GALICS I: A hybrid N-body semi-analytic model of hierarchical galaxy formation

By S. Hatton, J. Devriendt, Stéphane Ninin, F. Bouchet, B. Guiderdoni, D. Vibert. 2003

278 citations recorded by the source corpus.

This is the first paper of a series that describes the methods and basic results of the galics model (Galaxies In Cosmological Simulations). galics is a hybrid model for hierarchical galaxy formation studies, combining the outputs of large cosmological N-body simulations with simple, semi-analytic recipes to describe the fate of the baryons within dark matter haloes. The simulations produce a detailed merging tree for the dark matter haloes, including complete knowledge of the statistical properties arising from the gravitational forces. We intend to predict the overall statistical properties of galaxies, with special emphasis on the panchromatic spectral energy distribution emitted by galaxies in the ultraviolet/optical and infrared/submillimetre wavelength ranges. In this paper, we outline the physically motivated assumptions and key free parameters that go into the model, comparing and contrasting with other parallel efforts. We specifically illustrate the success of the model in comparison with several data sets, showing how it is able to predict the galaxy disc sizes, colours, luminosity functions from the ultraviolet to far infrared, the Tully–Fisher and Faber–Jackson relations, and the fundamental plane in the local Universe. We also identify certain areas where the model fails, or where the assumptions needed to succeed are at odds with observations, and pay special attention to understanding the effects of the finite resolution of the simulations on the predictions made. Other papers in this series will take advantage of different data sets available in the literature to extend the study of the limitations and predictive power of galics, with particular emphasis put on high-redshift galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1ff53dd0b709f70b9e44e1f6d6f66a56344043a1

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Citations in the corpus

Radial Variation of Attenuation and Star Formation in the Largest Late-Type Disks Observed with GALEX (2006, methodology): “As a result, it is also a fundamental element of any galaxy evolutionary model, e.g. Nbody/semi-analytical models like GALICS (Hatton et al. 2003), SPH/chemical evolution models (Lia et al. 2002), chemical / spectrophotometric evolution models (Boissier & Prantzos 1999).”
The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8 (2006, background): “These, interpreted using the latest theoretical techniques (Cole et al. 2000; Hatton et al. 2003; Springel et al. 2005; De Lucia et al. 2006), should provide important constraints on the physical mechanisms driving the formation and the evolution of cluster galaxies.”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, methodology): “This simple argument has been used to estimate the sizes of galaxies in many semi-analytic models (Lacey et al. 1993; Kauffman & Charlot 1994; Poli et al. 1999; Somerville & Primack 1999; Firmani & Avila-Reese 2000; Hatton et al. 2003).”
The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach (2008, methodology): “Following Hatton et al. (2003), we recompute the scale-length at each time-step by taking the mass-weighted average gas profile of the disk and that of the new material being accreted.”
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).”
How do galaxies populate dark matter haloes (2009, background): “…a hydrodynamical (e.g. Cen & Ostriker 2000; Springel & Hernquist 2003; Kereš et al. 2005; Pfrommer et al. 2006; Sijacki et al. 2007) or a semi-analytic (e.g. Kauffmann et al. 1999; Springel et al. 2001; Hatton et al. 2003; Springel et al. 2005; Kang et al. 2005) treatment of baryonic evolution.”
The hierarchical formation of the brightest cluster galaxies (2006, background): “As in Hatton et al. (2003) – see Guiderdoni & RoccaVolmerange (1987) for details – the extinction curve depends on the gas metallicity Zg and is based on an interpolation between the solar neighbourhood and the Large and Small Magellanic Clouds (s = 1.35 for λ < 2000 Å and s = 1.6 for λ > 2000 Å).”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “…phenomenological components of galaxy formation models is a practice that was established during the development of the first generation of semi-analytic galaxy formation models8 (Kauffmann, White & Guiderdoni 1993; Cole et al. 1994; Somerville & Primack 1999; Cole et al. 2000; Hatton et al. 2003).”
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).”
A calibration of the relation between the abundance of close galaxy pairs and the rate of galaxy mergers (2008, methodology): “Similar models but with different detailed treatments of various aspects of the baryonic physics have proposed by Cole et al. (1994, 2000), Somerville & Primack (1999), Hatton et al. (2003), Kang et al. (2005) among others.”
The age dependence of halo clustering (2005, background): “Examples of such models which graft a semi-analytic treatment of baryon physics onto a Nbody simulation can be found in Kauffmann et al (1999), Springel et al (2001, 2005), Helly et al (2003), Hatton et al (2003) and Kang et al (2005).”
On the onset of galactic winds in quiescent star forming galaxies (2007, methodology): “…of the hierarchical model, both in semi–analytical models (White & Frenk 1991; Somerville & Primack 1999; Kauffmann et al. 1999; Cole et al. 2000; Hatton et al. 2003; Monaco 2004; Bertone et al. 2005) and in numerical simulation (Cen & Ostriker 1992; Navarro & White 1993; Mihos & Hernquist…”
Galaxy bimodality due to cold flows and shock heating (2004, methodology): “In an associated paper (Cattaneo et al. 2005, C05) we have implemented the proposed new physics in a hybrid SAM/N-body simulation (GalICS Hatton et al. 2003).”
UV-Optical Colors as Probes of Early-Type Galaxy Evolution (2006, background): “…both at local and high redshift (Chiosi and Carraro 2002), without invoking hierarchical merger-driven processes (e.g. Toomre and Toomre 1972; Toomre 1977; Kauffmann et al. 1993; Somerville and Primack 1999; Benson et al. 2000; Cole et al. 2000; Hatton et al. 2003; Khochfar and Burkert 2003).”
DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “Models that are more sophisticated than empirical approaches attempt to follow the physics of galaxy formation in greater detail (e.g., Guiderdoni et al. 1998; Hatton et al. 2003; Granato et al. 2004; Silva et al. 2005).”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, methodology): “…a computationally inexpensive route to probing the phenomenology of galaxy formation and, in particular, the theoretical analysis of today’s large survey datasets (e.g. Cole et al. 2000; Hatton et al. 2003; Bower et al. 2006; Somerville et al. 2012; Overzier et al. 2013; Bernyk et al. 2016).”
The morgana model for the rise of galaxies and active nuclei (2006, background): “…and accrete on to the BH, at variance with the choice of switching cooling off whenever some fiducial criterion is satisfied, like, for example, in Hatton et al. (2003), Bower et al. (2006) or Croton et al. (2006), a choice that leads to better fits to the luminosity functions and correct red…”
Galactic star formation and accretion histories from matching galaxies to dark matter haloes (2012, methodology): “…& Hernquist 2003; Kereš et al. 2005; Crain et al. 2009; Schaye et al. 2010; Oppenheimer et al. 2010) or on a semi-analytic method (Kauffmann et al. 1999; Springel et al. 2001; Hatton et al. 2003; Springel et al. 2005; Kang et al. 2005; Croton et al. 2006; Bower et al. 2006; Guo et al. 2011).”
A Fitting Formula for the Merger Timescale of Galaxies in Hierarchical Clustering (2007, background): “…formation (e.g., Kauffmann et al. 1999; Cole et al. 2000; Monaco et al. 2000; Somerville & Primack 1999; Menci et al. 2002; Nagashima et al. 2002; Hatton et al. 2003; Khochfar & Ostriker 2007; Baugh 2006, for an excellent review) and in understanding the merger rates of galaxies in the…”