The VISTA Deep Extragalactic Observations (VIDEO) survey★

Jarvis, Matt J.; Bonfield, D. G.; Bruce, Victoria; Geach, J. E.; McAlpine, K.; McLure, R. J.; González-Solares, E.; Irwin, M. J.; Lewis, Jim; Yoldaș, A. Küpcü; Andreon, S.; Cross, N. J. G.; Emerson, J. P.; Dalton, Gavin; Dunlop, James; Hodgkin, S. T.; Le, Fèvre O.; Karouzos, Marios; Meisenheimer, K.; Oliver, Seb; Rawlings, Steve; Simpson, Chris; Smail, Ian; Smith, D. J. B.; Sullivan, M.; Sutherland, William J.; White, Sarah V.; Zwart, Jonathan T. L.

doi:10.1093/mnras/sts118

Cited by 311 publications

(281 citation statements)

References 113 publications

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“…Note that we correct for incompleteness arising from our slightly different EW and colour significance cuts. (Jarvis et al 2013), which is about 3.5 magnitudes deeper than VISTA. We also make use of the IR photometric data taken in the SA22 field as part of the second data release of the UKIDSS Deep Extragalactic Survey , which reaches magnitudes 23.4 and 22.8 in the J and Ks bands, respectively, with a catalogue from Sobral et al (2015b).…”

Section: Optical and Ir Datamentioning

confidence: 84%

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe

Sobral

2015

Mon. Not. R. Astron. Soc.

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We carried out the largest (> 3.5 × 10 5 Mpc 3 , 26 deg 2 ) Hα narrow band survey to date at z ∼ 0.2 in the SA22, W2 and XMMLSS extragalactic fields. Our survey covers a large enough volume to overcome cosmic variance and to sample bright and rare Hα emitters up to an observed luminosity of ∼ 10 42.4 erg s −1 , equivalent to ∼ 11M yr −1 . Using our sample of 220 sources brighter than > 10 41.4 erg s −1 (> 1M yr −1 ), we derive Hα luminosity functions, which are well described by a Schechter function with φ * = 10 −2.85±0.03 Mpc −3 and L * Hα = 10 41.71±0.02 erg s −1 (with a fixed faint end slope α = −1.35). We find that surveys probing smaller volumes (∼ 3 × 10 4 Mpc 3 ) are heavily affected by cosmic variance, which can lead to errors of over 100 per cent in the characteristic density and luminosity of the Hα luminosity function. We derive a star formation rate density of ρ SFRD = 0.0094 ± 0.0008 M yr −1 , in agreement with the redshift-dependent Hα parametrisation from Sobral et al. (2013). The two-point correlation function is described by a single power law ω(θ ) = (0.159 ± 0.012)θ (−0.75±0.05) , corresponding to a clustering length of r 0 = 3.3 ± 0.8 Mpc/h. We find that the most luminous Hα emitters at z ∼ 0.2 are more strongly clustered than the relatively fainter ones. The L * Hα Hα emitters at z ∼ 0.2 in our sample reside in ∼ 10 12.5−13.5 M dark matter haloes. This implies that the most star forming galaxies always reside in relatively massive haloes or group-like environments and that the typical host halo mass of star-forming galaxies is independent of redshift if scaled by L Hα /L * Hα (z), as proposed by Sobral et al. (2010).

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Section: Optical and Ir Datamentioning

confidence: 84%

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe

Sobral

2015

Mon. Not. R. Astron. Soc.

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“…The completeness reaches 80% at K s = 22; this was determined from a comparison with the deepest surveys UKIDSS Ultra-Deep Survey(UDS, Lawrence et al 2007) and VIDEO (Jarvis et al 2013) in overlapping regions. Because the primary optical detection is based on the gri − χ 2 image, we may miss the reddest high-redshift galaxies.…”

Section: Wircam K S Photometrymentioning

confidence: 94%

The VIPERS Multi-Lambda Survey

Moutard

Arnouts

Ilbert

et al. 2016

A&A

171

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We investigate the evolution of the galaxy stellar mass function and stellar mass density from redshift z = 0.2 to z = 1.5 of a K s < 22-selected sample with highly reliable photometric redshifts and over an unprecedentedly large area. Our study is based on near-infrared observations carried out with the WIRCam instrument at CFHT over the footprint of the VIPERS spectroscopic survey and benefits from the high-quality optical photometry from the CFHTLS and ultraviolet observations with the GALEX satellite. The accuracy of our photometric redshifts is σ ∆z/(1+z) < 0.03 and 0.05 for the bright (i AB < 22.5) and faint (i AB > 22.5) samples, respectively. The galaxy stellar mass function is measured with ∼760 000 galaxies down to K s ∼ 22 and over an effective area of ∼22.4 deg 2 , the latter of which drastically reduces the statistical uncertainties (i.e. Poissonian error and cosmic variance). We point out the importance of carefully controlling the photometric calibration, whose effect becomes quickly dominant when statistical uncertainties are reduced, which will be a major issue for future cosmological surveys with EUCLID or LSST, for instance. By exploring the rest-frame (NUV−r) vs. (r − K s ) colour-colour diagram with which we separated star-forming and quiescent galaxies, (1) we find that the density of very massive log(M * /M ) > 11.5 galaxies is largely dominated by quiescent galaxies and increases by a factor 2 from z ∼ 1 to z ∼ 0.2, which allows for additional mass assembly through dry mergers. (2) We also confirm the scenario in which star formation activity is impeded above a stellar mass log(M sf /M ) = 10.64 ± 0.01. This value is found to be very stable at 0.2 < z < 1.5. (3) We discuss the existence of a main quenching channel that is followed by massive star-forming galaxies, and we finally (4) characterise another quenching mechanism that is required to explain the clear excess of low-mass quiescent galaxies that is observed at low redshift.

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“…In the early phases this will be from surveys that are currently underway (e.g. McCracken et al 2012;Jarvis et al 2013;de Jong et al 2013;Edge et al 2013;Banerji et al 2014). …”

Section: Photometric Redshiftsmentioning

confidence: 99%

Cosmology with SKA Radio Continuum Surveys

Jarvis¹,

Bacon²,

Blake³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Radio continuum surveys have, in the past, been of restricted use in cosmology. Most studies have concentrated on cross-correlations with the cosmic microwave background to detect the integrated Sachs-Wolfe effect, due to the large sky areas that can be surveyed. As we move into the SKA era, radio continuum surveys will have sufficient source density and sky area to play a major role in cosmology on the largest scales. In this chapter we summarise the experiments that can be carried out with the SKA as it is built up through the coming decade. We show that the SKA can play a unique role in constraining the non-Gaussianity parameter to σ f NL ∼ 1, and provide a unique handle on the systematics that inhibit weak lensing surveys. The SKA will also provide the necessary data to test the isotropy of the Universe at redshifts of order unity and thus evaluate the robustness of the cosmological principle. Thus, SKA continuum surveys will turn radio observations into a central probe of cosmological research in the coming decades.Advancing Astrophysics with the Square Kilometre Array

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The VISTA Deep Extragalactic Observations (VIDEO) survey★

Cited by 311 publications

References 113 publications

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

The VIPERS Multi-Lambda Survey

Cosmology with SKA Radio Continuum Surveys

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