The Clustering of Faint Galaxies and the Evolution of XI (r)

Hudon, J. D.; Lilly, S. J.

doi:10.1086/177800

Cited by 34 publications

(39 citation statements)

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“…This variety of environments is not seen amongst local ULIRGs, which are generally not found in rich environments (Sanders & Mirabel 1996). The mean environmental richness of our sample, at 〈 B gh 〉= 190 ± 45 Mpc 1.77 , is higher, at just over 3σ significance, than the galaxy–galaxy correlation statistic both locally (Loveday et al 1995; Guzzo et al 1997) and at moderate redshifts (Hudon & Lilly 1996), though we note that the latter study measured values of B gg up to redshifts of only z ∼ 0.5. We infer that, in going from z ∼ 0 to z ∼ 1 the environments of IR‐luminous galaxies become more diverse, and that the mean environment becomes richer than that of normal galaxies both locally and at moderate redshifts.…”

Section: Discussionmentioning

confidence: 62%

The environments of hyperluminous infrared galaxies at 0.44 <z< 1.55

Farrah¹,

Fox²,

Serjeant³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present deep wide‐field Ks‐band observations of six Hyperluminous Infrared Galaxies (HLIRGs) spanning a redshift range 0.44 < z < 1.55. The sample resides in a wide variety of environments, from the field to Abell 2 clusters, with a mean galaxy–HLIRG clustering amplitude of 〈Bgh〉= 190 ± 45 Mpc1.77. The range in environments, and the mean clustering level, are both greater than those seen in local IR‐luminous galaxies, from which we infer that the range of galaxy evolution processes driving IR‐luminous galaxy evolution at z > 0.5 is greater than locally, and includes mergers between gas‐rich spiral galaxies in the field, but also includes encounters in clusters and hierarchical build‐up. The similarity in the range of environments and mean clustering amplitude between our sample and QSOs over a similar redshift range is consistent with the interpretation where evolutionary connections between IR‐luminous galaxies and QSOs are stronger at z > 0.5 than locally, and that, at these redshifts, the processes that drive QSO evolution are similar to those that drive IR‐luminous galaxy evolution. From comparison of the HLIRG and QSO host galaxies we further postulate that a larger fraction of IR‐luminous galaxies pass through an optical QSO stage at z > 0.5 than locally.

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Section: Discussionmentioning

confidence: 62%

The environments of hyperluminous infrared galaxies at 0.44 <z< 1.55

Farrah¹,

Fox²,

Serjeant³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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“…This is the correlation length of faint ( B >22) galaxies (e.g. Roche et al 1993; Efstathiou 1995; Hudon & Lilly 1996).…”

Section: Resultsmentioning

confidence: 99%

The environments of intermediate-redshift QSOs: 0.3 < z < 0.7

Smith

Boyle

Maddox

2000

Monthly Notices of the Royal Astronomical Society

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An angular correlation of low significance (2 sigma) is observed between 0.3 < z < 0.5 QSOs and V < 23 galaxies. Overall, the cross-correlation function between 82 intermediate-redshift (0.3 < z < 0.7), X-ray selected QSOs and V < 24 galaxies is investigated, but no signal is detected for the z > 0.5 QSOs. After converting to an excess of galaxies physically associated with the QSO, this lack of strong correlation is shown to be consistent with the clustering of normal galaxies at the same moderate redshifts. Combined with previous observations, these results imply that the environments of radio-quiet QSOs do not undergo significant evolution with respect to the galaxy population over a wide range of redshifts (0 < z < 1.5). This is in marked contrast to the rapid increase in the richness of the environments associated with radio-loud QSOs over the same redshift range.Comment: 12 pages, 8 figures, MNRAS TeX macro, to appear to MNRA

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“…3 in Hudon & Lilly (1996). It shows that there are about 3500 objects in the 4 square degrees CFRS survey with 0.35 < z < 0.45 and 19 < R < 23.5, essentially the magnitude range covered by the proposed survey.…”

Section: Case Study 2: Q 0 From Galaxy Countsmentioning

confidence: 74%

“…Figure 4 shows the redshift distributions expected for surveys reaching 22nd, 24th and 27th blue magnitudes. Hudon & Lilly (1996) have also computed redshift distributions in the R band. It must be noted (e.g.…”

Section: Case Study 2: Q 0 From Galaxy Countsmentioning

confidence: 99%

Cosmology at low redshifts

Borra

2003

A&A

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Abstract. It is argued that it is far more cost effective to carry out some projects with medium-sized dedicated zenith telescopes rather than large steerable telescopes, freeing the later to carry out projects that truly need them. I show that the large number of objects observed with a surveying 4-m zenith telescope allows one to carry out cosmological projects at low redshifts. Examining two case studies, I show first that a variability survey would obtain light curves for several thousands of type Ia supernovae per year up to z = 1 and easily discriminate among competing cosmological models. Finally, I discuss a second case study, consisting of a spectrophotometric survey carried out with interference filters, showing its power to discriminate among cosmological models and to study the large-scale distribution of galaxies in the Universe.

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The Clustering of Faint Galaxies and the Evolution of XI (r)

Cited by 34 publications

References 1 publication

The environments of hyperluminous infrared galaxies at 0.44 <z< 1.55

The environments of hyperluminous infrared galaxies at 0.44 <z< 1.55

The environments of intermediate-redshift QSOs: 0.3 < z < 0.7

Cosmology at low redshifts

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