The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies

Babyk, Iurii; McNamara, B. R.

doi:10.3847/1538-4357/acbf4b

Cited by 5 publications

(2 citation statements)

References 92 publications

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“…Eke et al 2004;Robotham et al 2011), from X-ray emission of hot gas within the halo's gravitational potential (e.g. Vikhlinin et al 2006Vikhlinin et al , 2009Babyk & McNamara 2023), or from gravitational lensing (e.g. Hoekstra et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles I: Kinematic tracers

Sullivan,

Power,

Bottrell

2024

Publ. Astron. Soc. Aust.

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We investigate the relationship between a dark matter halo’s mass profile and measures of the velocity dispersion of kinematic tracers within its gravitational potential. By predicting the scaling relation of the halo mass with the aperture velocity dispersion, Mvir – σap, we present the expected form and dependence of this halo mass tracer on physical parameters within our analytic halo model: parameterized by the halo’s negative inner logarithmic density slope, α, its concentration parameter, c, and its velocity anisotropy parameter, β. For these idealised halos, we obtain a general solution to the Jeans equation, which is projected over the line of sight and averaged within an aperture to form the corresponding aperture velocity dispersion profile. Through dimensional analysis, the Mvir – σap scaling relation is devised explicitly in terms of analytical bounds for these aperture velocity dispersion profiles: allowing constraints to be placed on this relation for motivated parameter choices. We predict the M200 – σap and M500 – σap scaling relations, each with an uncertainty of 60.5% and 56.2%, respectively. These halo mass estimates are found to be weakly sensitive to the halo’s concentration and mass scale, and most sensitive to the size of the aperture radius in which the aperture velocity dispersion is measured, the maximum value for the halo’s inner slope, and the minimum and maximum values of the velocity anisotropy. Our results show that a halo’s structural and kinematic profiles impose only a minor uncertainty in estimating its mass. Consequently, spectroscopic surveys aimed at constraining the halo mass using kinematic tracers can focus on characterising other, more complex sources of uncertainty and observational systematics.

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Section: Introductionmentioning

confidence: 99%

Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles I: Kinematic tracers

Sullivan,

Power,

Bottrell

2024

Publ. Astron. Soc. Aust.

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“…Different mass proxies are utilized in different surveys. In X-ray surveys, commonly used mass proxies include the gas mass, gas temperature, and gas luminosity in different X-ray bands or integrated (e.g., Mulroy et al 2019;Babyk & McNamara 2023). In Sunyaev-Zel'dovich (SZ) surveys, the projected integrated SZ flux is usually used (e.g., Planck Collaboration et al 2016a).…”

Section: Introductionmentioning

confidence: 99%

Intrinsic Mass–Richness Relation of Clusters from THE THREE HUNDRED Hydrodynamic Simulations

Chen,

Cui,

Fang

et al. 2024

ApJ

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The main systematics in cluster cosmology is the uncertainty in the mass–observable relation. In this paper, we focus on the most direct cluster observable in optical surveys, i.e., richness, and constrain the intrinsic mass–richness (MR) relation of clusters in THE THREE HUNDRED hydrodynamic simulations with two runs: GIZMO-SIMBA and GADGET-X. We find that modeling the richness at a fixed halo mass with a skewed Gaussian distribution yields a simpler and smaller scatter compared to the commonly used lognormal distribution. Additionally, we observe that baryon models have a significant impact on the scatter while exhibiting no influence on the mass dependence and a slight effect on the amplitude in the MR relation. We select member galaxies based on both stellar mass M ⋆ and absolute magnitude M . We demonstrate that the MR relations obtained from these two selections can be converted to each other by using the M ⋆ – M relation. Finally, we provide a seven-parameter fitting result comprehensively capturing the dependence of the MR relation on both stellar mass cutoff and redshift.

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Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles II: Intracluster gas emission

Sullivan,

Power,

Bottrell

et al. 2024

Publ. Astron. Soc. Aust.

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We investigate the connection between a cluster’s structural configuration and observable measures of its gas emission that can be obtained in X-ray and Sunyaev-Zeldovich (SZ) surveys. We present an analytic model for the intracluster gas density profile: parameterised by the dark matter halo’s inner logarithmic density slope, α, the concentration, c, the gas profile’s inner logarithmic density slope, ε, the dilution, d, and the gas fraction, η, normalised to cosmological content. We predict four probes of the gas emission: the emission-weighted, TX, and mean gas mass-weighted, Tmg, temperatures, and the spherically, Ysph, and cylindrically, Ycyl, integrated Compton parameters. Over a parameter space of clusters, we constrain the X-ray temperature scaling relations, M200 – TX and M500 – TX, within 57.3% and 41.6%, and M200 – Tmg and M500 – Tmg, within 25.7% and 7.0%, all respectively. When excising the cluster’s core, the M200 – TX and M500 – TX relations are further constrained, to within 31.3% and 17.1%, respectively. Similarly, we constrain the SZ scaling relations, M200 – Ysph and M500 – Ysph, within 31.1% and 17.7%, and M200 – Ycyl and M500 – Ycyl, within 25.2% and 22.0%, all respectively. The temperature observable Tmg places the strongest constraint on the halo mass, whilst TX is more sensitive to the parameter space. The SZ constraints are sensitive to the gas fraction, whilst insensitive to the form of the gas profile itself. In all cases, the halo mass is recovered with an uncertainty that suggests the cluster’s structural profiles only contribute a minor uncertainty in its scaling relations.

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The Halo Mass–Temperature Relation for Clusters, Groups, and Galaxies

Cited by 5 publications

References 92 publications

Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles I: Kinematic tracers

Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles I: Kinematic tracers

Intrinsic Mass–Richness Relation of Clusters from THE THREE HUNDRED Hydrodynamic Simulations

Predicting the scaling relations between the dark matter halo mass and observables from generalised profiles II: Intracluster gas emission

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