Guo, Q. and Cole, S. and Lacey, C.G. and Baugh, C.M. and Frenk, C.S. and Norberg, P. and Auld, R. and Baldry, I.K. and Bamford, S.P. and Bourne, N. and Buttiglione, E.S. and Cava, A. and Cooray, A. and Croom, S. and Dariush, A. and de Zotti, G. and Driver, S. and Dunne, L. and Dye, S. and Eales, S. and Fritz, J. and Hopkins, A. and Hopwood, R. and Ibar, E. and Ivison, R.J. and Jarvis, M. and Jones, D.H. and Kelvin, L. and Liske, J. and Loveday, J. and Maddox, S.J. and Parkinson, H. and Pascale, E. and Peacock, J.A. and Pohlen, M. and Prescott, M. and Rigby, E.E. and Robotham, A. and Rodighiero, G. and Sharp, R. and Smith, D.J.B. and Temi, P. and van Kampen, E. (2011) 'Which haloes host Herschel-ATLAS galaxies in the local Universe?', Monthly notices of the Royal Astronomical Society., 412 (4). pp. 2277-2285.
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.
|Keywords:||Galaxies: haloes, Dark matter, Infrared: galaxies.|
|Full text:||(VoR) Version of Record|
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|Publisher Web site:||http://dx.doi.org/10.1111/j.1365-2966.2010.18051.x|
|Publisher statement:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||15 December 2014|
|Date of first online publication:||April 2011|
|Date first made open access:||No date available|
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