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The Radial Distribution of Galaxies in LCDM clusters
Astrophysics · Submitted 14 Aug 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Using the simulations that include cooling and starformation, we show that the radial distribution of subhalos is in reasonable agreement with the observed radial distribution of galaxies in clusters for 0.1<R/R200<2.0, if subhalos are selected using the stellar mass of galaxies.
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The abstract, sentence by sentence
We study the radial distribution of subhalos and galaxies using high-resolution cosmological simulations of galaxy clusters formed in the concordance LCDM cosmology. In agreement with previous studies, we find that the radial distribution of subhalos is significantly less concentrated than that of the dark matter, when subhalos are selected using their present-day gravitationally bound mass. We show that the difference in the radial distribution is not a numerical artifact and is due to tidal stripping. The subhalos in the cluster core lose more than 70% of their initial mass since accretion, while the average tidal mass loss for halos near the virial radius is ~30%. This introduces a radial bias in the spatial distribution of subhalos when they are selected using their tidally truncated mass. We demonstrate that the radial bias disappears almost entirely if subhalos are selected using their mass or circular velocity at the accretion epoch. The comparisons of the results of dissipationless simulations to the observed distribution of galaxies in clusters are therefore sensitive to the selection criteria used to select subhalo samples. Using the simulations that include cooling and starformation, we show that the radial distribution of subhalos is in reasonable agreement with the observed radial distribution of galaxies in clusters for 0.1<R/R200<2.0, if subhalos are selected using the stellar mass of galaxies. The radial bias is minimized in this case because the stars are located in the centers of dark matter subhalos and are tightly bound. The stellar mass of an object is therefore approximately conserved as the dark matter is stripped from the outer regions. Nevertheless, the concentration of the radial distribution of galaxies is systematically lower than that of the dark matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the radial distribution of subhalos and galaxies using high-resolution cosmological simulations of galaxy clusters formed in the concordance LCDM cosmology. | contribution 0.80 | 0.93 | 0.04 | asserted 0.84 |
| s1 | In agreement with previous studies, we find that the radial distribution of subhalos is significantly less concentrated than that of the dark matter, when subhalos are selected using their present-day gravitationally bound mass. | result 1.00 | 0.91 | 0.19 | asserted 1.00 |
| s2 | We show that the difference in the radial distribution is not a numerical artifact and is due to tidal stripping. | interpretation 0.71 | 0.92 | 0.16 | asserted 1.00 |
| s3 | The subhalos in the cluster core lose more than 70% of their initial mass since accretion, while the average tidal mass loss for halos near the virial radius is ~30%. | result 1.00 | 0.93 | 0.08 | asserted 1.00 |
| s4 | This introduces a radial bias in the spatial distribution of subhalos when they are selected using their tidally truncated mass. | result 0.59 | 0.86 | 0.14 | asserted 1.00 |
| s5 | We demonstrate that the radial bias disappears almost entirely if subhalos are selected using their mass or circular velocity at the accretion epoch. | result 0.98 | 0.95 | 0.20 | asserted 1.00 |
| s6 | The comparisons of the results of dissipationless simulations to the observed distribution of galaxies in clusters are therefore sensitive to the selection criteria used to select subhalo samples. | interpretation 0.97 | 0.51 | 0.25 | asserted 0.80 |
| s7 | Using the simulations that include cooling and starformation, we show that the radial distribution of subhalos is in reasonable agreement with the observed radial distribution of galaxies in clusters for 0.1<R/R200<2.0, if subhalos are selected using the stellar mass of galaxies. | result 0.96 | 0.96 | 0.41 | asserted 0.98 |
| s8 | The radial bias is minimized in this case because the stars are located in the centers of dark matter subhalos and are tightly bound. | interpretation 0.94 | 0.83 | 0.09 | asserted 1.00 |
| s9 | The stellar mass of an object is therefore approximately conserved as the dark matter is stripped from the outer regions. | interpretation 0.88 | 0.69 | 0.08 | asserted 0.97 |
| s10 | Nevertheless, the concentration of the radial distribution of galaxies is systematically lower than that of the dark matter. | result 0.97 | 0.89 | 0.28 | asserted 1.00 |
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The paper
Original abstract
We study the radial distribution of subhalos and galaxies using high-resolution cosmological simulations of galaxy clusters formed in the concordance LCDM cosmology. In agreement with previous studies, we find that the radial distribution of subhalos is significantly less concentrated than that of the dark matter, when subhalos are selected using their present-day gravitationally bound mass. We show that the difference in the radial distribution is not a numerical artifact and is due to tidal stripping. The subhalos in the cluster core lose more than 70% of their initial mass since accretion, while the average tidal mass loss for halos near the virial radius is ~30%. This introduces a radial bias in the spatial distribution of subhalos when they are selected using their tidally truncated mass. We demonstrate that the radial bias disappears almost entirely if subhalos are selected using their mass or circular velocity at the accretion epoch. The comparisons of the results of dissipationless simulations to the observed distribution of galaxies in clusters are therefore sensitive to the selection criteria used to select subhalo samples. Using the simulations that include cooling and starformation, we show that the radial distribution of subhalos is in reasonable agreement with the observed radial distribution of galaxies in clusters for 0.1<R/R200<2.0, if subhalos are selected using the stellar mass of galaxies. The radial bias is minimized in this case because the stars are located in the centers of dark matter subhalos and are tightly bound. The stellar mass of an object is therefore approximately conserved as the dark matter is stripped from the outer regions. Nevertheless, the concentration of the radial distribution of galaxies is systematically lower than that of the dark matter.
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References
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8 arXiv papers cite this in 9 sentences
Papers citing it · 7 sentences without a confident label
Cites it as support 1 paper
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The latter model takes into account the effect of gravitational tidal disruption of subhalos that is stronger and reduces the number of subhalos towards the central regions of the halo, and indeed is more likely to be the case according to numerical simulations [ref] (see also Refs. [ref] ).
Gamma-ray background anisotropy from galactic dark matter substructure · Models · 1.00
Cites it as background 1 paper
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It has long been argued that stellar mass and luminosity should correlate more strongly with the maximum value of a halo's circular velocity profile than with its halo mass [ref] , as the maximum circular velocity more directly traces the depth of the central potential well, and hence the ability to retain gas against feedback-driven outflows, independently of the halo's outer mass distribution.
Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium · Correlation with halo concentration · 0.88
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