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Internal properties and environments of dark matter halos
Cosmology and Nongalactic Astrophysics · Submitted 5 Jul 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim For halos at a fixed mass, all the halo properties depend significantly on environment, particularly the tidal field.
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The abstract, sentence by sentence
We use seven high-resolution $N$-body simulations to study the correlations among different halo properties (assembly time, spin, shape and substructure), and how these halo properties are correlated with the large-scale environment in which halos reside. The large-scale tidal field estimated from halos above a mass threshold is used as our primary quantity to characterize the large-scale environment, while other parameters, such as the local overdensity and the morphology of large-scale structure, are used for comparison. For halos at a fixed mass, all the halo properties depend significantly on environment, particularly the tidal field. The environmental dependence of halo assembly time is primarily driven by local tidal field. The mass of the unbound fraction in substructure is boosted in strong tidal force region, while the bound fraction is suppressed. Halos have a tendency to spin faster in stronger tidal field and the trend is stronger for more massive halos. The spin vectors show significant alignment with the intermediate axis of the tidal field, as expected from the tidal torque theory. Both the major and minor axes of halos are strongly aligned with the corresponding principal axes of the tidal field. In general, a halo that can accrete more material after the formation of its main halo on average is younger, is more elongated, spins faster, and contains a larger amount of substructure. Higher density environments not only provide more material for halo to accrete, but also are places of stronger tidal field that tends to suppress halo accretion. The environmental dependencies are the results of these two competing effects. The tidal field based on halos can be estimated from observation, and we discuss the implications of our results for the environmental dependence of galaxy properties.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We use seven high-resolution $N$-body simulations to study the correlations among different halo properties (assembly time, spin, shape and substructure), and how these halo properties are correlated with the large-scale environment in which halos reside. | contribution 0.87 | 0.96 | 0.05 | asserted 0.80 |
| s1 | The large-scale tidal field estimated from halos above a mass threshold is used as our primary quantity to characterize the large-scale environment, while other parameters, such as the local overdensity and the morphology of large-scale structure, are used for comparison. | method 1.00 | 0.92 | 0.04 | asserted 0.97 |
| s2 | For halos at a fixed mass, all the halo properties depend significantly on environment, particularly the tidal field. | result 1.00 | 0.92 | 0.54 | asserted 1.00 |
| s3 | The environmental dependence of halo assembly time is primarily driven by local tidal field. | result 0.91 | 0.92 | 0.16 | asserted 1.00 |
| s4 | The mass of the unbound fraction in substructure is boosted in strong tidal force region, while the bound fraction is suppressed. | result 1.00 | 0.90 | 0.06 | asserted 1.00 |
| s5 | Halos have a tendency to spin faster in stronger tidal field and the trend is stronger for more massive halos. | result 1.00 | 0.93 | 0.09 | asserted 0.95 |
| s6 | The spin vectors show significant alignment with the intermediate axis of the tidal field, as expected from the tidal torque theory. | result 0.98 | 0.87 | 0.07 | asserted 1.00 |
| s7 | Both the major and minor axes of halos are strongly aligned with the corresponding principal axes of the tidal field. | result 1.00 | 0.92 | 0.09 | asserted 1.00 |
| s8 | In general, a halo that can accrete more material after the formation of its main halo on average is younger, is more elongated, spins faster, and contains a larger amount of substructure. | result 0.99 | 0.90 | 0.15 | asserted 0.88 |
| s9 | Higher density environments not only provide more material for halo to accrete, but also are places of stronger tidal field that tends to suppress halo accretion. | interpretation 0.84 | 0.63 | 0.13 | asserted 1.00 |
| s10 | The environmental dependencies are the results of these two competing effects. | interpretation 0.98 | 0.65 | 0.15 | asserted 1.00 |
| s11 | The tidal field based on halos can be estimated from observation, and we discuss the implications of our results for the environmental dependence of galaxy properties. | interpretation 0.91 | 0.55 | 0.05 | asserted 0.90 |
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The paper
Original abstract
We use seven high-resolution $N$-body simulations to study the correlations among different halo properties (assembly time, spin, shape and substructure), and how these halo properties are correlated with the large-scale environment in which halos reside. The large-scale tidal field estimated from halos above a mass threshold is used as our primary quantity to characterize the large-scale environment, while other parameters, such as the local overdensity and the morphology of large-scale structure, are used for comparison. For halos at a fixed mass, all the halo properties depend significantly on environment, particularly the tidal field. The environmental dependence of halo assembly time is primarily driven by local tidal field. The mass of the unbound fraction in substructure is boosted in strong tidal force region, while the bound fraction is suppressed. Halos have a tendency to spin faster in stronger tidal field and the trend is stronger for more massive halos. The spin vectors show significant alignment with the intermediate axis of the tidal field, as expected from the tidal torque theory. Both the major and minor axes of halos are strongly aligned with the corresponding principal axes of the tidal field. In general, a halo that can accrete more material after the formation of its main halo on average is younger, is more elongated, spins faster, and contains a larger amount of substructure. Higher density environments not only provide more material for halo to accrete, but also are places of stronger tidal field that tends to suppress halo accretion. The environmental dependencies are the results of these two competing effects. The tidal field based on halos can be estimated from observation, and we discuss the implications of our results for the environmental dependence of galaxy properties.
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References
How the literature uses it
10 arXiv papers cite this in 13 sentences
Papers citing it · 7 sentences without a confident label
Compares with it 2 papers
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Our results found in projection are consistent with previous 3D analyses [ref] (Ref. [ref] shows a 2D projected misalignment angle of order $10^∘$).
Boosting (In)direct Detection of Dark Matter · Correlation with Baryon Disk · 0.84
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Our results found in projection are consistent with previous 3D analyses [ref] (Ref. [ref] shows a 2D projected misalignment angle of order $10^∘$).
Spherical Cows in Dark Matter Indirect Detection · Correlation with Baryon Disk · 0.80
Cites it as support 1 paper
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It is known that the mass fraction of the main substructure $f_main$ is tightly correlated with $a_1/2$ in high-resolution N-body simulations [ref] ; the relationship is robust for different masses of the host halos.
Effects of Neutrino Masses and Asymmetries on Dark Matter Halo Assembly · Halo formation time $a_1/2$ · 0.97
Cites it as background 3 papers
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A large number of simulations have been used to study the correlations between halo properties like mass, concentration, accretion history, spin, shape, substructure and environment [ref] and to investigate the dependence of halo clustering on several of these parameters [ref] .
The correlation structure of dark matter halo properties · Introduction · 0.99
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While the spherically averaged density profiles of dark matter halos first described by [ref] (NFW) are good fits to both simulations and many observations, deviations from halo sphericity can be important for detailed comparisons of observations with the CDM model [ref] .
The Shapes and Alignments of Dark Matter Halos · Introduction · 0.96
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Examples include characterization of average properties (e.g. see [ref] for one early review, [ref] for some more recent papers and references within), identifying the web in observations and simulations (e.g., [ref] , tracing its relation to initial conditions (e.g., [ref] ) and comparing filamentary environments and properties of galaxies within them (spin, shapes, alignments and more: [ref] ).
The geometry of the filamentary environment of galaxy clusters · Introduction · 0.99
Discussion
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