A dataset provided by the European Space Agency

Name: The dark matter distribution in 0.9 < z < 1.1 clusters
Published: 2016-03-12T23:00:00Z
License: https://creativecommons.org/licenses/by-nc/3.0/igo

Proposal ID	074440
Title	The dark matter distribution in 0.9 < z < 1.1 clusters
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744400101 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744400201 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744400301 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744400401 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744400501 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0744401301
DOI	https://doi.org/10.5270/esa-fxuy8mi
Principal Investigator, PI	Dr Monique Arnaud
Abstract	We propose to measure the mass profiles of a complete sample of massive galaxyclusters at 0.9< z< 1.15, with a precision similar to that currently obtainedfor local objects. We will assess the evolution of the dark matter concentrationat cluster scales, a critical test of theoretical scenario of structureformation. This data set will also constrain the evolution of fundamentalmass-proxy relations and the evolution of the gas entropy and pressure profilesin the high mass regime, a test of gravitational gas heating
Publications	The Million Optical - Radio/X-ray Associations (MORX) Catalogue \|Flesch Eric W. \| PASA \| 33-52 \| 2016 \| 2016PASA...33...52F \| http://ui.adsabs.harvard.edu/#abs/2016PASA...33...52F Resolving galaxy cluster gas properties at z &tilde 1 with XMM-Newton and Chandra \|Bartalucci I. Arnaud M. et al. \| A&A \| 598-61 \| 2017 \| 2017A&A...598A..61B \| http://ui.adsabs.harvard.edu/#abs/2017A&A...598A..61B Recovering galaxy cluster gas density profiles with XMM-Newton and Chandra \|Bartalucci I. Arnaud M. et al. \| A&A \| 608-88 \| 2017 \| 2017A&A...608A..88B \| http://ui.adsabs.harvard.edu/#abs/2017A&A...608A..88B Resolving the hydrostatic mass profiles of galaxy clusters at z &tilde 1 with XMM-Newton and Chandra \|Bartalucci I. Arnaud M. et al. \| A&A \| 617-64 \| 2018 \| 2018A&A...617A..64B \| http://ui.adsabs.harvard.edu/#abs/2018A&A...617A..64B High density of active galactic nuclei in the outskirts of distant galaxy clusters \|Koulouridis E. Bartalucci I. \| A&A \| 623-10 \| 2019 \| 2019A&A...623L..10K \| http://ui.adsabs.harvard.edu/#abs/2019A&A...623L..10K The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population \|Pratt G. W. Arnaud M. et al. \| SSRv \| 215-25 \| 2019 \| 2019SSRv..215...25P \| http://ui.adsabs.harvard.edu/#abs/2019SSRv..215...25P X-Ray Properties of SPT-selected Galaxy Clusters at 0.2 < z < 1.5 Observed with XMM-Newton \|Bulbul Esra Chiu I.-Non et al. \| ApJ \| 871-50 \| 2019 \| 2019ApJ...871...50B \| http://ui.adsabs.harvard.edu/#abs/2019ApJ...871...50B The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state \|Bartalucci I. Arnaud M. et al. \| A&A \| 628-86 \| 2019 \| 2019A&A...628A..86B \| http://ui.adsabs.harvard.edu/#abs/2019A&A...628A..86B Mass calibration of the CODEX cluster sample using SPIDERS spectroscopy - II. The X-ray luminosity-mass relation \|Capasso R. Mohr J. J. et al. \| MNRAS \| 494-2736 \| 2020 \| 2020MNRAS.494.2736C \| http://ui.adsabs.harvard.edu/#abs/2020MNRAS.494.2736C Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z u223c 1 \|Gupta N. Pannella M. et al. \| MNRAS \| 494-1705 \| 2020 \| 2020MNRAS.494.1705G \| http://ui.adsabs.harvard.edu/#abs/2020MNRAS.494.1705G Constraints on the variation of fine