The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies
The halo mass–temperature ( M – T ) relation for a sample of 216 galaxy clusters, groups, and individual galaxies observed by the Chandra X-ray Observatory is presented. Using accurate spectral measurements of their hot atmospheres, we derive the M – T relation for systems with temperatures ranging...
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Format: | Article |
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IOP Publishing
2023-01-01
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Series: | The Astrophysical Journal |
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Online Access: | https://doi.org/10.3847/1538-4357/acbf4b |
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author | Iurii V. Babyk Brian R. McNamara |
author_facet | Iurii V. Babyk Brian R. McNamara |
author_sort | Iurii V. Babyk |
collection | DOAJ |
description | The halo mass–temperature ( M – T ) relation for a sample of 216 galaxy clusters, groups, and individual galaxies observed by the Chandra X-ray Observatory is presented. Using accurate spectral measurements of their hot atmospheres, we derive the M – T relation for systems with temperatures ranging between 0.4 and 15.0 keV. We measure the total masses of the clusters, groups, and galaxies at radius R _2500 , finding that the M _2500 ∝ T ^α relation follows a power law with α = 1.65 ± 0.06. Our relation agrees with recent lensing studies of the M – T relation at R _200 and is consistent with self-similar theoretical predictions and recent simulations. This agreement indicates that the M – T relation is weakly affected by nongravitational heating processes. Using lensing masses within R _200 we find M _200 – T follows a power law with a slope of 1.61 ± 0.19, consistent with the M _2500 – T relation. No evidence for a break or slope change is found in either relation. Potential biases associated with sample selection, evolution, and the assumption of hydrostatic equilibrium that may affect the scaling are examined. No significant impacts attributable to these biases are found. Non-cool-core clusters and early spirals produce higher scatter in the M – T relation than cool-core clusters and elliptical galaxies. |
first_indexed | 2024-03-12T04:42:55Z |
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institution | Directory Open Access Journal |
issn | 1538-4357 |
language | English |
last_indexed | 2024-03-12T04:42:55Z |
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series | The Astrophysical Journal |
spelling | doaj.art-65d4c51e7afc4a65a471804e93bab0cb2023-09-03T09:30:44ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194615410.3847/1538-4357/acbf4bThe Halo Mass–Temperature Relation for Clusters, Groups, and GalaxiesIurii V. Babyk0https://orcid.org/0000-0003-3165-9804Brian R. McNamara1https://orcid.org/0000-0002-2622-2627Center for Astrophysics ∣ Harvard-Smithsonian , 60 Garden Street, Cambridge, MA, 02138, USA ; babikyura@gmail.com; Main Astronomical Observatory of the National Academy of Sciences of Ukraine , 27 Academica Zabolotnoho str., Kyiv, 03134, UkraineDepartment of Physics and Astronomy, University of Waterloo , 200 University Avenue West, Waterloo, ON, N2L 3G1, CanadaThe halo mass–temperature ( M – T ) relation for a sample of 216 galaxy clusters, groups, and individual galaxies observed by the Chandra X-ray Observatory is presented. Using accurate spectral measurements of their hot atmospheres, we derive the M – T relation for systems with temperatures ranging between 0.4 and 15.0 keV. We measure the total masses of the clusters, groups, and galaxies at radius R _2500 , finding that the M _2500 ∝ T ^α relation follows a power law with α = 1.65 ± 0.06. Our relation agrees with recent lensing studies of the M – T relation at R _200 and is consistent with self-similar theoretical predictions and recent simulations. This agreement indicates that the M – T relation is weakly affected by nongravitational heating processes. Using lensing masses within R _200 we find M _200 – T follows a power law with a slope of 1.61 ± 0.19, consistent with the M _2500 – T relation. No evidence for a break or slope change is found in either relation. Potential biases associated with sample selection, evolution, and the assumption of hydrostatic equilibrium that may affect the scaling are examined. No significant impacts attributable to these biases are found. Non-cool-core clusters and early spirals produce higher scatter in the M – T relation than cool-core clusters and elliptical galaxies.https://doi.org/10.3847/1538-4357/acbf4bGalaxy clusters |
spellingShingle | Iurii V. Babyk Brian R. McNamara The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies The Astrophysical Journal Galaxy clusters |
title | The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies |
title_full | The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies |
title_fullStr | The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies |
title_full_unstemmed | The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies |
title_short | The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies |
title_sort | halo mass temperature relation for clusters groups and galaxies |
topic | Galaxy clusters |
url | https://doi.org/10.3847/1538-4357/acbf4b |
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