Abstract
The role of disc instabilities, such as bars and spiral arms, and the associated resonances, in growing bulges in the inner regions of disc galaxies have long been studied in the low-redshift nearby Universe. There it has long been probed observationally, in particular through peanut-shaped bulges (Chap. 14). This secular growth of bulges in modern disc galaxies is driven by weak, non-axisymmetric instabilities: it mostly produces pseudobulges at slow rates and with long star-formation timescales. Disc instabilities at high redshift (z > 1) in moderate-mass to massive galaxies (1010 to a few 1011 M⊙ of stars) are very different from those found in modern spiral galaxies. High-redshift discs are globally unstable and fragment into giant clumps containing 108−9 M⊙ of gas and stars each, which results in highly irregular galaxy morphologies. The clumps and other features associated to the violent instability drive disc evolution and bulge growth through various mechanisms on short timescales. The giant clumps can migrate inward and coalesce into the bulge in a few 108 years. The instability in the very turbulent media drives intense gas inflows toward the bulge and nuclear region. Thick discs and supermassive black holes can grow concurrently as a result of the violent instability. This chapter reviews the properties of high-redshift disc instabilities, the evolution of giant clumps and other features associated to the instability, and the resulting growth of bulges and associated sub-galactic components.
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Notes
- 1.
This estimate is simply based on the mass function of galaxies and assuming a random geometrical distribution of satellites within the virial radius.
- 2.
With a kinematics that could become preferentially consistent with that of the host galaxy disc through gravity torques and dynamical friction within one galactic dynamical time, i.e. about 100 Myr.
- 3.
Although the Toomre Q parameter is strictly meaningful only in an axisymmetric disc before strong perturbations arise. Note also that in a thick disc the instability limit is about 0.7 rather than Q < 1 (Behrendt et al. 2014, and references therein).
- 4.
Although these total gas fractions seem to remain lower than the observed molecular gas fractions, especially if these are the most gas-rich galaxies in simulated samples.
- 5.
Note that shorter migration timescales in cosmological simulations may also arise if the galaxies are too compact, or have too concentrated dark matter halos enhancing the dynamical friction process. Actually, the cosmological simulations of redshift two galaxies tend to have too low gas fraction because of some largely unexplained early consumption of the gas (e.g., Ceverino et al. (2012) and Kereš et al. (2012), with typical gas fractions at best around 30 % at z = 2 even counting all the cold gas within a large radius).
- 6.
The presence of large amounts of gas between the giant clumps cannot be mapped spatially in CO surveys yet, but is predicted in the idealized and cosmological simulations of gas-rich unstable discs cited above, and confirmed by two observational arguments: (1) the emission from young stars in the ultraviolet contains a widespread component behind the giant clumps, tracing relatively dense gas (Elmegreen and Elmegreen 2005) and (2) the CO spectral line energy distribution has two components, a high-excitation one attributable to dense clumps, and a low-excitation one corresponding to lower-density, large-scale background gas reservoirs (Daddi et al. 2015; Bournaud et al. 2015).
- 7.
Note that the clumps remain gas-rich as they re-accrete gas and lose aged stars, which compensates for the gas depletion through star formation and gaseous outflows.
- 8.
Resolving the giant clumps requires a resolution that is typically too costly to maintain down to redshift zero (Ceverino et al. 2010).
- 9.
After applying Gaussian time smoothing of FWHM 2 Myr to erase fluctuations related to the numerical sampling of star formation.
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Acknowledgements
I am grateful to Anna Cibinel, Jared Gabor, Marie Martig, Valentin Perret and Florent Renaud for providing some of the figures and material used in this review, and to Avishai Dekel and Bruce Elmegreen for triggering many new studies on the instability of high-redshift galaxies and the associated growth of bulges. The simulations shown in Fig. 13.7 were carried out on the GENCI computing resources and TGCC/Curie, under allocation GENCI-2015-04-2192.
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Bournaud, F. (2016). Bulge Growth Through Disc Instabilities in High-Redshift Galaxies. In: Laurikainen, E., Peletier, R., Gadotti, D. (eds) Galactic Bulges. Astrophysics and Space Science Library, vol 418. Springer, Cham. https://doi.org/10.1007/978-3-319-19378-6_13
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