The clustering evolution of dusty star-forming galaxies

Cowley, William I.; Lacey, Cedric G.; Baugh, C. M.; Cole, Shaun

doi:10.1093/mnras/stw1069

Cited by 28 publications

(35 citation statements)

References 120 publications

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“…The separation disappears at > z 3, as discussed in Section 5.2 this could be due to the increasing contamination of dusty galaxies on the UVJ-selected quiescent populations. The latest model predictions by Cowley et al (2016) on the clustering of both faint and bright SMGs are systematically lower in all three redshift bins.…”

Section: Discussionmentioning

confidence: 74%

“…The dotted curves show the autocorrelation functions of dark matter. We also show in green dashed curves the latest predictions based on the semi-analytic model GALFORM (Cowley et al 2016). At < z 3, the comparison quiescent galaxies have systematically higher clustering amplitude, whereas TCGs and comparison starforming galaxies are similarly clustered in all redshift bins.…”

Section: Two Point Autocorrelation Function and Large-scale Power-lawmentioning

confidence: 73%

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Faint Submillimeter Galaxies Identified Through Their Optical/Near-Infrared Colors. I. Spatial Clustering and Halo Masses

Chen

Smail

Swinbank

et al. 2016

ApJ

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The properties of submillimeter galaxies (SMGs) that are fainter than the confusion limit of blank-field single-dish surveys (  S 850 2 mJy) are poorly constrained. Using a newly developed color selection technique, OpticalInfrared Triple Color (OIRTC), that has been shown to successfully select such faint SMGs, we identify a sample of 2938 OIRTC-selected galaxies, dubbed Triple Color Galaxies (TCGs), in the UKIDSS-UDS field. We show that these galaxies have a median 850 μm flux of =  S 0.96 0.04 850 mJy (equivalent to a star formation rate SFR 60 100 - M yr −1 based on spectral energy distribution fitting), representing the first large sample of faint SMGs that bridges the gap between bright SMGs and normal star-forming galaxies in S 850 and L IR . We assess the basic properties of TCGs and their relationship with other galaxy populations atz 2. We measure the two-point autocorrelation function for this population and derive a typical halo mass of log 10 (M halo ) = -, 2-3, and 3-5, respectively. Together with the bright SMGs (  S 2 850 mJy) and a comparison sample of less far-infrared luminous star-forming galaxies, we find a lack of dependence between spatial clustering and S 850 (or SFR), suggesting that the difference between these populations may lie in their local galactic environment. Lastly, on the scale of~8 17 kpc -at < < z 1 5we find a tentative enhancement of the clustering of TCGs over the comparison star-forming galaxies, suggesting that some faint SMGs are physically associated pairs, perhaps reflecting a merging origin in their triggering.

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Section: Discussionmentioning

confidence: 74%

Section: Two Point Autocorrelation Function and Large-scale Power-lawmentioning

confidence: 73%

Faint Submillimeter Galaxies Identified Through Their Optical/Near-Infrared Colors. I. Spatial Clustering and Halo Masses

Chen

Smail

Swinbank

et al. 2016

ApJ

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“…However, when galaxies are selected by their star formation rates, N cen does not necessarily reach unity (e.g. Zheng et al 2005;Contreras et al 2015;Cowley et al 2016). This implies that haloes above a certain mass will not necessarily harbour a star forming galaxy or, in our case, an ELG.…”

Section: The Mean Halo Occupation Distributionmentioning

confidence: 99%

The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

González-Pérez¹,

Comparat²,

Norberg³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Emission line galaxies (ELGs) are used in several ongoing and upcoming surveys (SDSS-IV/eBOSS, DESI) as tracers of the dark matter distribution. Using a new galaxy formation model, we explore the characteristics of [O ii] emitters, which dominate optical ELG selections at z 1. Model [O ii] emitters at 0.5 < z < 1.5 are selected to mimic the DEEP2, VVDS, eBOSS and DESI surveys. The luminosity functions of model [O ii] emitters are in reasonable agreement with observations. The selected [O ii] emitters are hosted by haloes with M halo 10 10.3 h −1 M , with ∼ 90% of them being central star-forming galaxies. The predicted mean halo occupation distributions of [O ii] emitters has a shape typical of that inferred for star-forming galaxies, with the contribution from central galaxies, N [O ii] cen , being far from the canonical step function. The N [O ii] cen can be described as the sum of an asymmetric Gaussian for disks and a step function for spheroids, which plateaus below unity. The model [O ii] emitters have a clustering bias close to unity, which is below the expectations for eBOSS and DESI ELGs. At z ∼ 1, a comparison with observed g-band selected galaxy, which are expected to be dominated by [O ii] emitters, indicates that our model produces too few [O ii] emitters that are satellite galaxies. This suggests the need to revise our modelling of hot gas stripping in satellite galaxies.

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“…Predicted evolution of large-scale bias with redshift. Green squares with errorbars represent the bias measured directly from the 3D spatial correlation function of SMGs with S 850µm > 4 mJy, as is done in Cowley et al (2016). The 1σ errors are calculated using the volume bootstrap method advocated in Norberg et al (2009).…”

Section: A Cross-correlation Analysis Of Sub-mm Sourcesmentioning

confidence: 99%

“…Fakhouri et al 2010), which can then be compared to the halo masses inferred from the observed clustering of local galaxy populations. However, the spread in the host halo masses of SMG descendants could be significant (∼ 2 dex, Cowley et al 2016) due to the hierarchical growth of structure.…”

Section: Introductionmentioning

confidence: 99%

Blending bias impacts the host halo masses derived from a cross-correlation analysis of bright submillimetre galaxies

Cowley

Lacey

Baugh

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

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Placing bright sub-millimetre galaxies (SMGs) within the broader context of galaxy formation and evolution requires accurate measurements of their clustering, which can constrain the masses of their host dark matter halos. Recent work has shown that the clustering measurements of these galaxies may be affected by a 'blending bias,' which results in the angular correlation function of the sources extracted from single-dish imaging surveys being boosted relative to that of the underlying galaxies. This is due to confusion introduced by the coarse angular resolution of the single-dish telescope and could lead to the inferred halo masses being significantly overestimated. We investigate the extent to which this bias affects the measurement of the correlation function of SMGs when it is derived via a cross-correlation with a more abundant galaxy population. We find that the blending bias is essentially the same as in the auto-correlation case and conclude that the best way to reduce its effects is to calculate the angular correlation function using SMGs in narrow redshift bins. Blending bias causes the inferred host halo masses of the SMGs to be overestimated by a factor of ∼ 6 when a redshift interval of δz = 3 is used. However, this reduces to a factor of ∼ 2 for δz = 0.5. The broadening of photometric redshift probability distributions with increasing redshift can therefore impart a mild halo 'downsizing' effect onto the inferred host halo masses, though this trend is not as strong as seen in recent observational studies.

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The clustering evolution of dusty star-forming galaxies

Cited by 28 publications

References 120 publications

Faint Submillimeter Galaxies Identified Through Their Optical/Near-Infrared Colors. I. Spatial Clustering and Halo Masses

Faint Submillimeter Galaxies Identified Through Their Optical/Near-Infrared Colors. I. Spatial Clustering and Halo Masses

The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

Blending bias impacts the host halo masses derived from a cross-correlation analysis of bright submillimetre galaxies

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