Dark matter distribution in the Coma cluster from galaxy kinematics: breaking the mass–anisotropy degeneracy

Łokas, Ewa L.; Mamon, G. A.

doi:10.1046/j.1365-8711.2003.06684.x

Cited by 265 publications

(379 citation statements)

References 50 publications

(75 reference statements)

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“…The velocity dispersion agrees with the value in McConnell et al (2011McConnell et al ( , 2012, although the effective radius is smaller than their adopted 27 kpc. Further, we find rvir ≃ 2.45 Mpc and M d,vir ≃ 8.0 × 10 14 M⊙, which compare well to the values in Table A1 determined by Lokas & Mamon (2003). (This is even though NGC 4889 is not precisely at the centre of the Coma Cluster).…”

Section: A22 M87 and M49: σAp(re) ∼ 250 Km S −1supporting

confidence: 88%

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Dark-matter haloes and theM–σ relation for supermassive black holes

Larkin

McLaughlin

2016

Mon. Not. R. Astron. Soc.

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We develop models of two-component spherical galaxies to establish scaling relations linking the properties of spheroids at z = 0 (total stellar masses, effective radii R e and velocity dispersions within R e ) to the properties of their dark-matter halos at both z = 0 and higher redshifts. Our main motivation is the widely accepted idea that the accretion-driven growth of supermassive black holes (SMBHs) in protogalaxies is limited by quasar-mode feedback and gas blow-out. The SMBH masses, M BH , should then be connected to the dark-matter potential wells at the redshift z qso of the blowout. We specifically consider the example of a power-law dependence on the maximum circular speed in a protogalactic dark-matter halo: M BH ∝ V 4 d,pk , as could be expected if quasar-mode feedback were momentum-driven. For halos with a given V d,pk at a given z qso 0, our model scaling relations give a typical stellar velocity dispersion σ ap (R e ) at z = 0. Thus, they transform a theoretical "M BH -V d,pk relation" into a prediction for an observable M BH -σ ap (R e ) relation. We find the latter to be distinctly non-linear in log-log space. Its shape depends on the generic redshift-evolution of halos in a ΛCDM cosmology and the systematic variation of stellar-to-dark matter mass fraction at z = 0, in addition to any assumptions about the physics underlying the M BH -V d,pk relation. Despite some clear limitations of the form we use for M BH versus V d,pk , and even though we do not include any SMBH growth through dry mergers at low redshift, our results for M BH -σ ap (R e ) compare well to data for local early types if we take z qso ∼ 2-4.

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Section: A22 M87 and M49: σAp(re) ∼ 250 Km S −1supporting

confidence: 88%

“…The global dark matter properties of the Coma Cluster are taken from dynamical modelling by Lokas & Mamon (2003). They give values for rvir and M d,vir , rather than r200 and M d,200 like the other galaxies in Table A1, and a best-fitting NFW concentration of rvir/r−2 = 9.4.…”

Section: A13 Ngc 4889mentioning

confidence: 99%

Dark-matter haloes and theM–σ relation for supermassive black holes

Larkin

McLaughlin

2016

Mon. Not. R. Astron. Soc.

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“…where r −2 is the radius of density slope −2, in number (Lin et al 2004), luminosity (Łokas & Mamon 2003) and mass Biviano & Girardi 2003;Katgert et al 2004), with a concentration, c = r v /r −2 , of 3 to 5. For isotropic NFW models, the aperture velocity dispersion is (Appendix A of Mauduit & Mamon 2007) σ v = η v v , where η 0.62 (weakly dependent on concentration), and Eq.…”

