symfind : Addressing the Fragility of Subhalo Finders and Revealing the Durability of Subhalos

• Published in: The Astrophysical journal Vol. 970; no. 2; pp. 178 - 215
• Main Authors: Mansfield, Philip, Darragh-Ford, Elise, Wang, Yunchong, Nadler, Ethan O., Diemer, Benedikt, Wechsler, Risa H.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-08-2024; IOP Publishing
• Subjects: Astronomical models; ASTRONOMY AND ASTROPHYSICS; Computational methods; Disruption; Fragility; Galaxies; Galaxy dark matter halos; Galaxy distribution; Galaxy evolution; Radial distribution; Satellite tracking
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad4e33

Abstract A major question in ΛCDM is what this theory actually predicts for the properties of subhalo populations. Subhalos are difficult to accurately simulate and to find within simulations, and this propagates into uncertainty in theoretical predictions for satellite galaxies. We present Symfind , a new particle-tracking-based subhalo finder, and demonstrate that it can track subhalos to orders-of-magnitude lower masses than commonly used halo-finding tools, with a focus on Rockstar and consistent-trees . These longer survival times mean that at a fixed peak subhalo mass, we find ≈ 15%–40% more subhalos within the virial radius, R vir , and ≈35%–120% more subhalos within R vir /4 in the Symphony dark-matter-only simulation suite. More subhalos are found as the resolution is increased, in contrast to the Rockstar halo finder, which appears to be converged at smaller subhalo counts. We perform extensive numerical testing. In agreement with idealized simulations, we show that the v max , the maximum circular velocity, is systematically biased low until high resolutions ( n peak ≳ 3 × 10 4 ) are achieved, but that mass loss itself can be resolved at much more modest resolutions ( n peak ≳ 4 × 10 3 ). We show that Rockstar converges to false solutions for the mass function, radial distribution, and disruption masses of subhalos. We argue that our new method can trace resolved subhalos until the point of typical galaxy disruption without invoking post hoc orphan modeling. We outline a concrete set of steps for determining whether other subhalo finders meet the same criteria. We publicly release Symfind catalogs and particle data for the Symphony simulation suite at http://web.stanford.edu/group/gfc/symphony .