A constant dark matter halo surface density in galaxies

By F. Donato, G. Gentile, P. Salucci, C. Martins, M. Wilkinson, G. Gilmore, E. Grebel, Andreas Koch, R. Wyse. 2009

344 citations recorded by the source corpus.

We confirm and extend the recent finding that the central surface density � 0Dr0ρ0 of galaxy dark matter halos, where r0 and ρ0 are the halo core radius and central density, is nearly constant and independent of galaxy luminosity. Based on the co- added rotation curves of � 1000 spiral galaxies, mass models of individual dwarf irregular and spiral galaxies of late and early types with high-quality rotation curves and, galaxy-galaxy weak lensing signals from a sample of spiral and elliptical galaxies, we find that log � 0D = 2.15 ± 0.2, in units of log(M⊙ pc −2 ). We also show that the observed kinematics of Local Group dwarf spheroidal galaxies, are consistent with this value. Our results are obtained for galactic systems spanning over 14 magnitudes, belonging to different Hubble Types, and whose mass profiles have been determined by several independent methods. In the same objects, the approximate constancy of � 0D is in sharp contrast to the systematical variations, by several orders of magnitude, of galaxy properties, including ρ0 and central stellar surface density.

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

View Paper: https://www.semanticscholar.org/paper/923ed90425c116f2f0c41700c28601c21af60533

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Citations in the corpus

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “Let us eventually note that there is yet a final role played by a0, which is that it defines the central surface density of all dark matter halos as being on the order of a0/(2πG) [129, 167, 313].”
Forged in FIRE: cusps, cores and baryons in low-mass dwarf galaxies (2015, background): “The galaxy shuts down at this redshift because of two main effects: 1) the UV background prevents fresh gas accretion after z ∼ 6 and 2) stellar feedback acts to self-quench the system after the ionizing background lation as observations throughout the Local Group are not complete below this limit 7”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, background): “…profiles are shallower than the predictions of DM only simulations at scales of 0.1-1 kpc (e.g., Flores & Primack 1994; Moore et al. 1999; Swaters et al. 2003; Simon et al. 2005; de Blok et al. 2008; Donato et al. 2009; Primack 2009; Kuzio de Naray et al. 2010; Oh et al. 2010; Elson et al. 2010).”
“Non-cold” dark matter at small scales: a general approach (2017, background): “The situation both under the theoretical/numerical and observational point of view is not entirely clear, and there are continuous efforts to exploit astrophysical consequences of DM both in (spiral) galaxies [5, 6], dwarf galaxies of our Milky Way (MW), or, even more recently, tidal streams [7].”
Dark matter halo merger histories beyond cold dark matter – I. Methods and application to warm dark matter (2012, background): “…arising notably from the issue of cores versus cusps and the inner slope of dark matter density profiles (Salucci 2001; Donato, Gentile & Salucci 2004; Donato et al. 2009; Newman et al. 2009, 2011; de Blok 2010; Kuzio de Naray & Kaufmann 2011; Kuzio de Naray & Spekkens 2011; Salucci et al. 2012;…”