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On the Outskirts of Dark Matter Haloes
Cosmology and Nongalactic Astrophysics · Submitted 20 Oct 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that the (dimensionless) compensated halo profile, $r^3 \times \rho(r)/M_{200c}$ has a near-universal maximum in the small range $0.03-0.04$ around the virial radius, $r \simeq r_{\rm 200c}$, independent of the halo mass.
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The abstract, sentence by sentence
Halo Models of large scale structure provide powerful and indispensable tools for phenomenological understanding of the clustering of matter in the Universe. While the halo model builds structures out of the superposition of haloes, defining halo profiles in their outskirts - beyond their virial radii - becomes increasingly ambiguous, as one cannot assign matter to individual haloes in a clear way. In this paper, we tackle this question by using numerical N-body simulations to find a systematic definition of mean halo profile that can be extended to large radii. These profiles must be compensated and are the key ingredients for the computation of cosmological correlation functions in the Amended Halo Model. The latter, introduced in our earlier work (arXiv:1912.04872), provides a more physically accurate phenomenological description of nonlinear structure formation, which respects conservation laws on large scales. Here, we extend this model from the matter auto-power spectrum to the halo-matter cross-power spectra, using N-body simulations. We find that the (dimensionless) compensated halo profile, $r^3 \times \rho(r)/M_{200c}$ has a near-universal maximum in the small range $0.03-0.04$ around the virial radius, $r \simeq r_{\rm 200c}$, independent of the halo mass. The profiles cross zero into negative values in the halo outskirts, beyond 2-3$\times r_{\rm 200c}$, consistent with our previous results. We provide preliminary fitting functions for compensated Navarro-Frenk-White (NFW) profiles, and this can be used to compute more physical observables in the Amended Halo Model of large scale structure.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Halo Models of large scale structure provide powerful and indispensable tools for phenomenological understanding of the clustering of matter in the Universe. | background 1.00 | 0.04 | 0.02 | asserted 1.00 |
| s1 | While the halo model builds structures out of the superposition of haloes, defining halo profiles in their outskirts - beyond their virial radii - becomes increasingly ambiguous, as one cannot assign matter to individual haloes in a clear way. | gap 0.84 | 0.06 | 0.03 | asserted 0.99 |
| s2 | In this paper, we tackle this question by using numerical N-body simulations to find a systematic definition of mean halo profile that can be extended to large radii. | contribution 0.73 | 0.91 | 0.05 | asserted 0.91 |
| s3 | These profiles must be compensated and are the key ingredients for the computation of cosmological correlation functions in the Amended Halo Model. | background 0.56 | 0.23 | 0.07 | asserted 1.00 |
| s4 | The latter, introduced in our earlier work (arXiv:1912.04872), provides a more physically accurate phenomenological description of nonlinear structure formation, which respects conservation laws on large scales. | background 0.90 | 0.33 | 0.03 | asserted 1.00 |
| s5 | Here, we extend this model from the matter auto-power spectrum to the halo-matter cross-power spectra, using N-body simulations. | contribution 0.94 | 0.90 | 0.04 | asserted 0.93 |
| s6 | We find that the (dimensionless) compensated halo profile, $r^3 \times \rho(r)/M_{200c}$ has a near-universal maximum in the small range $0.03-0.04$ around the virial radius, $r \simeq r_{\rm 200c}$, independent of the halo mass. | result 1.00 | 0.97 | 0.60 | asserted 1.00 |
| s7 | The profiles cross zero into negative values in the halo outskirts, beyond 2-3$\times r_{\rm 200c}$, consistent with our previous results. | result 1.00 | 0.86 | 0.13 | hedged possibility 0.55 |
| s8 | We provide preliminary fitting functions for compensated Navarro-Frenk-White (NFW) profiles, and this can be used to compute more physical observables in the Amended Halo Model of large scale structure. | contribution 0.86 | 0.92 | 0.16 | asserted 0.53 |
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The paper
Original abstract
Halo Models of large scale structure provide powerful and indispensable tools for phenomenological understanding of the clustering of matter in the Universe. While the halo model builds structures out of the superposition of haloes, defining halo profiles in their outskirts - beyond their virial radii - becomes increasingly ambiguous, as one cannot assign matter to individual haloes in a clear way. In this paper, we tackle this question by using numerical N-body simulations to find a systematic definition of mean halo profile that can be extended to large radii. These profiles must be compensated and are the key ingredients for the computation of cosmological correlation functions in the Amended Halo Model. The latter, introduced in our earlier work (arXiv:1912.04872), provides a more physically accurate phenomenological description of nonlinear structure formation, which respects conservation laws on large scales. Here, we extend this model from the matter auto-power spectrum to the halo-matter cross-power spectra, using N-body simulations. We find that the (dimensionless) compensated halo profile, $r^3 \times \rho(r)/M_{200c}$ has a near-universal maximum in the small range $0.03-0.04$ around the virial radius, $r \simeq r_{\rm 200c}$, independent of the halo mass. The profiles cross zero into negative values in the halo outskirts, beyond 2-3$\times r_{\rm 200c}$, consistent with our previous results. We provide preliminary fitting functions for compensated Navarro-Frenk-White (NFW) profiles, and this can be used to compute more physical observables in the Amended Halo Model of large scale structure.
