SubHaloes going Notts: The SubHalo-Finder Comparison Project

ONIONS, JULIAN; KNEBE, ALEXANDER; PEARCE, FRAZER R. ; MULDREW, STUART I.; LUX, HANNI; KNOLLMANN, STEFFEN R. ; ASCASIBAR, YAGO ; BEHROOZI, PETER ; ELAHI, PASCAL; HAN, JIAXIN ; MACIEJEWSKI, MICHAL ; MERCHAN, MANUEL E.; NEYRINCK, MARK ; RUIZ, ANDRÉS NICOLÁS; SGRÓ, MARIO AGUSTÍN; SPRINGEL, VOLKER; TWEED, DYLAN

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Lugar: Londres; Año: 2012 vol. 423 p. 1200 - 1214

0035-8711

We present a detailed comparison of the substructure properties of a single Milky Way sized dark matter halo from the Aquarius suite at five different resolutions, as identified by a variety of different (sub)halo finders for simulations of cosmic structure formation. These finders span a wide range of techniques and methodologies to extract and quantify substructures within a larger non-homogeneous background density (e.g. a host halo). This includes real-space-, phase-space-, velocity-space- and time-space-based finders, as well as finders employing a Voronoi tessellation, Friends-of-Friends techniques or refined meshes as the starting point for locating substructure. A common post-processing pipeline was used to uniformly analyse the particle lists provided by each finder. We extract quantitative and comparable measures for the subhaloes, primarily focusing on mass and the peak of the rotation curve for this particular study. We find that all of the finders agree extremely well in the presence and location of substructure and even for properties relating to the inner part of the subhalo (e.g. the maximum value of the rotation curve). For properties that rely on particles near the outer edge of the subhalo the agreement is at around the 20 per cent level. We find that the basic properties (mass and maximum circular velocity) of a subhalo can be reliably recovered if the subhalo contains more than 100 particles although its presence can be reliably inferred for a lower particle number limit of 20. We finally note that the logarithmic slope of the subhalo cumulative number count is remarkably consistent and