Galaxy clustering as a function of surface brightness

Details Galaxy clustering as a function of surface brightness Galaxy clustering as a function of surface brightness

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299...15d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 15-20. NSF-supported research.

Astronomy and Astrophysics

Astrophysics

57

Brightness Distribution, Cosmology, Galactic Clusters, Galactic Evolution, Angular Correlation, Magnitude, Mass Distribution, Red Shift

Scientific paper

Using diameters and magnitudes of galaxies listed in the Nilson catalog, the angular correlation properties of highand low-surface brightness galaxies are examined. The low-surface brightness galaxies are less tightly clumped than the higher surface brightness galaxies; they also fill in some conspicuous holes in the distribution of the high-surface brightness galaxies. The angular correlations are weaker and shallower for the low-surface brightness galaxies; when account is taken for the differing redshift distribution of the subsets, it is found that the spatial clustering length scale is a factor of two smaller than for the high-surface brightness galaxies. This finding demonstrates that galaxy formation must have been dependent on the large-scale clustering environment and suggests that the luminous galaxy distribution may not be a fair tracer of the mass distribution on any scale. Although the effect is apparent from the sky-projected angular correlations, the relative amplitudes of the spatial clustering must be regarded as preliminary because they are derived from an incomplete and possibly biased redshift sample.

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