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Measuring the Angular Correlation Function for Faint Galaxies in High Galactic Latitude Fields | | David Woods
; Gregory G. Fahlman
; | | Date: |
11 Jul 1997 | | Subject: | astro-ph | | Affiliation: | University of British Columbia | | Abstract: | A photometric survey of faint galaxies in three high Galactic latitude fields (each $sim49~
m{arcmin^{2}}$) with sub-arcsecond seeing is used to study the clustering properties of the faint galaxy population. Multi-color photometry of the galaxies has been obtained to magnitude limits of $Vsim25$, $Rsim25$ and $Isim24$. Angular correlation analysis is applied to magnitude-limited and color-selected samples of galaxies from the three fields for angular separations ranging from $10-126’’$. General agreement is obtained with other recent studies which show that the amplitude of the angular correlation function, $omega( heta)$, is smoothly decreasing as a function of limiting magnitude. The observed decline of $omega( heta)$ rules out the viability of ``maximal merger’’ galaxy evolution models. Using redshift distributions extrapolated to faint magnitude limits, models of galaxy clustering evolution are calculated and compared to the observed I-band $omega( heta)$. Faint galaxies are determined to have correlation lengths and clustering evolution parameters of either $r_{0}sim4~h^{-1}~Mpc$ and $epsilonsim0-1$; $r_{0}sim5-6~h^{-1}~Mpc$ and $epsilon>1$; or $r_{0}sim2-3~h^{-1}~ Mpc$ and $epsilonsim-1.2$, assuming $q_{0}=0.5$ and with $h=H_{0}/100~ km~s^{-1}~Mpc^{-1}$. The latter case is for clustering fixed in co-moving coordinates and is probably unrealistic since most local galaxies are observed to be more strongly clustered. No significant variations in the clustering amplitude as a function of color are detected, for all the color-selected galaxy samples considered. (Abridged) | | Source: | arXiv, astro-ph/9707127 | | Services: | Forum | Review | PDF | Favorites | |
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