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References
How the literature uses it
1 arXiv paper cite this in 1 sentence
What it cites · 19 sentences without a confident label
Contests 1 paper
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However, SHM suffers from pathologies that stem from not enforcing the conservation laws [ref] .
Halo Models of Large Scale Structure · Introduction · contest 0.72
Builds on 1 paper
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In this paper, we built upon our previous study [ref] , to show that compensation – introduced as an important amendment of the halo model to respect physical conservation laws – can be applied to model both the auto-matter power spectrum and halo-matter cross-power spectra.
Amending the halo model to satisfy cosmological conservation laws · Conclusion and Future Prospects · 1.00
Uses the method or tool of 3 papers
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For calculating linear and numerical nonlinear power spectra for comparison with our model, we used the CAMB package in Python [ref] .
Revising the Halofit Model for the Nonlinear Matter Power Spectrum · Conclusion and Future Prospects · 0.99
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For calculating linear and numerical nonlinear power spectra for comparison with our model, we used the CAMB package in Python [ref] .
Halo occupation numbers and galaxy bias · Conclusion and Future Prospects · 0.99
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For calculating linear and numerical nonlinear power spectra for comparison with our model, we used the CAMB package in Python [ref] .
Efficient Computation of CMB anisotropies in closed FRW models · Conclusion and Future Prospects · 0.99
Uses data or values from 2 papers
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To find the compensated halo profile for AHM, $u_AHM(k|M)$ from Eq.([ref]), we use simulation data from DarkEmu [ref] for the auto halo power spectrum $P_hh$, and halo-mass cross-power spectrum $P_hm$.
Dark Quest. I. Fast and Accurate Emulation of Halo Clustering Statistics and Its Application to Galaxy Clustering · Results and Discussion · 0.95
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To do this, we adopt simulation data from the DarkEmu cosmological emulator suite [ref] - which uses Planck 2015 cosmology [ref] - to develop a novel and systematic method to directly measure mean compensated profiles from simulated (or emulated) halo-matter and halo-halo correlations.
Planck 2015 results. XV. Gravitational lensing · Introduction · 0.85
Compares with 1 paper
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We see that the nonlinear lensing power follows the data in Figures 2 $&$ 3 in [ref] more closely, which is what we would expect to see.
KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints · Lensing Power · 0.91
Cites as background 5 papers
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While the interior structure of dark matter haloes can be well modelled with the Navarro-Frenk-White (NFW) or Einasto profiles [ref] , the large scale distribution of dark matter in the outskirts of individual haloes is poorly understood in semi-analytic frameworks.
Einasto Profiles and the Dark Matter Power Spectrum · Introduction · 0.95
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While the interior structure of dark matter haloes can be well modelled with the Navarro-Frenk-White (NFW) or Einasto profiles [ref] , the large scale distribution of dark matter in the outskirts of individual haloes is poorly understood in semi-analytic frameworks.
The Structure of Cold Dark Matter Halos · Introduction · 0.95
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A potential observable for the power spectra of large scale structure is the cross halo-matter lensing power ( [ref] , [ref] ), which can be calculated using the Limber approximation [ref] .
Extended Limber Approximation · Lensing Power · 0.81
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