The underlying radial acceleration relation

Abstract

The radial acceleration relation (RAR) of late-type galaxies relates their dynamical acceleration, $g_{\text{obs}}$, to that sourced by baryons alone, $g_{\text{bar}}$, across their rotation curves. Literature fits to the RAR have fixed the galaxy parameters on which the relation depends -- distance, inclination, luminosity and mass-to-light ratios -- to their maximum a priori values with an uncorrelated Gaussian contribution to the uncertainties on $g_{\text{bar}}$ and $g_{\text{obs}}$. In reality these are free parameters of the fit, contributing systematic rather than statistical error. Assuming a range of possible functional forms for the relation with or without intrinsic scatter (motivated by Modified Newtonian Dynamics with or without the external field effect), I use Hamiltonian Monte Carlo to perform the full joint inference of RAR and galaxy parameters for the Spitzer Photometry and Accurate Rotation Curves (SPARC) dataset. This reveals the intrinsic RAR underlying that observed. I find an acceleration scale $a_0=(1.19\pm 0.04\text{(stat)}\pm 0.09\text{(sys)})\times 10^{-10}$ m s${}^{-2}$, an intrinsic scatter ${\sigma }_{\text{int}}=(0.034\pm 0.01\text{(stat)}\pm 0.01\text{(sys)})$ dex (assuming the SPARC error model is reliable) and weak evidence for the external field effect. I make summary statistics of all my analyses publicly available for future SPARC studies or applications of a calibrated RAR, for example redshift-independent distance measurement.

arXiv comment11 pages, 4 figures; revised to match MNRAS published version

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