 Solution

The effective radius is one tenth of the optical outer radius: $R_e\simeq 2.13$ kpc. A flat rotation speed then gives $M_{\mathrm{dyn}}(<R_e)\simeq 4.9\times 10^{10}{M}_{\odot }$. Half the luminosity, with the same mass-to-light ratio, implies $M_{\mathrm{luminous}}(<R_e)\simeq 4.9\times 10^{10}{M}_{\odot }$.The concentration of light into a small fraction of the optical radius suggests a high-surface-brightness, centrally concentrated disk galaxy, plausibly an early-type spiral or lenticular with a substantial bulge. The kinematic and photometric data do not uniquely distinguish those morphologies. Disk geometry, an unknown inclination correction, or a varying stellar mass-to-light ratio would alter the exact numerical inner comparison.