We have analyzed with the scaling formalism a statistical sample of northern dwarf and low surface brightness (LSB) galaxies with complete redshift information and such that δ ≥ 0° and b ≥ 40°. We subdivide the statistical sample into volume-limited samples and carry out the scaling analysis separately for dwarf and LSB galaxies. We then compare our results with those for bright galaxies (m_B ≤ 14.5) from the Center for Astrophysics (CfA) survey in the same volume-limited samples. The scaling formalism allows a separate analysis of regions with different density ranges. When galaxies in clusters are excluded, the null hypothesis that dwarf and LSB galaxies on the one hand, and bright galaxies on the other, trace the same density field can be ruled out at a 95% confidence level for both high- and moderate-density regions. We find bright galaxies to be more clustered than dwarf and LSB galaxies. The difference is not statistically significant for very low density regions, and in the region of the Local Supercluster, presumably because the redshift distances are more affected by peculiar velocities in the latter case. These results are not sensitive to changes in the absolute magnitude limit of the CfA subsamples, the intrinsic diameters of dwarf-LSB galaxies, and the morphological type of bright galaxies. The difference in the clustering properties between bright and dwarf-LSB galaxies increases considerably in the Local Supercluster when galaxies in the Virgo cluster are included. The result that LSB dwarfs are less clustered than bright galaxies is similar to that obtained for blue compact galaxies (BCGs), supporting the hypothesis that BCGs are LSB dwarfs undergoing intense bursts of star formation.
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