Publication details for Professor Ian SmailCochrane, R.K., Best, P.N., Sobral, D., Smail, I., Wake, D.A., Stott, J.P. & Geach, J.E. (2017). The H α luminosity-dependent clustering of star-forming galaxies from z ∼ 0.8 to ∼2.2 with HiZELS. MNRAS 469(3): 2913-2932.
- Publication type: Journal Article
- ISSN/ISBN: 0035-8711, 1365-2966
- DOI: 10.1093/mnras/stx957
- Further publication details on publisher web site
- Durham Research Online (DRO) - may include full text
Author(s) from Durham
We present clustering analyses of identically selected star-forming galaxies in three narrow redshift slices (at z = 0.8, 1.47 and 2.23), from the High-Redshift(Z) Emission Line Survey (HiZELS), a deep, near-infrared narrow-band survey. The HiZELS samples span the peak in the cosmic star formation rate density, identifying typical star-forming galaxies at each epoch. Narrow-band samples have well-defined redshift distributions and are therefore ideal for clustering analyses. We quantify the clustering of the three samples, and of H α luminosity-selected subsamples, initially using simple power-law fits to the two-point correlation function. We extend this work to link the evolution of star-forming galaxies and their host dark matter haloes over cosmic time using sophisticated dark matter halo models. We find that the clustering strength, r0, and the bias of galaxy populations relative to the clustering of dark matter increase linearly with H α luminosity (and, by implication, star formation rate) at all three redshifts, as do the host dark matter halo masses of the HiZELS galaxies. The typical galaxies in our samples are star-forming centrals, residing in haloes of mass Mhalo ∼ a few times 1012 M⊙. We find a remarkably tight redshift-independent relation between the H α luminosity scaled by the characteristic luminosity,
, and the minimum host dark matter halo mass of central galaxies. This reveals that the dark matter halo environment is a strong driver of galaxy star formation rate and therefore of the evolution of the star formation rate density in the Universe.