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Globular Cluster Systems and Galaxy Formation

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Abstract

Globular clusters (GCs) are compact, gravitationally bound systems of up to ∼1 million stars. The GCs in the Milky Way contain some of the oldest stars known, and provide important clues to the early formation and continuing evolution of our Galaxy. More generally, GCs are associated with galaxies of all types and masses, from low-mass dwarf galaxies to the most massive early-type galaxies which lie in the centres of massive galaxy clusters. GC systems show several properties which connect tightly with properties of their host galaxies. For example, the total mass of GCs in a system scales linearly with the dark matter halo mass of its host galaxy. Numerical simulations are at the point of being able to resolve globular cluster formation within a cosmological framework. Therefore, GCs link a range of scales, from the physics of star formation in turbulent gas clouds, to the large-scale properties of galaxies and their dark matter. In this chapter we review some of the basic observational approaches for GC systems, some of their key observational properties, and describe how GCs provide important clues to the formation of their parent galaxies.

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Notes

  1. 1.

    This is often called the “baryonic” component, since stars and gas are composed of protons and neutrons which are baryons (three quarks). The poor old electrons—which are leptons—are ignored in this terminology!

  2. 2.

    This qualifier is important to remember. Although GCs seem to have no dark matter now, this does not necessarily imply that they never had dark matter. Tidal processes could remove the vast majority of dark matter from a GC orbiting in a Milky Way-like potential over a Hubble time.

  3. 3.

    Stellar systems of masses at, or below that of GCs are observed, and they typically have very high mass-to-light ratios (M∕L V > 100) implying high dark matter fractions. However, these are generally low-concentration, low-surface brightness objects which are typically larger (r h > 50 pc) than GCs and are referred to as “ultra-faint dwarf” galaxies (UFDs; [13]).

  4. 4.

    The subject of photometry is a chapter in itself. Suffice to say that the standard techniques are reasonably straightforward, although a number of careful steps are required to achieve precise measurements.

  5. 5.

    The apparent movement on the sky of an object compared to a fixed background.

  6. 6.

    Parallax is the apparent change of position on the sky of an object when viewed from two different positions along a given baseline. If the length of the baseline is known, by measuring the parallax angle (i.e., how much the star appears to move), the distance to the star can be determined.

  7. 7.

    Magnesium and iron are produced in short-lived, massive stars which explode as type-II supernovae, whereas iron is produced in longer-lived, lower mass stars which is released in type Ia supernova explosions. Therefore [Mg/Fe] can be used as a chemical clock—generally the higher the ratio [Mg/Fe], the shorter the timescale of star formation since low-mass stars have not had time to pollute the interstellar medium.

  8. 8.

    Atomic diffusion is the collective term for processes that change the mixture of atmospheric abundances in stars due to gravity or radiation pressure. For example, heavier elements (e.g., Fe) tend to sink over long time-scales thereby lowering the observed surface abundance of the star.

  9. 9.

    https://physwww.mcmaster.ca/~harris/mwgc.dat.

  10. 10.

    Formed “in-place”. Astronomers like resorting to latin on occasion.

  11. 11.

    This is consistent with what we know about galaxy metallicities. Galaxies follow a stellar mass–metallicity relation in that more massive galaxies are, on average, more metal-rich. This is a consequence of the fact that more massive galaxies have more stars to form metals via nucleosynthesis, and are also better able to hold onto their gas “recycled” from star formation due to their deeper potential wells.

  12. 12.

    Here the term “field” refers to stars not in star clusters.

  13. 13.

    Not to be confused with “ultra-faint” galaxies which have smaller sizes and significantly lower stellar masses.

  14. 14.

    I.e., a model that describes relationships between observations, but does not stem directly from physical theory.

  15. 15.

    In the case of the SAM used by Beasley et al. [128], the main calibrations were to match the galaxy luminosity function and Tully-Fisher relations.

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Acknowledgements

The author thanks Núria Salvador Rusiñol for proof-reading and useful feedback on the text. This work has been supported through the RAVET project by the grant AYA2016-77237-C3-1-P from the Spanish Ministry of Science, Innovation and Universities (MCIU) and through the IAC project TRACES which is partially supported through the state budget and the regional budget of the Consejería de Economía, Industria, Comercio y Conocimiento of the Canary Islands Autonomous Community.

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    Michael A. Beasley

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    Petr Kabáth

  2. Instituto de Astrofisica de Canarias, La Laguna, Spain

    David Jones

  3. Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic

    Marek Skarka

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Beasley, M.A. (2020). Globular Cluster Systems and Galaxy Formation. In: Kabáth, P., Jones, D., Skarka, M. (eds) Reviews in Frontiers of Modern Astrophysics. Springer, Cham. https://doi.org/10.1007/978-3-030-38509-5_9

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