Feedback and metal enrichment in cosmological smoothed particle hydrodynamics simulations ¿ I. A model for chemical enrichment

By C. Scannapieco, Patricia B. Tissera, Simon D. M. White, Volker Springel. 2005

162 citations recorded by the source corpus.

We discuss a model for treating chemical enrichment by Type II and Type Ia supernova (SNII and SNIa) explosions in simulations of cosmological structure formation. Our model includes metal-dependent radiative cooling and star formation in dense collapsed gas clumps. Metals are returned into the diffuse interstellar medium by star particles using a local smoothed particle hydrodynamics (SPH) smoothing kernel. A variety of chemical abundance patterns in enriched gas arise in our treatment owing to the different yields and lifetimes of SNII and SNIa progenitor stars. In the case of SNII chemical production, we adopt metal-dependent yields. Because of the sensitive dependence of cooling rates on metallicity, enrichment of galactic haloes with metals can in principle significantly alter subsequent gas infall and the build-up of the stellar components. Indeed, in simulations of isolated galaxies we find that a consistent treatment of metal-dependent cooling produces 25 per cent more stars outside the central region than simulations with a primordial cooling function. In the highly enriched central regions, the evolution of baryons is however not affected by metal cooling, because here the gas is always dense enough to cool. A similar situation is found in cosmological simulations because we include no strong feedback processes which could spread metals over large distances and mix them into unenriched diffuse gas. We demonstrate this explicitly with test simulations which adopt suprasolar cooling functions leading to large changes both in the stellar mass and in the metal distributions. We also find that the impact of metallicity on the star formation histories of galaxies may depend on their particular evolutionary history. Our results hence emphasize the importance of feedback processes for interpreting the cosmic metal enrichment.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/af2445e1eea66bd162b1cb6599ef6a006e764cd5

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Citations in the corpus

The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “G3 refers to the standard Springel & Hernquist (2003) implementation; G3-CS refers to the code presented in Scannapieco et al. (2005, 2006); G3-TO to that developed by Okamoto et al. (2005, 2010) and Okamoto, Nemmen & Bower (2008); G3-GIMIC is described in Crain et al. (2009); G3-MM is introduced…”
The Baryon Content of Extremely Low Mass Dwarf Galaxies (2006, background): “For example, the importance of galactic winds in low mass galaxies will strongly affect our understanding of the mass-metallicity relation (Tremonti et al. 2004; Lee et al. 2006) and the enrichment of the intergalactic medium at high redshift (Scannapieco et al. 2005).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “Scannapieco et al. (2005) demonstrated that adopting a self-consistent calculation of the timescale for gas cooling in a model in which the gas metallicity evolves according to a chemical evolution model produces galaxies which are 25% bigger than if a fixed, primordial metallicity is assumed.”
Effects of supernova feedback on the formation of galaxy discs (2008, methodology): “In Scannapieco et al. (2005, 2006) we tested the code by studying the formation of disk galaxies of different mass from idealized initial conditions.”
High-resolution panchromatic spectral models of galaxies including photoionization and dust (2009, methodology): “Codes with better treatment of metal production and gas recycling from stars exist (e.g. Scannapieco et al. 2005; Stinson et al. 2006), and using such simulations would improve the accuracy of the radiation-transfer calculation.”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, methodology): “2008 for a review), but in recent years chemodynamical cosmological simulations have also become more common (e.g. Mosconi et al. 2001; Scannapieco et al. 2005; Kobayashi et al. 2007; Oppenheimer & Davé 2008).”
THE METALLICITY EVOLUTION OF INTERACTING GALAXIES (2011, background): “…is transferred from a single stellar particle to a set of nearest SPH neighbors (e.g. Steinmetz & Mueller 1994; Kawata 2001; Kawata & Gibson 2003; Okamoto et al. 2005; Scannapieco et al. 2005; Stinson et al. 2006; Tornatore et al. 2007; Wiersma et al. 2009; Montuori et al. 2010; Perez et al. 2011).”
Astrophysical smooth particle hydrodynamics (2009, background): “…starting point one may want to consult (Steinmetz and Müeller, 1994, 1995; Raiteri et al., 1996; Carraro et al., 1998; Berczik, 1999; Kawata and Gibson, 2003; Kobayashi, 2004; Tornatore et al., 2004; Scannapieco et al., 2005; Martinez-Serrano et al., 2008; Greif et al., 2009; Wiersma et al., 2009).”
Formation of isolated dwarf galaxies with feedback (2009, methodology): “As an extension, metal-dependent cooling, star formation, chemical enrichment and energy injection from type II and type Ia supernovae have been implemented in the multiphase gas model of Scannapieco et al. (2005, 2006).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “This implementation also includes metaldependent cooling, star formation, and chemical and thermal feedback into both gas phases. as described in Scannapieco et al. (2005) and Scannapieco et al. (2006).”
The effect of galaxy mass ratio on merger-driven starbursts (2007, methodology): “While we eventually intend to incor- porate these effects into our modeling (as has been done by several authors already, see, e.g, Tornatore et al. 2004; Scannapieco et al. 2005; Stinson et al. 2006), the relatively small difference (∼ 15”
The RAVE survey : the Galactic escape speed and the mass of the Milky Way (2013, background): “Details regarding the simulation code can be found in Scannapieco et al. (2005, 2006) and also in Springel (2005).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, methodology): “Sawala et al. (2010) used the multiphase scheme for the interstellar medium developed by Scannapieco et al. (2005, 2006), and constrained the fraction of metals given to the cold gas phase, later defining the final metallicity for a given stellar mass, on the metallicity-relation of dwarf galaxies.”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “…Katz et al. 1996; Wiersma et al. 2009a), and chemical enrichment (e.g., Steinmetz & Mueller 1994; Mosconi et al. 2001; Lia et al. 2002; Springel & Hernquist 2003a; Kobayashi 2004; Scannapieco et al. 2005; Tornatore et al. 2007; Oppenheimer & Davé 2008; Wiersma et al. 2009b; Few et al. 2012).”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, methodology): “…C© 2007 RAS, MNRAS 382, 1050–1072 Downloaded from https://academic.oup.com/mnras/article-abstract/382/3/1050/1008452 by guest on 30 July 2018 and Scannapieco et al. (2005) neglected delay times for SNII, assumed a fixed delay time for SNIa and neglected the contribution to enrichment from…”