Dark matter in the universe

By J. Bahcall, T. Piran, Steven Weinberg. 2004

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Dark matter in dwarf spheroidals – II. Observations and modelling of Draco (2001, background): “Subsequently, Aaronson & Olszewski (1987, 1988) obtained the velocities of ∼ 15 more stars and computed a velocity dispersion of ∼ 10 kms−1 and a mass-to-light ratio of > 50M⊙/L⊙.”
A MegaCam Survey of Outer Halo Satellites. III. Photometric and Structural Parameters (2018, background): “In a pioneering study, Aaronson & Olszewski (1987) measured a velocity dispersion of σvr = 11± 3 km s−1, for Ursa Minor, prompting many subsequent investigations into the dark matter content of this and other Galactic dSph galaxies (e.g., Pryor & Kormendy 1990; Lake 1990).”
THE OBSERVED PROPERTIES OF DWARF GALAXIES IN AND AROUND THE LOCAL GROUP (2012, background): “Numerous studies (e.g., Aaronson & Olszewski 1987; Mateo et al. 1993; Olszewski et al. 1996; Hargreaves et al. 1996) all concluded that, barring a pathological or extremely high binary population, binary stars were insufficient to boost a stellar system with σ 1 km s−1 to σ 8–10 km s−1, although…”
Primordial magnetogenesis (2010, background): “17) where λ1, λ2 and λ3 are the eigenvalues of the initial tidal field and determine the nature of the collapse [135,136].”