A mass-dependent density profile for dark matter haloes including the influence of galaxy formation

By A. Cintio, C. Brook, A. Dutton, A. Macciò, G. Stinson, A. Knebe. 2014

233 citations recorded by the source corpus.

ABSTRACT We introduce a mass dependent density proﬁle to describe the distribution of dark matterwithin galaxies, which takes into account the stellar-to-halo mass dependence of the responseof dark matter to baryonic processes. The study is based on the analysis of hydrodynamicallysimulated galaxies from dwarf to Milky Way mass, drawn from the MaGICC project, whichhave been shown to match a wide range of disk scaling relationships. We ﬁnd that the bestﬁt parameters of a generic double power-law density proﬁle v ary in a systematic manner thatdepends on the stellar-to-halo mass ratio of each galaxy. Thus, the quantity M ⋆ /M halo con-strains the inner (γ) and outer (β) slopes of dark matter density, and the sharpness of transitionbetween the slopes (α), reducing the number of free parameters of the model to two. Due tothe tight relation between stellar mass and halo mass, either of these quantities is sufﬁcient todescribe the dark matter halo proﬁle including the effects o f baryons. The concentrationof thehaloes in the hydrodynamicalsimulations is consistent with N-body expectations up to MilkyWay mass galaxies, at which mass the haloes become twice as concentrated as compared withpure dark matter runs.This mass dependent density proﬁle can be directly applied t o rotation curve data ofobserved galaxies and to semi analytic galaxy formation models as a signiﬁcant improvementover the commonly used NFW proﬁle.Key words:cosmology: dark matter galaxies: evolution - formation - hydrodynamics methods:N-bodysimulation

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5aea0c4525c92f2f2877628179c6a32a5295795d

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Citations in the corpus

The unexpected diversity of dwarf galaxy rotation curves (2015, background): “…2015, and our discussion below), there is growing consensus that the inner dark matter profiles can, in principle, be reshaped during the formation of a galaxy, even a dark-matterdominated one, in a manner that may depend on its merger history (see e.g. Di Cintio et al. 2014; Oñorbe et al. 2015).”
NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, methodology): “In comparison with a similar study performed earlier with the MaGICC sample (Di Cintio et al. 2014a, DC14)we have a larger and more coherent set of simulations, which have been performed with the latest compilation of cosmological parameters from the Planck Collaboration (2014).”
The milky way total mass profile as inferred from Gaia DR2 (2019, methodology): “Using the Di Cintio et al. (2014) predicted values for α, β and γ, we fitted the contracted NFW halo distribution in Figure 7 using Equation 13 with two free parameters, ρ0 and Rs.”
Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, background): “…in high resolution hydrodynamic simulations that resolve the interstellar medium (e.g. Mashchenko et al. 2008; Governato et al. 2010; Teyssier et al. 2013; Di Cintio et al. 2014; Trujillo-Gomez et al. 2015; Oñorbe et al. 2015; Read et al. 2016; and for a review see Pontzen & Governato 2014).”
The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, methodology): “Finally, Katz et al. (2016) have recently compared the Di Cintio et al. (2014) model to data for 147 rotation curves from the SPARC sample.”
Dark matter cores all the way down (2015, background): “Di Cintio et al. (2014) and Tollet et al. (2016) report a peak in core formation at ∼ 1010 M , with core formation ceasing below this mass scale; while Mashchenko et al. (2008), Madau et al. (2014), Oñorbe et al. (2015) and Verbeke et al. (2015) find substantial cores even in 109 M dwarfs.”
Core formation in dwarf haloes with self-interacting dark matter: no fine-tuning necessary (2014, background): “For example, baryonic processes may act to reduce and flatten the central densities of small galaxies in CDM (e.g. Pontzen & Governato, 2012; Governato et al., 2012; Di Cintio et al., 2014; Navarro et al., 1996).”
Dark matter heats up in dwarf galaxies (2018, methodology): “This is also in good quantitative agreement with predictions from recent DM heating models (Peñarrubia et al. 2012; Di Cintio et al. 2014a; Chan et al. 2015; Read et al. 2016a; Tollet et al. 2016).”
The Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations (2018, methodology): “…simulations, we follow Boylan-Kolchin et al. (2012) in fitting density profiles (here taken to be the α, β, γ model; e.g. Jaffe 1983; Hernquist 1990; Merritt et al. 2006 or Di Cintio et al. 2014b) to the resolved portion of each halo, then extrapolating the fits inward to compute Vcirc(r).”
NIHAO - XI. Formation of ultra-diffuse galaxies by outflows (2016, background): “…that feedback driven gas outflows are able to cause expansion not only of the central DM distribution in galaxies (e.g. Governato et al. 2010; Di Cintio et al. 2014a,b; Oñorbe et al. 2015; Tollet et al. 2016; Chan et al. 2015; Read et al. 2016), but also of the stellar one (e.g. Teyssier et…”
Is there a "too big to fail" problem in the field? (2014, background): “Nonetheless, the eff ct is still present at radii of 2− 3 kpc (e.g. Di Cintio et al. 2013, 2014), which means that it cannot be entirely ignored for most of the extreme dwarf galaxies in our sample.”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, methodology): “…in the small halo regime, M200 ≤ 1012 M , an (α, β, γ )-profile may be a good fit, the profiles of our most massive haloes, M200 ≥ 1013 M , show varying slopes down to small radii, r ≤ 0.05Rvir, and are unlikely to be well fit by such a function as was already suggested by Di Cintio et al. (2014).”
Gravitational probes of dark matter physics (2017, result): “Despite differences in code and the implementation of semi-analytic star formation prescriptions, there are now largely consistent results about the sign of the effect of baryons on halos on dwarf scales [255, 284, 372, 373, 374, 375, 376, 377, 378, 379, 352, 261].”