Clustering properties of radio sources in the FIRST survey

Details Clustering properties of radio sources in the FIRST survey Clustering properties of radio sources in the FIRST survey

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999elss.conf..337m&link_type=abstract

"Evolution of large scale structure : from recombination to Garching /edited by A. J. Banday, R. K. Sheth, L. N. da Costa. Garch

Computer Science

Scientific paper

We investigate the large-scale clustering of radio sources in the FIRST 1.4-GHz survey by analysing their distribution function. We select a reliable sample from the the FIRST catalogue, paying particular attention to the problem of how to define single radio sources from the multiple components listed and we also consider the incompleteness of the catalogue. We estimate the angular two-point correlation function w(θ), the variance Ψ2, and skewness Ψ3 of the distribution; both w(θ) and Ψ2 show power-law behaviour with an amplitude corresponding a spatial correlation length of r0 ˜ 10 h-1 Mpc. We detect significant skewness in the distribution, the first such detection in radio surveys. This skewness is found to be related to the variance through Ψ3=S3(Ψ2)α, with α=1.9± 0.1, consistent with the non-linear gravitational growth of perturbations from primordial Gaussian initial conditions. We also investigate how different theoretical predictions for w(θ) can match our measurements at different flux limits. The models have been worked out for three different functional forms of the redshift distribution N(z), and by allowing for evolution of bias b(z) with redshift. Models with either biasing strongly evolving with epoch or with an N(z) not showing a low-redshift component are ruled out. Models where the bias varies linearly as a function of redshift could be accepted only in the case of a redshift distribution strongly dominated by the low-redshift spike, even though the resulting values for the correlation length r0˜ 3-4h-1 Mpc are somewhat too small. The best fit is provided by models with constant biasing and a redshift distribution characterised by a lower-amplitude spike, both in the case of open/flat Universe. The correlation lengths corresponding to these models are r0˜ 9-11h-1 Mpc.

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