We used the $H\alpha$ images from a large sample of nearby late-type dwarfgalaxies to investigate properties of their emission structure. The sampleconsists of three hundred galaxies of the irregular (Irr), Magellanic irregular(Im), blue compact dwarf (BCD), and transition (Tr) types situated within adistance of 11 Mpc. In each galaxy, we indicated: the number of compactHII-regions, the presence of bubble-like or filament-like structures, thepresence of a faint diffuse emission, and a sign of the global burst. Thelarger luminosity of a galaxy, the greater number of compact HII-sources in it.The integral and specific star-formation rates of the dwarf increase steeplywith the increase of the number of HII-regions showing the evidence of theepidemic character of star-formation process. The dwarf galaxies withemission-line bubbles, or filaments, or signs of the global star-formationburst have approximately the same hydrogen-mass-to-luminosity ratio as that ofthe whole sample objects. However, their mean star-formation rate issignificantly higher than that of other galaxies in the sample. Emissionbubble-like structures are found in the nearby dwarfs with a frequency of 1case per 4-5 galaxies. Their linear diameters are close to those expected forsupernova remnants. The mean specific SFR for the nearby late-type dwarfs isclose to the Hubble parameter, $H_0 = -10.14$ dex (yr)$^{-1}$, consistent withthe sluggish cosmic star-formation history of galaxies of this kind.

Early-type galaxies -- slow and fast rotating ellipticals (E-SRs and E-FRs)and S0s/lenticulars -- define a Fundamental Plane (FP) in the space ofhalf-light radius $R_e$, enclosed surface brightness $I_e$ and velocitydispersion $\sigma_e$. Since $I_e$ and $\sigma_e$ are distance-independentmeasurements, the thickness of the FP is often expressed in terms of theaccuracy with which $I_e$ and $\sigma_e$ can be used to estimate sizes $R_e$.We show that: 1) The thickness of the FP depends strongly on morphology. If thesample only includes E-SRs, then the observed scatter in $R_e$ is $\sim 16\%$,of which only $\sim 9\%$ is intrinsic. Removing galaxies with$M_*<10^{11}M_\odot$ further reduces the observed scatter to $\sim 13\%$ ($\sim4\%$ intrinsic). The observed scatter increases to the $\sim 25\%$ usuallyquoted in the literature if E-FRs and S0s are added. If the FP is defined usingthe eigenvectors of the covariance matrix of the observables, then the E-SRsagain define an exceptionally thin FP, with intrinsic scatter of only $5\%$orthogonal to the plane. 2) The structure within the FP is most easilyunderstood as arising from the fact that $I_e$ and $\sigma_e$ are nearlyindependent, whereas the $R_e-I_e$ and $R_e-\sigma_e$ correlations are nearlyequal and opposite. 3) If the coefficients of the FP differ from thoseassociated with the virial theorem the plane is said to be `tilted'. If wemultiply $I_e$ by the global stellar mass-to-light ratio $M_*/L$ and we accountfor non-homology across the population by using S\'ersic photometry, then theresulting stellar mass FP is less tilted. Accounting self-consistently for$M_*/L$ gradients will change the tilt. The tilt we currently see suggests thatthe efficiency of turning baryons into stars increases and/or the dark matterfraction decreases as stellar surface brightness increases.