First Results on Galaxy Clustering from Early SDSS Data

Details First Results on Galaxy Clustering from Early SDSS Data First Results on Galaxy Clustering from Early SDSS Data

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.9701s&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #97.01; Bulletin of the American Astronomical Society, Vol. 33, p.1183

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We present the first results on the galaxy angular and redshift space correlation functions from early SDSS photometric and spectroscopic data. The Sloan Digital Sky Survey (SDSS) has so far obtained 5-band CCD images of over 8 million galaxies and spectroscopic redshifts for approximately 140,000 galaxies. We present clustering results for subsamples of 1.5 million galaxy images (r* < 22) and ~ 30,000 galaxy redshifts (r* < 17.6), corresponding to less than 3% of the projected survey totals. For the 2-dimensional data, covering a 2.5o x 90o slice to a depth of order 1h-1 Gpc, the angular autocorrelation function and angular power spectrum have been measured and inverted to obtain the 3-dimensional power spectrum. A parametrized estimate of power spectrum parameters has also been made from a Karhunen-Loeve analysis, indicating that the current sample probes the vicinity of the the ``turnover'' scale predicted by inflationary cosmological models. An exhaustive study of systematic errors and statistical uncertainties in the angular clustering analysis has been carried out, indicating that the sample is free from observable systematic effects. From the redshift data, the spatial correlation function is well described on small scales by a power law with correlation length r0 = 6 h-1 Mpc and slope γ = 1.8; the galaxy pairwise velocity dispersion is σ 12≈ 600 km/sec for projected separations below ~ 5 h-1 Mpc. Red galaxies exhibit a higher and steeper correlation function and a higher pairwise velocity dispersion than do the blue galaxies; similar trends hold when the sample is divided by surface brightness or profile concentration. On scales below 10 h-1 Mpc, we find a clear signal of scale-independent luminosity bias, consistent with a scaling ξ ~ L0.25, for galaxies with absolute magnitudes in the vicinity of M*.

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