The Weakness of C Iv Absorber Clustering in Keck Hires Spectra of Adjacent Qso Sightlines

We observe with Keck/HIRES the z ≈ 2.5 QSO triplet 1623+27 in order to explore on the scale of a Megaparsec the spatial clustering of C IV absorbers between adjacent sightlines. We find this signal to be significantly weaker than the clustering in velocity on corresponding scales along single sightlines, assuming that the relative velocity of absorbers is dominated by the Hubble flow. This indicates that small-scale clustering (200 km s < ∆v < 600 km s) of the C IV absorbers cannot be interpreted in terms of the positions of the absorbers in space, but must be considered as internal motions within individual absorbers, or within clusters of absorbers whose internal velocities dominate over Hubble expansion across the cluster scale. If the single-sightline signal is due to spatial clustering, it is caused by absorber clusters smaller than would be implied by their velocities if a Hubble flow is assumed. The spatial clustering of C IV absorbers at z ≈ 2 is consistent with data on Ly α forest clustering measured in the same way at the same redshifts. However, present-day galaxy clustering, evolved back to z ≈ 2, is consistent with C IV spatial clustering but perhaps not with that of the Ly α forest. Even so, one cannot as yet distinguish the two absorber populations on the basis of spatial clustering on these small scales.