structure constant from joint SPT-SZ and XMM-Newton observations \|Bora Kamal Desai Shantanu \| JCAP \| 2-12 \| 2021 \| 2021JCAP...02..012B \| http://ui.adsabs.harvard.edu/#abs/2021JCAP...02..012B A test of cosmic distance duality relation using SPT-SZ galaxy clusters Type Ia supernovae and cosmic chronometers \|Bora Kamal Desai Shantanu \| JCAP \| 6-52 \| 2021 \| 2021JCAP...06..052B \| http://ui.adsabs.harvard.edu/#abs/2021JCAP...06..052B Classification of 4XMM-DR9 sources by machine learning \|Zhang Yanxia Zhao Yongheng \| MNRAS \| 503-5263 \| 2021 \| 2021MNRAS.503.5263Z \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.503.5263Z Dynamical state of galaxy clusters evaluated from X-ray images \|Yuan Z. S. Han J. L. \| MNRAS \| 513-3013 \| 2022 \| 2022MNRAS.513.3013Y \| http://ui.adsabs.harvard.edu/#abs/2022MNRAS.513.3013Y Linking a universal gas density profile to the core-excised X-ray luminosity in galaxy clusters up to z u223c 1.1 \|Pratt G. W. Arnaud M. et al. \| A&A \| 665-24 \| 2022 \| 2022A&A...665A..24P \| http://ui.adsabs.harvard.edu/#abs/2022A&A...665A..24P The first evidence of tidally induced activity in a brown dwarf-M dwarf pair: a Chandra study of the NLTT 41135/41136 system \|Iliu0107 Nikoleta Poppenhaeger Katja et al. \| MNRAS \| 524-5954 \| 2023 \| 2023MNRAS.524.5954I \| http://ui.adsabs.harvard.edu/#abs/2023MNRAS.524.5954I The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII O VIII and Fe L-shell Transitions \|Pan Zeyang Qu Zhijie et al. \| ApJS \| 271-62 \| 2024 \| 2024ApJS..271...62P \| http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P From Active Stars to Black Holes: A Discovery Tool for Galactic X-Ray Sources \|Rodriguez Antonio C. \| PASP \| 136-054201 \| 2024 \| 2024PASP..136e4201R \| http://ui.adsabs.harvard.edu/#abs/2024PASP..136e4201R Robust constraints on feebly interacting particles using XMM-Newton \|Luque Pedro De la Torre Balaji Shyam \| PhRvD \| 109-L101305 \| 2024 \| 2024PhRvD.109j1305L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L Multimessenger search for electrophilic feebly interacting particles from supernovae \|Luque Pedro De la Torre Balaji Shyam \| PhRvD \| 109-103028 \| 2024 \| 2024PhRvD.109j3028L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints \|De la Torre Luque Pedro Balaji Shyam \| ApJ \| 968-46 \| 2024 \| 2024ApJ...968...46D \| http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints \|De la Torre Luque Pedro Balaji Shyam \| ApJ \| 973-L6 \| 2024 \| 2024ApJ...973L...6D \| http://ui.adsabs.harvard.edu/#abs/2024ApJ...973L...6D
Instrument	EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage	2014-05-05T10:59:17Z/2015-02-23T21:40:27Z
Version	21.51_20241115_1113
Mission Description	The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
Creator Contact	https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published	2016-03-12T23:00:00Z
Last Update	2026-07-09
Keywords	"pressure profiles", "complete sample", "gravitational gas heating", "mass profiles", "mass regime", "dark matter distribution", "gas entropy", "massive galaxy cluster", "data set", "cluster scales", "local objects", "structure formation", "dark matter concentration"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Monique Arnaud, 2016, 'The dark matter distribution in 0.9 < z < 1.1 clusters', 21.51_20241115_1113, European Space Agency, https://doi.org/10.5270/esa-fxuy8mi
Rights	Data hosted in the ESA Space Science Archives are distributed under the CC BY-NC 3.0 IGO license.