A survey of galaxy redshifts. IV - The data

Huchra, J.; