Bayesian reconstruction of the Milky Way dark matter distribution
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1088/1475-7516/2019/09/046 http://hdl.handle.net/11449/199774 |
Resumo: | We develop a novel Bayesian methodology aimed at reliably and precisely inferring the distribution of dark matter within the Milky Way using rotation curve data. We identify a subset of the available rotation curve tracers that are mutually consistent with each other, thus eliminating data sets that might suffer from systematic bias. We investigate different models for the mass distribution of the luminous (baryonic) component that bracket the range of likely morphologies. We demonstrate the statistical performance of our method on simulated data in terms of coverage, fractional distance, and mean squared error. Applying it to Milky Way data we measure the local dark matter density at the solar circle ρ0 to be ρ0 = 0.43 ± 0.02(stat) ± 0.01(sys) GeV/cm3, with an accuracy ∼ 6%. This result is robust to the assumed baryonic morphology. The scale radius and inner slope of the dark matter profile are degenerate and cannot be individually determined with high accuracy. We show that these results are robust to several possible residual systematic errors in the rotation curve data. |
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Repositório Institucional da UNESP |
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spelling |
Bayesian reconstruction of the Milky Way dark matter distributiongalaxy dynamicsrotation curves of galaxiesWe develop a novel Bayesian methodology aimed at reliably and precisely inferring the distribution of dark matter within the Milky Way using rotation curve data. We identify a subset of the available rotation curve tracers that are mutually consistent with each other, thus eliminating data sets that might suffer from systematic bias. We investigate different models for the mass distribution of the luminous (baryonic) component that bracket the range of likely morphologies. We demonstrate the statistical performance of our method on simulated data in terms of coverage, fractional distance, and mean squared error. Applying it to Milky Way data we measure the local dark matter density at the solar circle ρ0 to be ρ0 = 0.43 ± 0.02(stat) ± 0.01(sys) GeV/cm3, with an accuracy ∼ 6%. This result is robust to the assumed baryonic morphology. The scale radius and inner slope of the dark matter profile are degenerate and cannot be individually determined with high accuracy. We show that these results are robust to several possible residual systematic errors in the rotation curve data.ICTP-SAIFR IFT-UNESP, R. Dr. Bento Teobaldo Ferraz 271IFT-UNESP, R. Dr. Bento Teobaldo Ferraz 271Physics Department Astrophysics Group Imperial Centre for Inference and Cosmology Blackett Laboratory Imperial College London, Prince Consort RdData Science Institute William Penney Laboratory Imperial College LondonAstrocent Nicolaus Copernicus Astronomical Center Polish Academy of Sciences, ul. Bartycka 18ICTP-SAIFR IFT-UNESP, R. Dr. Bento Teobaldo Ferraz 271IFT-UNESP, R. Dr. Bento Teobaldo Ferraz 271Universidade Estadual Paulista (Unesp)Imperial College LondonPolish Academy of SciencesKarukes, E. V. [UNESP]Benito, M. [UNESP]Iocco, F. [UNESP]Trotta, R.Geringer-Sameth, A.2020-12-12T01:49:01Z2020-12-12T01:49:01Z2019-09-23info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1088/1475-7516/2019/09/046Journal of Cosmology and Astroparticle Physics, v. 2019, n. 9, 2019.1475-7516http://hdl.handle.net/11449/19977410.1088/1475-7516/2019/09/0462-s2.0-85076117737Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengJournal of Cosmology and Astroparticle Physicsinfo:eu-repo/semantics/openAccess2021-10-23T09:41:38Zoai:repositorio.unesp.br:11449/199774Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T18:23:10.991793Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Bayesian reconstruction of the Milky Way dark matter distribution |
title |
Bayesian reconstruction of the Milky Way dark matter distribution |
spellingShingle |
Bayesian reconstruction of the Milky Way dark matter distribution Karukes, E. V. [UNESP] galaxy dynamics rotation curves of galaxies |
title_short |
Bayesian reconstruction of the Milky Way dark matter distribution |
title_full |
Bayesian reconstruction of the Milky Way dark matter distribution |
title_fullStr |
Bayesian reconstruction of the Milky Way dark matter distribution |
title_full_unstemmed |
Bayesian reconstruction of the Milky Way dark matter distribution |
title_sort |
Bayesian reconstruction of the Milky Way dark matter distribution |
author |
Karukes, E. V. [UNESP] |
author_facet |
Karukes, E. V. [UNESP] Benito, M. [UNESP] Iocco, F. [UNESP] Trotta, R. Geringer-Sameth, A. |
author_role |
author |
author2 |
Benito, M. [UNESP] Iocco, F. [UNESP] Trotta, R. Geringer-Sameth, A. |
author2_role |
author author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (Unesp) Imperial College London Polish Academy of Sciences |
dc.contributor.author.fl_str_mv |
Karukes, E. V. [UNESP] Benito, M. [UNESP] Iocco, F. [UNESP] Trotta, R. Geringer-Sameth, A. |
dc.subject.por.fl_str_mv |
galaxy dynamics rotation curves of galaxies |
topic |
galaxy dynamics rotation curves of galaxies |
description |
We develop a novel Bayesian methodology aimed at reliably and precisely inferring the distribution of dark matter within the Milky Way using rotation curve data. We identify a subset of the available rotation curve tracers that are mutually consistent with each other, thus eliminating data sets that might suffer from systematic bias. We investigate different models for the mass distribution of the luminous (baryonic) component that bracket the range of likely morphologies. We demonstrate the statistical performance of our method on simulated data in terms of coverage, fractional distance, and mean squared error. Applying it to Milky Way data we measure the local dark matter density at the solar circle ρ0 to be ρ0 = 0.43 ± 0.02(stat) ± 0.01(sys) GeV/cm3, with an accuracy ∼ 6%. This result is robust to the assumed baryonic morphology. The scale radius and inner slope of the dark matter profile are degenerate and cannot be individually determined with high accuracy. We show that these results are robust to several possible residual systematic errors in the rotation curve data. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-09-23 2020-12-12T01:49:01Z 2020-12-12T01:49:01Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://dx.doi.org/10.1088/1475-7516/2019/09/046 Journal of Cosmology and Astroparticle Physics, v. 2019, n. 9, 2019. 1475-7516 http://hdl.handle.net/11449/199774 10.1088/1475-7516/2019/09/046 2-s2.0-85076117737 |
url |
http://dx.doi.org/10.1088/1475-7516/2019/09/046 http://hdl.handle.net/11449/199774 |
identifier_str_mv |
Journal of Cosmology and Astroparticle Physics, v. 2019, n. 9, 2019. 1475-7516 10.1088/1475-7516/2019/09/046 2-s2.0-85076117737 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Journal of Cosmology and Astroparticle Physics |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1808128926164189184 |