Mass Accretion Rates and Histories of Dark Matter Haloes

Chung-Pei Ma; James McBride; Onsi Fakhouri

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Mass Accretion Rates and Histories of Dark Matter Haloes

James McBride, Onsi Fakhouri, Chung-Pei Ma

Cosmology and Nongalactic Astrophysics · Submitted 23 Feb 2009

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We find only about 25% of the haloes to have MAHs that are well described by a 1-parameter exponential form.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.42 · human participants 0.01 · controlled comparison 0.14 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.42 · mentions code or data availability 0.03.

The abstract, sentence by sentence

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We use the extensive catalog of dark matter haloes from the Millennium simulation to investigate the statistics of the mass accretion histories (MAHs) and accretion rates of ~500,000 haloes from redshift z=0 to 6. We find only about 25% of the haloes to have MAHs that are well described by a 1-parameter exponential form. For the rest of the haloes, between 20% (Milky-Way mass) to 50% (cluster mass) experience late-time growth that is steeper than an exponential, whereas the remaining haloes show plateau-ed late-time growth that is shallower than an exponential. The haloes with slower late-time growth tend to reside in denser environments, suggesting that either tidal stripping or the "hotter" dynamics are suppressing the accretion rate of dark matter onto these haloes. These deviations from exponential growth are well fit by introducing a second parameter: M(z) \propto (1+z)^beta exp(-gamma z). The full distribution of beta and gamma as a function of halo mass is provided. From the analytic form of M(z), we obtain a simple formula for the mean accretion rate of dark matter, dM/dt, as a function of redshift and mass. At z=0, this rate is 42 Msun/yr for 1e12 Msun haloes, which corresponds to a mean baryon accretion rate of dMbaryon/dt=7 Msun/yr. This mean rate increases approximately as (1+z)^1.5 at low z and (1+z)^2.5 at high z, reaching dMbaryon/dt = 27, 69, and 140 Msun/yr at z=1, 2, and 3. The specific rate depends on halo mass weakly: dlogM/dt \propto M^0.127. Results for the broad distributions about the mean rates are also discussed.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We use the extensive catalog of dark matter haloes from the Millennium simulation to investigate the statistics of the mass accretion histories (MAHs) and accretion rates of ~500,000 haloes from redshift z=0 to 6.	method 0.68	0.95	0.04	asserted 0.92
s1	We find only about 25% of the haloes to have MAHs that are well described by a 1-parameter exponential form.	result 1.00	0.97	0.21	asserted 1.00
s2	For the rest of the haloes, between 20% (Milky-Way mass) to 50% (cluster mass) experience late-time growth that is steeper than an exponential, whereas the remaining haloes show plateau-ed late-time growth that is shallower than an exponential.	result 1.00	0.95	0.24	asserted 1.00
s3	The haloes with slower late-time growth tend to reside in denser environments, suggesting that either tidal stripping or the "hotter" dynamics are suppressing the accretion rate of dark matter onto these haloes.	interpretation 0.97	0.85	0.10	hedged possibility 0.99
s4	These deviations from exponential growth are well fit by introducing a second parameter: M(z) \propto (1+z)^beta exp(-gamma z).	result 0.74	0.92	0.21	asserted 1.00
s5	The full distribution of beta and gamma as a function of halo mass is provided.	result 0.77	0.94	0.08	asserted 0.97
s6	From the analytic form of M(z), we obtain a simple formula for the mean accretion rate of dark matter, dM/dt, as a function of redshift and mass.	result 0.50	0.95	0.11	asserted 1.00
s7	At z=0, this rate is 42 Msun/yr for 1e12 Msun haloes, which corresponds to a mean baryon accretion rate of dMbaryon/dt=7 Msun/yr.	result 1.00	0.92	0.09	asserted 1.00
s8	This mean rate increases approximately as (1+z)^1.5 at low z and (1+z)^2.5 at high z, reaching dMbaryon/dt = 27, 69, and 140 Msun/yr at z=1, 2, and 3.	result 1.00	0.94	0.09	asserted 0.99
s9	The specific rate depends on halo mass weakly: dlogM/dt \propto M^0.127.	result 1.00	0.93	0.06	asserted 1.00
s10	Results for the broad distributions about the mean rates are also discussed.	result 0.70	0.85	0.03	unclear 0.64

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 0.77.

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arXiv listing abstract v2

not examined

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The paper

Original abstract

We use the extensive catalog of dark matter haloes from the Millennium simulation to investigate the statistics of the mass accretion histories (MAHs) and accretion rates of ~500,000 haloes from redshift z=0 to 6. We find only about 25% of the haloes to have MAHs that are well described by a 1-parameter exponential form. For the rest of the haloes, between 20% (Milky-Way mass) to 50% (cluster mass) experience late-time growth that is steeper than an exponential, whereas the remaining haloes show plateau-ed late-time growth that is shallower than an exponential. The haloes with slower late-time growth tend to reside in denser environments, suggesting that either tidal stripping or the "hotter" dynamics are suppressing the accretion rate of dark matter onto these haloes. These deviations from exponential growth are well fit by introducing a second parameter: M(z) \propto (1+z)^beta exp(-gamma z). The full distribution of beta and gamma as a function of halo mass is provided. From the analytic form of M(z), we obtain a simple formula for the mean accretion rate of dark matter, dM/dt, as a function of redshift and mass. At z=0, this rate is 42 Msun/yr for 1e12 Msun haloes, which corresponds to a mean baryon accretion rate of dMbaryon/dt=7 Msun/yr. This mean rate increases approximately as (1+z)^1.5 at low z and (1+z)^2.5 at high z, reaching dMbaryon/dt = 27, 69, and 140 Msun/yr at z=1, 2, and 3. The specific rate depends on halo mass weakly: dlogM/dt \propto M^0.127. Results for the broad distributions about the mean rates are also discussed.

