Dependency of halo concentration on mass, redshift and fossilness in Magneticum hydrodynamic simulations

Ragagnin, Antonio; Dolag, K.; Moscardini, L.; Biviano, A.; D’Onofrio, M.

doi:10.1093/mnras/stz1103

Cited by 51 publications

(49 citation statements)

References 85 publications

(120 reference statements)

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“…Once the virial radius is specified as the outer limit of the halo, equation 2.1 completely specifies the density profile for given ρ 0 and R s . For any given virial mass, there is a range of corresponding NFW density profiles, with the distributions of ρ 0 and R s emerging from the mass-concentration-redshift relation seen in N-body simulations and observations [30,31].…”

Section: The Nfw Profile Of Cdmmentioning

confidence: 99%

The core-cusp problem revisited: ULDM vs. CDM

Kendall

Easther

2020

Publ. Astron. Soc. Aust.

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The core-cusp problem is often cited as a motivation for the exploration of dark matter models beyond standard CDM [cold dark matter]. One such alternative is ULDM [ultra-light dark matter]; particles exhibiting wavelike properties on kiloparsec scales. ULDM dynamics are governed by the Schrödinger-Poisson equations, which have solitonic ground state solutions consisting of gravitationally-bound condensates with no internal kinetic energy. Astrophysically realistic ULDM halos would consist of larger NFW-like configurations with a possible solitonic core. We describe a parameterisation for the radial density profiles of ULDM halos that accounts for the environmental variability of the core-halo mass relation. We then compare the semi-analytic profiles of ULDM and CDM with astrophysical data, and find that a ULDM particle mass of 10 −23 eV can yield a reasonably good fit to observed rotation data, particularly at small radii. This ULDM mass is in tension with other constraints but we note that this analysis ignores any contribution from baryonic feedback.It is widely agreed that non-baryonic dark matter constitutes the majority of the mass of the observable universe, but its precise nature remains an open question. Many dark matter models have been proposed, with particle CDM [Cold Dark Matter] being the most widely studied. This scenario successfully accounts for the large scale structure of the universe [1] and the spectrum of anisotropies in the microwave background [2-8], but the so-called "smallscale crisis" remains a challenge [9]. A key issue is the tension between the central density profiles of dark matter halos in simulations containing only gravitationally interacting CDM, and those inferred from observational data. Simulations tend to produce 'cuspy' central density profiles [10], which grow as 1/r at small radii, but observational data appears to favour flattened central cores [11]. This so-called core-cusp problem has been the focus of much recent attention [12][13][14].The seriousness of the core-cusp problem is the subject of ongoing debate, and may be ameliorated by adding baryonic matter to CDM simulations [15]. Nevertheless, the wider category of "small-scale" problems in standard CDM along with tighter constraints from direct-detection experiments [16] motivates the study of alternative dark matter models. One scenario which has gained substantial traction is ultra-light dark matter [ULDM], also known as scalar-field dark matter, Ψ dark matter, axion dark matter, BEC dark matter and fuzzy dark matter. As reviewed by Hui et al. [17], ULDM consists of an axion-like particle whose very small mass (O(∼ 10 −22 eV )) corresponds to a kiloparsec-scale de Broglie wavelength. ULDM thus exhibits novel wave-like behaviour on astrophysically interesting scales and can form soliton-like gravitationally confined Bose-Einstein condensates. ULDM simulations suggest that realistic astrophysical halos have an inner core consisting of a kiloparsec scale Bose-Einstein condensate or soliton, while the outer halo is ...

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Section: The Nfw Profile Of Cdmmentioning

confidence: 99%

The core-cusp problem revisited: ULDM vs. CDM

Kendall

Easther

2020

Publ. Astron. Soc. Aust.

