共查询到20条相似文献，搜索用时 31 毫秒
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A. Ratcliffe T. Shanks Q. A. Parker A. Broadbent F. G. Watson A. P. Oates C. A. Collins & R. Fong 《Monthly notices of the Royal Astronomical Society》1998,300(2):417-462
We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ∼2500 galaxy redshifts to a limiting apparent magnitude of B J ⋍17 mag, covering a ∼1500-deg2 area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of ±150 km s−1 . The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b J ⋍17 mag, over a wide area of the sky. 相似文献
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Vincent R. Eke Shaun Cole Carlos S. Frenk & J. Patrick Henry 《Monthly notices of the Royal Astronomical Society》1998,298(4):1145-1158
The evolution of the abundance of galaxy clusters depends sensitively on the value of the cosmological density parameter, Ω0 . Recent ASCA data are used to quantify this evolution as measured by the cluster X-ray temperature function. A χ2 minimization fit to the cumulative temperature function, as well as a maximum-likelihood estimate (which requires additional assumptions about cluster luminosities), leads to the estimate Ω0 ≈ 0.45 ± 0.25 (1σ statistical error). Various systematic uncertainties are considered, none of which significantly enhances the probability that Ω0 = 1. These conclusions hold for models with or without a cosmological constant, i.e., with Λ0 = 0 or Λ0 = 1 − Ω0 . The statistical uncertainties are at least as large as any of the individual systematic errors that have been considered here, suggesting that additional temperature measurements of distant clusters will allow an improvement in this estimate. An alternative method that uses the highest redshift clusters to place an upper limit on Ω0 is also presented and tentatively applied, with the result that Ω0 1 can be ruled out at the 98 per cent confidence level. Whilst this method does not require a well-defined statistical sample of distant clusters, there are still modelling uncertainties that preclude a firmer conclusion at this time. 相似文献
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Scott T. Kay Richard G. Bower 《Monthly notices of the Royal Astronomical Society》1999,308(3):664-676
In this paper we have extended the entropy-driven model of cluster evolution developed by Bower in order to be able to predict the evolution of galaxy clusters for a range of cosmological scenarios. We have applied this model to recent measurements of the evolution of the L x − T normalization and X-ray luminosity function in order to place constraints on cosmological parameters. We find that these measurements alone do not select a particular cosmological framework. An additional constraint is required on the effective slope of the power spectrum to break the degeneracy that exists between this and the background cosmology. We therefore include a theoretical calculation of the Ω0 dependence on the power spectrum, based on the cold dark matter paradigm, which infers Ω0 <0.55 (0.1<Ω0 <0.7 for Ω0 +Λ0 =1), at the 95 per cent confidence level. Alternatively, an independent measurement of the slope of the power spectrum from galaxy clustering requires Ω0 <0.6 (Ω0 <0.65 for Ω0 +Λ0 =1), again to 95 per cent confidence. The rate of entropy evolution is insensitive to the values of Ω0 considered, although it is sensitive to changes in the distribution of the intracluster medium. 相似文献
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We perform Monte Carlo simulations of synthetic EMSS cluster samples, to quantify the systematic errors and the statistical uncertainties on the estimate of Ω0 derived from fits to the cluster number density evolution and to the X-ray temperature distribution up to z =0.83 . We identify the scatter around the relation between cluster X-ray luminosity and temperature to be a source of systematic error, of the order of Δsyst Ω0 =0.09 , if not properly taken into account in the modelling. After correcting for this bias, our best Ω0 is 0.66. The uncertainties on the shape and normalization of the power spectrum of matter fluctuations imply relatively large uncertainties on this estimate of Ω0 , of the order of Δstat Ω0 =0.1 at the 1 σ level. On the other hand, the statistical uncertainties due to the finite size of the high-redshift sample are twice as small. Therefore, what is needed in order to improve the accuracy of Ω0 estimates based on cluster number density evolution is a more reliable measure of the local temperature function and a better understanding of the cluster observed properties both in the local Universe and at high redshift, that is the relation between cluster mass, temperature and luminosity. This requires detailed observations of X-ray selected cluster samples, in comparison with hydrodynamic simulations including refined physics. 相似文献
