The radial acceleration relation is a natural consequence of the baryonic Tully-Fisher relation

Abstract

Galaxies covering several orders of magnitude in stellar mass and a variety of Hubble types have been shown to follow the "Radial Acceleration Relation" (RAR), a relationship between $g_{\mathrm{obs}}$, the observed circular acceleration of the galaxy, and $g_{\mathrm{bar}}$, the acceleration due to the total baryonic mass of the galaxy. For accelerations above $10^{10}{\mathrm{m}\mathrm{s}}^{-2}$, $g_{\mathrm{obs}}$ traces $g_{\mathrm{bar}}$, asymptoting to the 1:1 line. Below this scale, there is a break in the relation such that ${\mathrm{g}}_{\mathrm{obs}}\sim {\mathrm{g}}_{\mathrm{bar}}^{1/2}$. We show that the RAR slope, scatter and the acceleration scale are all natural consequences of the well-known baryonic Tully-Fisher relation (BTFR). We further demonstrate that galaxies with a variety of baryonic and dark matter (DM) profiles and a wide range of dark halo and galaxy properties (well beyond those expected in CDM) lie on the RAR if we simply require that their rotation curves satisfy the BTFR. We explore conditions needed to break this degeneracy: sub-kpc resolved rotation curves inside of "cored" DM-dominated profiles and/or outside $\gg 100$kpc could lie on BTFR but deviate in the RAR, providing new constraints on DM.

5 pages, submitted to MNRAS

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• On the radial acceleration relation for galaxies in a wide range of redshifts
• On a critical acceleration scale of dark matter in Lambda-CDM and dynamical dark energy
• On a Generalized Mass-Velocity Relation for Disk Galaxies and Galaxy Clusters