Updated results on the galaxy–halo connection from satellite kinematics in SDSS

Lange, J.; Bosch, Frank C. van den; Zentner, Andrew R.; Wang, Kuan; Villarreal, Antonio

doi:10.1093/mnras/stz1466

Cited by 53 publications

(62 citation statements)

References 100 publications

(212 reference statements)

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“…Vale & Ostriker 2006;Behroozi, Wechsler & Conroy 2013;Hearin et al 2013;Newton et al 2018;Nadler et al 2019Nadler et al , 2020Nadler et al , 2021 and thus can be used to constrain cosmology through their impact on small-scale clustering statistics (e.g. Benson et al 2001;Berlind et al 2003;van den Bosch et al 2005a;Lange et al 2019;. Clearly, accurately modelling the evolution of DM subhalo populations is a prerequisite for their use as a cosmological probe and as a tool to study the particle nature of DM.…”

mentioning

confidence: 99%

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

Green

Bosch

Jiang

2021

Monthly Notices of the Royal Astronomical Society

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Several recent studies have indicated that artificial subhalo disruption (the spontaneous, non-physical disintegration of a subhalo) remains prevalent in state-of-the-art dark matter-only cosmological simulations. In order to quantify the impact of disruption on the inferred subhalo demographics, we augment the semi-analytical SatGen dynamical subhalo evolution model with an improved treatment of tidal stripping that is calibrated using the DASH database of idealized high-resolution simulations of subhalo evolution, which are free from artificial disruption. We also develop a model of artificial disruption that reproduces the statistical properties of disruption in the Bolshoi simulation. Using this framework, we predict subhalo mass functions (SHMFs), number density profiles, and substructure mass fractions and study how these quantities are impacted by artificial disruption and mass resolution limits. We find that artificial disruption affects these quantities at the $10-20\%$ level, ameliorating previous concerns that it may suppress the SHMF by as much as a factor of two. We demonstrate that semi-analytical substructure modeling must include orbit integration in order to properly account for splashback haloes, which make up roughly half of the subhalo population. We show that the resolution limit of N-body simulations, rather than artificial disruption, is the primary cause of the radial bias in subhalo number density found in dark matter-only simulations. Hence, we conclude that the mass resolution remains the primary limitation of using such simulations to study subhaloes. Our model provides a fast, flexible, and accurate alternative to studying substructure statistics in the absence of both numerical resolution limits and artificial disruption.

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mentioning

confidence: 99%

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

Green

Bosch

Jiang

2021

Monthly Notices of the Royal Astronomical Society

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“…Satellite kinematics (e.g. Conroy et al 2007;More et al 2011;Wojtak & Mamon 2013;Lange et al 2019) and especially weak lensing (e.g. Mandelbaum et al 2006Mandelbaum et al , 2016Tinker et al 2013;Hudson et al 2015;Taylor et al 2020) are, in principle, reliable tracers of halo masses out to very large radii.…”

Section: Statistical Estimates Of the Shmrmentioning

confidence: 99%

“…There is already some evidence for secondary correlations between the SHMR and other properties of galaxies. This evidence comes from weak lensing (Mandelbaum et al 2006(Mandelbaum et al , 2016Tinker et al 2013;Hudson et al 2015;Taylor et al 2020), satellite kinematics (Conroy et al 2007;More et al 2011;Wojtak & Mamon 2013;Lange et al 2019), empirical models (Rodríguez-Puebla et al 2015), abundance matching (Hearin et al 2014;Saito et al 2016), or a combination of these methods (Dutton et al 2010). The results of these studies are consistent with the expectation that early-type galaxies occupy more massive halos than late-type galaxies of the same stellar mass.…”

