We report on some aspects of our efforts to establish properties of the extremely faint galaxy population by applying our photometric redshift technique to the HDF and HDF–S WFPC2 and NICMOS fields. We find that cosmological surface brightness dimming effects play a dominant role in setting what is observed at redshifts z > 2, that the comoving number density of high intrinsic surface brightnes...

We present observational evidence for a galaxy ‘Type’ dependence to the location of a spiral galaxy’s disk parameters in the μ0–log h plane. With a sample of ∼40 Low Surface Brightness galaxies (both bulgeand disk-dominated) and ∼80 High Surface Brightness galaxies, the early-type disk galaxies (≤Sc) tend to define a bright envelope in the μ0–logh plane, while the late-type (≥Scd) spiral galaxi...

wire-brushing is used for different purposes such as removing metal surfaces oxides, increasing surface brightness, improving fatigue properties and surface activation before coating. the wire-brushing severely scratches and stirs the metals in the surface layers, so that complicated metal flow gives rise to very large amount of plastic strain and increases dislocation density of the surface la...

We present B, R, and Hα imaging data of 19 large disk galaxies whose properties are intermediate between classical low surface brightness galaxies and ordinary high surface brightness galaxies. We use data taken from the Lowell 1.8m Perkins telescope to determine the galaxies’ overall morphology, color, and star formation properties. Morphologically, the galaxies range from Sb through Irr and i...

We study the innermost regions of bulges with surface brightness data derived from combined HST/NICMOS and ground-based NIR profiles. Bulge profiles to 1-2 kpc may be fit with Sersic laws, and show a trend with bulge-to-disk ratio: low-B/D bulges are roughly exponential, whereas higher-B/D bulges show increasing Sersic shape index n, indicating higher peak central densities and more extended br...

Surface brightness data can distinguish between a Friedman-Robertson-Walker expanding universe and a nonexpanding universe. For surface brightness measured in AB magnitudes per angular area, all FRW models, regardless of cosmological parameters, predict that surface brightness declines with redshift as (z+1), while any non-expanding model predicts that surface brightness is constant with distan...