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Cusp-core transformations induced by AGN feedback in the progenitors of cluster galaxies
Cosmology and Nongalactic Astrophysics · Submitted 12 Nov 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo.
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The abstract, sentence by sentence
In a recent study (Martizzi et al. 2012), we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important in determining the spatial distribution of stars and dark matter in the central regions of these systems. The hierarchical assembly of dark matter, baryons and black holes obscures the physical mechanism behind the restructuring process. Here we use idealized simulations to follow the response of a massive dark matter halo as we feed the central black hole with a controlled supply of cold gas. This removes most of the complexity taking place in the cosmological simulations that may have biased our previous study. We confirm our previous results: gas heated and expelled from the central regions of the halo by AGN feedback can return after cooling; repeated cycles generate gravitational potential fluctuations responsible for irreversible modifications of the dark matter mass profile. The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo. According to the work presented here, outflow induced fluctuations represent the only mechanism able to efficiently create dark matter cores in clusters of galaxies.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In a recent study (Martizzi et al. 2012), we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important in determining the spatial distribution of stars and dark matter in the central regions of these systems. | background 0.97 | 0.63 | 0.04 | asserted 0.64 |
| s1 | The hierarchical assembly of dark matter, baryons and black holes obscures the physical mechanism behind the restructuring process. | gap 0.74 | 0.08 | 0.02 | asserted 0.99 |
| s2 | Here we use idealized simulations to follow the response of a massive dark matter halo as we feed the central black hole with a controlled supply of cold gas. | method 0.89 | 0.93 | 0.03 | asserted 0.93 |
| s3 | This removes most of the complexity taking place in the cosmological simulations that may have biased our previous study. | method 0.69 | 0.43 | 0.03 | hedged possibility 0.80 |
| s4 | We confirm our previous results: gas heated and expelled from the central regions of the halo by AGN feedback can return after cooling; repeated cycles generate gravitational potential fluctuations responsible for irreversible modifications of the dark matter mass profile. | result 0.97 | 0.88 | 0.22 | asserted 1.00 |
| s5 | The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo. | result 1.00 | 0.90 | 0.93 | asserted 1.00 |
| s6 | According to the work presented here, outflow induced fluctuations represent the only mechanism able to efficiently create dark matter cores in clusters of galaxies. | interpretation 0.91 | 0.72 | 0.52 | asserted 1.00 |
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The paper
Original abstract
In a recent study (Martizzi et al. 2012), we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important in determining the spatial distribution of stars and dark matter in the central regions of these systems. The hierarchical assembly of dark matter, baryons and black holes obscures the physical mechanism behind the restructuring process. Here we use idealized simulations to follow the response of a massive dark matter halo as we feed the central black hole with a controlled supply of cold gas. This removes most of the complexity taking place in the cosmological simulations that may have biased our previous study. We confirm our previous results: gas heated and expelled from the central regions of the halo by AGN feedback can return after cooling; repeated cycles generate gravitational potential fluctuations responsible for irreversible modifications of the dark matter mass profile. The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo. According to the work presented here, outflow induced fluctuations represent the only mechanism able to efficiently create dark matter cores in clusters of galaxies.
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References
How the literature uses it
12 arXiv papers cite this in 19 sentences
Papers citing it · 10 sentences without a confident label
Uses its method or tool 1 paper
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For the spatial distribution of bound gas, we adopt the profile of [ref] , which is a simplified version of the model from [ref] , chosen for its simplicity for calculations in Fourier space.
Probing baryonic feedback with fast radio bursts: joint analyses with cosmic shear and galaxy clustering · Bound gas · 0.90
Compares with it 4 papers
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The model demonstrated its robustness predicting before simulations the density flattening and shape produced by heating of DM, for galaxies [ref] in agreement with subsequent SPH simulations [ref] [ref] , and similarly for clusters of galaxies [ref] in agreement with hydro-simulations of [ref] , the inner density slope dependence on the halo mass and on the total baryonic content to the total mass ratio [ref] , in agreement with [ref] .
Barions and $\Lambda$CDM Model Problems · Summary of our semi-analytical model · 0.81
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Our cored DM profiles have a mean slope of $α=0.54 ±0.05$, in agreement with [ref] and [ref] .
Correlations in the matter distribution in CLASH galaxy clusters · Results and discussion · 0.97
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[Note that [ref] and [ref] adopted different dominant mechanisms.] * it aforetime predicted the halo mass dependence of cusps inner slope [ref] beforehand the similar result in the non-extrapolated part of the plot in [ref] , expressed in terms of $V_c$, as it corresponds to $2.8 ×10^-2 M_vir^0.316$ [ref] . * it also preceded [ref] in predicting [ref] that the inner slope depends on the total baryonic content to total mass ratio. * Fig. 6 in [ref] compares well with the inner slope change with mass of [ref] . * it moreover provides a comparison of the Tully-Fisher and Faber-Jackson, $M_Star-M_halo$, relationships with simulations [ref] .
Cluster density slopes from Dark Matter-Baryons Energy Transfer · Model robustness · 0.92
Cites it as background 2 papers
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However, some possible failures have been identified in the standard $Λ$CDM model at galactic and sub-galactic scales (e.g. the mismatch between the observed and expected numbers of satellites in the Milky Way; for a review of the small scale problems of the standard paradigm see [ref] ), although it is not clear if these issues can be resolved within the standard paradigm by considering e.g. baryonic effects [ref] .
N-body simulations of structure formation in thermal inflation cosmologies · Introduction · 0.83
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However, some possible shortcomings on small scales have been identified in the standard $Λ$CDM model (e.g. the mismatch in the number of satellites predicted by CDM and observed in the Milky Way; see [ref] for a recent review on these problems) although it is possible they can be solved within the standard paradigm by invoking e.g. baryonic physics [ref] .
A new smooth-$k$ space filter approach to calculate halo abundances · Introduction · 0.82
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