Feedback and metal enrichment in cosmological SPH simulations – II. A multiphase model with supernova energy feedback

By C. Scannapieco, Patricia B. Tissera, Simon D. M. White, Volker Springel. 2006

191 citations recorded by the source corpus.

We have developed a new scheme to treat a multiphase interstellar medium in smoothed particle hydrodynamics simulations of galaxy formation. This scheme can represent a co-spatial mixture of cold and hot ISM components, and is formulated without scale-dependent parameters. It is thus particularly suited to studies of cosmological structure formation where galaxies with a wide range of masses form simultaneously. We also present new algorithms for energy and heavy element injection by supernovae, and show that together these schemes can reproduce several important observed effects in galaxy evolution. Both in collapsing systems and in quiescent galaxies our codes can reproduce the Kennicutt relation between the surface densities of gas and of star formation. Strongly metal-enhanced winds are generated in both cases with ratios of mass-loss to star formation which are similar to those observed. This leads to a self-regulated cycle for star formation activity. The overall impact of feedback depends on galaxy mass. Star formation is suppressed at most by a factor of a few in massive galaxies, but in low-mass systems the effects can be much larger, giving star formation an episodic, bursty character. The larger the energy fraction assumed available in feedback, the more massive the outflows and the lower the final stellar masses. Winds from forming discs are collimated perpendicular to the disc plane, reach velocities up to ∼ 1000 km s -1 , and efficiently transport metals out of the galaxies. The asymptotically unbound baryon fraction drops from >95 per cent to ∼30 per cent from the least to the most massive of our idealized galaxies, but the fraction of all metals ejected with this component exceeds 60 per cent regardless of mass. Such winds could plausibly enrich the intergalactic medium to observed levels.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8768c4a08db5668bb5d4f5159ee8c6ac1a9d0370

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Citations in the corpus

ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “…SPH simulations of galaxy formation in halos of masses in the range Mhalo = 1011 − 3× 1012 M , Aumer et al. (2013) studied the impact of their feedback model based on the multiphase SPH code presented in Scannapieco et al. (2006), with the addition of momentum input from radiation pressure.”
The formation and survival of discs in a ΛcDM universe (2008, methodology): “This study used an extension of the Tree-PM SPH code GADGET-2 (Springel 2005) which includes star formation, chemical enrichment and SN feedback, metal-dependent cooling and a multiphase model for the gas component (Scannapieco et al. 2005, 2006; hereafter S05, S06 respectively).”
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.”
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds (2012, background): “However, in its simplest form, such an approach is relatively ineffective and does not create outflows, prompting a number of ‘delayed cooling’ models (e.g. Thacker & Couchman 2000; Scannapieco et al. 2006) that try to suppress a rapid cooling loss of the injected heat energy.”
The formation of disc galaxies in a ΛCDM universe (2010, methodology): “Various recipes of supernovae feedback have been developed for numerical simulations (e.g. Navarro & White 1993; Kay et al. 2002; Scannapieco et al. 2006), and the methods have proven successful in removing low angular momentum material from central parts of galaxies (e.g. Sommer-Larsen et al.…”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, methodology): “…through the heating of the gas, in either homogeneous ISM (Gerritsen 1997; Mori et al. 1997; Thacker & Couchman 2000; Sommer-Larsen et al. 2003; Brook et al. 2004; Stinson et al. 2006) or a multiphase ISM (Yepes et al. 1997; Hultman & Pharasyn 1999; Marri & White 2003; Scannapieco et al. 2006).”
Simulating galactic outflows with kinetic supernova feedback (2008, background): “…of its mean density (e.g. Springel & Hernquist 2003) and, at least for the case of smoothed particle hydrodynamics simulations, explictly decoupling thermal phases by using different types of particles to represent the hot and cold gas phases (e.g. Marri & White 2003; Scannapieco et al. 2006).”
Simulating galactic outflows with thermal supernova feedback (2012, background): “…et al. 1997; Thacker & Couchman 2000; Kay et al. 2002; Sommer-Larsen, Götz, & Portinari 2003; Brook et al. c© 0000 RAS 2004; Stinson et al. 2006; Piontek & Steinmetz 2011), and decoupling the different thermal phases by hand (e.g. Marri & White 2003; Scannapieco et al. 2006; Murante et al. 2010).”
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).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “20 Theoretical Challenges in Galaxy Formation A ’two phase’ approach is followed in Scannapieco et al. (2006) where the hot and the cold gas phase are evolved separately using SPH (Marri & White 2003).”
Dark matter response to galaxy formation (2009, methodology): “These were carried out with a version of GADGET-3 which includes a multi-phase treatment of metal-dependent cooling, star formation and SN feedback (Scannapieco et al. 2005, 2006).”
On the onset of galactic winds in quiescent star forming galaxies (2007, background): “One of the key outcome of such numerical simulation is the fractionof the injected supernovae energy which is transferred up to the large scale galactic wind and is truely available for feedback (Fujita et al. 2004; Scannapieco et al. 2006).”
Towards a more realistic population of bright spiral galaxies in cosmological simulations (2013, methodology): “We have presented an extensive update to the multiphase SPH galaxy formation code by Scannapieco et al. (2005, 2006).”
Formation of isolated dwarf galaxies with feedback (2009, methodology): “This model has previously been used to study the effect of feedback on galaxy evolution in general terms (Scannapieco et al. 2006) and the formation of disk galaxies in particular (Scannapieco et al. 2008, 2009).”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “Similarly, outflows appear necessary to reach the level of observed CGM and intergalactic medium (IGM) metal enrichment (Oppenheimer & Davé 2006; Scannapieco et al. 2006; Shen et al. 2010, 2012; Booth et al. 2012; Oppenheimer et al. 2012; Stinson et al. 2012; Ford et al. 2013; Crain et al. 2013;…”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, methodology): “Scannapieco et al. (2005) presented another implementation of a model of chemical enrichment in the GADGET-2 code, coupled to a self-consistent model for SF and feedback (see also Scannapieco et al. 2006).”
Galaxy formation theory (2010, methodology): “…using a semianalytic approach (Thacker and Couchman 2000; Kay et al. 2002; Marri and White 2003; White 2004; Stinson et al. 2006; Cox et al. 2006; Scannapieco et al. 2006a; Tasker and Bryan 2006; Stinson 2007; Vecchia and Schaye 2008; Oppenheimer and Davé 2008; Okamoto et al. 2008b; Booth and…”
Feedback in simulations of disc-galaxy major mergers (2005, methodology): “We intend to implement a more realistic approach where star particles return a fraction of their mass and metals back to the interstellar medium in the future (see, e.g., Mosconi et al. 2001; Tornatore et al. 2004; Okamoto et al. 2005; Scannapieco et al. 2006, 2005).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, methodology): “This naturally results in self-regulated winds which are adapted to the depth of the potential well in which star formation is occurring (Scannapieco et al. 2006, 2009; Sawala et al. 2010, 2011; De Rossi et al. 2010).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…the hot gas density, in which particles with temperatures below 12 000K are ignored when computing the density of gas particles with temperatures in excess of T = 105K. Scannapieco et al. (2006) describe a SPH code with a co-spatial treatment of the hot and cold phases of the interstellar medium.”