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References

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Baryonic Imprints on DM Halos: the concentration-mass relation and its dependence on 28 model parameters in the CAMELS suite
astro-ph.CO 2026-10 conditional novelty 6.0 of 10

The concentration-mass relation responds measurably to all 28 varied simulation parameters, and three fitted patterns capture most of the baryonic imprints.
Constraining Dissipative Dark Matter Self-Interactions
hep-ph 2018-09 conditional novelty 6.0 of 10

Dissipative dark matter self-interactions with 0.1 to 1 times the elastic cross section and 10 to 100 km/s energy loss per collision would have collapsed the cores of observed dwarf galaxies within 10 Gyr, so they are...

How later papers used it

66 later papers cite it

Evidence: substantial. 65 of the citing papers share no author with it, and 21 of those carry a confident label from Pith's citation classifier.

Pith read 22 of the 104 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

6 later papers by other authors are listed below: 3 used its method or tool, 2 used its data or values and 1 compared its own results with it.

Uses its method or tool 3 of 10 papers with this label

We use the parameterization of [ref] (equation [ref]) to functionally model all the mass accretion histories in our simulation: once over the entire history and again over a portion of the early history out to specified truncation points.

Reversing Arrested Development: A New Method to Address Halo Assembly Bias (2024) · Fitting the Mass Accretion Histories · 0.97
Assumed an NFW profile for the dark matter component at each timestep, with mass growth following this paper.

The impact of hot mode accretion and angular momentum conservation on metallicity gradients of galactic discs (2026) · 0.87 · paraphrased: the licence does not allow quoting
Fit the mass accretion history with this paper's functional form, with two free parameters.

Characterizing the assembly of dark matter halos with protohalo size histories: I. Redshift evolution, relation to descendant halos, and halo assembly bias (2023) · 1.00 · paraphrased: the licence does not allow quoting

Uses its data or values 2 of 6 papers with this label

Chose its accretion rates to match the mean rates measured in the Millennium simulation by this paper, multiplying the dark matter accretion rate by the cosmic baryon fraction of about 0.16.

First results from SMAUG: Uncovering the Origin of the Multiphase Circumgalactic Medium with a Comparative Analysis of Idealized and Cosmological Simulations (2020) · 0.98 · paraphrased: the licence does not allow quoting
A fiducial value for the capture rate is the accretion rate calculated for the Millennium simulation [ref] , modified for a contribution from PBH DM, as expressed in the PBH mass fraction $f_PBH$: [equation] This is of the same order of magnitude as the accretion rate obtained by integrating over all PBHs with a characteristic mass of $100 M_⊙$ in a $10^12 M_h$ halo at $z=0$, as given by Equ.([ref])-([ref]).

Distinguishing the impact and signature of black holes from different origins in early cosmic history (2023) · Black Holes in haloes · 0.82

Compares with it 1 of 5 papers with this label

Compared its own median mass accretion history of the Auriga suite with this paper's curve, finding it coincident for z<1 and roughly following it for z>2.

The Hestia project: simulations of the Local Group (2020) · 0.85 · paraphrased: the licence does not allow quoting

How the literature uses it

7 arXiv papers cite this in 11 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 7 sentences without a confident label

Uses its data or values 1 paper

We begin with the dark matter accretion rate from [ref] and [ref] , which quantified the mass accretion histories of all dark matter halos with masses above $∼10^10$ M$_⊙$ in the two Millennium simulations of a $Λ$CDM universe [ref] .

The Gas Consumption History to z ~ 4 · Comparing $d/dt$ to Dark Matter Accretion Rate · 0.98

Compares with it 1 paper

[ref] have also recently computed the formation times of massive halos from the MS and fitted to the relation $z_f = a log_10(M/10^12 M_⊙) + b$.

Resolving Cosmic Structure Formation with the Millennium-II Simulation · Formation Times · 0.86

Cites it as support 1 paper

On the contrary, GCs sustain a continuously replenished cool gas reservoir through cosmological accretion with more massive halos [ref] , tidal-torque-driven inflow from satellite encounters [ref] , and minor mergers.

Even central galaxies feel their environment: cosmic siphoning of cool gas accretion · Discussion · 0.99

Cites it as background 1 paper

A more stringent test is to consider the mass accretion history[for a discussion of the statistical properties of mass accretion histories, see [ref] .] for each Aquarius halo and to compare results from the Aquarius resimulations and from the .

Resolving Cosmic Structure Formation with the Millennium-II Simulation · Comparing Aquarius and Millennium-II halos · 0.96

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