Higher-Order Correlation Functions and the FIRST Survey

Details Higher-Order Correlation Functions and the FIRST Survey Higher-Order Correlation Functions and the FIRST Survey

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.8705b&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #87.05; Bulletin of the American Astronomical Society, Vol. 29, p.1354

Astronomy and Astrophysics

Astronomy

Scientific paper

The moments of a two-dimensional distribution of sources on the sky can be explicitly obtained by integrating the corresponding projected k-space spectra (known from linear perturbation theory), weighted by appropriate window functions. We derive the results for the normalized skewness of a two-dimensional survey, s_3 = frac ^ {2}}, where delta_R is the overdensity of counts in a window of angular radius R and is biased relative to the overdensity in the underlying mass distribution, delta_m , via delta = sum {(1)/(k!)bk delta_ {m}(k}) . We incorporate the full dependence of the result for s_3 on Omega_0 and, as well as the b_1 and b_2 terms in the bias expansion, in addition to the dependence on the index of the power spectrum and the redshift selection function. These results will be compared to the observed values for the VLA FIRST survey, and the resulting constraints will be discussed.

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