The relationships between lightness and brightness responses under the condition that achromatic "surface color " appears and the relationships between perceived illumination and brightness were examined. The Ss were required to make categorical judgments upon both lightness and brightness of the test patches presented on black and white backgrounds and upon the over-all illumination in the vis...

Low-surface-brightness galaxies (LSBGs) -- defined as systems that are fainter than the surface-brightness limits of past wide-area surveys form overwhelming majority in dwarf regime (M* < 10^9 MSun). Using NewHorizon, a high-resolution cosmological simulation, we study origin LSBGs and explain why at similar stellar mass show large observed spread surface brightness. New Horizon populate well-...

L-band brightness predicted by the land surface process/radiobrightness (LSP/R) model for prairie grassland appears to be somewhat lower than expected [1]. A crucial reason for the underestimate of the L-band brightness is that the soil surface was treated as smooth. In this paper, surface scattering of the soil determined by the IEM model is incorporated into the LSP/R model to examine its imp...

The brightness of an achromatic surface with luminance S on an achromatic background with luminance B varies with S, with B, and with the luminance step deltaL at the border of the surface. In agreement with previous findings indicating that the visual system can perform as a photometer, the results of the two experiments reported here show that S and B determined surface brightness independent...

We present results of broad band BVRI observations of a sample of galaxies with a low surface brightness (LSB) disk and a bulge. These galaxies are well described as exponential disks and exponential bulges with no preferred value for either scale length or central surface brightness. The median B band disk scale length is 12.6 kpc (H0 = 75 km s−1 Mpc−1) which is much larger than scale lengths ...

We present near-infrared H-band (1.65 μm) surface brightness profile decomposition for 1157 galaxies in five nearby clusters of galaxies: Coma, A1367, Virgo, A262 and Cancer, and in the bridge between Coma and A1367 in the “Great Wall”. The optically selected (mpg ≤ 16.0) sample is representative of all Hubble types, from E to Irr+BCD, except dE and of significantly different environments, span...

We study the variation of the dark matter mass fraction of elliptical galaxies as a function of their luminosity, stellar mass, and size using a sample of 29,469 elliptical galaxies culled from the Sloan Digital Sky Survey. We model ellipticals as a stellar Hernquist profile embedded in an adiabatically compressed dark matter halo. This model allows us to estimate a dynamical mass (Mdynm) at th...

In spite of their overall success, semi-analytic models of galaxy formation and evolution predict slopes of luminosity functions which are steeper than the observed ones. This discrepancy has generally been explained by subtle surface brightness effects acting on the observational samples. In this paper, we explicitly implement the computation of surface brightness in a simple semi– analytic mo...