Mass accretion rates and histories of dark matter haloes

By James McBride, Onsi Fakhouri, Chung-Pei Ma. 2009

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We use the extensive catalogue 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 per cent of the haloes to have MAHs that are well described by a 1-parameter exponential form. For the rest of the haloes, between 20 per cent (Milky Way mass) and 50 per cent (cluster mass) experience late-time growth that is steeper than an exponential, whereas the remaining haloes show plateaued 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 on to these haloes. These deviations from exponential growth are well fit by introducing a second parameter: M(z) ∝ (1 + z) β e ―γz . The full distribution of β and γ 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, M, as a function of redshift and mass. At z = 0, this rate is 42 M ⊙ yr ―1 for 10 12 M ⊙ haloes, which corresponds to a mean baryon accretion rate of M b = 7 M ⊙ yr ―1 . This mean rate increases approximately as (1 + z) 1.5 at low z and (1 + z) 2.5 at high z, reaching M b = 27, 69 and 140 M ⊙ yr ―1 at z = 1, 2 and 3. The specific rate depends on halo mass weakly: M/M ∝ M 0.127 . Results for the broad distributions about the mean rates are also discussed.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Instrumentation

View Paper: https://www.semanticscholar.org/paper/709ad0c56d0577c43031fa5decd58c273d2c13d2

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Citations in the corpus

THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8 (2012, methodology): “The mass bin we choose 6 Note that, forindividual halos, as opposed to ensemble medians or averages, the McBride et al. (2009) formula provides a reasonable fit: high pre- cision is not as necessary for cases when individual stochasti ity in merger events results in higher deviations than those…”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, methodology): “Equation 1 is important as it is very reminiscent of the halo mean growth rate, which has been shown to be Ṁh ∝ Mh s(1 + z)t with a mass index s greater than unity s ≃ 1.1 (Neistein & Dekel 2008; Genel et al. 2008; McBride et al. 2009) that is set by the shape of the initial dark matter (DM) power ”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, methodology): “…studied extensively via N -body simulations and extended Press-Schechter (1974) theory (Lacey & Cole 1993, 1994; Wechsler et al. 2002; van den Bosch 2002; Zhao et al. 2003b,a; Tasitsiomi et al. 2004; Cohn & White 2005; Neistein et al. 2006; Li et al. 2008; Zhao et al. 2009; McBride et al. 2009).”
A LINK BETWEEN STAR FORMATION QUENCHING AND INNER STELLAR MASS DENSITY IN SLOAN DIGITAL SKY SURVEY CENTRAL GALAXIES (2013, methodology): “The mass growth timescale can be estimated using the results of e.g., Wechsler et al. (2002); McBride et al. (2009); Dekel et al. (2013).”
A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, background): “46∗ ; Leauthaud et al. 2012) and the dark matter halo growth rates from N -body simulations (Ṁhalo ∝ (Mhalo)1.1; Wechsler et al. 2002; McBride et al. 2009; Fakhouri & Ma 2010) suggest a main sequence relationship of SFR ∝ M1.”
The impact of star formation feedback on the circumgalactic medium (2016, methodology): “The accretion rate at the turn around radius, Ṁta, is calibrated to match the mean rates measured by McBride et al. (2009) in the large, dark matter only, Millennium Simulation (Springel et al. 2005) – scaled appropriately by the cosmic baryon fraction fb = 0.17.”
A unified multiwavelength model of galaxy formation (2015, background): “McBride et al. (2009) found that a two parameter fit could describe halo formation histories measured from the Millennium Simulation of Springel et al. (2005), provided that the halos are divided into four different classes for which different values of the two parameters are adopted.”
The merger rates and mass assembly histories of dark matter haloes in the two Millennium simulations (2010, methodology): “In this paper, as in our previous work (Fakhouri & Ma 2008; McBride et al. 2009), our focus is on the merger and assembly histories of FOF haloes.”
The baryonic assembly of dark matter haloes (2011, methodology): “…the Press–Schechter and excursion set formalisms (Press & Schechter 1974; Bond et al. 1991) and fitting formulae for their merger and accretion rates (e.g. FMB10; Wechsler et al. 2002; Fakhouri & Ma 2008; Neistein & Dekel 2008; McBride et al. 2009; Genel et al. 2010), can be extended for baryons.”
Matter power spectrum and the challenge of percent accuracy (2015, background): “For the cosmological boxes investigated here, most haloes form around redshift two (see for example McBride et al. 2009) and the initial redshift should therefore not exceed z = 100.”
Lyα COOLING EMISSION FROM GALAXY FORMATION (2010, background): “…by Neistein & Dekel (2008) for the average halo mass accretion rate, we can write (for the WMAP5 cosmology) Ṁgas ≈ 210 M yr−1 ( M 1012 M )1.4( 1 + z 4 )2.5( fgas 0.165 ) , (A1) where fgas is the fraction of the accreted mass that is gaseous (see also McBride et al. 2009; Fakhouri et al. 2010).”
The local nanohertz gravitational-wave landscape from supermassive black hole binaries (2017, methodology): “We scale the stellar mass of the galaxy, M∗ , by a factor of 0.7, Ref (De Lucia & Blaizot 2007; McBride et al. 2009) (see Supplementary Figure 4), to estimate the mass of the descendent galaxy when we begin the SMBHB evolution, in the dynamical friction phase.”
ACCURATE UNIVERSAL MODELS FOR THE MASS ACCRETION HISTORIES AND CONCENTRATIONS OF DARK MATTER HALOS (2008, methodology): “Several months after this current paper was submitted to the Journal and the Internet, McBride et al. (2009) modeled the distribution of halo MAHs of the Millennium simulation by fitting individual MAHs with a twoparameter function, instead of the one-parameter function of W02.”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, background): “This assumption is well justified by dark matter mass accretion rates derived from N-body simulations (Wechsler et al. 2002; McBride et al. 2009; Fakhouri et al. 2010).”