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Redshift Space (redshift + space)
Selected AbstractsThe properties of the heterogeneous Shakhbazyan groups of galaxies in the SDSSMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 2 2009D. Capozzi ABSTRACT We present a systematic study of the subsample of Shakhbazyan (SHK) groups covered by the Sloan Digital Sky Survey Data Release 5 (SDSS DR5). SHK groups probe an environment with characteristics which are intermediate between those of loose and very compact groups. Surprisingly, we found that several groups identifying algorithms, e.g. Berlind et al. and Tago et al., miss this type of structures. Using the SDSS DR5 spectroscopic data and the photometric redshifts derived in D'Abrusco et al., we identified possible group members in photometric redshift space and derived, for each group, several individual properties (richness, size, mean photometric redshift, fraction of red galaxies, etc.). We also combined pointed and stacked Rosat All Sky Survey (RASS) data to investigate the X-ray luminosities of these systems. Our study confirms that the majority of groups are physical entities with richness in the range 3,13 galaxies, and properties ranging between those of loose and compact groups. We confirm that SHK groups are richer in early-type galaxies than the surrounding environment and the field, as expected from the morphology,density relation and from the selection of groups of red galaxies. Furthermore, our work supports the existence of two subclasses of structures, the first one being formed by compact and isolated groups and the second formed by extended structures. We suggest that while the first class of objects dwells in less dense regions like the outer parts of clusters or the field, possibly sharing the properties of Hickson Compact Groups, the more extended structures represent a mixture of [core + halo] configurations and cores of rich clusters. X-ray luminosities for SHK groups are generally consistent with these results and with the expectations for the LX,,v relation, but also suggest the velocity dispersions reported in literature are underestimated for some of the richest systems. [source] Clustering of luminous red galaxies , II.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 2 2009Small-scale redshift-space distortions ABSTRACT This is the second paper of a series where we study the clustering of luminous red galaxies (LRG) in the recent spectroscopic Sloan Digital Sky Survey (SDSS) data release, DR6, which has 75 000 LRG covering over 1 Gpc3 h,3 for 0.15 < z < 0.47. Here, we focus on modelling redshift-space distortions in ,(,, ,), the two-point correlation in separate line-of-sight and perpendicular directions, at small scales and in the line-of-sight. We show that a simple Kaiser model for the anisotropic two-point correlation function in redshift space, convolved with a distribution of random peculiar velocities with an exponential form, can describe well the correlation of LRG on all scales. We show that to describe with accuracy the so-called ,fingers-of-God' (FOG) elongations in the radial direction, it is necessary to model the scale dependence of both bias b and the pairwise rms peculiar velocity ,12 with the distance. We show how both quantities can be inferred from the ,(,, ,) data. From r, 10 Mpc h,1 to r, 1 Mpc h,1, both the bias and ,12 are shown to increase by a factor of 2: from b= 2 to 4 and from ,12= 400 to 800 km s,1. The latter is in good agreement, within a 5 per cent accuracy in the recovered velocities, with direct velocity measurements in dark matter simulations with ,m= 0.25 and ,8= 0.85. [source] Cluster correlations in redshift spaceMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 2 2002N.D. Padilla We test an analytic model for the two-point correlations of galaxy clusters in redshift space using the Hubble volume N -body simulations. The correlation function of clusters shows no enhancement along the line of sight, owing to the lack of any virialized structures in the cluster distribution. However, the distortion of the clustering pattern arising from coherent bulk motions is clearly visible. The distribution of cluster peculiar motions is well described by a Gaussian, except in the extreme high-velocity tails. The simulations produce a small but significant number of clusters with large peculiar motions. The form of the redshift-space power spectrum is strongly influenced by errors in measured cluster redshifts in extant surveys. When these errors are taken into account, the model reproduces the power spectrum recovered from the simulation to an accuracy of 15 per cent or better over a decade in wavenumber. We compare our analytic predictions with the power spectrum measured from the APM cluster redshift survey. The cluster power spectrum constrains the amplitude of density fluctuations, as measured by the linear rms variance in spheres of radius 8 h,1 Mpc, denoted by ,8. When combined with the constraints on ,8 and the density parameter , derived from the local abundance of clusters, we find a best-fitting cold dark matter model with and , for a power spectrum shape that matches that measured for galaxies. However, for the best-fitting value of , and given the value of Hubble's constant from recent measurements, the assumed shape of the power spectrum is incompatible with the most readily motivated predictions from the cold dark matter