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“…All the simulations include the description of the same physical processes and use the same sub-grid model parameters. Our basic assumption is that the variation of the cosmological model should not directly affect the microscopic processes that these sub-grid parameters describe and therefore, these sub-grid physics parameters have been tuned to reproduce observed properties of galaxy clusters at an arbitrarily (but reasonable, and consistent with observations) chosen reference cosmology (Bocquet et al 2016;Gupta et al 2016;Dolag, Mevius & Remus 2017;Remus, Dolag & Hoffmann 2017;Biffi, Dolag & Merloni 2018;Ragagnin et al 2019). In other words, their numerical value does not carry any physical meaning.…”

Section: Introductionmentioning

confidence: 99%

Cosmology dependence of galaxy cluster scaling relations

Singh

Saro

Costanzi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The abundance of galaxy clusters as a function of mass and redshift is a well known powerful cosmological probe, which relies on underlying modelling assumptions on the mass-observable relations (MOR). MOR parameters have to be simultaneously fit together with the parameters describing the cosmological model. Some of the MOR parameters can be constrained directly from multi-wavelength observations, as the normalization at some reference cosmology, the mass-slope, the redshift evolution and the intrinsic scatter. However, the cosmology dependence of MORs cannot be tested with multi-wavelength observations alone. We use Magneticum simulations to explore the cosmology dependence of galaxy cluster scaling relations. We run fifteen different hydro-dynamical cosmological simulations varying Ω m , Ω b , h 0 and σ 8 (around a reference cosmological model). The MORs considered in this work are gas mass, gas temperature, Y and velocity dispersion as a function of the spherical overdensity virial mass. We verify that the mass and redshift slopes and the intrinsic scatter of the MORs are nearly independent of cosmology with variations significantly smaller than current observational uncertainties. We show that the gas mass sensitively depends only on the baryon fraction, velocity dispersion and gas temperature sensitively depend on the hubble constant, and Y depends on both baryon fraction and the hubble constant. We investigate the cosmological implications of our MOR parameterization on a mock catalog created for an idealized eROSITA-like experiment. We show that our parametrization introduces a strong degeneracy between the cosmological parameters and the normalization of the MOR, degeneracy that can be broken by combining multiple observables and hence improve the cosmological parameter constraints. Finally, the parameter constraints derived at different overdensity (∆ 500c ), for X-ray bolometric gas luminosity and stellar mass, and for different subgrid physics prescriptions are shown in the appendix.

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“…Note that the similarity solution shows that clusters are almost in hydrostatic equilibrium in the sense that gas motion is negligible within clusters even if they are not in virial equilibrium [39]. The relation between matter accretion and the cluster structure has also been numerically studied (e.g., Reference [18]). Figure 5 shows the projection of the fundamental plane shown in Figure 3 on the log r s -log M s plane.…”

Section: Origin Of the Fundamental Plane And Cluster Growthmentioning

confidence: 99%

“…This means that, since older halos formed when the density of the universe was higher, they tend to have larger characteristic densities ρ s and become more concentrated with larger c ∆ . This issue has been addressed in many studies, especially by N-body simulations [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18]. These studies have indicated that the halo structure is determined by their mass-growth history.…”

Section: Introductionmentioning

confidence: 99%

Halo Concentrations and the Fundamental Plane of Galaxy Clusters

et al. 2019

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According to the standard cold dark matter (CDM) cosmology, the structure of dark halos including those of galaxy clusters reflects their mass accretion history. Older clusters tend to be more concentrated than younger clusters. Their structure, represented by the characteristic radius r s and mass M s of the Navarro–Frenk–White (NFW) density profile, is related to their formation time. In this study, we showed that r s , M s , and the X-ray temperature of the intracluster medium (ICM), T X , form a thin plane in the space of ( log r s , log M s , log T X ) . This tight correlation indicates that the ICM temperature is also determined by the formation time of individual clusters. Numerical simulations showed that clusters move along the fundamental plane as they evolve. The plane and the cluster evolution within the plane could be explained by a similarity solution of structure formation of the universe. The angle of the plane shows that clusters have not achieved “virial equilibrium” in the sense that mass/size growth and pressure at the boundaries cannot be ignored. The distribution of clusters on the plane was related to the intrinsic scatter in the halo concentration–mass relation, which originated from the variety of cluster ages. The well-known mass–temperature relation of clusters ( M Δ ∝ T X 3 / 2 ) can be explained by the fundamental plane and the mass dependence of the halo concentration without the assumption of virial equilibrium. The fundamental plane could also be used for calibration of cluster masses.

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Dependency of halo concentration on mass, redshift and fossilness in Magneticum hydrodynamic simulations

Cited by 51 publications

References 85 publications

The core-cusp problem revisited: ULDM vs. CDM

The core-cusp problem revisited: ULDM vs. CDM

Cosmology dependence of galaxy cluster scaling relations

Halo Concentrations and the Fundamental Plane of Galaxy Clusters

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