Two measures of the shape of the dark halo of the Milky Way

By R. Olling, M. Merrifield. 2000

133 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/df794a9ac8843042afd24c644eba9fcad9cf6396

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Citations in the corpus

The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, background): “Concerning the MW, the empirical evidence is that its DM halo may be somewhat flattened (oblate) with qd\ 0.8 within Rt 60 kpc (Olling & Merrifield 2000, 2001; Ibata et al. 2001; Majewski et al. 2003; Martı́nezDelgado et al. 2004).”
DOES THE STELLAR DISTRIBUTION FLARE? A COMPARISON OF STELLAR SCALE HEIGHTS WITH LAB H i DATA (2014, methodology): “Olling & Merrifield (2000, 2001) assumed constant scale heights for the stellar distribution and note that their results do not depend on the details of the vertical distribution.”
The Great disk of Milky Way satellites and cosmological sub-structures (2004, background): “The empirical evidence is that the MW dark halo is somewhat flattened (oblate) with qd >∼ 0.8 within R<∼ 60 kpc (Olling & Merrifield 2000, 2001; Ibata et al. 2001; Majewski et al. 2003; Martínez-Delgado et al. 2004).”
Dark matter in the Milky Way II. The HI gas distribution as a tracer of the gravitational potential (2007, methodology): “Our solution is close to a single-component model with an effective constant velocity dispersion of 8.3 km s−1, somewhat low in comparion to the preferred value of 9.2 km s−1 of Olling & Merrifield (2000, 2001).”
Halo Properties in Cosmological Simulations of Self-interacting Cold Dark Matter (2000, background): “There are suggestions that the rotation curve rises somewhat beyond the solar circle (though this is uncertain; see Olling & Merrifield 2000), in which case cM is reduced; let us take cM = 8 as a working estimate.”
High-Resolution Measurements of the Halos of Four Dark Matter-Dominated Galaxies: Deviations from a Universal Density Profile (2004, background): “A variety of techniques suggest that the gravitational potential of the dark matter halo of the Milky Way is close to spherical (Kuijken & Tremaine 1994; Olling & Merrifield 2000).”
THE SHAPE OF THE INNER MILKY WAY HALO FROM OBSERVATIONS OF THE PAL 5 AND GD–1 STELLAR STREAMS (2016, background): “…budget (e.g., Flynn et al. 2006; Bovy & Rix 2013; McKee et al. 2015), the dark–matter halo’s shape and radial profile near and within its scale radius (e.g., Olling & Merrifield 2000; Binney & Piffl 2015), and the abundance of lowmass substructure (e.g., Johnston et al. 2002; Ibata et al. 2002).”
Mass and shape of the Milky Way’s dark matter halo with globular clusters from Gaia and Hubble (2018, methodology): “…mass and the axis ratio of the isodensity surfaces of the total mass distribution of the Galaxy, similarly to previous work using the kinematics of individual stars in the Milky Way halo (e.g. Olling & Merrifield 2000; Smith, Wyn Evans, & An 2009; Bowden, Evans, & Williams 2016; Posti et al. 2017).”
THE SAGITTARIUS DWARF GALAXY: A MODEL FOR EVOLUTION IN A TRIAXIAL MILKY WAY HALO (2010, methodology): “Similarly, is a triaxial Galactic halo consistent with observations of the Galactic HI disk (e.g., Olling & Merrifield 2000; Kalberla et al. 2005; and references therein)?”
AN IMPROVED DISTANCE AND MASS ESTIMATE FOR SGR A* FROM A MULTISTAR ORBIT ANALYSIS (2016, methodology): “The adopted value of Ro affects estimates of the Milky Way’s rotation curve and thereby also measurements of the mass and shape of the dark matter distribution (e.g., Olling & Merrifield 2000).”
Internal and External Alignment of the Shapes and Angular Momenta of ΛCDM Halos (2004, methodology): “Other measures of the Milky Way ellipticity using the flaring of the gas disk at large radius or the anisotropy of stellar velocities suggest that the halo is oblate with a flattening of c/a ∼ 0.8 (Olling & Merrifield 2000).”