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Durham University

Department of Physics

Staff profile

Publication details for Prof Carlos Frenk

Guo, Q., Cole, S., Lacey, C.G., Baugh, C.M., Frenk, C.S., Norberg, P., Auld, R., Baldry, I.K., Bamford, S.P., Bourne, N., Buttiglione, E.S., Cava, A., Cooray, A., Croom, S., Dariush, A., de Zotti, G., Driver, S., Dunne, L., Dye, S., Eales, S., Fritz, J., Hopkins, A., Hopwood, R., Ibar, E., Ivison, R.J., Jarvis, M., Jones, D.H., Kelvin, L., Liske, J., Loveday, J., Maddox, S.J., Parkinson, H., Pascale, E., Peacock, J.A., Pohlen, M., Prescott, M., Rigby, E.E., Robotham, A., Rodighiero, G., Sharp, R., Smith, D.J.B., Temi, P. & van Kampen, E. (2011). Which haloes host Herschel-ATLAS galaxies in the local Universe? Monthly Notices of the Royal Astronomical Society 412(4): 2277-2285.

Author(s) from Durham

Abstract

We measure the projected cross-correlation between low-redshift (z < 0.5) far-infrared selected galaxies in the science demonstration phase (SDP) field of the Herschel-ATLAS (H-ATLAS) survey and optically selected galaxies from the Galaxy and Mass Assembly (GAMA) redshift survey. In order to obtain robust correlation functions, we restrict the analysis to a subset of 969 out of 6900 H-ATLAS galaxies, which have reliable optical counterparts with r < 19.4 mag and well-determined spectroscopic redshifts. The overlap region between the two surveys is 12.6 deg2; the matched sample has a median redshift of z≈ 0.2. The cross-correlation of GAMA and H-ATLAS galaxies within this region can be fitted by a power law, with correlation length r0≈ 4.63 ± 0.51 Mpc. Comparing with the corresponding autocorrelation function of GAMA galaxies within the SDP field yields a relative bias (averaged over 2–8 Mpc) of H-ATLAS and GAMA galaxies of bH/bG≈ 0.6. Combined with clustering measurements from previous optical studies, this indicates that most of the low-redshift H-ATLAS sources are hosted by haloes with masses comparable to that of the Milky Way. The correlation function appears to depend on the 250-μm luminosity, L250, with bright (median luminosity νL250∼ 1.6 × 1010 L⊙) objects being somewhat more strongly clustered than faint (νL250∼ 4.0 × 109 L⊙) objects. This implies that galaxies with higher dust-obscured star formation rates are hosted by more massive haloes.