The tidal evolution of dark matter substructure – II. The impact of artificial disruption on subhalo mass functions and radial profiles

Green, Sheridan B.; Bosch, Frank C. van den; Jiang, Fangzhou

doi:10.1093/mnras/stab696

Cited by 58 publications

(76 citation statements)

References 124 publications

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“…Budzynski et al (2012) also showed that models based on cosmological N-body simulations that included modelling of 'orphan' galaxies to account for the loss of subhaloes in simulated catalogues due to resolution, also generally produced galaxy number density profiles close to those of matter or even steeper. Recently, Green, van den Bosch & Jiang (2021) presented a systematic study and calibration of the resolution and 'artificial disruption' effects on the number density profile of subhaloes in cosmological simulations. They showed that if resolution effects are corrected for, the subhalo number density profile is close to that of the matter distribution, while if a modest contribution of artificial disruption is additionally accounted for, the predicted number density profile is even mildly steeper than the matter density profile (see e.g.…”

Section: Comparison With N-body and Hydrodynamical Simulationsmentioning

confidence: 99%

The mass and galaxy distribution around SZ-selected clusters

Shin

Jain

Adhikari

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2 − 20h−1 Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology and astrophysics are discussed.

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Section: Comparison With N-body and Hydrodynamical Simulationsmentioning

confidence: 99%

The mass and galaxy distribution around SZ-selected clusters

Shin

Jain

Adhikari

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…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%

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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“…The expected subhalo mass function is largely uncertain, due to tidal effects, baryonic feedback, and DM physics. In addition, the radial dependence and expected profiles of the subhalos can also heavily depend on these factors and vary from the assumptions made in this paper (see, e.g., [43][44][45]). Future work could look into the constraints on the mass function, as well as consider other radial dependencies and mass profiles.…”

Section: B Discussion and Future Workmentioning

confidence: 95%

Detecting dark matter subhalos with the Nancy Grace Roman Space Telescope

Pardo

Doré

2021

Phys. Rev. D

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The dark matter subhalo mass function is a promising way of distinguishing between dark matter models. While cold dark matter predicts halos down to Earth-sized masses, other dark matter models typically predict a cutoff in the subhalo mass function. Thus a definitive detection or limits on the existence of subhalos at small masses can give us insight into the nature of dark matter. If these subhalos exist in the Milky Way, they would produce weak lensing signatures, such as modified apparent positions, on background stars. These signatures would generate correlations in the apparent velocities and accelerations of these stars, which could be observable given sufficient astrometric resolution and cadence. The Nancy Grace Roman Space Telescope's exoplanet microlensing survey will be perfectly suited to measuring the acceleration signatures of these halos. Here we forward model these acceleration signatures and explore the Roman Space Telescope's future constraints on lens profiles and populations. We find that the Roman Space Telescope could place competitive bounds on point-source, Gaussian, and Navarro-Frenk-White (NFW) profile lenses that are complementary to other proposed methods. In particular, it could place 95% upper limits on the NFW concentration c 200 < 10 2.5 . We discuss possible systematic effects that could hinder these efforts but argue they should not prevent the Roman Space Telescope from placing strong limits. We also discuss further analysis methods for improving these constraints.

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The tidal evolution of dark matter substructure – II. The impact of artificial disruption on subhalo mass functions and radial profiles

Cited by 58 publications

References 124 publications

The mass and galaxy distribution around SZ-selected clusters

The mass and galaxy distribution around SZ-selected clusters

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

Detecting dark matter subhalos with the Nancy Grace Roman Space Telescope

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