Galacticus: A Semi-Analytic Model of Galaxy Formation

By A. Benson. 2010

269 citations recorded by the source corpus.

We describe a new, free and open source semi-analytic model of galaxy formation, GALACTICUS. The GALACTICUS model was designed to be highly modular to facilitate expansion and the exploration of alternative descriptions of key physical ingredients. We detail the GALACTICUS engine for evolving galaxies through a merging hierarchy of dark matter halos and give details of the specific implementations of physics currently available in GALACTICUS. Finally, we show results from an example model that is in reasonably good agreement with several observational datasets. We use this model to explore numerical convergence and to demonstrate the types of information which can be extracted from GALACTICUS.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1db64e3a7522e1f2faeb538655b2eed7ba633b64

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Citations in the corpus

A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “Semi-analytical models (e.g., White & Frenk 1991; Kauffmann et al. 1993; Baugh 2006; Croton et al. 2006; Guo et al. 2011; Benson 2012) account for baryonic physics by adding galaxy formation as a post-processing step on top of the output of N-body simulations or onto Monte-Carlo realisations of…”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, methodology): “An alternative is to use a semi-analytical model f galaxy formation (see, e.g., Somerville et al. 2012; Lu et al. 2012; Henriques et al. 2012; Benson 2012 for recent examples).”
Dark matter halo merger histories beyond cold dark matter – I. Methods and application to warm dark matter (2012, methodology): “Control files and scripts to generate all results presented in this paper using GALACTICUS can be found at http://users.obs.carnegiescience.edu/abenson/ galacticus/ parameters/dmMergingBeyondCDM1.tar.bz2.”
First results from the IllustrisTNG simulations: the galaxy colour bimodality (2017, background): “The co-evolution of a central blackhole and its host galaxy is an important ingredient (Bower et al. 2006; Somerville et al. 2008; Benson 2012), and more recent efforts continue to explore galaxy color as a fundamental observational constraint (e.g. Henriques et al. 2015; Zu & Mandelbaum 2017).”
A unified multiwavelength model of galaxy formation (2015, background): “Since then, semi-analytical models based on the same general principles have been developed by several other groups (e.g. Somerville & Primack 1999; Nagashima et al. 1999; Menci et al. 2002; Hatton et al. 2003; Monaco et al. 2007; Lagos et al. 2008; Benson 2012).”
SEMI-ANALYTIC GALAXY EVOLUTION (SAGE): MODEL CALIBRATION AND BASIC RESULTS (2016, methodology): “In this sense, sage is following a similar path to that already established by scientific codes such as gadget2 (Springel 2005) and galacticus12 (Benson 2012), as well as many others (see the Astrophysics Source Code Library13 for further examples).”
First results from the IllustrisTNG simulations: matter and galaxy clustering (2017, background): “…matching a large variety of observational data, both at the present epoch and at high redshift (e.g. Kauffmann, White & Guiderdoni 1993; De Lucia et al. 2006; Somerville et al. 2008; Benson 2012; Clay et al. 2015; Henriques et al. 2015; Croton et al. 2016; Lacey et al. 2016; Cattaneo et al. 2017).”
Simulating galaxy formation with the IllustrisTNG model (2017, background): “…Vogelsberger & Angulo 2012; Kim et al. 2014; Skillman et al. 2014) and coupled with ever-more comprehensive semi-analytical models for galaxy formation (from Kauffmann, White & Guiderdoni 1993; Springel et al. 2001 to Benson 2012; Henriques et al. 2015; Lacey et al. 2016; Croton et al. 2016).”
Moving mesh cosmology: numerical techniques and global statistics (2011, background): “…so-called semianalytical modelling of galaxy formation (e.g. White & Frenk 1991; Kauffmann, White & Guiderdoni 1993; Baugh 2006; Croton et al. 2006; Benson 2010, 2012; Guo et al. 2011) or the closely related approach of halo occupation distributions (Benson et al. 2000), or (ii) using direct…”
Gravitational probes of dark matter physics (2017, background): “How do we make predictions for observations of ensembles of objects as a function of dark matter physics, given the enormous computational cost to model even a single system for fixed dark matter physics? The solution is almost certainly a hybrid program of simulations of various types, and semi-ana”
The origin and evolution of the galaxy mass–metallicity relation (2015, unknown): “Semi-analytic models (SAMs) of galaxy formation include physically and/or empirically motivated prescriptions of heating and cooling, star formation, metal enrichment, gas outflows, accretion, and AGN feedback (e.g. Croton et al. 2006; Somerville et al. 2008; Benson 2012; Lu et al. 2014).”
ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES (2013, methodology): “Whereas the Lacey et al. (2010) model required a topheavy stellar initial mass function, the Benson (2012) model merely has enhanced dust production in starbursts.”
Warm dark matter chills out: constraints on the halo mass function and the free-streaming length of dark matter with eight quadruple-image strong gravitational lenses (2019, methodology): “To determine the scaling function F (Mhalo, z), we run a suite of simulations using the semi-analytic modelling code GALACTICUS5 (Benson 2012; Pullen, Benson & Moustakas 2014), simulating host haloes and their substructure in the redshift range 0.2 < z < 0.8 and mass range 0.8–3 × 1013 M , with a su”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, background): “…decades, semi-analytical models (e.g. White & Rees 1978; White & Frenk 1991; Kauffmann et al. c© 0000 RAS, MNRAS 000, 000–000 1993; Hatton et al. 2003; Baugh 2006; Benson 2012) have been successful in reproducing many of the bulk properties of galaxies over a significant fraction of cosmic time.”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, result): “While we have been unable to compare directly with the B05 model, we have compared our results with those of a SAM that uses a similar radiative transfer treatment (Benson 2012).”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “The 1.4 mm redshift distribution is compared to several literature models which employ a phenomenological approach (Béthermin et al., 2012b), hybrid cosmological hydrodynamic approach (Hayward et al., 2013a), and semi-analytic approach (Lacey et al., 2010; Benson, 2012).”
De re metallica: the cosmic chemical evolution of galaxies (2018, background): “…formation efficiency, feedback from SNe, feedback from AGN, morphological transformation, and metals distribution (e.g., Kauffmann et al., 1993; Lacey & Cole, 1993; Cole et al., 2000; Kauffmann et al., 2004; Croton et al., 2006; De Lucia & Blaizot, 2007; Benson, 2012; Collacchioni et al., 2018).”
The current status of galaxy formation (2012, background): “The popularity of SAMs has increased with public-domain outputs (Bower et al., 2006; Croton et al., 2006; De Lucia & Blaizot, 2007; Guo et al., 2011) and codes (Benson, 2012).”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, background): “…from the dark-matterdominated growth of structure by post-processing halo merger trees with a series of physically motivated recipes (White & Frenk 1991; Kauffmann,White &Guiderdoni 1993; Cole et al. 1994; Somerville & Primack 1999; Kang et al. 2005; Monaco, Fontanot & Taffoni 2007; Benson 2012).”