those satellites that enter with cored DM halos (Peñarrubia et al. 2010), further increasing the discrepancy in the central masses predicted by DM+baryon and DM-only simulations.”
The milky way total mass profile as inferred from Gaia DR2 (2019, background): “…number and orbits of satellites are a key test of properties of the DM, such as the mass of the DM particle and its interaction cross-section (e.g. Peñarrubia et al. 2010; Vogelsberger et al. 2012; Kennedy et al. 2014; Lovell et al. 2014; Cautun & Frenk 2017; Kahlhoefer et al. 2019), and also…”
Dark matter cores all the way down (2015, background): “Such cored dwarfs are also much more efficiently tidally stripped, which can significantly alleviate the missing satellites problem (Read et al. 2006c; Peñarrubia et al. 2010; Zolotov et al. 2012; Brooks et al. 2013).”
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).”