The 2dF QSO Redshift Survey

Boyle, B. J.; Croom, S. M.; Smith, R. J.; Shanks, T.; Outram, P. J.; Hoyle, F.; Miller, Leon K.; Loaring, N. S.

doi:10.1007/10854354_75

Cited by 58 publications

(144 citation statements)

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“…A significant advantage of the SHS data over its rivals is the ability to detect point sources that have been photometrically calibrated to CCD standards (e.g. Boyle, Shanks & Croom 1995; Croom et al 1999). With measurements of isophotal magnitude and object classifications, it is possible to apply a photometric calibration to the Hα and SR films by comparing the SuperCOSMOS raw magnitudes of stars from the Tycho‐2 Catalogue (Hog et al 2000) and the Guide Star Photometric Catalogue (Lasker et al 1988).…”

Section: Shs Point Source Photometrymentioning

confidence: 99%

“…With measurements of isophotal magnitude and object classifications, it is possible to apply a photometric calibration to the Hα and SR films by comparing the SuperCOSMOS raw magnitudes of stars from the Tycho‐2 Catalogue (Hog et al 2000) and the Guide Star Photometric Catalogue (Lasker et al 1988). These in turn are checked against photometric standards derived from the CCD observations given by Croom et al (1999) and Boyle et al (1995). The narrow‐band Hα images are calibrated to an ‘R‐equivalent’ scale.…”

Section: Shs Point Source Photometrymentioning

confidence: 99%

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The AAO/UKST SuperCOSMOS Hα survey

Parker

Phillipps

Pierce

et al. 2005

Monthly Notices of the Royal Astronomical Society

307

276

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The UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory completed a narrowband Hα plus [N II] 6548, 6584-Å survey of the Southern Galactic Plane and Magellanic Clouds in late 2003. The survey, which was the last UKST wide-field photographic survey and the only one undertaken in a narrow-band, is now an online digital data product of the Wide-Field Astronomy Unit of the Royal Observatory Edinburgh (ROE). The survey utilized a high specification, monolithic Hα interference bandpass filter of exceptional quality. In conjunction with the fine-grained Tech-Pan film as a detector it has produced a survey with a powerful combination of area coverage (4000 square degrees), resolution (∼1 arcsec) and sensitivity ( 5 Rayleighs), reaching a depth for continuum point sources of R 20.5. The main survey consists of 233 individual fields on a grid of centres separated by 4 • at declinations below +2 • and covers a swathe approximately 20 • wide about the Southern Galactic Plane. The original survey films were scanned by the SuperCOSMOS measuring machine at the Royal Observatory, Edinburgh, to provide the online digital atlas called the SuperCOSMOS Hα Survey (SHS). We present the background of the survey, the key survey characteristics, details and examples of the data product, calibration process, comparison with other surveys and a brief description of its potential for scientific exploitation.

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Section: Shs Point Source Photometrymentioning

confidence: 99%

Section: Shs Point Source Photometrymentioning

confidence: 99%

The AAO/UKST SuperCOSMOS Hα survey

Parker

Phillipps

Pierce

et al. 2005

Monthly Notices of the Royal Astronomical Society

307

276

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“…In this case, according to the convolution theorem, the resulting power spectrum signal is damped along the radial direction where g ( k x ) = exp[−( k x σ x ) 2 ] is the square of the Fourier transform of f ( x ). The power spectrum of the resulting distribution is measured using standard estimation tools: essentially this involves taking the Fourier transform of the density field, subtracting that of the survey window function and binning up the resulting modes in k ‐space (see e.g. Hoyle et al 2002; note that we do not use the optimal weighting technique presented by Feldman, Kaiser & Peacock (1994) because this does not represent a simple convolution of the density field and consequently step (xiii) below would not be possible). Power spectrum modes in Fourier space are divided into bins of total k , up to a maximum of k lin .…”

