The mass dependence of dark matter halo alignments with large-scale structure. Issue 1 (3rd November 2017)

• Record Type: Journal Article
• Authors: Piras, Davide; Joachimi, Benjamin; Schäfer, Björn Malte; Bonamigo, Mario; Hilbert, Stefan; van Uitert, Edo
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 474:Issue 1(2018)
• Page Start: 1165
• Page End: 1175
• Publication Date: 2017-11-03
• Subjects: galaxies: haloes -- dark matter -- large-scale structure of Universe; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stx2846
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: Tidal gravitational forces can modify the shape of galaxies and clusters of galaxies, thus correlating their orientation with the surrounding matter density field. We study the dependence of this phenomenon, known as intrinsic alignment (IA), on the mass of the dark matter haloes that host these bright structures, analysing the Millennium and Millennium-XXL N -body simulations. We closely follow the observational approach, measuring the halo position–halo shape alignment and subsequently dividing out the dependence on halo bias. We derive a theoretical scaling of the IA amplitude with mass in a dark matter universe, and predict a power law with slope βM in the range 1/3 to 1/2, depending on mass scale. We find that the simulation data agree with each other and with the theoretical prediction remarkably well over three orders of magnitude in mass, with the joint analysis yielding an estimate of $\beta _{\mathrm{M}} = 0.36^{+0.01}_{-0.01}$ . This result does not depend on redshift or on the details of the halo shape measurement. The analysis is repeated on observational data, obtaining a significantly higher value, $\beta _{\mathrm{M}} = 0.56^{+0.05}_{-0.05}$ . There are also small but significant deviations from our simple model in the simulation signals at both the high- and low-mass end. We discuss possible reasons for these discrepancies, and argue that they can be attributed to physical processes not captured in the model or in the dark matter-only simulations.