Populating a cluster of galaxies - I. Results at z=0

By Volker Springel, Simon D. M. White, G. Tormen, Guinevere Kauffmann Mpa, Harvard-CfA, Padova. 2000

1,683 citations recorded by the source corpus.

ABSTRA C T We simulate the assembly of a massive rich cluster and the formation of its constituent galaxies in a flat, low-density universe. Our most accurate model follows the collapse, the star formation history and the orbital motion of all galaxies more luminous than the Fornax dwarf spheroidal, while dark halo structure is tracked consistently throughout the cluster for all galaxies more luminous than the SMC. Within its virial radius this model contains about 2 10 7 dark matter particles and almost 5000 distinct dynamically resolved galaxies. Simulations of this same cluster at a variety of resolutions allow us to check explicitly for numerical convergence both of the dark matter structures produced by our new parallel N-body and substructure identification codes, and of the galaxy populations produced by the phenomenological models we use to follow cooling, star formation, feedback and stellar aging. This baryonic modelling is tuned so that our simulations reproduce the observed properties of isolated spirals outside clusters. Without further parameter adjustment our simulations then produce a luminosity function, a mass-to-light ratio, luminosity, number and velocity dispersion profiles, and a morphology ‐radius relation which are similar to those observed in real clusters. In particular, since our simulations follow galaxy merging explicitly, we can demonstrate that it accounts quantitatively for the observed cluster population of bulges and elliptical galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/82536fbc19563946f6f9ce46ce8a8b265f593e43

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Citations in the corpus

How do galaxies populate dark matter haloes (2009, methodology): “The SUBFIND algorithm (Springel et al. 2001) was then applied to each FOF group in order to split it into a set of disjoint, self-bound subhalos, which represent locally overdense and dynamically stable subunits within the larger system.”
The eagle simulations of galaxy formation: Public release of halo and galaxy catalogues (2015, methodology): “Self-bound “subhaloes”, which can contain both baryonic and dark matter, are later identified using the subfind algorithm (Springel et al., 2001; Dolag et al., 2009) using all particle species.”
Dark matter halo merger histories beyond cold dark matter – I. Methods and application to warm dark matter (2012, methodology): “In each of the simulations, haloes and subhaloes were identified at each of the 128 output times using the FOF (Davis et al. 1985) and SUBFIND (Springel et al. 2001) algorithms, respectively.”
Moving mesh cosmology: tracing cosmological gas accretion (2013, methodology): “We identify dark matter haloes using the SUBFIND algorithm (Springel et al. 2001) which begins with a friends-offriends procedure (linking length b = 0.2) applied to dark matter particles.”
Intracluster stars in simulations with active galactic nucleus feedback (2010, methodology): “As a first step, we run a friends-of-friends (FoF) group finder with a linking length of 0.2 in units of the mean interparticle distance, as well as the SUBFIND substructure finder (Springel et al. 2001).”
The statistics of lambda CDM Halo Concentrations (2007, methodology): “We have also used SUBFIND, the subhalo finder algorithm described in Springel et al. (2001), in order to clean up the group catalogue of loosely-bound FOF structures, and to analyse the substructure within each halo (see Sec.”
The distribution of satellite galaxies: the great pancake (2005, methodology): “In the current model, the positions of satellite galaxies and the time when they merge is determined by using information from SUBFIND.”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, methodology): “…clustering (e.g., Conroy et al. 2006; Guo & White 2013; Moster et al. 2017; Campbell et al. 2017), semi-analytical models for galaxy formation (e.g., Springel et al. 2001; Kang et al. 2005; Kitzbichler & White 2008), and other studies that rely on the phase-space distribution of subhaloes (e.g.,…”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, methodology): “FOF groups were searched for bound substructure using the SUBFIND algorithm (Springel et al. 2001).”
A calibration of the relation between the abundance of close galaxy pairs and the rate of galaxy mergers (2008, methodology): “…techniques originally introduced by White & Frenk (1991), Kauffmann et al. (1993, 1999), Kauffmann & Charlot (1998), Kauffmann & Haehnelt (2000), Springel et al. (2001a) and De Lucia, Kauffmann & White (2004), principally gas cooling, star formation, chemical and hydrodynamic feedback from…”
Velocity and spatial biases in cold dark matter subhalo distributions (2004, methodology): “Ghigna et al. (2000); Colin, Klypin, & Kravtsov (2000) claim a positive velocity bias, whilst Springel et al. (2001) report a negative velocity bias.”
A Catalog of Newly Identified Star Clusters in Gaia DR2 (2019, methodology): “The linking length is set to =r b NFoF star 1 5. bFoF is set to 0.2, which is commonly adopted in the dark matter halo identification of cosmological simulations (Springel et al. 2001).”
Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles (2010, methodology): “We then used the subfind algorithm (Springel et al. 2001; Dolag et al. 2009) to decompose the FOF group into separate, self-bound substructures, including the main halo itself.”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, methodology): “Each snapshot was post-processed by extended and optimized versions of the FOF and SUBFIND algorithms (Davis et al. 1985; Springel et al. 2001; Dolag et al. 2009), to identify haloes and subhaloes and their properties.”
What determines satellite galaxy disruption (2009, methodology): “Several analyses assume that a satellite galaxy survives the disruption of its subhalo and eventually merges with its central galaxy by imposing an analytic infall timescale to a galaxy after subhalo disruption (Springel et al. 2001; Kitzbichler & White 2008; Saro et al. 2008; Moster et al. 2009).”
The correlation of star formation quenching with internal galaxy properties and environment (2008, background): “…(e.g. White & Frenk 1991; Kauffmann, White & Guiderdoni 1993; Kauffmann et al. 1999; Somerville & Primack 1999; Cole et al. 2000; Somerville, Primack & Faber 2001; Springel et al. 2001; Benson et al. 2003; Hatton et al. 2003; Khochfar & Burkert 2003; Kang et al. 2005; Khochfar & Burkert 2005).”
Feedback and the fundamental line of low-luminosity low-surface-brightness/dwarf galaxies (2002, background): “The trend of increasing total-mass-to-light ratio with decreasing mass, which results naturally from supernova feedback and reproduces the fundamental line, may not be enough for fully resolving the mystery of missing dwarf galaxies (Klypin et al. 1999; Moore et al. 1999; Springel et al. 2001).”