Effects of supernova feedback on the formation of galaxy discs

By C. Scannapieco, Patricia B. Tissera, Simon D. M. White, Volker Springel Max-Planck Institute for Astrophysics - G Astronomy, Space Physics - Buenos Aires. 2008

216 citations recorded by the source corpus.

We use cosmological simulations in order to study the effects of supernova (SN) feedback on the formation of a Milky Way-type galaxy of virial mass ∼ 10 12 h -1 M ⊙ . We analyse a set of simulations run with the code described by Scannapieco et al., where we have tested our star formation and feedback prescription using isolated galaxy models. Here, we extend this work by simulating the formation of a galaxy in its proper cosmological framework, focusing on the ability of the model to form a disc-like structure in rotational support. We find that SN feedback plays a fundamental role in the evolution of the simulated galaxy, efficiently regulating the star-formation activity, pressurizing the gas and generating mass-loaded galactic winds. These processes affect several galactic properties such as final stellar mass, morphology, angular momentum, chemical properties, and final gas and baryon fractions. In particular, we find that our model is able to reproduce extended disc components with high specific angular momentum and a significant fraction of young stars. The galaxies are also found to have significant spheroids composed almost entirely of stars formed at early times. We find that most combinations of the input parameters yield disc-like components, although with different sizes and thicknesses, indicating that the code can form discs without fine-tuning the implemented physics. We also show how our model scales to smaller systems. By analysing simulations of virial masses 10 9 and 1010 h -1 M ⊙ , we find that the smaller the galaxy, the stronger the SN feedback effects.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/48e1f15f934db71b8c522023058c5009f21e76e7

