Low-surface-brightness spheroidal galaxies as Milgromian isothermal spheres. (arXiv:2104.03861v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Sanders_R/0/1/0/all/0/1">R.H. Sanders</a>
I consider a sample of eight pressure-supported low-surface brightness
galaxies (seven nearby dwarfs and one ultra-diffuse object) in terms of
Milgrom’s modified Newtonian dynamics (MOND). These objects are modelled as
Milgromian isotropic isothermal spheres characterised by two parameters that
are constrained by observations: the constant line-of-sight velocity dispersion
and the central surface density. The velocity dispersion determines the total
mass, and, with the implied mass-to-light ratio, the central surface
brightness. This then specifies the radial run of surface brightness over the
entire isothermal sphere. For the objects in this sample the predicted radial
distribution of surface brightness is shown to be entirely consistent with
observations which constitutes a success for MOND that is independent of the
reduced dynamical mass.
I consider a sample of eight pressure-supported low-surface brightness
galaxies (seven nearby dwarfs and one ultra-diffuse object) in terms of
Milgrom’s modified Newtonian dynamics (MOND). These objects are modelled as
Milgromian isotropic isothermal spheres characterised by two parameters that
are constrained by observations: the constant line-of-sight velocity dispersion
and the central surface density. The velocity dispersion determines the total
mass, and, with the implied mass-to-light ratio, the central surface
brightness. This then specifies the radial run of surface brightness over the
entire isothermal sphere. For the objects in this sample the predicted radial
distribution of surface brightness is shown to be entirely consistent with
observations which constitutes a success for MOND that is independent of the
reduced dynamical mass.
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