Effects of feedback on the morphology of galaxy discs

By T. Okamoto, V. Eke, Carlos S. Frenk, Adrian Jenkins. 2005

188 citations recorded by the source corpus.

We have performed hydrodynamic simulations of galaxy formation in a cold dark matter (ACDM) universe. We have followed galaxy formation in a dark matter halo, chosen to have a relatively quiet recent merger history, using different models for star formation and feedback. In all cases, we have adopted a multiphase description of the interstellar medium and modelled star formation in quiescent and burst modes. We have explored two triggers for starbursts -strong shocks and high gas density - allowing for the possibility that stars in the burst may form with a top-heavy initial mass function. We find that the final morphology of the galaxy is extremely sensitive to the modelling of star formation and feedback. Starting from identical initial conditions, galaxies spanning the entire range of Hubble types, with B-band disc-to-total luminosity ratios ranging from 0.2 to 0.9, can form in the same dark matter halo. Models in which starbursts are induced by high gas density (qualitatively similar to models in which feedback is produced by active galactic nuclei) generate energetic winds and result in galaxies with an early-type morphology. Models in which the starbursts are induced by strong shocks lead to extended discs. In this case, the feedback associated with the bursts suppresses the collapse of baryons in small haloes, helping to create a reservoir of hot gas that is available for cooling after z ≃ 1, following the bulk of the dynamical activity that builds up the halo. This gas then cools to form an extended, young stellar disc.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a85c8aeb74563ffde8fa17a19c2c85c3333478f2

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Citations in the corpus

The formation of disc galaxies in a ΛCDM universe (2010, methodology): “…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. 2003; Okamoto et al. 2005; Governato et al. 2007), yielding more extended galaxies in comparison to models without feedback.”
THE ROLE OF STELLAR FEEDBACK IN THE FORMATION OF GALAXIES (2007, background): “…improvements in both the resolution (sub-kpc scales) and modeling of the feedback have resulted in simulations with extended galactic disks (SommerLarsen et al. 2003; Governato et al. 2004; Robertson et al. 2004; Brook et al. 2004; Okamoto et al. 2005; D’Onghia et al. 2006; Governato et al. 2007).”
Forming disc galaxies in ΛCDM simulations (2006, background): “Our DWF1 and MW1 galaxy models have a higher fraction of stars on circular orbits when compared with the distributions showed by Abadi et al. (2003) and Okamoto et al. (2005).”
Towards a more realistic population of bright spiral galaxies in cosmological simulations (2013, background): “…continue to be plagued by a range of problems, with different codes often producing very different galaxies for the same initial conditions (Okamoto et al. 2005; Kereš et al. 2011; Scannapieco et al. 2012). c© 2013 RAS The formation of realistic disc galaxies has been shown to be…”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “…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 by Murante et al.…”
On the onset of galactic winds in quiescent star forming galaxies (2007, background): “…large disc galaxies observed at our epoch (Weil et al. 1998; Thacker & Couchman 2001), the morphology of galactic discs (Sommer-Larsen et al. 2003; Okamoto et al. 2005), to stabilize the gaseous disc against the Toomre instability (Robertson et al. 2004) or to fit the temperature of the…”
THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “…starburst (Mihos & Hernquist 1994), in which a large portion of the gas35 is exhausted (depending on gas fraction; see Springel & Hernquist 2005; Okamoto et al. 2005; Robertson et al. 2006; Cox et al. 2008; Governato et al. 2007, 2009), and through subsequent feedback, from supernovae and/or…”
Effects of supernova feedback on the formation of galaxy discs (2008, background): “Many recent studies have attempted to prevent the early cooling of gas and the loss of angular momentum, some of them successfully reproducing disks as big as observed spirals (e.g. Abadi et al. 2003; Governato et al. 2004; Robertson et al. 2004; Okamoto et al. 2005; Governato et al. 2007).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, methodology): “In numerical simulations, the angular momentum vector of a galaxy is seen to change orientation after merger events, which could explain some of the difficulties in finding galaxies of the observed radius (Okamoto et al. 2005).”
Feedback in simulations of disc-galaxy major mergers (2005, methodology): “In addition, several authors investigated a range of values for c⋆ (Bekki & Shioya 1998; Thacker & Couchman 2000) as we do in §5.2, or use a hybrid model where c⋆ can change with redshift or environment (Sommer-Larsen et al. 2003; Okamoto et al. 2005).”
A Merger-driven Scenario for Cosmological Disk Galaxy Formation (2005, background): “…these discrepancies in a cosmological context have mainly relied on increasing the impact of feedback from star formation (Weil et al. 1998; Sommer-Larsen et al. 1999, 2003; Thacker & Couchman 2000, 2001; Abadi et al. 2003a; Governato et al. 2004; Robertson et al. 2004; Okamoto et al. 2005).”
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).”
Theoretical Challenges in Galaxy Formation (2016, background): “Investigators quickly discovered that, while the detailed implementation can change the results significantly (e.g. Navarro & White 1993; Okamoto et al. 2005; Robertson et al. 2004; Sommer-Larsen, Gelato & Vedel 1999; Thacker & Couchman 2000) almost all cosmological simulations resulted in the…”
MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “…disks (both high-resolution and cosmological; see e.g. Springel & Hernquist 2005; Robertson et al. 2006; Cox et al. 2008; Robertson & Bullock 2008; Okamoto et al. 2005; Scannapieco et al. 2008; Governato et al. 2007, 2008), and for the global census of bulge and disk populations and survival of…”
HOW DO DISKS SURVIVE MERGERS? (2008, background): “…et al. 1998; Sommer-Larsen et al. 1999, 2003; Thacker & Couchman 2000, 2001; Abadi et al. 2003; Governato et al. 2004, 2007; Robertson et al. 2004; Okamoto et al. 2005; Scannapieco et al. 2008), in order to enable disks to survive their expected violent merger histories without completely losing…”
Cosmological simulations of the formation of the stellar haloes around disc galaxies (2011, result): “This is in contrast with many of the previous cosmological modelling studies of Milky Way-type galaxies, which usually select their simulation candidates from systems that have not undergone any major mergers in the recent past (e.g., Diemand et al. 2005; Okamoto et al. 2005; Cooper et al. 2010).”
X-ray coronae in simulations of disc galaxy formation (2010, background): “Recently, high-resolution simulations of individual objects have demonstrated the importance of feedback in mitigating this problem (e.g. Okamoto et al. 2005; Scannapieco et al. 2008), a finding supported by the large sample of galaxies we present here.”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “…with sizes and rotation curves that are, for particular galaxy masses, consistent with observational measurements (e.g. Governato et al. 2004; Okamoto et al. 2005; Sales et al. 2010; Guedes et al. 2011; Brook et al. 2012; McCarthy et al. 2012; Aumer et al. 2013; Munshi et al. 2013;…”
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time (2016, background): “The final outcome of the simulations appears to be dependent on details of the implementation of feedback and star formation (see Okamoto et al. 2005), a sensitivity which is exacerbated by resolution changes.”