Correlations of galaxies at Z = 0.3

Details Correlations of galaxies at Z = 0.3 Correlations of galaxies at Z = 0.3

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426..516b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 2, p. 516-523

Astronomy and Astrophysics

Astrophysics

18

Angular Correlation, Galactic Clusters, Galactic Evolution, Stellar Magnitude, Amplitudes, Astronomical Photography, Errors, Estimates, Star Formation

Scientific paper

The angular correlation functions for galaxies with magnitudes 20 less than bJ less than 21.5 and 21 less than bJ less than 22.5 are measured from photographic images of nine distinct fields. New expressions for the variance of correlation function estimates are used, which show that the nine fields are consistent with a single angular correlation function w(theta) and with previous estimates of its amplitude and slope -- though the errors on previously published w(theta) values are probably underestimated. Assuming a spatial correlation function of the form xi(r,z) = (r/r0)-gamma(1 + z)-3-epsilon, and using the measured N(z) for these magnitude ranges, we derive xi(r = 250 kpc/h, z = 0.18) = 48 +/- 10, and xi(r = 250 kpc/h, z = 0.27) = 55(+11; -9) for galaxies in these samples, largely independent of gamma and epsilon (1 sigma errors). This is approximately 2 times lower than the small-scale clustering seen in nearby galaxies at bJ less than 18 (after allowing for modest growth in clustering since z = 0.27), yet very similar to the clustering of the nearby IRAS-selected galaxy population. The correlations of the reddest third of the bJ approximately 22 galaxies, however, are larger and consistent with the bJ less than 18 clustering, not the IRAS clustering, for a clustering growth rate of epsilon equal to or greater than -1. Thus to bJ less than 22.5, most of the apparent evolution in clustering of blue-selected galaxies appears to be due to an increasing fraction of late-type or star-forming galaxies at fainter magnitudes, combined with weaker small-scale clustering for late types. These conclusions are entirely empirical and independent of galaxy evolution models.

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