Estimating the dark matter velocity anisotropy to the cluster edge

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Standard

Estimating the dark matter velocity anisotropy to the cluster edge. / Svensmark, Jacob; Hansen, Steen H.; Martizzi, Davide; Moore, Ben; Teyssier, Romain.

I: Monthly Notices of the Royal Astronomical Society, Bind 500, 23.10.2020, s. 3151-3161.

Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt

Harvard

Svensmark, J, Hansen, SH, Martizzi, D, Moore, B & Teyssier, R 2020, 'Estimating the dark matter velocity anisotropy to the cluster edge', Monthly Notices of the Royal Astronomical Society, bind 500, s. 3151-3161. https://doi.org/10.1093/mnras/staa3279

APA

Svensmark, J., Hansen, S. H., Martizzi, D., Moore, B., & Teyssier, R. (2020). Estimating the dark matter velocity anisotropy to the cluster edge. Monthly Notices of the Royal Astronomical Society, 500, 3151-3161. https://doi.org/10.1093/mnras/staa3279

Vancouver

Svensmark J, Hansen SH, Martizzi D, Moore B, Teyssier R. Estimating the dark matter velocity anisotropy to the cluster edge. Monthly Notices of the Royal Astronomical Society. 2020 okt. 23;500:3151-3161. https://doi.org/10.1093/mnras/staa3279

Author

Svensmark, Jacob ; Hansen, Steen H. ; Martizzi, Davide ; Moore, Ben ; Teyssier, Romain. / Estimating the dark matter velocity anisotropy to the cluster edge. I: Monthly Notices of the Royal Astronomical Society. 2020 ; Bind 500. s. 3151-3161.

Bibtex

@article{5d7f99420251488fa894ef8030adfda9,
title = "Estimating the dark matter velocity anisotropy to the cluster edge",
abstract = "Dark matter (DM) dominates the properties of large cosmological structures such as galaxy clusters, and the mass profiles of the DM have been inferred for these equilibrated structures for years by using cluster X-ray surface brightnesses and temperatures. A new method has been proposed, which should allow us to infer a dynamical property of the DM, namely the velocity anisotropy. For the gas, a similar velocity anisotropy is zero due to frequent collisions; however, the collisionless nature of DM allows it to be non-trivial. Numerical simulations have for years found non-zero and radially varying DM velocity anisotropies. Here we employ the method proposed by Hansen & Piffaretti, and developed by H{\o}st et al. to infer the DM velocity anisotropy in the bright galaxy cluster Perseus, to near five times the radii previously obtained. We find the DM velocity anisotropy to be consistent with the results of numerical simulations, however, still with large error bars. At half the virial radius, we find the DM velocity anisotropy to be non-zero at 1.7σ⁠, lending support to the collisionless nature of DM.",
keywords = "astro-ph.CO, 85A04",
author = "Jacob Svensmark and Hansen, {Steen H.} and Davide Martizzi and Ben Moore and Romain Teyssier",
note = "20 pages, 10 figures",
year = "2020",
month = oct,
day = "23",
doi = "10.1093/mnras/staa3279",
language = "English",
volume = "500",
pages = "3151--3161",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",

}

RIS

TY - JOUR

T1 - Estimating the dark matter velocity anisotropy to the cluster edge

AU - Svensmark, Jacob

AU - Hansen, Steen H.

AU - Martizzi, Davide

AU - Moore, Ben

AU - Teyssier, Romain

N1 - 20 pages, 10 figures

PY - 2020/10/23

Y1 - 2020/10/23

N2 - Dark matter (DM) dominates the properties of large cosmological structures such as galaxy clusters, and the mass profiles of the DM have been inferred for these equilibrated structures for years by using cluster X-ray surface brightnesses and temperatures. A new method has been proposed, which should allow us to infer a dynamical property of the DM, namely the velocity anisotropy. For the gas, a similar velocity anisotropy is zero due to frequent collisions; however, the collisionless nature of DM allows it to be non-trivial. Numerical simulations have for years found non-zero and radially varying DM velocity anisotropies. Here we employ the method proposed by Hansen & Piffaretti, and developed by Høst et al. to infer the DM velocity anisotropy in the bright galaxy cluster Perseus, to near five times the radii previously obtained. We find the DM velocity anisotropy to be consistent with the results of numerical simulations, however, still with large error bars. At half the virial radius, we find the DM velocity anisotropy to be non-zero at 1.7σ⁠, lending support to the collisionless nature of DM.

AB - Dark matter (DM) dominates the properties of large cosmological structures such as galaxy clusters, and the mass profiles of the DM have been inferred for these equilibrated structures for years by using cluster X-ray surface brightnesses and temperatures. A new method has been proposed, which should allow us to infer a dynamical property of the DM, namely the velocity anisotropy. For the gas, a similar velocity anisotropy is zero due to frequent collisions; however, the collisionless nature of DM allows it to be non-trivial. Numerical simulations have for years found non-zero and radially varying DM velocity anisotropies. Here we employ the method proposed by Hansen & Piffaretti, and developed by Høst et al. to infer the DM velocity anisotropy in the bright galaxy cluster Perseus, to near five times the radii previously obtained. We find the DM velocity anisotropy to be consistent with the results of numerical simulations, however, still with large error bars. At half the virial radius, we find the DM velocity anisotropy to be non-zero at 1.7σ⁠, lending support to the collisionless nature of DM.

KW - astro-ph.CO

KW - 85A04

U2 - 10.1093/mnras/staa3279

DO - 10.1093/mnras/staa3279

M3 - Journal article

VL - 500

SP - 3151

EP - 3161

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

ER -

ID: 229808078