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Citations in the corpus

ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, background): “…the last two decades (e.g. Katz 1992; Navarro & White 1993; Katz et al. 1996; Thacker & Couchman 2001; Stinson et al. 2006; Governato et al. 2007; Scannapieco et al. 2008; Colín et al. 2010; Agertz et al. 2011; Avila-Reese et al. 2011; Guedes et al. 2011; Scannapieco et al. 2012; Hopkins et al.…”
A fundamental relation between mass, SFR and metallicity in local and high redshift galaxies (2010, background): “C O ] 2 man 1996; Garnett 2002; Tremonti et al. 2004; Kobayashi et al. 2007; Scannapieco et al. 2008; Spitoni et al. 2010), “downsizing”, i.e., a systematic dependence of the efficiency of star formation with galaxy mass (e.g., Brooks et al. 2007; Mouchine et al. 2008; Calura et al. 2009),…”
The formation and survival of discs in a ΛcDM universe (2008, background): “…abundances (e.g. Springel & Hernquist 2003; Brook et al. 2004; Okamoto et al. 2005; Oppenheimer & Davé 2006; Stinson et al. 2006; Governato et al. 2007; Dalla Vecchia & Schaye 2008; Dubois & Teyssier 2008; Finlator & Davé 2008; Scannapieco et al. 2008 (hereafter S08); among recent examples).”
The relation between metallicity, stellar mass and star formation in galaxies: an analysis of observational and model data (2011, background): “…Royal Astronomical Society C© 2012 RASDownloaded from https://academic.oup.com/mnras/article-abstract/422/1/215/1020516 by guest on 30 July 2018 & White 2007; Scannapieco et al. 2008), this does not mean that outflows are the only process at work in regulating the metallicities of real galaxies.”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “However, whatever physical processes are now invoked to explain the fj values of spirals must simultaneously allow for much lower fj in ellipticals (e.g., by having less efficient feedback; Zavala et al. 2008; Scannapieco et al. 2008).”
Metallicity gradients in disks - Do galaxies form inside-out? (2012, background): “…several studies of chemistry within cosmological hydrodynamical simulations (e.g. Raiteri et al. 1996b; Kawata & Gibson 2003; Okamoto et al. 2008; Scannapieco et al. 2008; Zolotov et al. 2010; Rahimi et al. 2010; Wiersma et al. 2011; Kobayashi & Nakasato 2011), each modelling certain…”
Moving mesh cosmology: numerical techniques and global statistics (2011, background): “…(e.g. Springel & Hernquist 2003a), radiative cooling (Katz, Weinberg & Hernquist 1996b; Smith, Sigurdsson & Abel 2008), chemical enrichment (e.g. Wiersma et al. 2009) and various feedback processes relevant for low- and high-mass systems (e.g. Sijacki et al. 2007; Scannapieco et al. 2008).”
MODELING MOLECULAR HYDROGEN AND STAR FORMATION IN COSMOLOGICAL SIMULATIONS (2008, unknown): “The standard approach in galaxy formation modeling so far (c.f. recent studies by Brooks et al. 2007; Governato et al. 2007; Ceverino & Klypin 2007; Scannapieco et al. 2008; Croft et al. 2008; Oppenheimer & Davé 2008; Tasker & Bryan 2008; Mayer et al. 2008, and many earlier works, comprehensively…”
Forming a large disc galaxy from a z < 1 major merger (2008, background): “The maximum halo mass and lowest redshift at which mergers can regrow discs are obviously a function of the feedback efficiency (Brook et al. 2004a; Scannapieco et al. 2008) and could therefore provide useful qualitative tests of models of SF and feedback.”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “…a consequence of our SN feedback model which results in larger promotion rates (relative to the star formation rate) in systems with shallower potential wells: smaller haloes experience more significant winds (Scannapieco et al. 2008; Sawala et al. 2010; De Rossi et al. 2010; Sawala et al. 2011).”
Self-regulated star formation in galaxies via momentum input from massive stars (2011, background): “Other models explicitly disable certain interactions between gas flagged as ‘cold’ and ‘hot’ or deposit feedback energy in a noncooling reservoir that serves to move gas from cold to hot phases (Scannapieco et al. 2008).”
Galaxies–intergalactic medium interaction calculation – I. Galaxy formation as a function of large-scale environment (2009, background): “…dark matter (e.g. Navarro & Benz 1991; Weil, Eke & Efstathiou 1998; Thacker & Couchman 2001; Abadi et al. 2003a,b; Sommer-Larsen, Götz & Portinari 2003; Governato et al. 2004; Robertson et al. 2004; Okamoto et al. 2005; Governato et al. 2007; Scannapieco et al. 2008; Zavala, Okamoto & Frenk 2008).”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “(Scannapieco et al. 2008, 2009), making it unlikely that the in situ star formation could have enriched the ISM to the presently observed values.”
The effects of gas on morphological transformation in mergers: implications for bulge and disc demographics (2009, background): “…fragmentation and angular momentum transport (Weil, Eke & Efstathiou 1998; Sommer-Larsen, Gelato & Vedel 1999; Thacker & Couchman 2000, 2001; Abadi et al. 2003; Sommer-Larsen, Götz & Portinari 2003; Governato et al. 2004, 2007; Robertson et al. 2004; Okamoto et al. 2005; Scannapieco et al. 2008).”
Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, background): “Stellar feedback is the favored way of reducing star formation and launching outflows (Scannapieco et al. 2008; Schaye et al. 2010).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “…can indeed be alleviated when feedback from evolving stars, in particular supernovae (SNe), is included (e.g. Okamoto et al. 2005; Governato et al. 2007; Scannapieco et al. 2008, 2009; Ceverino & Klypin 2009; Joung, Cen & Bryan 2009; Colin et al. 2010; Sales et al. 2010; Stinson et al. 2010).”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, background): “Supernovae enrich the inter-stellar medium with metals, and inject thermal and kinetic energy into the ambient gas (e.g. Scannapieco et al. 2008).”
The properties of satellite galaxies in simulations of galaxy formation (2009, methodology): “…modelling using various recipes leading to a new generation of simulations which are producing increasingly realistic disc galaxies (Springel & Hernquist 2003a; Robertson et al. 2004; Okamoto et al. 2005; Stinson et al. 2006; Governato et al. 2007; Scannapieco et al. 2008; Ceverino & Klypin 2009).”