Journal Article

Testing subhalo abundance matching in cosmological smoothed particle hydrodynamics simulations

Vimal Simha, David H. Weinberg, Romeel Davé, Mark Fardal, Neal Katz and Benjamin D. Oppenheimer

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 423, issue 4, pages 3458-3473
Published in print July 2012 | ISSN: 0035-8711
Published online July 2012 | e-ISSN: 1365-2966 | DOI:
Testing subhalo abundance matching in cosmological smoothed particle hydrodynamics simulations

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Subhalo abundance matching (also known as SHAM) is a technique for populating simulated dark matter distributions with galaxies, assuming a monotonic relation between a galaxy’s stellar mass or luminosity and the mass of its parent dark matter halo or subhalo. We examine the accuracy of SHAM in two cosmological smoothed particle hydrodynamics (SPH) simulations, one of which includes momentum-driven galactic winds. The SPH simulations indeed show a nearly monotonic relation between stellar mass and halo mass provided that, for satellite galaxies, we use the mass of the subhalo at the epoch zsat when it became a satellite. In each simulation, the median relation for central and satellite galaxies is nearly identical, though a somewhat larger fraction of satellites is outliers because of stellar mass loss. SHAM-assigned masses (at z= 0–2), luminosities (R-band at z= 0) or star formation rates (at z= 2) have a 68 per cent scatter of 0.09–0.15 dex relative to the true simulation values. When we apply SHAM to the subhalo population of a collisionless N-body simulation with the same initial conditions as the SPH runs, we find generally good agreement for the halo occupation distributions and halo radial profiles of galaxy samples defined by thresholds in stellar mass. However, because a small fraction of SPH galaxies suffer severe stellar mass loss after becoming satellites, SHAM slightly overpopulates high-mass haloes; this effect is more significant for the wind simulation, which produces galaxies that are less massive and more fragile. SHAM recovers the two-point correlation function of the SPH galaxies in the no-wind simulation to better than 10 per cent at scales 0.1 < r < 10 h−1 Mpc. For the wind simulation, agreement is better than 15 per cent at r > 2 h−1 Mpc, but overpopulation of massive haloes increases the correlation function by a factor of ∼2.5 on small scales. The discrepancy in the wind simulation is greatly reduced if we raise the stellar mass threshold from 6 × 109 to 3 × 1010 M; in this case SHAM overpredicts the SPH galaxy correlation function by ∼20 per cent at r < 1 h−1 Mpc but agrees well with SPH clustering at larger scales.

Keywords: methods: numerical; galaxies: evolution; galaxies: formation

Journal Article.  9974 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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