Modeling Nearly Spherical Pure-bulge Galaxies with a Stellar Mass-to-light Ratio Gradient under the ΛCDM and MOND Paradigms. I. Methodology, Dynamical Stellar Mass, and Fundamental Mass Plane

We carry out spherical Jeans modeling of nearly round pure-bulge galaxies selected from the ATLAS^3D sample. Our modeling allows for gradients in the stellar mass-to-light ratio (M _⋆/L) through analytic prescriptions parameterized with a “gradient strength” K introduced to accommodate any viable gradient. We use a generalized Osipkov-Merritt model for the velocity dispersion (VD) anisotropy. We produce Monte Carlo sets of models based on the stellar VD profiles under both the ΛCDM and MOND paradigms. Here, we describe the galaxy data, the empirical inputs, and the modeling procedures of obtaining the Monte Carlo sets. We then present the projected dynamical stellar mass, {M}_{\star {{e}}}, within the effective radius R _e, and the fundamental mass plane (FMP) as a function of K. We find the scaling of the K-dependent mass with respect to the ATLAS^3D reported mass as: {log}}₁₀[{M}_{\star {{e}}}(K)/{M}_{\star {{e}}}^{{A}3{{D}}}]=a^\prime +b^\prime K with a‧ = -0.019 ± 0.012 and b‧ = -0.18 ± 0.02 (ΛCDM), or a‧ = -0.023 ± 0.014 and b‧ = -0.23 ± 0.03 (MOND), for 0 ≤ K < 1.5. The FMP has coefficients consistent with the virial expectation and only the zero-point scales with K. The median value of K for the ATLAS^3D galaxies is < K> ={0.53}_-0.04^+0.05. We perform a similar analysis of the much larger SDSS DR7 spectroscopic sample. In this case, only the VD within a single aperture is available, so we impose the additional requirement that the VD slope be similar to that in the ATLAS^3D galaxies. Our analysis of the SDSS galaxies suggests a positive correlation of K with stellar mass.