The asymptotic tidal remnants of cold dark matter subhaloes

Errani, Raphaël; Navarro, Julio F.

doi:10.1093/mnras/stab1215

Cited by 64 publications

(105 citation statements)

References 67 publications

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“…This has been demonstrated recently in idealized simulations (e.g. Errani & Navarro 2021) for systematic studies of tailored situations. We explore the dependencies and implications of our sample of disrupted and surviving satellites at standard resolution and their high-resolution counterparts in Fig.…”

Section: Satellite Evolution and Disruptionmentioning

confidence: 65%

“…This indicates that our high resolution simulation at least partially mitigates some artificial disruption effects that tailored N-body simulations have highlighted (e.g. van den Bosch et al 2018;Errani & Navarro 2021). These effects are a concern primarily in the ultra-faint regime, although they seem to play a subdominant role in the ability of the simulations to reproduce the faint-end of the luminosity function compared to the effect of forming faint galaxies in the first place.…”

Section: Discussionmentioning

confidence: 78%

“…Recent studies have questioned the effectiveness of tidal disruption, with some arguing that it is not needed to solve the 'missing satellites' problem (Kim, Peter & Hargis 2018;Fielder et al 2019) and that too effective tidal disruption may in fact invert the problem (Kelley et al 2019). Other, idealized dark matter-only N-body simulations claim that satellites orbiting in close proximity to the central galaxy experience some degree of 'artificial tidal disruption' (van den Bosch & Ogiya 2018; Errani & Peñarrubia 2020;Errani & Navarro 2021;Green, van den Bosch & Jiang 2021), with effects worsening for faint galaxies typically represented by a fewer number of particles relative to bright galaxies.…”

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confidence: 99%

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Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Grand

Marinacci

Pakmor

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the formation of the satellite galaxy population of a Milky Way-mass halo in a very highly resolved magneto-hydrodynamic cosmological zoom-in simulation (baryonic mass resolution mb = 800 $\rm M_{\odot }$). We show that the properties of the central star-forming galaxy, such as the radial stellar surface density profile and star formation history, are: i) robust to stochastic variations associated with the so-called ‘Butterfly Effect’; and ii) well converged over 3.5 orders of magnitude in mass resolution. We find that there are approximately five times as many satellite galaxies at this high resolution compared to a standard ($m_b\sim 10^{4-5}\, \rm M_{\odot }$) resolution simulation of the same system. This is primarily because 2/3rds of the high resolution satellites do not form at standard resolution. A smaller fraction (1/6th) of the satellites present at high resolution form and disrupt at standard resolution; these objects are preferentially low-mass satellites on intermediate- to low-eccentricity orbits with impact parameters ≲ 30 kpc. As a result, the radial distribution of satellites becomes substantially more centrally concentrated at higher resolution, in better agreement with recent observations of satellites around Milky Way-mass haloes. Finally, we show that our galaxy formation model successfully forms ultra-faint galaxies and reproduces the stellar velocity dispersion, half-light radii, and V-band luminosities of observed Milky Way and Local Group dwarf galaxies across 6 orders of magnitude in luminosity (103-$10^{9}\, \rm L_{\odot }$).

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Section: Satellite Evolution and Disruptionmentioning

confidence: 65%

Section: Discussionmentioning

confidence: 78%

mentioning

confidence: 99%

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Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Grand

Marinacci

Pakmor

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…However, considering the fact that a NFW subhalo should never fully disrupt (see e.g. van den Bosch et al 2018;Errani & Peñarrubia 2020;Errani & Navarro 2021), we emphasize that this reduced abundance is not due to 'disruption', but is instead a consequence of enhanced mass-loss combined with a fixed resolution limit.…”

Section: Discussionmentioning

confidence: 86%

SatGen – II. Assessing the impact of a disc potential on subhalo populations

Green

Bosch

Jiang

2021

Monthly Notices of the Royal Astronomical Society

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The demographics of dark matter substructure depend sensitively on the nature of dark matter. Optimally leveraging this probe requires accurate theoretical predictions regarding the abundance of subhaloes. These predictions are hampered by artificial disruption in numerical simulations, by large halo-to-halo variance, and by the fact that the results depend on the baryonic physics of galaxy formation. In particular, numerical simulations have shown that the formation of a central disc can drastically reduce the abundance of substructure compared to a dark matter-only simulation, which has been attributed to enhanced destruction of substructure due to disc shocking. We examine the impact of discs on substructure using the semi-analytical subhalo model SatGen, which accurately models the tidal evolution of substructure free of the numerical disruption that still hampers N-body simulations. Using a sample of 10,000 merger trees of Milky Way-like haloes, we study the demographics of subhaloes that are evolved under a range of composite halo–disc potentials with unprecedented statistical power. We find that the overall subhalo abundance is relatively insensitive to properties of the disc aside from its total mass. For a disc that contains 5% of Mvir, the mean subhalo abundance within rvir is suppressed by ${\lesssim }10\%$ relative to the no-disc case, a difference that is dwarfed by halo-to-halo variance. For the same disc mass, the abundance of subhaloes within 50 kpc is reduced by ${\sim }30\%$. We argue that the disc mainly drives excess mass loss for subhaloes with small pericentric radii and that the impact of disc shocking is negligible.

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“…We have therefore constructed an estimate of the mass and half-mass radius of a halo shorn of its outer layers by tidal effects at 20 kpc. Note that we do not attempt to model further evolution of the halo profile (see Errani & Navarro 2021, for a recent discussion on stripping to small fractions of the infall mass.) Having generated a model for the gap-generating subhaloes, we turn to the whole subhalo population.…”

Section: Subhalo Density and Radial Distributionmentioning

confidence: 99%

The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

Lovell

Cautun

Frenk

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The spatial distribution of Milky Way (MW) subhaloes provides an important set of observables for testing cosmological models. These include the radial distribution of luminous satellites, planar configurations, and the abundance of dark subhaloes whose existence or absence is key to distinguishing amongst dark matter models. We use the coco N-body simulations of cold dark matter (CDM) and 3.3 keV thermal relic warm dark matter (WDM) to predict the satellite spatial distribution in the limit that the impact of baryonic physics is minimal. We demonstrate that the radial distributions of CDM and 3.3 keV-WDM luminous satellites are identical if the minimum pre-infall halo mass to form a galaxy is >108.5 ${\, \rm M_\odot }$. The distribution of dark subhaloes is significantly more concentrated in WDM due to the absence of low mass, recently accreted substructures that typically inhabit the outer parts of a MW halo in CDM. We show that subhaloes of mass [107, 108] ${\, \rm M_\odot }$ and within 30 kpc of the centre are the stripped remnants of larger haloes in both models. Therefore their abundance in WDM is 3 × higher than one would anticipate from the overall WDM subhalo population. We estimate that differences between CDM and WDM concentration–mass relations can be probed for subhalo–stream impact parameters <2 kpc. Finally, we find that the impact of WDM on planes of satellites is likely negligible. Comprehensive comparisons with observations will require further work with high resolution, self-consistent hydrodynamical simulations.

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The asymptotic tidal remnants of cold dark matter subhaloes

Cited by 64 publications

References 67 publications

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

SatGen – II. Assessing the impact of a disc potential on subhalo populations

The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

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