Estimating the local dark matter density in a non-axisymmetric wobbling disc

The density of dark matter near the Sun, ρDM, ⊙, is important for experiments hunting for dark matter particles in the laboratory, and for constraining the local shape of the Milky Way's dark matter halo. Estimates to date have typically assumed that the Milky Way's stellar disc is axisymm...

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Autores: Sivertsson, S., Read, Justin I., Silverwood, H., Salas, P. F. de, Malhan, K., Widmark, Axel, Laporte, Chervin F. P., Garbari, S., Freese, K.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/276433
Acceso en línea:http://hdl.handle.net/10261/276433
Access Level:acceso abierto
Palabra clave:Galaxy. disc
Galaxies: kinematics and dynamics
Dark matter
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spelling Estimating the local dark matter density in a non-axisymmetric wobbling discSivertsson, S.Read, Justin I.Silverwood, H.Salas, P. F. deMalhan, K.Widmark, AxelLaporte, Chervin F. P.Garbari, S.Freese, K.Galaxy. discGalaxies: kinematics and dynamicsDark matterThe density of dark matter near the Sun, ρDM, ⊙, is important for experiments hunting for dark matter particles in the laboratory, and for constraining the local shape of the Milky Way's dark matter halo. Estimates to date have typically assumed that the Milky Way's stellar disc is axisymmetric and in a steady-state. Yet the Milky Way disc is neither, exhibiting prominent spiral arms and a bar, and vertical and radial oscillations. We assess the impact of these assumptions on determinations of ρDM, ⊙ by applying a free-form, steady-state, Jeans method to two different N-body simulations of Milky Way-like galaxies. In one, the galaxy has experienced an ancient major merger, similar to the hypothesized Gaia-Sausage-Enceladus; in the other, the galaxy is perturbed more recently by the repeated passage and slow merger of a Sagittarius-like dwarf galaxy. We assess the impact of each of the terms in the Jeans-Poisson equations on our ability to correctly extract ρDM, ⊙ from the simulated data. We find that common approximations employed in the literature - axisymmetry and a locally flat rotation curve - can lead to significant systematic errors of up to a factor ∼1.5 in the recovered surface mass density ∼2 kpc above the disc plane, implying a fractional error on ρDM, ⊙ of the order of unity. However, once we add in the tilt term and the rotation curve term in our models, we obtain an unbiased estimate of ρDM, ⊙, consistent with the true value within our 95 per cent confidence intervals for realistic 20 per cent uncertainties on the baryonic surface density of the disc. Other terms - the axial tilt, 2nd Poisson and time-dependent terms - contribute less than 10 per cent to ρDM, ⊙ (given current data) and can be safely neglected for now. In the future, as more data become available, these terms will need to be included in the analysis.We acknowledge support by the Oskar Klein Centre for Cosmoparticle Physics and Vetenskapsrådet (Swedish Research Council): SS, PFdS, KM, and KF through No. 638-2013-8993; AW through No. 621-2014-5772. AW also acknowledges support from the Carlsberg Foundation via a Semper Ardens grant (CF15-0384). KF gratefully acknowledges support from the Jeff and Gail Kodosky Endowed Chair in Physics at the University of Texas, Austin; the U.S. Department of Energy, Office of Science, Office of High Energy Physics program under Award Number DE-SC-0022021 at the University of Texas, Austin; the DoE grant DE- SC007859 at the University of Michigan; and the Leinweber Center for Theoretical Physics at the University of Michigan.This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. CL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 852839).Royal Astronomical SocietySwedish Research CouncilCarlsberg FoundationUniversity of TexasDepartment of Energy (US)University of MichiganMinistry of Education, Culture, Sports, Science and Technology (Japan)European Research CouncilEuropean CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2022202220222022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/276433reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/852839The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac094http://doi.org/10.1093/mnras/stac094Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2764332026-05-22T06:33:51Z
dc.title.none.fl_str_mv Estimating the local dark matter density in a non-axisymmetric wobbling disc
title Estimating the local dark matter density in a non-axisymmetric wobbling disc
spellingShingle Estimating the local dark matter density in a non-axisymmetric wobbling disc
Sivertsson, S.
Galaxy. disc
Galaxies: kinematics and dynamics
Dark matter
title_short Estimating the local dark matter density in a non-axisymmetric wobbling disc
title_full Estimating the local dark matter density in a non-axisymmetric wobbling disc
title_fullStr Estimating the local dark matter density in a non-axisymmetric wobbling disc
title_full_unstemmed Estimating the local dark matter density in a non-axisymmetric wobbling disc
title_sort Estimating the local dark matter density in a non-axisymmetric wobbling disc
dc.creator.none.fl_str_mv Sivertsson, S.
Read, Justin I.
Silverwood, H.
Salas, P. F. de
Malhan, K.
Widmark, Axel
Laporte, Chervin F. P.
Garbari, S.
Freese, K.
author Sivertsson, S.
author_facet Sivertsson, S.
Read, Justin I.
Silverwood, H.
Salas, P. F. de
Malhan, K.
Widmark, Axel
Laporte, Chervin F. P.
Garbari, S.
Freese, K.
author_role author
author2 Read, Justin I.
Silverwood, H.
Salas, P. F. de
Malhan, K.
Widmark, Axel
Laporte, Chervin F. P.
Garbari, S.
Freese, K.
author2_role author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Swedish Research Council
Carlsberg Foundation
University of Texas
Department of Energy (US)
University of Michigan
Ministry of Education, Culture, Sports, Science and Technology (Japan)
European Research Council
European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxy. disc
Galaxies: kinematics and dynamics
Dark matter
topic Galaxy. disc
Galaxies: kinematics and dynamics
Dark matter
description The density of dark matter near the Sun, ρDM, ⊙, is important for experiments hunting for dark matter particles in the laboratory, and for constraining the local shape of the Milky Way's dark matter halo. Estimates to date have typically assumed that the Milky Way's stellar disc is axisymmetric and in a steady-state. Yet the Milky Way disc is neither, exhibiting prominent spiral arms and a bar, and vertical and radial oscillations. We assess the impact of these assumptions on determinations of ρDM, ⊙ by applying a free-form, steady-state, Jeans method to two different N-body simulations of Milky Way-like galaxies. In one, the galaxy has experienced an ancient major merger, similar to the hypothesized Gaia-Sausage-Enceladus; in the other, the galaxy is perturbed more recently by the repeated passage and slow merger of a Sagittarius-like dwarf galaxy. We assess the impact of each of the terms in the Jeans-Poisson equations on our ability to correctly extract ρDM, ⊙ from the simulated data. We find that common approximations employed in the literature - axisymmetry and a locally flat rotation curve - can lead to significant systematic errors of up to a factor ∼1.5 in the recovered surface mass density ∼2 kpc above the disc plane, implying a fractional error on ρDM, ⊙ of the order of unity. However, once we add in the tilt term and the rotation curve term in our models, we obtain an unbiased estimate of ρDM, ⊙, consistent with the true value within our 95 per cent confidence intervals for realistic 20 per cent uncertainties on the baryonic surface density of the disc. Other terms - the axial tilt, 2nd Poisson and time-dependent terms - contribute less than 10 per cent to ρDM, ⊙ (given current data) and can be safely neglected for now. In the future, as more data become available, these terms will need to be included in the analysis.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/276433
url http://hdl.handle.net/10261/276433
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/852839
The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac094
http://doi.org/10.1093/mnras/stac094
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Royal Astronomical Society
publisher.none.fl_str_mv Royal Astronomical Society
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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