Wilman, R. J. and Morris, S. L. and Jannuzi, B. T. and Davé, R. and Shone, A. M. (2007) 'The association between gas and galaxies II : the two-point correlation function.', Monthly notices of the Royal Astronomical Society., 375 (2). pp. 735-744.
We measure the two-point correlation function, ξAG, between galaxies and quasar absorption-line systems at z < 1, using the data set of Morris & Jannuzi on 16 lines-of-sight (LOS) with ultraviolet (UV) spectroscopy and galaxy multi-object spectroscopy (Paper I). The measurements are made in 2D redshift space out to π = 20 h1 Mpc (comoving) along the LOS and out to σ = 2 h1 Mpc projected; as a function of H i column density in the range NH I = 1013–1019 cm2, also for C iv absorption systems, and as a function of galaxy spectral type. This extends the absorber–galaxy pair analysis of Paper I. We find that the amplitude of the peak in ξAG at the smallest separations increases slowly as the lower limit on NH I is increased from 1013 to 1016 cm2, and then jumps sharply (albeit with substantial uncertainties) for NH I > 1017 cm2. For C iv absorbers, the peak strength of ξAG is roughly comparable to that of H i absorbers with NH I > 1016.5 cm2, consistent with the finding that the C iv absorbers are associated with strong H i absorbers. We do not reproduce the differences reported by Chen et al. between 1D ξAG measurements using galaxy subsamples of different spectral types. However, the full impact on the measurements of systematic differences in our samples is hard to quantify. We compare the observations with smoothed particle hydrodynamical (SPH) simulations and discover that in the observations ξAG is more concentrated to the smallest separations than in the simulations. The latter also display a 'finger of god' elongation of ξAG along the LOS in redshift space, which is absent from our data, but similar to that found by Ryan-Weber for the cross-correlation of quasar absorbers and H i-emission-selected galaxies. The physical origin of these 'fingers of god' is unclear, and we thus highlight several possible areas for further investigation.
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|Publisher Web site:||http://dx.doi.org/10.1111/j.1365-2966.2006.11342.x|
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|Record Created:||02 May 2008|
|Last Modified:||09 Aug 2011 16:38|
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