Section: Introductionmentioning

confidence: 99%

The universal distribution of halo interlopers in projected phase space

Mamon

Biviano

Murante

2010

A&A

105

148

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When clusters of galaxies are viewed in projection, one cannot avoid picking up a fraction of foreground/background interlopers, that lie within the virial cone, but outside the virial sphere. Structural and kinematic deprojection equations are known for the academic case of a static Universe, but not for the real case of an expanding Universe, where the Hubble flow (HF) stretches the line-of-sight distribution of velocities. Using 93 mock relaxed clusters, built from the dark matter (DM) particles of a hydrodynamical cosmological simulation, we quantify the distribution of interlopers in projected phase space (PPS), as well as the biases in the radial and kinematical structure of clusters produced by the HF. The stacked mock clusters are well fit by an m = 5 Einasto DM density profile (but only out to 1.5 virial radii), with velocity anisotropy (VA) close to the Mamon-Łokas model with characteristic radius equal to that of density slope −2. The surface density of interlopers is nearly flat out to the virial radius, while their velocity distribution shows a dominant Gaussian cluster-outskirts component and a flat field component. This distribution of interlopers in PPS is nearly universal, showing only small trends with cluster mass, and is quantified. A local κ = 2.7 sigma velocity cut is found to return the line-ofsight velocity dispersion profile (LOSVDP) expected from the NFW density and VA profiles measured in three dimensions. The HF causes a shallower outer LOSVDP that cannot be well matched by the Einasto model for any value of κ. After this velocity cut, which removes 1 interloper out of 6, interlopers still account for 23 ± 1% of all DM particles with projected radii within the virial radius (surprisingly very similar to the observed fraction of cluster galaxies lying off the Red Sequence) and over 60% between 0.8 and 1 virial radius. The HF causes the best-fit projected NFW or m = 5 Einasto model to the stacked cluster to underestimate the true concentration measured in 3D by 6 ± 6% (16 ± 7%) after (before) the velocity cut. These biases in concentration are reduced by over a factor two once a constant background is included in the fit. The VA profile recovered from the measured LOSVDP by assuming the correct mass profile recovers fairly well the VA measured in 3D, with a slight, marginally significant, bias towards more radial orbits in the outer regions. These small biases in the concentration and VA of the galaxy system are overshadowed by important cluster-to-cluster fluctuations caused by cosmic variance and by the strong inefficiency caused by the limited numbers of observed galaxies in clusters. An appendix provides an analytical approximation to the surface density, projected mass and tangential shear profiles of the Einasto model. Another derives the expressions for the surface density and mass profiles of the NFW model projected on the sphere (for future kinematic modeling).

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“…Girardi et al 1998;Lokas & Mamon 2003;Lokas et al 2006;Mamon & Boué 2010;Falco et al 2014). Clusters of galaxies are a very important cosmological probe.…”

Section: Motivationmentioning

confidence: 99%

Weak lensing reconstructions in 2D and 3D: implications for cluster studies

Leonard

Lanusse

Starck

2015

Monthly Notices of the Royal Astronomical Society

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We compare the efficiency with which 2D and 3D weak lensing mass mapping techniques are able to detect clusters of galaxies using two state-of-the-art mass reconstruction techniques: MRLens in 2D and GLIMPSE in 3D. We simulate otherwise-empty cluster fields for 96 different virial mass-redshift combinations spanning the ranges 3 × 10 13 h −1 M ⊙ M vir 10 15 h −1 M ⊙ and 0.05 z cl 0.75, and for each generate 1000 realisations of noisy shear data in 2D and 3D. For each field, we then compute the cluster (false) detection rate as the mean number of cluster (false) detections per reconstruction over the sample of 1000 reconstructions. We show that both MRLens and GLIMPSE are effective tools for the detection of clusters from weak lensing measurements, and provide comparable quality reconstructions at low redshift. At high redshift, GLIMPSE reconstructions offer increased sensitivity in the detection of clusters, yielding cluster detection rates up to a factor of ∼ 10× that seen in 2D reconstructions using MRLens. We conclude that 3D mass mapping techniques are more efficient for the detection of clusters of galaxies in weak lensing surveys than 2D methods, particularly since 3D reconstructions yield unbiased estimators of both the mass and redshift of the detected clusters directly.

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Dark matter distribution in the Coma cluster from galaxy kinematics: breaking the mass–anisotropy degeneracy

Cited by 265 publications

References 50 publications

Dark-matter haloes and theM–σ relation for supermassive black holes

Dark-matter haloes and theM–σ relation for supermassive black holes

The universal distribution of halo interlopers in projected phase space

Weak lensing reconstructions in 2D and 3D: implications for cluster studies

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