On the density-profile slope of clusters of galaxies

Popolo, A. Del

doi:10.1111/j.1365-2966.2012.21141.x

Cited by 64 publications

(60 citation statements)

References 171 publications

(354 reference statements)

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“…6 (the non-extrapolated part of the plot) of [102], in terms of V c (which is 2.8 × 10 − 2M 0.316 vir [111]). We also found that the inner slope depends on the total baryonic content to total mass ratio [27], as seen later in [102]. [20,21] show a comparison of the change of the inner slope with mass with the simulations of [102].…”

Section: Ii3 Star Formation and Feedbacksupporting

confidence: 63%

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Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the ΛCDM model

et al. 2018

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Using a semianalytic code, we show how baryon physics in a ΛCDM cosmology could solve the discrepancy between numerical predictions of dark matter haloes and observations, ranging from dwarf galaxies to clusters, without the need of nonstandard dark matter models as advocated, for example, by [Kaplinghat et al., Phys. Rev. Lett. 116, 041302, (2016)]. Combining well established results, we show, for the first time, how accounting for baryon physics, in particular dynamical friction mechanisms, leads to flat galaxy-cluster profiles and correlations in several of their properties, solves the so-called "diversity problem" and reproduces very well the challenging, extremely low-rising rotation curve of IC2574. We therefore suggest treating baryonic physics properly before introducing new exotic features, albeit legitimate, in the standard cosmological model. * Corresponding author. adelpopolo@oact.inaf.it † francesco.pace@manchester.ac.uk ‡ delliou@ift.unesp.br § xgl@impcas.ac.cn 1 Note that the ΛCDM model suffers from others drawbacks like the cosmological constant problem [3,4], and the cosmic coincidence problem.

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Section: Ii3 Star Formation and Feedbacksupporting

confidence: 63%

“…Here we recall the model used above. First introduced by [17,18], many of its features were developed in [19][20][21], and allowed studies of the density profiles' universality [22,23], of the density profile of galaxies [24][25][26] and clusters [25,27], and of the inner surface-density of galaxies [28].…”

Section: Modelmentioning

confidence: 99%

Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the ΛCDM model

et al. 2018

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“…Despite recent progress in complex hydrodynamical simulations of clusters, there is still no consensus on the net effect of such feedback mechanisms on the inner density slope (see, e.g., Gnedin et al 2004;Martizzi et al 2012;Schaller et al 2015). In addition, dynamical processes due to infalling galaxies may also play a relevant role in producing a flat central slope (Nipoti et al 2004;Del Popolo 2012).…”

Section: Introductionmentioning

confidence: 99%

Mass distribution in the core of MACS J1206

Caminha

Grillo

Rosati

et al. 2017

A&A

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We present a new strong lensing analysis of the galaxy cluster MACS J1206.2−0847 (MACS 1206), at z = 0.44, using deep spectroscopy from CLASH-VLT and VLT/MUSE archival data in combination with imaging from the Cluster Lensing and Supernova survey with Hubble. MUSE observations enable the spectroscopic identification of 23 new multiply imaged sources, extending the previous compilations by a factor of approximately five. In total, we use the positional measurements of 82 spectroscopic multiple images belonging to 27 families at z = 1.0 − 6.1 to reconstruct the projected total mass distribution of MACS 1206. Remarkably, 11 multiple images are found within 50 kpc of the brightest cluster galaxy, making this an unprecedented set of constraints for the innermost projected mass distribution of a galaxy cluster. We thus find that, although dynamically relaxed, the smooth matter component (dark matter plus hot gas) of MACS 1206 shows a significant asymmetry, which closely follows the asymmetric distribution of the stellar component (galaxy members and intracluster light). We determine the value of the innermost logarithmic slope of the projected total mass density profile and find it to be close to the canonical Navarro-Frenk-White value. We demonstrate that this quantity is very robust against different parametrizations of the diffuse mass component; however, this is not the case when only one central image is used in the mass reconstruction. We also show that the mass density profile from our new strong lensing model is in very good agreement with dynamical and X-ray measurements at larger radii, where they overlap.

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“…In fact, this process transfers kinetic energy from baryons to dark matter, and this translates into a flattening of the dark matter density profile (e.g. El-Zant et al 2001;Del Popolo 2012).…”

Section: Stellar Mass Density Profilementioning

confidence: 99%

CLASH-VLT: Environment-driven evolution of galaxies in thez= 0.209 cluster Abell 209

Annunziatella

Mercurio

Biviano

et al. 2016

A&A

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Context. The analysis of galaxy properties, such as stellar masses, colors, sizes and morphologies, and the relations among them and the environment, in which the galaxies reside, can be used to investigate the physical processes driving galaxy evolution. Aims. We conduct a thorough study of the cluster A209 with a new large spectro-photometric dataset to investigate possible environmental effects on galaxy properties that can provide information on galaxy evolution in cluster hostile environments. Methods. We use the dataset obtained as part of the CLASH-VLT spectroscopic survey, supplemented with Subaru/SuprimeCam high-quality imaging in BVRIz-bands, which yields 1916 cluster members (50% of them spectroscopically confirmed) down to a stellar mass M = 10 8.6 M . We determine the stellar mass function of these galaxies in different regions of the cluster, by separating the sample into star-forming and passive cluster members. We then determine the intra-cluster light and its properties. We also derive the orbits of low-(M ≤ 10 10.0 M ) and high-mass (M > 10 10.0 M ) passive galaxies and study the effect of the environment on the mass-size relation of early-type galaxies, selected according to their Sérsic index; the effects are studied separately for the galaxies in each mass range. Finally, we compare the cluster stellar mass density profile with the number density and total-mass density profiles. Results. The stellar mass function of the star-forming cluster galaxies does not depend on the environment. The slope found for passive galaxies becomes flatter in the densest cluster region, which implies that the low-mass component starts to dominate when moving away from the cluster center. The color distribution of the intra-cluster light is consistent with the color of passive cluster members. The analysis of the dynamical orbits of passive galaxies shows that low-mass galaxies have tangential orbits, avoiding small pericenters around the BCG. The mass-size relation of low-mass passive early-type galaxies is flatter than that of high-mass galaxies, and its slope is consistent with the slope of the relation of field star-forming galaxies. Low-mass galaxies are also more compact within the scale radius of 0.65 Mpc. The ratio between the stellar and number density profiles shows a mass segregation effect in the cluster center. The comparative analysis of the stellar and total density profiles indicates that this effect is due to dynamical friction. Conclusions. Our results are consistent with a scenario in which the "environmental quenching" of low-mass galaxies is due to mechanisms such as harassment out to r 200 , starvation, and ram-pressure stripping at smaller radii. This scenario is supported by the analysis of the mass function, of the dynamical orbits and of the mass-size relation of passive early-type galaxies in different cluster regions. Moreover, our analyses support the idea that the intra-cluster light is formed through the tidal disruption of subgiant (M ∼ 10 9.5−10.0 M ) galaxies. In fact, o...

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On the density-profile slope of clusters of galaxies

Cited by 64 publications

References 171 publications

Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the ΛCDM model

Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the ΛCDM model

Mass distribution in the core of MACS J1206

CLASH-VLT: Environment-driven evolution of galaxies in thez= 0.209 cluster Abell 209

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