Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.5405n&link_type=abstract
American Astronomical Society, 185th AAS Meeting, #54.05; Bulletin of the American Astronomical Society, Vol. 26, p.1404
Statistics
1
Scientific paper
We investigate the dependence of the galaxy clustering versus galaxy-type, size and F606W-F814W color, using Medium-Deep Survey Cycle 4 WFPC2 data. The MDS fields used for this study are complete down to F814W<22--23 mag, corresponding to predicted median redshifts zmed =~ 0.5. We detect, determine object classifications and measure image parameters (e.g., half-light radius, axis ratio, position angle) for several hundred objects per MDS field. Of the catalogued objects, more than 80% are classifiable as galaxies, half of which have sufficient S/N to distinguish between disk and bulge morphology. This work extends upon, and is compared, with a similar analysis applied to Cycles 1--3 WF/PC data, and goes =~ 1.5 magnitudes deeper than that for WF/PC. On sub-arcsec scales, the two-point correlation function, w(theta ), and nearest neighbor statistics are used to determine small-scale clustering not visible from ground-based data. On arcminute scales, the amplitude of w(theta ) is used to test type-, color- and size dependences of galaxy clustering. Relative to a model in which galaxy clusters are comoving with the Hubble flow, preliminary results show: 1) weak clustering at F814W=21-23 mag for full galaxy samples (selected without respect to galaxy type or color), consistent with ground-based deep surveys; 2) strong and weak clustering among bulge- and disk-selected samples, consistent with the morphology density relation; 3) strong and weak clustering among red- and blue-selected samples. We interpret weak clustering observed from ground-based surveys as the superposition of weakly and strongly clustered galaxy populations which, by the above observations, are associated with bulge and disk galaxies, which are observed to be characteristically red and blue, respectively. This work was supported by NASA/HST grants GO-2684 from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555.
Casertano S. C.
Ellis Richard S.
Gilmore Gerard
Green Richard F.
Griffiths Richard E.
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