Section: Modelling the Power Spectrum Of Photometric Redshift Surveysmentioning

confidence: 99%

Cosmology with photometric redshift surveys

Blake¹,

Bridle²

2005

Monthly Notices of the Royal Astronomical Society

124

169

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We explore the utility of future photometric redshift imaging surveys for delineating the large-scale structure of the Universe, and assess the resulting constraints on the cosmological model. We perform two complementary types of analysis: (1) We quantify the statistical confidence and the accuracy with which such surveys will be able to detect and measure characteristic features in the clustering power spectrum such as the acoustic oscillations and the turnover, in a 'model-independent' fashion. We show for example that a 10,000 deg^2 imaging survey with depth r = 22.5 and photometric redshift accuracy dz/(1+z) = 0.03 will detect the acoustic oscillations with 99.9% confidence, measuring the associated preferred cosmological scale with 2% precision. Such a survey will also detect the turnover with 95% confidence, determining the corresponding scale with 20% accuracy. (2) By assuming a Lambda-CDM model power spectrum we calculate the confidence with which a non-zero baryon fraction can be deduced from such future galaxy surveys. We quantify 'wiggle detection' by calculating the number of standard deviations by which the baryon fraction is measured, after marginalizing over the shape parameter. This is typically a factor of four more significant (in terms of number of standard deviations) than the 'model-independent' result. We conclude that the precision with which the clustering pattern may be inferred from future photometric redshift surveys will be competitive with contemporaneous spectroscopic redshift surveys, assuming that systematic effects can be controlled. We also note that an analysis of Luminous Red Galaxies in the Sloan Digital Sky Survey may yield a marginal detection of acoustic oscillations in the imaging survey, in addition to that recently reported for the spectroscopic component.Comment: 23 pages, 22 figures, version accepted by MNRA

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“…The spectra of the first 10 000 2QZ QSOs were released in 2001 April (Croom et al 2001a) and can be obtained at http://www.2dfquasar.org. Hoyle et al (2002) used these QSOs to measure the QSO power spectrum. They found that the QSO power spectrum has similar amplitude to that of local galaxies, and little evolution is seen with redshift.…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we re‐apply the power spectrum analysis described in Hoyle et al (2002) to the final 2QZ catalogue containing 22 652 QSOs. As well as having more than twice as many QSOs as available to Hoyle et al this data set has a much cleaner window function, significantly reducing the potential systematics on large scales.…”

Section: Introductionmentioning

confidence: 99%

The 2dF QSO Redshift Survey -- XI. The QSO power spectrum

Outram¹,

Hoyle²,

Shanks³

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We present a power spectrum analysis of the final 2dF Quasi-Stellar Object (QSO) Redshift Survey catalogue containing 22 652 QSOs. Utilizing the huge volume probed by the QSOs, we can accurately measure power out to scales of ∼500 h −1 Mpc and derive new constraints, at z ∼ 1.4, on the matter and baryonic contents of the Universe. Importantly, these new cosmological constraints are derived at an intermediate epoch between the cosmic microwave background observations at z ∼ 1000, and local (z ∼ 0) studies of large-scale structure; the average QSO redshift corresponds to a look-back time of approximately two-thirds of the age of the Universe. We find that the amplitude of clustering of the QSOs at z ∼ 1.4 is similar to that of present-day galaxies. The power spectra of the QSOs at high and low redshift are compared and we find little evidence for any evolution in the amplitude. Assuming a cosmology to derive the comoving distances, r (z), to the QSOs, the power spectrum derived can be well described by a model with shape parameter = 0.13 ± 0.02. If an Einstein-de Sitter model r(z) is instead assumed, a slightly higher value of = 0.16 ± 0.03 is obtained. A comparison with the Hubble Volume cold dark matter (CDM) simulation shows very good agreement over the whole range of scales considered. A standard ( m = 1) CDM model, however, predicts a much higher value of than is observed, and it is difficult to reconcile such a model with these data. We fit CDM model power spectra (assuming scale-invariant initial fluctuations), convolved with the survey window function, and corrected for redshift space distortions, and we find that models with baryon oscillations are slightly preferred, with the baryon fraction b / m = 0.18 ± 0.10. The overall shape of the power spectrum provides a strong constraint on m h (where h is the Hubble parameter), with m h = 0.19 ± 0.05.

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The 2dF QSO Redshift Survey

Cited by 58 publications

References 0 publications

The AAO/UKST SuperCOSMOS Hα survey

The AAO/UKST SuperCOSMOS Hα survey

Cosmology with photometric redshift surveys

The 2dF QSO Redshift Survey -- XI. The QSO power spectrum

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