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An Accurate Comprehensive Approach to Substructure: II. Stripped Subhaloes
Cosmology and Nongalactic Astrophysics · Submitted 14 Sep 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This derivation clarifies the role of halo concentration in substructure and unravels the origin of some key features found in simulations including the dependence of substructure on halo mass.
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The abstract, sentence by sentence
In Paper I we used the CUSP formalism to derive from first principles and no single free parameter the accurate abundance and radial distribution of both diffuse DM (dDM) and subhaloes accreted onto haloes and their progenitors at all previous times. Here we use those results as initial conditions for the monitoring of the evolution of subhaloes and dDM within the host haloes. Specifically, neglecting dynamical friction, we accurately calculate the effects of repetitive tidal stripping and heating on subhaloes as they orbit inside the host halo and infer the amount of dDM and subsubhaloes they release into the intra-halo medium. We then calculate the expected abundance and radial distribution of stripped subhaloes and dDM. This derivation clarifies the role of halo concentration in substructure and unravels the origin of some key features found in simulations including the dependence of substructure on halo mass. In addition, it unveils the specific effects of dynamical friction on substructure. The results derived here are for purely accreting haloes. In Paper III we complete the study by addressing the case of low-mass subhaloes, unaffected by dynamical friction, in ordinary haloes having suffered major mergers.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In Paper I we used the CUSP formalism to derive from first principles and no single free parameter the accurate abundance and radial distribution of both diffuse DM (dDM) and subhaloes accreted onto haloes and their progenitors at all previous times. | background 0.98 | 0.59 | 0.07 | asserted 1.00 |
| s1 | Here we use those results as initial conditions for the monitoring of the evolution of subhaloes and dDM within the host haloes. | method 0.91 | 0.84 | 0.04 | asserted 0.99 |
| s2 | Specifically, neglecting dynamical friction, we accurately calculate the effects of repetitive tidal stripping and heating on subhaloes as they orbit inside the host halo and infer the amount of dDM and subsubhaloes they release into the intra-halo medium. | method 0.89 | 0.95 | 0.10 | asserted 1.00 |
| s3 | We then calculate the expected abundance and radial distribution of stripped subhaloes and dDM. | result 0.67 | 0.95 | 0.30 | asserted 0.99 |
| s4 | This derivation clarifies the role of halo concentration in substructure and unravels the origin of some key features found in simulations including the dependence of substructure on halo mass. | interpretation 0.99 | 0.91 | 0.36 | asserted 1.00 |
| s5 | In addition, it unveils the specific effects of dynamical friction on substructure. | result 0.40 | 0.80 | 0.09 | asserted 1.00 |
| s6 | The results derived here are for purely accreting haloes. | limitation 1.00 | 0.66 | 0.05 | asserted 1.00 |
| s7 | In Paper III we complete the study by addressing the case of low-mass subhaloes, unaffected by dynamical friction, in ordinary haloes having suffered major mergers. | future work 0.98 | 0.25 | 0.04 | asserted 0.93 |
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Original abstract
In Paper I we used the CUSP formalism to derive from first principles and no single free parameter the accurate abundance and radial distribution of both diffuse DM (dDM) and subhaloes accreted onto haloes and their progenitors at all previous times. Here we use those results as initial conditions for the monitoring of the evolution of subhaloes and dDM within the host haloes. Specifically, neglecting dynamical friction, we accurately calculate the effects of repetitive tidal stripping and heating on subhaloes as they orbit inside the host halo and infer the amount of dDM and subsubhaloes they release into the intra-halo medium. We then calculate the expected abundance and radial distribution of stripped subhaloes and dDM. This derivation clarifies the role of halo concentration in substructure and unravels the origin of some key features found in simulations including the dependence of substructure on halo mass. In addition, it unveils the specific effects of dynamical friction on substructure. The results derived here are for purely accreting haloes. In Paper III we complete the study by addressing the case of low-mass subhaloes, unaffected by dynamical friction, in ordinary haloes having suffered major mergers.
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1 arXiv paper cite this in 1 sentence
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With the aim to shed light on this issue, a novel approach was applied in Paper I [ref] making use of the so-called ConflUent System of Peak trajectories (CUSP) formalism [ref] .
An Accurate Comprehensive Approach to Substructure: I. Accreted Subhaloes · INTRODUCTION · 0.86
Cites as background 2 papers
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High-resolution $N$-bdy simulations (e.g. [ref] ; [ref] , hereafter SWV; [ref] ) and, more recently, hydrodynamical simulations ( [ref] ; see also [ref] for the inclusion of gas using a semi-analytic treatment) have allowed to characterise their properties, while analytic models have been used to try to understand the origin of those properties (e.g. [ref] ).
The Uchuu Simulations: Data Release 1 and Dark Matter Halo Concentrations · INTRODUCTION · 0.99
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High-resolution $N$-bdy simulations (e.g. [ref] ; [ref] , hereafter SWV; [ref] ) and, more recently, hydrodynamical simulations ( [ref] ; see also [ref] for the inclusion of gas using a semi-analytic treatment) have allowed to characterise their properties, while analytic models have been used to try to understand the origin of those properties (e.g. [ref] ).
Can cosmological simulations capture the diverse satellite populations of observed Milky Way analogues? · INTRODUCTION · 0.99
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