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P. A. Thomas Orrarujee Muanwong F. R. Pearce H. M. P. Couchman A. C. Edge A. Jenkins L. Onuora 《Monthly notices of the Royal Astronomical Society》2001,324(2):450-462
We have extracted over 400 clusters, covering more than two decades in mass, from three simulations of the τ CDM cosmology. This represents the largest uniform catalogue of simulated clusters ever produced. The clusters exhibit a wide variety of density profiles. Only a minority are well-fitted in their outer regions by the widely used density profile of Navarro, Frenk & White (NFW), which is applicable to relaxed haloes. Others have steeper outer density profiles, show sharp breaks in their density profiles, or have significant substructure. If we force a fit to the NFW profile, then the best-fitting concentrations decline with increasing mass, but this is driven primarily by an increase in substructure as one moves to higher masses. The temperature–mass relations for properties measured within a sphere enclosing a fixed overdensity all follow the self-similar form, T ∝ M 2/3 ; however, the normalization is lower than the value inferred for observed clusters. The temperature–mass relations for properties measured within a fixed physical radius are significantly steeper then this. Both can be accurately predicted using the NFW model. 相似文献
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Michael E. Jones Alastair C. Edge Keith Grainge William F. Grainger Rüdiger Kneissl G. G. Pooley Richard Saunders Shigeru J. Miyoshi Taisuke Tsuruta Koujun Yamashita Yuzuru Tawara Akihiro Furuzawa Akihiro Harada Isamu Hatsukade 《Monthly notices of the Royal Astronomical Society》2005,357(2):518-526
We have observed the Sunyaev–Zel'dovich (SZ) effect in a sample of five moderate-redshift clusters with the Ryle Telescope, and used them in conjunction with X-ray imaging and spectral data from ROSAT and ASCA to measure the Hubble constant. This sample was chosen with a strict X-ray flux limit using both the Bright Cluster Sample and the Northern ROSAT All-Sky Survey (RASS) cluster catalogues to be well above the surface brightness limit of the RASS, and hence to be unbiased with respect to the orientation of the cluster. This controls a major potential systematic effect in the SZ/X-ray method of measuring H 0 . Taking the weighted geometric mean of the results and including the main sources of error, namely the noise in the SZ measurement, the uncertainty in the X-ray temperatures and the unknown ellipticity and substructure of the clusters, we find H 0 = 59+10 −9 (random)+8 −7 (systematic) km s−1 Mpc−1 assuming a standard cold dark matter model with ΩM = 1.0, ΩΛ = 0.0 or H 0 = 66+11 −10 +9 −8 km s−1 Mpc−1 if ΩM = 0.3, ΩΛ = 0.7 . 相似文献
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J. M.Diego E.Martínez-González J. L.Sanz N.Benitez J.Silk 《Monthly notices of the Royal Astronomical Society》2002,331(3):556-568
We show how future measurements of the Sunyaev–Zel'dovich effect (SZE) can be used to constrain the cosmological parameters. We combine the SZ information expected from the Planck full-sky survey, N ( S ), where no redshift information is included, with the N ( z ) obtained from an optically identified SZ-selected survey covering less than 1 per cent of the sky. We demonstrate how with a small subsample (≈300 clusters) of the whole SZ catalogue observed optically it is possible to reduce the degeneracy among the cosmological parameters drastically. We have studied the requirements for performing the optical follow-up and we show the feasibility of such a project. Finally, we have compared the cluster expectations for Planck with those expected for Newton–XMM during their lifetimes. It is shown that, owing to its larger sky coverage, Planck will detect a factor of ∼5 times more clusters than Newton–XMM and also provide a larger redshift coverage. 相似文献
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Michael Rowan-Robinson 《Monthly notices of the Royal Astronomical Society》2002,332(2):352-360
The evidence for positive cosmological constant Λ from Type Ia supernovae is re-examined.
