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We perform full spectrum fitting stellar population analysis and JeansAnisotropic modelling (JAM) of the stellar kinematics for about 2000 early-typegalaxies (ETGs) and spiral galaxies from the MaNGA DR14 sample. Galaxies withdifferent morphologies are found to be located on a remarkably tight mass planewhich is close to the prediction of the virial theorem, extending previousresults for ETGs. By examining an inclined projection (`the mass-size' plane),we find that spiral and early-type galaxies occupy different regions on theplane, and their stellar population properties (i.e. age, metallicity andstellar mass-to-light ratio) vary systematically along roughly the direction ofvelocity dispersion, which is a proxy for the bulge fraction. Galaxies withhigher velocity dispersions have typically older ages, larger stellarmass-to-light ratios and are more metal rich, which indicates that galaxiesincrease their bulge fractions as their stellar populations age and becomeenriched chemically. The age and stellar mass-to-light ratio gradients forlow-mass galaxies in our sample tend to be positive ($\rm centre<outer$), whilethe gradients for most massive galaxies are negative. The metallicity gradientsshow a clear peak around velocity dispersion $\log_{10} \sigma_{\rm e}\approx2.0$, which corresponds to the critical mass $\sim 3\times 10^{10}M_{\odot}$ ofthe break in the mass-size relation. Spiral galaxies with large mass and sizehave the steepest gradients, while the most massive ETGs, especially above thecritical mass $M_{\rm crit}\ge 2\times 10^{11} M_{\odot}$, where slow rotatorETGs start dominating, have much flatter gradients. This may be due todifferences in their evolution histories, e.g. mergers.

SDSS-IV MaNGA: Global stellar population and gradients for about 2000 early-type and spiral galaxies on the mass-size plane