Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis

We performed a free-form strong lensing analysis of the galaxy cluster MACS J1206.2?0847 in order to estimate and constrain its inner dark matter distribution. The free-form method estimates the cluster total mass distribution without using any prior information about the underlying mass. We used 97...

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Autores: Manjón García, Alberto|||0000-0002-7413-8825, Diego Rodríguez, José María|||0000-0001-9065-3926, Herranz Muñoz, Diego|||0000-0003-4540-1417, Lam, Daniel
Tipo de recurso: artículo
Fecha de publicación:2020
País:España
Institución:Universidad de Cantabria (UC)
Repositorio:UCrea Repositorio Abierto de la Universidad de Cantabria
Idioma:inglés
OAI Identifier:oai:repositorio.unican.es:10902/24981
Acceso en línea:http://hdl.handle.net/10902/24981
Access Level:acceso abierto
Palabra clave:Galaxies: clusters: individual: MACS J1206.2−0847
Gravitational lensing: strong
Cosmology: observations
Dark matter
Methods: numerical
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spelling Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisisManjón García, Alberto|||0000-0002-7413-8825Diego Rodríguez, José María|||0000-0001-9065-3926Herranz Muñoz, Diego|||0000-0003-4540-1417Lam, DanielGalaxies: clusters: individual: MACS J1206.2−0847Gravitational lensing: strongCosmology: observationsDark matterMethods: numericalWe performed a free-form strong lensing analysis of the galaxy cluster MACS J1206.2?0847 in order to estimate and constrain its inner dark matter distribution. The free-form method estimates the cluster total mass distribution without using any prior information about the underlying mass. We used 97 multiple lensed images belonging to 27 background sources and derived several models, which are consistent with the data. Among these models, we focus on those that better reproduce the radial images that are closest to the centre of the cluster. These radial images are the best probes of the dark matter distribution in the central region and constrain the mass distribution down to distances ?7 kpc from the centre. We find that the morphology of the innermost radial arcs is due to the elongated morphology of the dark matter halo. We estimate the stellar mass contribution of the brightest cluster galaxy and subtracted it from the total mass in order to quantify the amount of dark matter in the central region. We fitted the derived dark matter density profile with a gNFW, which is characterised by rs = 167 kpc, ?s = 6.7 × 106?M? kpc?3, and ?gNFW = 0.70. These results are consistent with a dynamically relaxed cluster. This inner slope is smaller than the cannonical ??=?1 predicted by standard CDM models. This slope does not favour self-interacting models for which a shallower slope would be expected.A.M.G., J.M.D., and D.H. acknowledge the support of project AYA2015-64508-P (MCIU/AEI/MINECO/FEDER, UE) funded by the Ministerio de Economia y Competitividad and project PGC2018-101814-B-100 (MCIU/AEI/MINECO/FEDER, UE) funded by Ministerio de Ciencia, Investigación y Universidades. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We specially thank all people involved in Caminha et al. (2017) for their essential multiple image identification using data taken under the ESO programme IDs 095.A-0181(A), 097.A-0269(A), and 186.A-0798(A); and for making their identifications public. A.M.G. thanks the Department of Physics and Astronomy of the University of Pennsylvania for their hospitality during his stay there, in which he did part of the work shown here. The authors thank the anonymous referee for making valuable suggestions that helped us improve this paper.EDP SciencesUniversidad de Cantabria20202020-01-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttp://hdl.handle.net/10902/24981Astronomy & Astrophysics. Vol. 639, July 2020 . A125reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/249812026-06-02T12:39:31Z
dc.title.none.fl_str_mv Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
title Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
spellingShingle Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
Manjón García, Alberto|||0000-0002-7413-8825
Galaxies: clusters: individual: MACS J1206.2−0847
Gravitational lensing: strong
Cosmology: observations
Dark matter
Methods: numerical
title_short Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
title_full Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
title_fullStr Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
title_full_unstemmed Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
title_sort Constraining the abundance of dark matter in the central region of the galaxy cluster MACS J1206.2?0847 with a free-form strong lensing análisis
dc.creator.none.fl_str_mv Manjón García, Alberto|||0000-0002-7413-8825
Diego Rodríguez, José María|||0000-0001-9065-3926
Herranz Muñoz, Diego|||0000-0003-4540-1417
Lam, Daniel
author Manjón García, Alberto|||0000-0002-7413-8825
author_facet Manjón García, Alberto|||0000-0002-7413-8825
Diego Rodríguez, José María|||0000-0001-9065-3926
Herranz Muñoz, Diego|||0000-0003-4540-1417
Lam, Daniel
author_role author
author2 Diego Rodríguez, José María|||0000-0001-9065-3926
Herranz Muñoz, Diego|||0000-0003-4540-1417
Lam, Daniel
author2_role author
author
author
dc.contributor.none.fl_str_mv Universidad de Cantabria
dc.subject.none.fl_str_mv Galaxies: clusters: individual: MACS J1206.2−0847
Gravitational lensing: strong
Cosmology: observations
Dark matter
Methods: numerical
topic Galaxies: clusters: individual: MACS J1206.2−0847
Gravitational lensing: strong
Cosmology: observations
Dark matter
Methods: numerical
description We performed a free-form strong lensing analysis of the galaxy cluster MACS J1206.2?0847 in order to estimate and constrain its inner dark matter distribution. The free-form method estimates the cluster total mass distribution without using any prior information about the underlying mass. We used 97 multiple lensed images belonging to 27 background sources and derived several models, which are consistent with the data. Among these models, we focus on those that better reproduce the radial images that are closest to the centre of the cluster. These radial images are the best probes of the dark matter distribution in the central region and constrain the mass distribution down to distances ?7 kpc from the centre. We find that the morphology of the innermost radial arcs is due to the elongated morphology of the dark matter halo. We estimate the stellar mass contribution of the brightest cluster galaxy and subtracted it from the total mass in order to quantify the amount of dark matter in the central region. We fitted the derived dark matter density profile with a gNFW, which is characterised by rs = 167 kpc, ?s = 6.7 × 106?M? kpc?3, and ?gNFW = 0.70. These results are consistent with a dynamically relaxed cluster. This inner slope is smaller than the cannonical ??=?1 predicted by standard CDM models. This slope does not favour self-interacting models for which a shallower slope would be expected.
publishDate 2020
dc.date.none.fl_str_mv 2020
2020-01-01
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
NA
http://purl.org/coar/version/c_be7fb7dd8ff6fe43
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10902/24981
url http://hdl.handle.net/10902/24981
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Astronomy & Astrophysics. Vol. 639, July 2020 . A125
reponame:UCrea Repositorio Abierto de la Universidad de Cantabria
instname:Universidad de Cantabria (UC)
instname_str Universidad de Cantabria (UC)
reponame_str UCrea Repositorio Abierto de la Universidad de Cantabria
collection UCrea Repositorio Abierto de la Universidad de Cantabria
repository.name.fl_str_mv
repository.mail.fl_str_mv
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