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Galaxy Alignments: An Overview

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Abstract

The alignments between galaxies, their underlying matter structures, and the cosmic web constitute vital ingredients for a comprehensive understanding of gravity, the nature of matter, and structure formation in the Universe. We provide an overview on the state of the art in the study of these alignment processes and their observational signatures, aimed at a non-specialist audience. The development of the field over the past one hundred years is briefly reviewed. We also discuss the impact of galaxy alignments on measurements of weak gravitational lensing, and discuss avenues for making theoretical and observational progress over the coming decade.

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Notes

  1. For an alternative formation hypothesis of spheroids involving cold gas streams, which is also closely linked to alignments with the surrounding dark matter and gas distribution, see e.g. Dekel et al. (2009).

  2. There is a subtlety involved in this approximation: for an individual galaxy, as Eq. (2) has been written, the expansion produces another term that is first order in the shear and proportional to \(g^{*} (\epsilon^{\mathrm{s}})^{2}\). However, since the relation is only considered in practice when averaging over large numbers of galaxies, this term (as well as all higher-order terms) becomes negligible if the intrinsic galaxy shapes are uncorrelated, or only weakly correlated, with the shear acting on them.

  3. The minus sign in these definitions ensures that the tangential alignment of shear around an object yields a positive signal. As a caveat, measurements of galaxy alignments tend to omit the minus sign in related statistics because in this situation the generally expected radial alignment is desired to yield a positive signal.

  4. Note that even for a non-tomographic cosmic shear analysis the overall redshift distribution of source galaxies is needed, although the requirements on accuracy and precision are less stringent in this case.

  5. An aside on nomenclature: galaxy alignments often receive the attribute ‘intrinsic’, especially if the physical alignments inherent to the galaxy population need to be distinguished from the apparent alignments on galaxy images induced by gravitational lensing (occasionally denoted as ‘extrinsic’; see Catelan et al. 2001). The term is also applied in a slightly different context to distinguish between the physical three-dimensional shape of a galaxy and its projected shape we observe on the sky (see Sandage et al. 1970 for the earliest occurence that we could trace).

  6. As we will discuss later, this model describes the observed galaxy alignments of bright early-type galaxies rather well, including its redshift evolution, albeit within large error bars (see also Kirk et al. 2015). This is somewhat puzzling because these galaxies are thought to have been created only recently (typically at redshifts below two) by major mergers, disruptive events that one would naively expect to erase all memory of alignment processes during galaxy formation. Hence, the assumptions underlying Eq. (14) may not be fully valid, but it could be that any modifications would primarily affect the amplitude of the predicted correlations, which is unconstrained by the model anyway.

  7. These sizes are difficult to relate to modern measurements such as the half-light radius, but it is enough to consider that these are 23 of the largest galaxies, in apparent size, that there are.

  8. http://aps.umn.edu/ .

  9. Efstathiou (2003) provides an excellent description of the conference proceedings in which Hoyle first proposed his theory. In fact, as highlighted by Efstathiou (2003), Hoyle makes a remarkably prescient statement in a later work (Hoyle 1966) that ‘‘the properties of the individual stars that make up the galaxies form the classical study of astrophysics, while the phenomena of galaxy formation touches on cosmology. In fact, the study of galaxies forms a bridge between conventional astronomy and astrophysics on the one hand, and cosmology on the other.’’

  10. Constraints on potential misalignments could in principle also be obtained from halo shape measurements via galaxy-galaxy lensing, stacking galaxies and orienting them with respect to their major axes (Hoekstra et al. 2004; Mandelbaum et al. 2006b; van Uitert et al. 2012; Adhikari et al. 2015).

  11. In hindsight this nomenclature is unfortunate, since Sastry’s observation took place before that of Holmberg.

  12. Including the Kilo Degree Survey, http://kids.strw.leidenuniv.nl ; the Dark Energy Survey, http://www.darkenergysurvey.org ; and the Hyper Suprime-Cam Survey, http://www.naoj.org/Projects/HSC .

  13. Including the Large Synoptic Survey Telescope (Abell et al. 2009), http://www.lsst.org/lsst ; the ESA Euclid satellite (Laureijs et al. 2011), http://sci.esa.int/euclid and http://www.euclid-ec.org ; and the NASA Wide-Field Infrared Survey Telescope (WFIRST, Spergel et al. 2013), http://wfirst.gsfc.nasa.gov .

  14. For instance with the Dark Energy Spectroscopic Instrument, http://desi.lbl.gov/cdr ; the Subaru Prime Focus Spectrograph http://sumire.ipmu.jp/pfs ; as well as Euclid and WFIRST.

  15. Such as PRIMUS, http://primus.ucsd.edu ; PAU, http://www.ieec.cat/project/pau-physics-of-the-accelerating-universe ; J-PAS, http://j-pas.org ; and (limited to bright galaxies) the proposed SPHEREx mission, http://spherex.caltech.edu , which employs filters with spatially varying response.

  16. https://www.skatelescope.org .

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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 thank E. Brunnstrom for an investigation into alignments in Palomar Sky Survey catalogues, and our referee, J. Blazek, for many helpful comments and stimulating discussions. We are grateful to B. Binggeli, C. Heymans, S. Singh, A. Slosar, A. Tenneti, and I. Trujillo for sharing their data.

BJ acknowledges support by an STFC Ernest Rutherford Fellowship, grant reference ST/J004421/1. MC was supported by the Netherlands organisation for Scientific Research (NWO) Vidi grant 639.042.814. TDK is supported by a Royal Society URF. AL acknowledges the support of the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 624151. RM acknowledges the support of NASA ROSES 12-EUCLID12-0004. CS and HH acknowledge support from the European Research Council under FP7 grant number 279396. AK was supported in part by JPL, run under a contract by Caltech for NASA. AK was also supported in part by NASA ROSES 13-ATP13-0019 and NASA ROSES 12-EUCLID12-0004.

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Authors and Affiliations

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

    Benjamin Joachimi, Adrienne Leonard & Donnacha Kirk

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

    Marcello Cacciato, Cristóbal Sifón & Henk Hoekstra

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

    Thomas D. Kitching

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

    Rachel Mandelbaum

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

    Björn Malte Schäfer

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

    Alina Kiessling

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

    Anais Rassat

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Joachimi, B., Cacciato, M., Kitching, T.D. et al. Galaxy Alignments: An Overview. Space Sci Rev 193, 1–65 (2015). https://doi.org/10.1007/s11214-015-0177-4

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