A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion

By A. Dutton, Frank C. van den Bosch, A. Dekel, S. Courteau. 2006

225 citations recorded by the source corpus.

We use observed rotation velocity-luminosity (VL) and size-luminosity (RL) relations to single out a specific scenario for disk galaxy formation in the ΛCDM cosmology. Our model involves four independent lognormal random variables: dark halo concentration c, disk spin λgal, disk mass fraction mgal, and stellar mass-to-light ratio ϒI. A simultaneous match of the VL and RL zero points with adiabatic contraction requires low-c halos, but this model has V2.2 ~ 1.8Vvir (where V2.2 and Vvir are the circular velocity at 2.2 disk scale lengths and the virial radius, respectively), which will be unable to match the luminosity function (LF). Similarly models without adiabatic contraction but standard c also predict high values of V2.2/Vvir. Models in which disk formation induces an expansion rather than the commonly assumed contraction of the dark matter halos have V2.2 ~ 1.2Vvir, which allows a simultaneous fit of the LF. This may result from nonspherical, clumpy gas accretion, where dynamical friction transfers energy from the gas to the dark matter. This model requires low λgal and mgal values, contrary to naive expectations. However, the low λgal is consistent with the notion that disk galaxies predominantly survive in halos with a quiet merger history, while a low mgal is also indicated by galaxy-galaxy lensing. The smaller than expected scatter in the RL relation and the lack of correlation between the residuals of the VL and RL relations, respectively, imply that the scatter in λgal and in c needs to be smaller than predicted for ΛCDM halos, again consistent with the idea that disk galaxies preferentially reside in halos with a quiet merger history.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3e2822be2068cbb520b396b6e4ad1ab49d44f338

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. Volker Springel
4. R. Somerville
5. Simon D. M. White
6. R. Dav'e
7. A. Dekel
8. T. Naab

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. Simon D. M. White
4. R. Somerville
5. Volker Springel
6. A. Dekel
7. R. Dav'e
8. T. Naab

Citations in the corpus

• HALO EXPANSION IN COSMOLOGICAL HYDRO SIMULATIONS: TOWARD A BARYONIC SOLUTION OF THE CUSP/CORE PROBLEM IN MASSIVE SPIRALS (2011, methodology): “In order to reproduce observational data, like the rotation velocity-luminosity and size-luminosity relations, models with NO adiabatic contraction (Gnedin et al. 2007, Courteau et al. 2007) or even with expansion (Dutton et al. 2007, 2011) are required (but also see Trujillo et al. 2010).”
• Ultradiffuse galaxies: the high-spin tail of the abundant dwarf galaxy population (2016, unknown): “In this paper, we show that the properties and abundance of UDGs in clusters are largely compatible with the classical model of disk formation (e.g., Fall & Efstathiou 1980; Dalcanton et al. 1997b; Mo et al. 1998; Dutton et al. 2007).”
• Towards a concordant model of halo occupation statistics (2006, background): “In addition, this reduction in halo concentrations also has important implications for the Tully–Fisher zero-point (see discussions in van den Bosch et al. 2003b and Dutton et al. 2007).”
• Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, methodology): “Indeed, including the effects of the baryons are important since they could increase the maximum circular velocity as a result of their gravitational effect over the halo (but see Dutton et al. 2007).”
• ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, result): “Our conclusions about spiral galaxies echo similar findings in the literature, which have typically inferred 〈fj〉 ∼ 0.5–0.6 overall (e.g., Navarro & Steinmetz 2000; Dutton et al. 2007; Burkert 2009; Dutton & van den Bosch 2012; Kassin et al. 2012).”
• THE CENTRAL SLOPE OF DARK MATTER CORES IN DWARF GALAXIES: SIMULATIONS VERSUS THINGS (2010, background): “Here we do not decontract the halos since in these galaxies adiabatic contraction does not occur and rather expansion happens as shown in Governato et al. (2010) (see also Dutton et al. 2007).”
• GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “The normalization of the current ΛCDM cosmological model is σ8 = 0.82 based on cosmic microwave background (CMB) and other data (e.g., Jarosik et al. 2011), which results in halo con centrations that are ∼30% lower than what Dutton et al. (2007) used in their preferred model.”
• There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, methodology): “Many more recent versions of the Mo, Mao, and White model (e.g., Dutton et al. 2007) modify this assumption only slightly.”
• Scaling relations and the fundamental line of the local group dwarf galaxies (2008, methodology): “The actual scalings of the stellar disc will be affected by the physics of the baryon gas and its interactions with the dark matter halo (Dutton et al. 2007).”
• The properties of the star-forming interstellar medium at z = 0.84-2.23 from HiZELS : mapping the internal dynamics and metallicity gradients in high-redshift disc galaxies. (2012, background): “8 we also show the relation between stellar mass and Hα half-light radius for the galaxies in our sample compared to the z = 0 relation from Dutton et al. (2007).”
• Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles (2014, background): “They also provide the backbone for the structural properties of galaxies and galaxy scaling relations (e.g., Mo et al. 1998; Dutton et al. 2007).”
• Scaling Relations of Spiral Galaxies (2007, background): “…reproduce the slope, zero-point, scatter, and color trends of the V L relation, match the shape and normalization of the local luminosity function, and explain the sizes, colors, and metallicity of disk galaxies (see, e.g., vdB00; Bell et al. 2003a; Dutton et al. 2007, hereafter D07).”
• THE SIZE–VIRIAL RADIUS RELATION OF GALAXIES (2012, background): “…first shown by Fall & Efstathiou (1980) and elaborated by Mo, Mao, & White (1998, see also Dalcanton et al. (1997); Avila-Reese et al. (1998, 2008); Dutton et al. (2007); Dutton (2009); Fu et al. (2010)), these scaling relations can be reproduced in a fairly simple framework, in which sizes of…”
• The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations (2015, methodology): “The distribution of matter in galaxies effectively determines the Tully-Fisher relation (e.g. Tully & Fisher 1976; Dutton et al. 2007).”
• Galaxy formation theory (2010, background): “…efficiency and supernovae feedback without the need for viscous redistribution of angularmomentum (Dutton 2009; Stringer et al. 2010), although the detailed properties (e.g. scale length distributions)of the disks do not necessarily agree perfectly with what is observed (Dutton et al. 2007).”
• THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, background): “…star formation and feedback, as well as on the disk formation mechanism and cosmological parameters, it represents a crucial test for galaxy evolution models (e.g. Silk et al. 1997; Steinmetz & Navarro 1999; 8 Cresci et al. van den Bosch 2000, 2002; Sommer-Larsen et al. 2003; Dutton et al. 2007).”