Section: Introductionmentioning

confidence: 99%

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies

Posti

Fall

2021

A&A

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We derive the stellar-to-halo mass relation (SHMR), namely f⋆ ∝ M⋆/Mh versus M⋆ and Mh, for early-type galaxies from their near-infrared luminosities (for M⋆) and the position-velocity distributions of their globular cluster systems (for Mh). Our individual estimates of Mh are based on fitting a flexible dynamical model with a distribution function expressed in terms of action-angle variables and imposing a prior on Mh from the correlation between halo concentration and mass in the standard Λ cold dark matter (ΛCDM) cosmology. We find that the SHMR for early-type galaxies declines with mass beyond a peak at M⋆ ∼ 5 × 1010 M⊙ and Mh ∼ 1 × 1012 M⊙ (near the mass of the Milky Way). This result is consistent with the standard SHMR derived by abundance matching for the general population of galaxies, and also with previous, less robust derivations of the SHMR for early-type galaxies. However, it contrasts sharply with the monotonically rising SHMR for late-type galaxies derived from extended HI rotation curves and the same ΛCDM prior on Mh that we adopt for early-type galaxies. We show that the SHMR for massive galaxies varies more or less continuously with disc fraction and Hubble type between these rising and falling branches. We also show that the different SHMRs for late-type and early-type galaxies are consistent with the similar scaling relations between their stellar velocities and masses (the Tully–Fisher and the Faber–Jackson relations). As we demonstrate explicitly, differences in the relations between the stellar and halo virial velocities account for the similarity of the scaling relations. We argue that all these empirical findings are natural consequences of a picture in which galactic discs are built mainly by relatively smooth and gradual inflow, regulated by feedback from young stars, while galactic spheroids are built by a combination of merging, black-hole fuelling, and feedback from active galactic nuclei.

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“…The velocities of satellites are drawn from a local Gaussian velocity distribution without orbital anisotropy. The mean of the distribution is that of the host halo core and the second moment σ is obtained by solving the spherically symmetric, time-independent Jeans equation (van den Bosch et al 2004;More et al 2011;Lange et al 2019b). Thus, for a satellite at distance r in a halo with mass M , concentration c and halo radius r h :…”

Section: Galaxy-halo Connection Gmentioning

confidence: 99%

Cosmological Evidence Modelling: a new simulation-based approach to constrain cosmology on non-linear scales

Lange

Bosch

Zentner

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Extracting accurate cosmological information from galaxy-galaxy and galaxy-matter correlation functions on non-linear scales ( < ∼ 10 h −1 Mpc) requires cosmological simulations. Additionally, one has to marginalise over several nuisance parameters of the galaxy-halo connection. However, the computational cost of such simulations prohibits naive implementations of stochastic posterior sampling methods like Markov chain Monte Carlo (MCMC) that would require of order O(10 6 ) samples in cosmological parameter space. Several groups have proposed surrogate models as a solution: a so-called emulator is trained to reproduce observables for a limited number of realisations in parameter space. Afterwards, this emulator is used as a surrogate model in an MCMC analysis. Here, we demonstrate a different method called Cosmological Evidence Modelling (CEM). First, for each simulation, we calculate the Bayesian evidence marginalised over the galaxy-halo connection by repeatedly populating the simulation with galaxies. We show that this Bayesian evidence is directly related to the posterior probability of cosmological parameters. Finally, we build a physically motivated model for how the evidence depends on cosmological parameters as sampled by the simulations. We demonstrate the feasibility of CEM by using simulations from the Aemulus simulation suite and forecasting cosmological constraints from BOSS CMASS measurements of redshift-space distortions. Our analysis includes an exploration of how galaxy assembly bias affects cosmological inference. Overall, CEM has several potential advantages over the more common approach of emulating summary statistics, including the ability to easily marginalise over highly complex models of the galaxy-halo connection and greater accuracy, thereby reducing the number of simulations required.

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Updated results on the galaxy–halo connection from satellite kinematics in SDSS

Cited by 53 publications

References 100 publications

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

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

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies

Cosmological Evidence Modelling: a new simulation-based approach to constrain cosmology on non-linear scales

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