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Tides in Colliding Galaxies

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Tides in Astronomy and Astrophysics

Part of the book series: Lecture Notes in Physics ((LNP,volume 861))

Abstract

Long tails and streams of stars are the most noticeable traces of galaxy collisions. However, their tidal origin was recognized only less than 50 years ago and more than 10 years after their first observations. This review describes how the idea of galactic tides has emerged thanks to advances in numerical simulations, from the first simulations that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic/molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and the content of present-day galaxies, including their dark components, and explains how they may be used to probe the past evolution of galaxies and the history of their mass assembly. On-going deep wide-field surveys disclose many new low-surface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

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Notes

  1. 1.

    According to Arp [8], the same mechanism would account for the creation of spiral arms in rotating galaxies.

  2. 2.

    Note that the position of some of the galaxies in the sequence has been recently discussed thanks to new numerical models (see e.g. [126]).

  3. 3.

    http://galmer.obspm.fr/.

  4. 4.

    http://www.nrao.edu/astrores/HIrogues/.

  5. 5.

    Though, a stellar component has been found associated to the Magellanic Bridge.

  6. 6.

    Wetzstein et al. [238] claimed that the clumps formed in N-body models that do not include gas are numerical artifacts.

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Acknowledgements

First of all, we express our gratitude to the two main organizers of the school, Jean Souchay and Stéphane Mathis. We not only enjoyed the marvelous premises—Cargèse in Corsica—but also the very stimulating discussions that took place between experts in terrestrial, planetary, stellar and galactic tides. We are very grateful to Frédéric Bournaud for daily discussions on galaxy collisions and numerical simulations. Many thanks as well to Pierre-Emmanuel Belles for his careful reading of the manuscript. We finally wish to thank all our collaborators and colleagues for their crucial contributions to the various works presented here.

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  1. AIM Paris-Saclay, CNRS/INSU, CEA/Irfu, Service d’Astrophysique, Université Paris-Diderot, Orme des Merisiers, 91191, Gif sur Yvette cedex, France

    Pierre-Alain Duc

  2. Observatoire de Strasbourg, CNRS UMR 7550 and AIM Paris-Saclay, CEA/Irfu, CNRS/INSU, Service d’astrophysique, Université Paris-Diderot, Orme des Merisiers, 91191, Gif sur Yvette cedex, France

    Florent Renaud

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  1. Dépt. Astronomie Fondamental, Observatoire de Paris, avenue de l Observatoire 61, Paris, 75014, France

    Jean Souchay

  2. IRFU/SAP Centre de Saclay, Laboratoire AIM Paris Saclay Diderot, Bat. 709, Gif-sur-Yvette, 91191, France

    Stéphane Mathis

  3. University of Cambridge, Trinity Hall, Cambridge, CB2 1TJ, United Kingdom

    Tadashi Tokieda

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Duc, PA., Renaud, F. (2013). Tides in Colliding Galaxies. In: Souchay, J., Mathis, S., Tokieda, T. (eds) Tides in Astronomy and Astrophysics. Lecture Notes in Physics, vol 861. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-32961-6_9

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