Abstract
The Milky Way bulge offers a unique opportunity to investigate in detail the role that different processes such as dynamical instabilities, hierarchical merging, and dissipational collapse may have played in the history of the Galaxy formation and evolution based on its resolved stellar population properties. Large observation programs and surveys of the bulge are providing for the first time a look into the global view of the Milky Way bulge that can be compared with the bulges of other galaxies, and be used as a template for detailed comparison with models. The Milky Way has been shown to have a boxy/peanut (B/P) bulge and recent evidence seems to suggest the presence of an additional spheroidal component. In this review we summarize the global chemical abundances, kinematics and structural properties that allow us to disentangle these multiple components and provide constraints to understand their origin. The investigation of both detailed and global properties of the bulge now provide us with the opportunity to characterize the bulge as observed in models, and to place the mixed component bulge scenario in the general context of external galaxies. When writing this review, we considered the perspectives of researchers working with the Milky Way and researchers working with external galaxies. It is an attempt to approach both communities for a fruitful exchange of ideas.
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Notes
- 1.
To be complete, we must mention the pioneering work of Eggen et al. (1962), who suggested that the first stage in the formation of the Milky Way was a fast ( < 108 yr) monolithic collapse of a single massive gas cloud, which could have formed both the Galaxy stellar halo and the bulge. This scenario was later replaced with the merger-driven scenario mostly due to the widely varying ages of different components of the Galaxy and the hierarchical nature of LCDM theory. We refer the reader to Brooks and Christensen (this volume) for a review on merger-driven bulge formation. In the last decade or two, the secular evolution scenario has slowly, but unequivocally, gained terrain over the merger-driven scenario. Another bulge building scenario we do not discuss here has recently been put forward by e.g. Elmegreen et al. (2008, – see review by Gadotti 2012). In this scenario, bulges form by the coalescence of giant clumps in primordial discs. This scenario can explain the formation of spheroids but does not account for boxy/peanuts.
- 2.
Editorial comment: barlenses are recognized from direct images – without any assumption of massive classical bulges first subtracted from the images, as done in Fig. 9.8. By definition barlenses are not inner discs embedded in classical bulges.
- 3.
Gas outside corotation receives angular momentum from the bar, and other factors govern the gas infall rate at these outer radii, such as dynamical effects induced by spiral arms and the dissipative nature of the ISM. At these distances the infall of gas no longer occurs in a dynamical time scale.
- 4.
Some simulations (Kraljic et al. 2012) have reported the early formation of bars, at redshifts above 1. However, these bars are short-lived. In these simulations, bars formed at ≤ 1 generally persist down to z = 0.
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Acknowledgements
We are grateful to an anonymous referee for many useful comments. We warmly thank Istvan Dekany for kindly providing us the table of individual distances to the RR-lyrae that we used to produce Fig. 9.1.
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Gonzalez, O.A., Gadotti, D. (2016). The Milky Way Bulge: Observed Properties and a Comparison to External 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_9
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