Forming disc galaxies in  CDM simulations

Governato, Fabio; Willman, Beth; Mayer, Lucio; Brooks, Alyson; Stinson, Gregory S.; Valenzuela, O.; Wadsley, James; Quinn, Thomas

doi:10.1111/j.1365-2966.2006.11266.x

Cited by 607 publications

(810 citation statements)

References 132 publications

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“…Khochfar & Burkert 2003;Naab, Khochfar & Burkert 2006), while gas-rich major mergers have been shown to produce disc galaxies (e.g. Springel & Hernquist 2005;Robertson et al 2006;Governato et al 2007). Both of these ideas seem to be manifested statistically in the different panels of Fig.…”

Section: Resultsmentioning

confidence: 99%

The role of mergers and halo spin in shaping galaxy morphology

Rodríguez-Gómez

Sales

Genel

et al. 2017

Monthly Notices of the Royal Astronomical Society

182

157

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Mergers and the spin of the dark matter halo are factors traditionally believed to determine the morphology of galaxies within a ΛCDM cosmology. We study this hypothesis by considering approximately 18,000 central galaxies at z = 0 with stellar masses M * = 10 9 -10 12 M selected from the Illustris cosmological hydrodynamic simulation. The fraction of accreted stars -which measures the importance of massive, recent and dry mergers -increases steeply with galaxy stellar mass, from less than 5 per cent in dwarfs to 80 per cent in the most massive objects, and the impact of mergers on galaxy morphology increases accordingly. For galaxies with M * 10 11 M , mergers have the expected effect: if gas-poor they promote the formation of spheroidal galaxies, whereas gas-rich mergers favour the formation and survivability of massive discs. This trend, however, breaks at lower masses. For objects with M * 10 11 M , mergers do not seem to play any significant role in determining the morphology, with accreted stellar fractions and mean merger gas fractions that are indistinguishable between spheroidal and disc-dominated galaxies. On the other hand, halo spin correlates with morphology primarily in the least massive objects in the sample (M * 10 10 M ), but only weakly for galaxies above that mass. Our results support a scenario where (1) mergers play a dominant role in shaping the morphology of massive galaxies, (2) halo spin is important for the morphology of dwarfs, and (3) the morphology of medium-sized galaxies -including the Milky Way -shows little dependence on galaxy assembly history or halo spin, at least when these two factors are considered individually.

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Section: Resultsmentioning

confidence: 99%

The role of mergers and halo spin in shaping galaxy morphology

Rodríguez-Gómez

Sales

Genel

et al. 2017

Monthly Notices of the Royal Astronomical Society

182

157

View full text Add to dashboard Cite

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“…In fact, to produce disk-dominated galaxies numerical simulations of spiral galaxies set in a cosmological context have had to select to model systems in underdense environments, a reflection on what is now understood to relate to the details of the angular momentum accretion history (cf. Governato et al 2007;Sales et al 2012). Therefore, the importance of environment in the genesis of these galaxies is hardwired into detailed physics-oriented models, in opposition to what is often done in statistically-oriented theoretical treatments.…”

Section: Introductionmentioning

confidence: 99%

Giant disk galaxies : Where environment trumps mass in galaxy evolution

Courtois

2015

Proc. IAU

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We identify some of the most HI massive and fastest rotating disk galaxies in the local universe with the aim of probing the processes that drive the formation of these extreme disk galaxies. By combining data from the Cosmic Flows project, which has consistently reanalyzed archival galaxy HI profiles, and 3.6µm photometry obtained with the Spitzer Space Telescope, with which we can measure stellar mass, we use the baryonic Tully-Fisher (BTF) relationship to explore whether these massive galaxies are distinct. We discuss several results, but the most striking is the systematic offset of the HI-massive sample above the BTF. These galaxies have both more gas and more stars in their disks than the typical disk galaxy of similar rotational velocity. The "condensed" baryon fraction, f C , the fraction of the baryons in a dark matter halo that settle either as cold gas or stars into the disk, is twice as high in the HImassive sample than typical, and almost reaches the universal baryon fraction in some cases, suggesting that the most extreme of these galaxies have little in the way of a hot baryonic component or cold baryons distributed well outside the disk. In contrast, the star formation efficiency, measured as the ratio of the mass in stars to that in both stars and gas, shows no difference between the HI-massive sample and the typical disk galaxies. We conclude that the star formation efficiency is driven by an internal, self-regulating process, while f C is affected by external factors. Neither the morphology nor the star formation rate of these galaxies is primarily determined by either their dark or stellar mass. We also found that the most massive HI detected galaxies are located preferentially in filaments. We present the first evidence of an environmental effect on galaxy evolution using a dynamical definition of a filament.

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“…Further discussion of how star formation is treated in semi-analytical models is given in the next section. A key limitation on the use of gas dynamics simulations to model galaxy clustering is their computational expense and the requirement for 'sufficient' resolution in mass and length scales (Governato et al 2007). …”

Section: Physical Modelling Of Galaxy Formationmentioning

confidence: 99%

Luminosity Bias: From Haloes to Galaxies

Baugh

2013

Publ. Astron. Soc. Aust.

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Large surveys of the local Universe have shown that galaxies with different intrinsic properties such as colour, luminosity and morphological type display a range of clustering amplitudes. Galaxies are therefore not faithful tracers of the underlying matter distribution. This modulation of galaxy clustering, called bias, contains information about the physics behind galaxy formation. It is also a systematic to be overcome before the large-scale structure of the Universe can be used as a cosmological probe. Two types of approaches have been developed to model the clustering of galaxies. The first class is empirical and filters or weights the distribution of dark matter to reproduce the measured clustering. In the second approach, an attempt is made to model the physics which governs the fate of baryons in order to predict the number of galaxies in dark matter haloes. I will review the development of both approaches and summarise what we have learnt about galaxy bias.

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Forming disc galaxies in CDM simulations

Cited by 607 publications

References 132 publications

The role of mergers and halo spin in shaping galaxy morphology

The role of mergers and halo spin in shaping galaxy morphology

Giant disk galaxies : Where environment trumps mass in galaxy evolution

Luminosity Bias: From Haloes to Galaxies

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