Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-27T11:07:34.196Z Has data issue: false hasContentIssue false
  • English
  • Français

How the cosmic web induces intrinsic alignments of galaxies

Published online by Cambridge University Press:  12 October 2016

S. Codis ,
Y. Dubois ,
C. Pichon ,
J. Devriendt  and
A. Slyz
S. Codis*
Affiliation:
Sorbonne Universités, UPMC Univ. Paris 06 & CNRS, UMR7095, Institut d'Astrophysique de Paris, 98 bis Boulevard Arago, 75014, Paris, France
Y. Dubois
Affiliation:
Sorbonne Universités, UPMC Univ. Paris 06 & CNRS, UMR7095, Institut d'Astrophysique de Paris, 98 bis Boulevard Arago, 75014, Paris, France
C. Pichon
Affiliation:
Sorbonne Universités, UPMC Univ. Paris 06 & CNRS, UMR7095, Institut d'Astrophysique de Paris, 98 bis Boulevard Arago, 75014, Paris, France
J. Devriendt
Affiliation:
Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH
A. Slyz
Affiliation:
Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH
*
†Email: codis@iap.fr
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Intrinsic alignments are believed to be a major source of systematics for future generation of weak gravitational lensing surveys like Euclid or LSST. Direct measurements of the alignment of the projected light distribution of galaxies in wide field imaging data seem to agree on a contamination at a level of a few per cent of the shear correlation functions, although the amplitude of the effect depends on the population of galaxies considered. Given this dependency, it is difficult to use dark matter-only simulations as the sole resource to predict and control intrinsic alignments. We report here estimates on the level of intrinsic alignment in the cosmological hydrodynamical simulation Horizon-AGN that could be a major source of systematic errors in weak gravitational lensing measurements. In particular, assuming that the spin of galaxies is a good proxy for their ellipticity, we show how those spins are spatially correlated and how they couple to the tidal field in which they are embedded. We will also present theoretical calculations that illustrate and qualitatively explain the observed signals.

Keywords

large-scale structure of universegravitational lensingmethod: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 437 - 442
Copyright
Copyright © International Astronomical Union 2016 

References

Aragòn-Calvo, M. A. et al. 2007, ApJ Let., 655, L5 CrossRefGoogle Scholar
Blazek, J., Mandelbaum, R., Seljak, U., & Nakajima, R. 2012, JCAP, 5, 41 Google Scholar
Catelan, P., Kamionkowski, M., & Blandford, R. D. 2001, MNRAS, 320, L7 CrossRefGoogle Scholar
Codis, S. et al. 2012 MNRAS, 427, 3320 CrossRefGoogle Scholar
Codis, S. et al. 2014, ArXiv e-prints Google Scholar
Croft, R. A. C. & Metzler, C. A. 2000, ApJ, 545, 561 Google Scholar
Dubois, Y. et al. 2014, ArXiv e-prints Google Scholar
Hahn, O., Teyssier, R., & Carollo, C. M. 2010, MNRAS, 405, 274 Google Scholar
Heavens, A., Refregier, A., & Heymans, C. 2000, MNRAS, 319, 649 Google Scholar
Hirata, C. M. & Seljak, U. 2004, Phys. Rev. D, 70, 063526 CrossRefGoogle Scholar
Joachimi, B. et al. 2013, MNRAS, 431, 477 Google Scholar
Joachimi, B. et al. 2013, MNRAS, 436, 819 Google Scholar
Lee, J. & Pen, U.-L. 2001, ApJ, 555, 106 Google Scholar
Paz, D. J., Stasyszyn, F., & Padilla, N. D. 2008, MNRAS, 389, 1127P Google Scholar
Pogosyan, D., Bond, J. R., & Kofman, L. 1998, JRASC, 92, 313 Google Scholar
Schneider, M. D. & Bridle, S. 2010, MNRAS, 402, 2127 CrossRefGoogle Scholar
Teyssier, R. 2002, MNRAS, 402, 2127 Google Scholar