paradigm. [source] Non-linear redshift distortions: the two-point correlation functionMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 2 2001Somnath Bharadwaj We consider a situation where the density and peculiar velocities in real space are linear, and we calculate ,s, the two-point correlation function in redshift space, incorporating all non-linear effects which arise as a consequence of the map from real to redshift space. Our result is non-perturbative and it includes the effects of possible multi-streaming in redshift space. We find that the deviations from the predictions of the linear redshift distortion analysis increase for the higher spherical harmonics of ,s. While the deviations are insignificant for the monopole ,0, the hexadecapole ,4 exhibits large deviations from the linear predictions. For a COBE normalized , cold dark matter (CDM) power spectrum, our results for ,4 deviate from the linear predictions by a factor of two on the scale of ,10 h,1 Mpc. The deviations from the linear predictions depend separately on f(,) and b. This holds the possibility of removing the degeneracy that exists between these two parameters in the linear analysis of redshift surveys which yields only . We also show that the commonly used phenomenological model, where the non-linear redshift two-point correlation function is calculated by convolving the linear redshift correlation function with an isotropic pair velocity distribution function, is a limiting case of our result. [source] Comparison of the ENEAR peculiar velocities with the PSCz gravity fieldMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 3 2001Adi Nusser We present a comparison between the peculiar velocity field measured from the ENEAR all-sky Dn,, catalogue and that derived from the galaxy distribution of the IRAS Point Source Catalog Redshift Survey (PSCz). The analysis is based on a modal expansion of these data in redshift space by means of spherical harmonics and Bessel functions. The effective smoothing scale of the expansion is almost linear with redshift reaching 1500 km s,1 at 3000 km s,1. The general flow patterns in the filtered ENEAR and PSCz velocity fields agree well within 6000 km s,1, assuming a linear biasing relation between the mass and the PSCz galaxies. The comparison allows us to determine the parameter where , is the cosmological density parameter and b is the linear biasing factor. A likelihood analysis of the ENEAR and PSCz modes yields in good agreement with values obtained from Tully,Fisher surveys. [source] The luminosity dependence of clustering and higher order correlations in the PSCz surveyMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 4 2000István Szapudi We investigate the spatial clustering of galaxies in the PSCz galaxy redshift survey, as revealed by the two-point correlation function, the luminosity mark correlations and the moments of counts-in-cells. We construct volume-limited subsamples at different depths and search for a luminosity dependence of the clustering pattern. We find no statistically significant effect in either the two-point correlation function or the mark correlations and so we take each subsample (of different characteristic luminosity) as representing the same statistical process. We then carry out a counts-in-cells analysis of the volume-limited subsamples, including a rigorous error calculation based on the recent theory of Szapudi, Colombi & Bernardeau. In this way, we derive the best estimates to date of the skewness and kurtosis of IRAS galaxies in redshift space. Our results agree well with previous measurements in both the parent angular catalogue and the derived redshift surveys. This is in contrast with smaller, optically selected surveys, where there is a discrepancy between the redshift space and projected measurements. Predictions from cold dark matter theory, obtained using the recent semi-analytical model of galaxy formation of Benson et al., provide an excellent description of our clustering data. [source] Protoclusters associated with distant radio galaxiesASTRONOMISCHE NACHRICHTEN, Issue 2-3 2006B. P. Venemans Abstract The results of a large program conducted with the Very Large Telescope and the Keck telescope to search for forming clusters of galaxies near powerful radio galaxies at 2 < z < 5.2 are presented. Deep narrow- and broad-band images of eight radio galaxies and their surroundings were obtained. In the images a total of 335 candidate Ly, emitting galaxies at the redshift of the radio galaxies were selected. Subsequently, follow-up spectroscopy was performed to obtain redshifts for the candidate Ly, emitters. In at least six of eight fields (75%) an overdensity of Ly, emitters is found near the radio galaxy. Taken together with a significant clustering in redshift space of the emitters, we argue that we have discovered six forming clusters of galaxies (protoclusters). Based on the estimated masses and the volume density, we conclude that the observed structures are the likely progenitors of present-day massive (,1015 M,) clusters of galaxies. Finally, we compare the observed galaxy overdensities with numerical simulations of the development of large scale structure in the Universe. The preliminary results of this comparison provide strong additional evidence for the hypothesis that the radio galaxy protoclusters are forming massive clusters. (© 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source] | ||||||||||