Subhaloes going Notts: The subhalo-finder comparison project
Author
Onions, Julian; Knebe, Alexander; Pearce, Frazer R.; Muldrew, Stuart I.; Lux, Hanni; Knollmann, Steffen R.; Ascasibar Sequeiros, Yago; Behroozi, Peter; Elahi, Pascal; Han, Jiaxin; MacIejewski, Michal; Merchán, Manuel E.; Neyrinck, Mark; Ruiz, Andrés N.; Sgró, Mario A.; Springel, Volker; Tweed, DylanEntity
UAM. Departamento de Física TeóricaPublisher
Royal Astronomical SocietyDate
2012-06-01Citation
10.1111/j.1365-2966.2012.20947.x
Monthly Notices of the Royal Astronomical Society 423.2 (2012): 1200-1214
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1111/j.1365-2966.2012.20947.xFunded by
AK is supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramon y Cajal programme as well as the grants AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009-00064 and CAM S2009/ESP-1496. HL acknowledges a fellowship from the European Commission’s Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). MNacknowledges support through Alex Szalay from the Gordon and Betty Moore Foundation. YA is also supported by the Ramon y Cajal programme as well as grant AYA 2010-21887-C04-03. JXH is supported by the European Commissions Framework Programme 7, through the Marie Curie Initial Training Network Cosmo-Comp (PITNGA-2009-238356) and partially supported by NSFC (10878001,11033006, 11121062) and the CAS/SAFEA International Partnership Programme for Creative Research Teams (KJCX2-YW-T23). VS acknowledges partial support by SFB 881 ‘The Milky Way System’ of the DFG. PE acknowledges financial support from the Chinese Academy of Sciences (CAS), from NSFC grants (No. 11121062, 10878001, 11033006), and by the CAS/SAFEA International Partnership Programme for Creative Research Teams (KJCX2-YW-T23).Project
Comunidad de Madrid. S2009/ESP-1496/ASTROMADRID; info:eu-repo/grantAgreement/EC/FP7/238356Editor's Version
http://dx.doi.org/10.1111/j.1365-2966.2012.20947.xSubjects
Cosmology: theory; Dark matter; Galaxies: evolution; Galaxies: haloes; Methods: numerical; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 RAS © The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedRights
© 2012 Royal Astronomical Society; © 2012 The Authors. Monthly Notices of the Royal Astronomical SocietyAbstract
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 20per 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 <1 for all the finders that reached high resolution. If correct, this would indicate that the larger and more massive, respectively, substructures are the most dynamically interesting and that higher levels of the (sub)subhalo hierarchy become progressively less important
Files in this item
Google Scholar:Onions, Julian
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Knebe, Alexander
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Pearce, Frazer R.
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Muldrew, Stuart I.
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Lux, Hanni
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Knollmann, Steffen R.
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Ascasibar Sequeiros, Yago
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Behroozi, Peter
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Elahi, Pascal
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Han, Jiaxin
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MacIejewski, Michal
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Merchán, Manuel E.
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Neyrinck, Mark
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Ruiz, Andrés N.
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Sgró, Mario A.
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Springel, Volker
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Tweed, Dylan
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