Dark halo response and the stellar initial mass function in early-type and late-type galaxies

By A. Dutton, C. Conroy, Frank C. van den Bosch, L. Simard, J. Trevor Mendel, S. Courteau, A. Dekel, S. More, Francisco Prada. 2010

143 citations recorded by the source corpus.

We investigate the origin of the relations between stellar mass and optical circular velocity for early-type galaxies (ETGs) and late-type galaxies (LTGs) – the Faber–Jackson (FJ) and Tully–Fisher (TF) relations. We combine measurements of dark halo masses (from satellite kinematics and weak lensing), and the distribution of baryons in galaxies (from a new compilation of galaxy scaling relations), with constraints on dark halo structure from cosmological simulations. The principal unknowns are the halo response to galaxy formation and the stellar initial mass function (IMF). The slopes of the TF and FJ relations are naturally reproduced for a wide range of halo response and IMFs. However, models with a universal IMF and universal halo response cannot simultaneously reproduce the zero-points of both the TF and FJ relations. For a model with a universal Chabrier IMF, LTGs require halo expansion, while ETGs require halo contraction. A Salpeter IMF is permitted for high-mass (σ≳ 180 km s−1) ETGs, but is inconsistent for intermediate masses, unless Vcirc(Re)/σe≳ 1.6. If the IMF is universal and close to Chabrier, we speculate that the presence of a major merger may be responsible for the contraction in ETGs while clumpy accreting streams and/or feedback leads to expansion in LTGs. Alternatively, a recently proposed variation in the IMF disfavours halo contraction in both types of galaxies. Finally we show that our models naturally reproduce flat and featureless circular velocity profiles within the optical regions of galaxies without fine-tuning.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/452d556a3f398741536dc94218bf9bdf956c6448

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Citations in the corpus

Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, methodology): “While there is an extensive discussion in the literature of what is the right value for K, following Dutton et al. (2011) here we assume that K = 1.54 which is a value halfway between different groups.”
H0LiCOW – IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant (2018, unknown): “(ii) Option COMPOSITE: We split the luminous and dark component of the lens model into two composite parts (see, e.g., Dutton et al. 2011).”
Cosmological simulations with self-interacting dark matter – II. Halo shapes versus observations (2012, result): “…density within 10 kpc may also be a sign that the inner part of the dark-matter halo has been compressed as a consequence of assembly of the elliptical galaxy, a compression that has been observed in other studies of elliptical galaxies (Schulz, Mandelbaum & Padmanabhan 2010; Dutton et al. 2011).”
Self-Interacting Dark Matter from a Non-Abelian Hidden Sector (2014, background): “Conversely, observations show that low-surface-brightness spiral galaxies (LSBs) [35–42], satellite dwarf galaxies [41, 43], and galaxy clusters [44–49] exhibit constant-density cores.”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “1 of Dutton et al. (2011b).”
Why does the environmental influence on group and cluster galaxies extend beyond the virial radius (2012, background): “…to the lowest (stellar) mass galaxies in our sample, however, appears to be at odds with observations, which show that it is in factlow-massgalaxies that tend to have c© 0000 RAS, MNRAS000, 000–000 larger cold gas mass fractions (e.g., Dutton et al. 2011) andsSFRs (e.g., Salim et al. 2007).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “9 shows the projected half-mass radius of cold gas in the simulated galaxies (at z = 0) as a function of stellar mass and compares them with H I observations compiled by Dutton et al. (2011) from Swaters et al. (1999) and Verheijen (2001).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “Other authors have come to the same conclusions (e.g., Williams et al. 2010; Dutton et al. 2010, 2011).”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, methodology): “This dataset was already analysed by Dutton et al. (2011) and we follow their method to convert galaxy luminosities into (MPA/JHU group) stellar masses, with the appropriate normalization for a Chabrier (2003) IMF.”
The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, background): “Un-contracted or expandedhaloes are required (Dutton et al. 2007, 2011).”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, methodology): “In addition, following McCarthy et al. (2012) and Dutton et al. (2011), we applied a small correction to the stellar masses using the expression given in the appendix of Li & White (2009) to improve the consistency with those derived from more accurate five-band SDSS data.”
Galaxy Masses: A Review (2013, background): “The total mass of the disk is Md = 2πΣ0R 2 d. Dutton et al. (2011b) show that disk scale lengths of the gas are on average 1.5 times greater than disk scale lengths measured in the R-band light.”
A mass-dependent density profile for dark matter haloes including the influence of galaxy formation (2014, unknown): “Finally, a high concentration could arise possible tensions with the Tully–Fisher relation (Dutton et al. 2011 ) and the Fundamental Plane (Dutton et al. 2013) for high-mass spirals, but this issue has to be explored in more detail once other effects relevant at L ∗ scales, such as feedback from…”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “…less concentrated and less cuspy than predicted in CDM simulations (e.g. Flores & Primack 1994; Simon et al. 2005; Kuzio de Naray et al. 2008; de Blok 2010; Dutton et al. 2011; Kuzio de Naray & Spekkens 2011; Oh et al. 2011; Walker & Peñarrubia 2011; Salucci et al. 2012; Castignani et al. 2012).”
How sensitive are predicted galaxy luminosities to the choice of stellar population synthesis model (2013, result): “A3 compares the predicted and observed me-Figure dian half-light radii of early and late-type galaxies at z = 0 (Shen et al. 2003; Dutton et al. 2011).”
The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, methodology): “The recovered stellar mass depends on both the assumed DM profile in the centre and at large radii (Dutton et al. 2011b).”