On the interpretation of clustering from the angular APM Galaxy Survey

Abstract

We analyze the uncertainties in the amplitudes of the spatial correlation functions estimated from angular correlations in a sample from the APM Galaxy Survey, with $b_J=17-20$. We model the uncertainties in the selection function and in the evolution of clustering. In particular we estimate $σ_8^{APM}$, the rms galaxy number fluctuations in spheres of radius at $8 \Mpc$, from the measured angular variance in the APM. The uncertainty in $σ_8^{APM}$ has three main contributions: 8\% from sampling and selection function uncertainties, 7\% from the uncertainty in the evolution of clustering and 3\% from the uncertainty in the value of $Ω_0$. Including all these contributions, we find $σ_8^{APM}$ is in the range $0.78-1.08$. If the galaxy clustering in the APM evolves as expected from gravitational clustering of matter fluctuations, then $σ_8^{APM}=0.95 \pm 0.07$ ($1.00 \pm 0.08$) for $Ω_0 \simeq 1$ ($Ω_0 \simeq 0$), close to the values for nearby optical samples. On the other hand, if we assume that clustering evolution is fixed in comoving coordinates $σ_8^{APM}=0.83 \pm 0.05$ ($0.87 \pm 0.06$), closer to the results for nearby IRAS samples. The final uncertainty in the range of values for the hierarchical amplitudes $S_J\equiv \xibar_J/\xibar_2^{J-1}$ is typically twice the estimated sampling errors, with the highest values for the case of less clustering evolution. We compare our estimates with other results and discuss the implications for models of structure formation.