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Galaxy Alignments: Theory, Modelling & Simulations

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An Erratum to this article was published on 12 November 2015

Abstract

The shapes of galaxies are not randomly oriented on the sky. During the galaxy formation and evolution process, environment has a strong influence, as tidal gravitational fields in the large-scale structure tend to align nearby galaxies. Additionally, events such as galaxy mergers affect the relative alignments of both the shapes and angular momenta of galaxies throughout their history. These “intrinsic galaxy alignments” are known to exist, but are still poorly understood. This review will offer a pedagogical introduction to the current theories that describe intrinsic galaxy alignments, including the apparent difference in intrinsic alignment between early- and late-type galaxies and the latest efforts to model them analytically. It will then describe the ongoing efforts to simulate intrinsic alignments using both \(N\)-body and hydrodynamic simulations. Due to the relative youth of this field, there is still much to be done to understand intrinsic galaxy alignments and this review summarises the current state of the field, providing a solid basis for future work.

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Notes

  1. However, there are methods to measure dark matter halo ellipticities through observations, e.g. galaxy-galaxy lensing (e.g. Natarajan and Refregier 2000; Hoekstra et al. 2004; Mandelbaum et al. 2006a; Parker et al. 2007; van Uitert et al. 2012; Schrabback et al. 2015).

  2. E.g. the Kilo Degree Survey, KiDS: http://kids.strw.leidenuniv.nl; the Dark Energy Survey, DES: http://www.darkenergysurvey.org; the Hyper Suprime-Cam Survey, HSC: http://www.naoj.org/Projects/HSC; Euclid: http://www.euclid-ec.org and http://sci.esa.int/euclid; the Large Synoptic Survey Telescope, LSST: http://www.lsst.org/lsst; and the Wide Field InfraRed Suvery Telescope, WFIRST: http://wfirst.gsfc.nasa.gov.

  3. The term gravitational shear could be misleading here since the intrinsic ellipticity, \(\epsilon^{\mathrm{S}}\), is also influenced by (tidal) gravitational effects as shown in this section. However, the term gravitational shear for the effects of gravitational lensing has been in use for a long time and it would be unwise to adopt a different convention here. Throughout, the term gravitational shear is synonymous with gravitational lensing.

  4. If a two-component ellipticity seems unfamiliar, it is worth considering that the standard geometric representation of an ellipse using an axis ratio and a position angle also requires two numbers.

  5. Note that the terms satellite and satellite distribution are interchangeable with subhalo and subhalo distribution when measuring dark matter alignments.

  6. The terms “sheet” and “wall” are used interchangeably throughout the literature and this review.

  7. This may not be true in the presence of photometric redshift errors, where the relative positions of galaxies along the line of sight may be confused.

  8. Note that Hirata and Seljak (2010) is an updated version of the original Hirata and Seljak (2004) paper that fixes an error in a conversion factor that propagated through several equations.

  9. Navarro et al. (1996) fitted a universal density profile to dark matter haloes in \(N\)-body simulations. This profile is now known as the NFW profile.

  10. Note that some studies consider overdensities relative to the underlying matter density, rather than the critical density. Such overdensities can be easily scaled, due to the fact that \(\varOmega_{M}\) is the ratio between the mean matter density and the critical density.

  11. This equation is actually the quadrupole tensor of the mass distribution, but as it is regularly referred to as the moment of inertia tensor in the literature, this is the convention followed throughout this review.

  12. Note that the subscript ‘H’ in this alignment is the cluster cosmic web element and the ‘S’ represents the galaxy-sized and smaller halo substructure within the cluster.

  13. While this simulation includes hydrodynamics, the results are focused on dark matter haloes and appear to be independent of the baryons, hence its inclusion in this section.

  14. Note that the terms “hydrodynamic” and “gasdynamic” are used interchangeably in the literature, although hydrodynamic is adopted in this review.

  15. There are measurements in the literature that use as few as 20 particles. The results in this paper suggest that those results should be approached with caution.

  16. Some of these studies use a halo occupation distribution (HOD; e.g. Berlind and Weinberg 2002) approach to reproduce observed galaxy properties. This is a more statistical approach to matching galaxy properties than semi-analytic modelling.

  17. The large box size would account for the large scales that should be accounted for in studies of the large-scale structure and the high mass resolution would resolve the shapes and details of individual galaxies with high precision.

  18. Some differences between the hydrodynamic and dark matter-only simulation haloes should be expected and may arise if the halo finders split a structure into different haloes or some haloes fall below the minimum particle threshold between the realisations etc.

  19. In order to match ellipticity distributions, hydrodynamic simulations would need to resolve the thickness of the discs accurately, which would require resolving interstellar medium processes accurately. It is not clear that this final point will be possible in the simulations, so this task may have to remain on the “wish” list.

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Acknowledgements

We acknowledge the support of the International Space Science Institute Bern for two workshops at which this work was conceived. We would like to thank Henk Hoekstra for very useful discussions and for his comments on drafts of this work. We would also like to thank the anonymous referee for their careful reading and detailed suggestions that helped to improve the clarity of this review. We are grateful to J. Blazek, S. Singh and M. Velliscig for sharing their data and figures. We would also like to thank the participants of the Lorentz workshop: Extracting information from weak lensing: Small scales = Big problem, for their useful discussions and insights.

A. Kiessling was supported in part by JPL, run under a contract by Caltech for NASA. A. Kiessling was also supported in part by NASA ROSES 13-ATP13-0019 and NASA ROSES 12-EUCLID12-0004. M. Cacciato was supported by the Netherlands organisation for Scientific Research (NWO) Vidi grant 639.042.814. B. Joachimi acknowledges support by an STFC Ernest Rutherford Fellowship, grant reference ST/J004421/1. T.D. Kitching is supported by a Royal Society URF. A. Leonard acknowledges the support of the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 624151. R. Mandelbaum acknowledges the support of NASA ROSES 12-EUCLID12-0004. C. Sifón acknowledges support from the European Research Council under FP7 grant number 279396. M.L. Brown is supported by the European Research Council (EC FP7 grant number 280127) and by a STFC Advanced/Halliday fellowship (grant number ST/I005129/1).

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  1. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA

    Alina Kiessling

  2. Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA, Leiden, The Netherlands

    Marcello Cacciato & Cristóbal Sifón

  3. Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK

    Benjamin Joachimi, Donnacha Kirk & Adrienne Leonard

  4. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK

    Thomas D. Kitching

  5. Department of Physics, McWilliams Center for Cosmology, Carnegie Mellon University, Pittsburgh, PA, 15213, USA

    Rachel Mandelbaum

  6. Zentrum für Astronomie der Universität Heidelberg, Astronomisches Recheninstitut, Philosophenweg 12, 69120, Heidelberg, Germany

    Björn Malte Schäfer

  7. Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL, UK

    Michael L. Brown

  8. Laboratoire d’astrophysique (LASTRO), Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290, Versoix, Switzerland

    Anais Rassat

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  1. Alina Kiessling
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Kiessling, A., Cacciato, M., Joachimi, B. et al. Galaxy Alignments: Theory, Modelling & Simulations. Space Sci Rev 193, 67–136 (2015). https://doi.org/10.1007/s11214-015-0203-6

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