Mass, metal, and energy feedback in cosmological simulations

By B. Oppenheimer, R. Dav'e. 2007

427 citations recorded by the source corpus.

Using GADGET-2 cosmological hydrodynamic simulations including an observationally constrained model for galactic outflows, we investigate how feedback from star formation distributes mass, metals, and energy on cosmic scales from z = 6 → 0. We include instantaneous enrichment from Type II supernovae (SNe), as well as delayed enrichment from Type Ia SNe and stellar [asymptotic giant branch (AGB)] mass loss, and we individually track carbon, oxygen, silicon and iron using the latest yields. Following on the success of the momentum-driven wind scalings, we improve our implementation by using an on-the-fly galaxy finder to derive wind properties based on host galaxy masses. By tracking wind particles in a suite of simulations, we find: (1) wind material re-accretes on to a galaxy (usually the same one it left) on a recycling time-scale that varies inversely with galaxy mass (e.g. <1 Gyr for L ∗ galaxies at

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c3cc9c10a35db1cc0b5aa43855d3b800e3ae0f2c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Stellar Feedback in Galaxies and the Origin of Galaxy-scale Winds (2011, background): “…lacking the ability to directly resolve the relevant feedback processes, put in winds ‘by hand’ by e.g. forcing an outflow rate that scales in a user-specified manner with the SFR or other parameters (Springel & Hernquist 2003a; Oppenheimer & Davé 2008; Sales et al. 2010; Genel et al. 2012).”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, background): “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 properties of satellite galaxies in simulations of galaxy formation (2009, methodology): “Similar, but different wind models have been used successfully to investigate the ejection of intergalactic metals (Oppenheimer & Davé 2006, 2008) and the galaxy mass-metallicity relation of massive galaxies (M∗ & 10 9M⊙; Finlator & Davé 2008).”
SHORT-LIVED STAR-FORMING GIANT CLUMPS IN COSMOLOGICAL SIMULATIONS OF z ≈ 2 DISKS (2010, methodology): “We have, however, modified the Oppenheimer & Davé (2008) code to ensure that the velocity kicks are perpendicular to the disk (e.g. Bordoloi et al. 2011, Bouché et al. in prep.).”
THE COSMOLOGICAL SIZE AND VELOCITY DISPERSION EVOLUTION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “…Schaye et al. 2010), radiative feedback from stars (e.g Oppenheimer & Davé 2006; Petkova & Springel 2009; Hopkins et al. 2011) and feedback from supernovae type II (e.g Scannapieco et al. 2008; Schaye et al. 2010; Sales et al. 2010) and Ia (e.g Ciotti & Ostriker 2007; Oppenheimer & Davé 2008).”
Galaxy formation theory (2010, background): “…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 Schaye 2009; Ciotti 2009).”
Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses (2014, background): “This implementation agrees qualitatively with the behaviour seen by Oppenheimer & Davé (2008) and Oppenheimer et al. (2010) in their numerical simulations.”
CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 (2014, methodology): “Other studies favor these simple models because they produce the best-fit to a variety of quasar absorption line studies of the intergalactic medium, while also reproducing the observed cosmic star formation history (e.g., Oppenheimer & Davé 2006, 2008).”
Galaxies in a simulated ΛCDM universe – II. Observable properties and constraints on feedback (2009, background): “Some fraction of the mass that is ejected from low-mass galaxies could be re-accreted by higher mass galaxies at later times when such feedback might be less efficient (e.g. Oppenheimer & Davé 2008).”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, methodology): “We note that the actual implementation of this wind model in our simulations has evolved owing to advances in modeling techniques and changes in cosmology (Oppenheimer & Davé 2008; Oppenheimer et al. 2010).”
THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, background): “Cosmological hydrodynamic simulations (Brooks et al. 2007; Oppenheimer & Davé 2008) have predicted an evolution in the MZ relation and recent observations at intermediate redshifts (z ∼ 0.7) have provided strong evidence for an evolution.”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “We set the mass loading and wind velocity based on the local DM velocity dispersion (similar to Oppenheimer & Davé 2008; Okamoto et al. 2010): to this end, each gas cell calculates the local one-dimensional DM velocity dispersion (σ1DDM) at its current © 0000 RAS, MNRAS 000, 000–000 location, and…”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “Hydrodynamic Simulation of Davé et al. This simulation was run with an extended version of the cosmological smooth particle hydrodynamic code Gadget-2 (Springel et al. 2005) described by Oppenheimer & Davé (2008).”
The birth of a galaxy – II. The role of radiation pressure (2012, background): “Several groups (Springel & Hernquist 2003; Oppenheimer & Davé 2008; Dalla Vecchia & Schaye 2008; Sales et al. 2010) have modelled momentum transfer from radiation by adding momentum, so-called “kicking”, to nearby particles to a velocity that is comparable to the circular velocity Vc of the halo.”
The most metal-poor damped Lyα systems: insights into chemical evolution in the very metal-poor regime★ (2011, background): “It is possible, however, that VMP DLAs acquired some of their metals at later times from nearby sources that delivered metals into the IGM via galactic superwinds (see e.g. Oppenheimer & Davé 2008), which may complicate the interpretation.”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “…adopts the popular convention of prescribing feedback parameters according to local conditions inferred from neighbouring dark matter particles (Oppenheimer & Davé 2006, 2008; Okamoto et al. 2010; Oppenheimer et al. 2010; Puchwein & Springel 2013; Vogelsberger et al. 2013, 2014a; Khandai et…”
PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z ∼ 1–3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES (2012, methodology): “…corrected, average gas fractions of z~0 and z~1-2.5 SFGs in the stellar mass range 10 10…11.5 M is remarkably well matched by momentum driven wind models proposed by Oppenheimer & Davé (2006, 2008), including the extrapolation of the gas fractions to lower masses shown in Figures 12 and 13.”