Статья

Tracing the cosmic web

Noam I. LibeskindLeibniz-Institute für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, GermanyRien van de WeygaertKapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the NetherlandsMarius CautunInstitute for Computational Cosmology, Durham University, South Road, Durham, DH1 3LE, UKBridget FalckInstitute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, N-0315 Oslo, NorwayElmo TempelTartu Observatory, Observatooriumi 1, 61602 Tõravere, EstoniaTom AbelDepartment of Physics, Stanford University, Stanford, CA 94305, USAMehmet AlpaslanNASA Ames Research Center N232, Moffett Field, Mountain View, CA 94035, USAMiguel A. Aragón-CalvoInstituto Astronomico de Ensenada,UNAM, MexicoJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, Bogotá, 111711, ColombiaRoberto GonzálezInstituto de Astrofísica, Pontificia Universidad Catolica de Chile, Santiago, 8970117 ChileStefan GottlöberLeibniz-Institute für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, GermanyOliver HahnObservatoire de la Cote d'Azur, Laboratoire Lagrange, Boulevard de l'Observatoire, CS 34229, F-06304 NICE, FranceWojciech A. HellwingInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UKYehuda HoffmanRacah Institute of Physics, Hebrew University of Jerusalem, Givat Ram, Jerusalem 91904, IsraelBernard J. T. JonesKapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the NetherlandsFrancisco-Shu KitauraDepartamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, SpainAlexander KnebeAstro-UAM, UAM, Unidad Asociada CSICS. MantiScuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, ItalyMark C. NeyrinckInstitute for Computational Cosmology, Durham University, South Road, Durham, DH1 3LE, UKSebastián E. NuzaInstituto de Astronomía y Física del Espacio (IAFE, CONICETUBA), CC 67, Suc. 28, 1428 Buenos Aires, ArgentinaNelson PadillaCentro de Astro-Ingeniería, Pontificia Universidad Catolica de Chile, Santiago, 8970117 ChileErwin PlatenKapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the NetherlandsNesar RamachandraDepartment of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USAA. S. G. RobothamICRAR, M468, University of Western Australia, Crawley, WA 6009, AustraliaE. SaarTartu Observatory, Observatooriumi 1, 61602 Tõravere, EstoniaS. F. ShandarinDepartment of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USAMatthias SteinmetzLeibniz-Institute für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, GermanyRadu S. StoicaInstitut Elie Cartan de Lorraine, Université de Lorraine, F-54506 Vandoeuvre-lés-Nancy Cedex, FranceT. SousbieInstitut d'Astrophysique de Paris, CNRS UMR 7095 and UPMC, 98bis, bd Arago, F-75014 Paris, FranceGustavo YepesDepartamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain

2017en

ABI

Аннотация

The cosmic web is one of the most striking features of the distribution of galaxies and dark matter on the largest scales in the Universe. It is composed of dense regions packed full of galaxies, long filamentary bridges, flattened sheets and vast low-density voids. The study of the cosmic web has focused primarily on the identification of such features, and on understanding the environmental effects on galaxy formation and halo assembly. As such, a variety of different methods have been devised to classify the cosmic web -depending on the data at hand, be it numerical simulations, large sky surveys or other. In this paper, we bring 12 of these methods together and apply them to the same data set in order to understand how they compare. In general, these cosmic-web classifiers have been designed with different cosmological goals in mind, and to study different questions. Therefore, one would not a priori expect agreement between different techniques; however, many of these methods do converge on the identification of specific features. In this paper, we study the agreements and disparities of the different methods. For example, each method finds that knots inhabit higher density regions than filaments, etc. and that voids have the lowest densities. For a given web environment, we find a substantial overlap in the density range assigned by each web classification scheme. We also compare classifications on a halo-by-halo basis; for example, we find that 9 of 12 methods classify around a third of group-mass haloes (i.e. M halo 10 13.5 h -1 M ) as being in filaments. Lastly, so that any future cosmic-web classification scheme can be compared to the 12 methods used here, we have made all the data used in this paper public.

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Идентификаторы

DOI: 10.1093/mnras/stx1976

Цитирования и источники

Цитирований: 2Использованных источников: 0

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