Mock 2dF and SDSS galaxy redshift surveys

Cole, Shaun; Hatton, Steve; Weinberg, David H.; Frenk, Carlos S.

doi:10.1046/j.1365-8711.1998.t01-1-01936.x

Cited by 132 publications

(187 citation statements)

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“…To characterize the uncertainty in the angle v, we have used "mock" 2dF and SDSS galaxy redshift surveys constructed from a set of large, high-resolution cosmological N-body simulations (Cole et al 1998). These simulations do not resolve detail on the scale of a galaxy, so we have assumed for this test that all the galaxies were edge-on with the position angle of the rotation axis uniformly distributed in the sky plane.…”

Section: Void-based Methods and Sample Selectionmentioning

confidence: 99%

Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

Trujillo¹,

Carretero²,

Patiri³

2006

ApJ

118

152

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Galaxies are not distributed randomly throughout space but are instead arranged in an intricate "cosmic web" of filaments and walls surrounding bubble-like voids. There is still no compelling observational evidence of a link between the structure of the cosmic web and how galaxies form within it. However, such a connection is expected on the basis of our understanding of the origin of galaxy angular momentum: disk galaxies should be highly inclined relative to the plane defined by the large-scale structure surrounding them. Using the two largest galaxy redshift surveys currently in existence (2dFGRS and SDSS), we show at the 99.7% confidence level that these alignments do indeed exist: spiral galaxies located on the shells of the largest cosmic voids have rotation axes that lie preferentially on the void surface.

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Section: Void-based Methods and Sample Selectionmentioning

confidence: 99%

Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

Trujillo¹,

Carretero²,

Patiri³

2006

ApJ

118

152

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“…Similarly, the luminosity functions of the mock catalogs and the data must be similar. Simple bias schemes that produce a population of galaxies above some luminosity cut (e.g., Cole et al 1998) will not produce the information we need to find clusters. Mock catalogs created from more detailed semianalytic models of galaxy formation (e.g., Kauffmann et al 1999;Eke et al 2004) do produce colors and luminosities; unfortunately, at this stage none of these models are yet producing galaxies with properties that reproduce those seen in the SDSS data closely enough.…”

Section: A Mock Sdss Galaxy Catalogmentioning

confidence: 99%

The C4 Clustering Algorithm: Clusters of Galaxies in the Sloan Digital Sky Survey

et al. 2005

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We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers $2600 deg 2 of sky and ranges in redshift from z ¼ 0:02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r ¼ 17:7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L r ), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the ÃCDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog. These mock catalogs indicate that the C4 catalog is '90% complete and 95% pure above M 200 ¼ 1 ; 10 14 h À1 M and within 0:03 z 0:12. Using the SDSS DR2 data, we show that the C4 algorithm finds 98% of X-ray-identified clusters and 90% of Abell clusters within 0:03 z 0:12. Using the mock galaxy catalogs and the full HV dark matter simulations, we show that the L r of a cluster is a more robust estimator of the halo mass (M 200 ) than the galaxy line-of-sight velocity dispersion or the richness of the cluster. However, if we exclude clusters embedded in complex large-scale environments, we find that the velocity dispersion of the remaining clusters is as good an estimator of M 200 as L r . The final C4 catalog will contain '2500 clusters using the full SDSS data set and will represent one of the largest and most homogeneous samples of local clusters.

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“…Such mock surveys allow a rigorous assessment of statistical and systematic errors, aid in the design of new statistical analyses and enable the survey results to be directly related to cosmological theory. Mock catalogues based on cosmological simulations were first used in the 1980s, in connection with the CfA galaxy survey (Davis et al 1985; White, Tully & Davis 1988) and redshift surveys of IRAS galaxies (Saunders et al 1991), and have been extensively deployed for analyses of the 2dFGRS and the SDSS (Cole et al 1998; Blaizot et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Mock galaxy redshift catalogues from simulations: implications for Pan-STARRS1

Cai¹,

Angulo²,

Baugh³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We describe a method for constructing mock galaxy catalogues which are well suited for use in conjunction with large photometric surveys. We use the semi‐analytic galaxy formation model of Bower et al. implemented in the Millennium N‐body simulation of the evolution of dark matter clustering in a Λ cold dark matter cosmology. We apply our method to the specific case of the surveys soon to commence with PS1, the first of four telescopes planned for the Pan‐STARRS. PS1 has five photometric bands, g, r, i, z and y and will carry out an all‐sky ‘3π’ survey and a medium deep survey (MDS) over 84 deg2. We calculate the expected magnitude limits for extended sources in the two surveys. We find that, after 3 year, the 3π survey will have detected over 108 galaxies in all five bands, 10 million of which will lie at redshift z > 0.9, while the MDS will have detected over 107 galaxies with 0.5 million lying at z > 2. These numbers at least double if the detection in the shallowest band, y, is not required. We then evaluate the accuracy of photometric redshifts estimated using an off‐the‐shelf photo‐z code. With the grizy bands alone, it is possible to achieve an accuracy in the 3π survey of Δz/(1 +z) ∼ 0.06 in the range 0.25 < z < 0.8, which could be reduced by about 15 per cent using near‐infrared photometry from the Infrared Deep Sky Survey (UKIDDS) survey, but would increase by about 25 per cent for the deeper sample without the y‐band photometry. For the MDS, an accuracy of Δz/(1 +z) ∼ 0.05 is achievable for 0.02 < z < 1.5 using grizy. A dramatic improvement in accuracy is possible by selecting only red galaxies. In this case, Δz/(1 +z) ∼ 0.02–0.04 is achievable for ∼100 million galaxies at 0.4 < z < 1.1 in the 3π survey and for 30 million galaxies in the MDS at 0.4 < z < 2. We investigate the effect of using photometric redshifts in the estimate of the baryonic acoustic oscillation scale. We find that PS1 will achieve a similar accuracy in this estimate as a spectroscopic survey of 20 million galaxies.

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Mock 2dF and SDSS galaxy redshift surveys

Cited by 132 publications

References 0 publications

Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

The C4 Clustering Algorithm: Clusters of Galaxies in the Sloan Digital Sky Survey

Mock galaxy redshift catalogues from simulations: implications for Pan-STARRS1

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