Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006mnras.369.1667h&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 369, Issue 4, pp. 1667-1676.
Astronomy and Astrophysics
Astronomy
3
Galaxies: Clusters: Individual: Abell 2029: Cosmology: Theory: Dark Matter: X-Rays: Galaxies: Clusters, Galaxies: Clusters: Individual: Abell 2029, Cosmology: Theory, Dark Matter, X-Rays: Galaxies: Clusters
Scientific paper
Conformal gravity has a weak-field limit that augments the Newtonian potential -GM/R by a linear potential γc2R/2. Mannheim has shown that an appropriate choice of γ enables a satisfying fit to the flat rotation curves of large spiral galaxies and simultaneously to the rising rotation curves of low surface brightness galaxies, without invoking dark matter. Here, we extend to larger scales the comparison of Newtonian and conformal gravity by analysis of X-ray gas in the Abell 2029 galaxy cluster. The Newtonian analysis yields a mass profile rising roughly as M ~ R2 from 1010Msolar at 2kpc to 1014Msolar at 200kpc, and this can be interpreted as the profile of an extensive dark matter halo that dominates the cluster potential. In conformal gravity, the potential is non-uniform inside a spherical shell, so that both interior and exterior mass distributions must be taken into account. We derive the conformal gravity potential both inside and outside a spherical shell, enabling the evaluation of potentials for spherically symmetric mass distributions. A conformal gravity analysis of X-ray gas in Abell 2029 then yields a total mass profile that rises from 1010Msolar at 2kpc to 1.4 × 1012Msolar at 30kpc, and then remains roughly constant out to 300kpc. With this mass profile, conformal gravity is able to bind the X-ray gas with no need for dark matter. However, integrating the X-ray gas density profile gives a baryon mass of 1013Msolar inside 200kpc, nearly 10 times more than what is required to hold the hot gas in hydrostatic equilibrium. This discrepancy may rule out conformal gravity unless there is a significant breakdown of hydrostatic equilibrium in the outskirts of the potential well. The required velocities, V ~ 2000kms-1, may be observable via Doppler profiles in high-resolution X-ray spectroscopy. It is also possible that the mass distribution outside the cluster significantly reduces conformal gravity in the cluster outskirts. Our approximate treatment of this effect suggests that it is negligible, but a more sophisticated analysis might yield a different conclusion.
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