The tight correlation between total galaxy stellar mass and star formationrate (SFR) has become known as the star forming main sequence. Using ~487,000spaxels from galaxies observed as part of the Sloan Digital Sky Survey MappingGalaxies at Apache Point Observatory (MaNGA) survey, we confirm previousresults that a correlation also exists between the surface densities of starformation (Sigma_SFR) and stellar mass (Sigma_mass) on kpc scales, representinga `resolved' main sequence. Using a new metric (Delta Sigma_SFR), whichmeasures the relative enhancement or deficit of star formation on aspaxel-by-spaxel basis relative to the resolved main sequence, we investigatethe SFR profiles of 864 galaxies as a function of their position relative tothe global star forming main sequence (Delta SFR). For galaxies above theglobal main sequence (positive Delta SFR) Delta Sigma_SFR is elevatedthroughout the galaxy, but the greatest enhancement in star formation occurs atsmall radii (< 3 kpc, or 0.5 R_e). Moreover, galaxies that are at least afactor of three above the main sequence show diluted gas phase metallicitiesout to 2 R_e, indicative of metal-poor gas inflows accompanying the starbursts.For quiescent/passive galaxies that lie at least a factor of 10 below the starforming main sequence there is an analogous deficit of star formationthroughout the galaxy with the lowest values of Delta Sigma_SFR in the central3 kpc. Our results are in qualitative agreement with the `compaction' scenarioin which a central starburst leads to mass growth in the bulge and mayultimately precede galactic quenching from the inside-out.

Using integral field spectroscopy we investigate the kinematic properties of35 massive centrally-dense and compact star-forming galaxies($\log{(M_*[\mathrm{M_{\odot}}])}>10$,$\log{(\Sigma_\mathrm{1kpc}[\mathrm{M_{\odot}~kpc}^{-2}])}>9.5$,$\log{(M_\ast/r_e^{1.5}[\mathrm{M_{\odot}~kpc}^{-1.5}])}>10.3$) at$z\sim0.7-3.7$ within the KMOS$^\mathrm{3D}$ survey. We spatially resolve 23compact star-forming galaxies (SFGs) and find that the majority are dominatedby rotational motions with velocities ranging from 95-500 km/s. The range ofrotation velocities is reflected in a similar range of integrated H$\alpha$linewidths, 75-400 km/s, consistent with the kinematic properties ofmass-matched extended galaxies from the full KMOS$^\mathrm{3D}$ sample. Thefraction of compact SFGs that are classified as `rotation-dominated' or`disk-like' also mirrors the fractions of the full KMOS$^\mathrm{3D}$ sample.We show that integrated line-of-sight gas velocity dispersions fromKMOS$^\mathrm{3D}$ are best approximated by a linear combination of theirrotation and turbulent velocities with a lesser but still significantcontribution from galactic scale winds. The H$\alpha$ exponential disk sizes ofcompact SFGs are on average $2.5\pm0.2$ kpc, $1-2\times$ the continuum sizes,in agreement with previous work. The compact SFGs have a $1.4\times$ higher AGNincidence than the full KMOS$^\mathrm{3D}$ sample at fixed stellar mass withaverage AGN fraction of 76%. Given their high and centrally concentratedstellar masses as well as stellar to dynamical mass ratios close to unity, thecompact SFGs are likely to have low molecular gas fractions and to quench on ashort time scale unless replenished with inflowing gas. The rotation in thesecompact systems suggests that their direct descendants are rotating passivegalaxies.

The hierarchical galaxy formation scenario in the Cold Dark Matter cosmogonywith a non-vanishing cosmological constant and geometrically flat space hasbeen very successful in explaining the large-scale distribution of galaxies.However, there have been claims that the scenario predicts too many satellitegalaxies associated with massive galaxies compared to observations, called themissing satellite galaxy problem. Isolated groups of galaxies hosted bypassively evolving massive early-type galaxies are ideal laboratories forfinding the missing physics in the current theory. Here we report from a deepspectroscopic survey of such satellite systems that isolated massive early-typegalaxies with no recent star formation through wet mergers or accretion havealmost no satellite galaxies fainter than the r-band absolute magnitude ofabout Mr =-14. If only early-type satellites are used, the cutoff is atsomewhat brighter magnitude of about Mr =-15. Such a cutoff has not been foundin other nearby satellite galaxy systems hosted by late-type galaxies or thosewith merger features. Various physical properties of satellites depend stronglyon the host-centric distance. Our observation indicates that the satellitegalaxy luminosity function is largely determined by the interaction ofsatellites with the environment provided by their host, which sheds light onthe missing satellite galaxy problem.