Abstract / Description of output
We use the UKIDSS Ultra Deep Survey to trace the evolution of galaxy
clustering to z = 3. Using photometric redshifts derived from data
covering the wavelength range 0.3-4.5μm, we examine this clustering
as a function of absolute K-band luminosity, colour and star formation
rate. Comparing the deprojected clustering amplitudes, we find that red
galaxies are more strongly clustered than blue galaxies out to at least
z = 1.5, irrespective of rest-frame K-band luminosity. We then construct
passive and star-forming samples based on stellar age, colour and star
formation histories calculated from the best-fitting templates. The
clustering strength of star-forming galaxies declines steadily from
r0 ~= 7h-1Mpc at z ~= 2 to r0 ~=
3h-1Mpc at z ~= 0, while passive galaxies have clustering
strengths up to a factor of 2 higher. Within the passive and
star-forming subsamples, however, we find very little dependence of
galaxy clustering on K-band luminosity. Galaxy `passivity' appears to be
the strongest indicator of clustering strength. We compare these
clustering measurements with those predicted for dark matter haloes and
conclude that passive galaxies typically reside in haloes of mass M
>= 1013Msolar while luminous star-forming
galaxies occupy haloes an order of magnitude less massive over the range
0.5 <z <1.5. The decline in the clustering strength of
star-forming galaxies with decreasing redshift indicates a decline in
the hosting halo mass for galaxies of a given luminosity. We find
evidence for convergence of clustering in star-forming and passive
galaxies around z ~ 2, which is consistent with this being the epoch at
which the red sequence of galaxies becomes distinct.
Original language | English |
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Pages (from-to) | 1212-1222 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 407 |
DOIs | |
Publication status | Published - 1 Sept 2010 |