Mass Density Profiles of Low Surface Brightness Galaxies

By W. D. de Blok, S. McGaugh, A. Bosma, V. R. Atnf, Sydney Univ Maryland Obs. de Marseille Dtm, Dc Washington. 2001

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We derive the mass density profiles of dark matter halos that are implied by high spatial resolution rotation curves of low surface brightness galaxies. We find that, at small radii, the mass density distribution is dominated by a nearly constant density core with a core radius of a few kiloparsecs. For ρ(r) ~ rα, the distribution of inner slopes α is strongly peaked around α = -0.2. This is significantly shallower than the cuspy α ≤ -1 halos found in cold dark matter simulations. While the observed distribution of α does have a tail toward such extreme values, the derived value of α is found to depend on the spatial resolution of the rotation curves: α ≈ -1 is found only for the least well resolved galaxies. Even for these galaxies, our data are also consistent with constant-density cores (α = 0) of modest (~1 kpc) core radius, which can give the illusion of steep cusps when insufficiently resolved. Consequently, there is no clear evidence for a cuspy halo in any of the low surface brightness galaxies observed.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

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Citations in the corpus

A Neutral Hydrogen Survey of the Large Magellanic Cloud: Aperture Synthesis and Multibeam Data Combined (2003, unknown): “The shape of the inner velocity field, using H i as a tracer, can discriminate between different halo models (de Blok et al. 2001).”
Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, result): “G A ] 1991; Moore 1994; Navarro et al. 1996b) in stark contrast with observed rotation curves that favour constant density ‘cores’ (e.g. Flores & Primack 1994; de Blok et al. 2001; de Blok 2009; Oh et al. 2011, 2015; Hague & Wilkinson 2013, 2014; Adams et al. 2014; Oh et al. 2015).”
Maximum feedback and dark matter profiles of dwarf galaxies (2001, background): “Recent observations of the gasrich dwarfs show a nearly solid-body rotation curve, which implies a finite core inside a few hundred pc (van den Bosch et al. 2000; de Blok et al. 2001).”
The First Cosmic Structures and Their Effects (2004, background): “…curves of Low Surface Brightness Galaxies (LSBGs) and late-type dwarf galaxies (e.g. van den Bosch et al. 2000; Borriello & Salucci 2001; de Blok et al. 2001; van den Bosch & Swaters 2001; de Blok, Bosma & McGaugh 2003; Kleyna et al. 2003), which are sometimes consistent with both a…”
The structure of voids (2003, background): “…matter satellites of haloes the size of the Milky Way (Klypin et al. 1999a; Moore et al. 1999); and problems with explaining rotation curves in central parts of dwarf and low-surface-brightness galaxies (e.g. Flores & Primack 1994; Moore 1994; de Blok et al. 2001; van den Bosch & Swaters 2001).”
Uncovering cold dark matter halo substructure with tidal streams (2001, background): “However, this appears not to be the case, as recent (high spatial resolution) Hα rotation curves have shown (Côté et al. 2000; de Blok et al. 2001; Marchesini et al. 2001).”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “…in the range 50 − 130 km/s, constant-density cores with sizes of∼ 0.5 − 8 kpc and central densities of approximately∼ 0.01 − 0.5M⊙/pc 3 have been observed (de Blok et al. 2001; Simon et al. 2005; Sánchez-Salcedo 2005; Kuzio de Naray et al. 2008, 2010; Oh et al. 2011; Salucci et al. 2012).”
Simulating observations of dark matter dominated galaxies: towards the optimal halo profile (2002, background): “…the empirically determined mass distribution can be well described by a central kpc-sized constant-density core (i.e. α ∼ 0 in the inner parts) (de Blok et al. 2001; de Blok & Bosma 2002 [hereafter dBMBR and dBB02 respectively]). dBMBR and dBB02 base their conclusions on observations of…”
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II (2016, result): “However, observational results have consistently pointed to shallower profiles (e.g., de Blok et al. 2001; Walker & Penarrubia 2011; Adams et al. 2014), and theoretical calculations have been developed to explain why cusps are not found (e.g., Governato et al. 2012; Pontzen & Governato 2012; Di…”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Low surface brightness (LSB) and giant spiral galaxies rotate too fast to be supported by their stars and gas alone, indicating the presence of dark matter [286, 833, 153, 512].”
NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, background): “The observational data are split in three groups, the grey symbols areresults from dwarf and Low Surface Brightness (LSB) galaxies (de Blok et al. 2001; de Blok & Bosma 2002; Swaters et al. 2003), cyan filled squares are the results from the THINGS survey (Oh et al. 2011a), while open blue squares…”
Convergence and scatter of cluster density profiles (2004, background): “This is especially timely given the abundance of new highresolution data that probe the central structure of galaxies (e.g. de Blok et al. 2001a; de Blok, McGaugh & Rubin 2001b; McGaugh, Rubin & de Blok 2001; de Blok & Bosma 2002; Swaters et al. 2003) and clusters (e.g. Sand et al. 2004).”
Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles (2014, background): “…matter haloes are of particular interest as they provide a non-linear scale test of the cold dark matter paradigm, cosmological parameters, and more generally for the nature of dark matter itself (e.g., Moore 1994; Flores & Primack 1994; de Blok et al. 2001; Zentner & Bullock 2002; McGaugh 2004).”