Both high redshift supernova teams are found to underestimate the effects of host galaxy extinction. The evidence for an absolute magnitude–decay time relation is much weakened if supernovae not observed before maximum light are excluded. Inclusion of such objects artificially suppresses the scatter about the mean relation.
With a consistent treatment of host galaxy extinction and elimination of supernovae not observed before maximum, the evidence for a positive lambda is not very significant (3–4 σ ) . A factor which may contribute to apparent faintness of high- z supernovae is evolution of the host galaxy extinction with z .
The Hubble diagram using all high- z distance estimates, including SZ clusters and gravitational lens time-delay estimates, does not appear inconsistent with an Ωo =1 model.
Although a positive Λ can provide an (albeit physically unmotivated) resolution of the low curvature implied by cosmic microwave background (CMB) experiments and evidence that Ωo <1 from large-scale structure, the direct evidence from Type Ia supernovae seems at present to be inconclusive. 相似文献
Both high redshift supernova teams are found to underestimate the effects of host galaxy extinction. The evidence for an absolute magnitude–decay time relation is much weakened if supernovae not observed before maximum light are excluded. Inclusion of such objects artificially suppresses the scatter about the mean relation.
With a consistent treatment of host galaxy extinction and elimination of supernovae not observed before maximum, the evidence for a positive lambda is not very significant (3–4 σ ) . A factor which may contribute to apparent faintness of high- z supernovae is evolution of the host galaxy extinction with z .
The Hubble diagram using all high- z distance estimates, including SZ clusters and gravitational lens time-delay estimates, does not appear inconsistent with an Ω
Although a positive Λ can provide an (albeit physically unmotivated) resolution of the low curvature implied by cosmic microwave background (CMB) experiments and evidence that Ω
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Phillip Helbig 《Monthly notices of the Royal Astronomical Society》1998,298(2):395-398
Recently, Park &38; Gott claimed that there is a statistically significant, strong, negative correlation between the image separation Δθ and source redshift z s for gravitational lenses. This is somewhat puzzling if one believes in a flat ( k = 0) universe, since in this case the typical image separation is expected to be independent of the source redshift, while one expects a negative correlation in a k = −1 universe and a positive one in a k = +1 universe. Park &38; Gott explored several effects that could cause the observed correlation, but no combination of these can explain the observations with a realistic scenario. Here, I explore this test further in three ways. First, I show that in an inhomogeneous universe a negative correlation is expected regardless of the value of k . Secondly, I test whether the Δθ– z s relation can be used as a test to determine λ0 and Ω0 , rather than just the sign of k . Thirdly, I compare the results of the test from the Park &38; Gott sample with those using other samples of gravitational lenses, which can illuminate (unknown) selection effects and probe the usefulness of the Δθ– z s relation as a cosmological test. 相似文献
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Asantha R. Cooray 《Monthly notices of the Royal Astronomical Society》1999,307(4):841-848
We present the observed relation between Δ T SZ , the cosmic microwave background (CMB) temperature decrement due to the Sunyaev–Zeldovich (SZ) effect, and L , the X-ray luminosity of galaxy clusters. We discuss this relation in terms of the cluster properties, and show that the slope of the observed Δ T SZ – L relation is in agreement with both the L – T e relation based on numerical simulations and X-ray emission observations, and the M gas – L relation based on observation. The slope of the Δ T SZ – L relation is also consistent with the M tot – L relation, where M tot is the cluster total mass based on gravitational lensing observations. This agreement may be taken to imply a constant gas mass fraction within galaxy clusters, however, there are large uncertainties, dominated by observational errors, associated with these relations. Using the Δ T SZ – L relation and the cluster X-ray luminosity function, we evaluate the local cluster contribution to arcmin-scale cosmic microwave background anisotropies. The Compton distortion y -parameter produced by galaxy clusters through the SZ effect is roughly two orders of magnitude lower than the current upper limit based on FIRAS observations. 相似文献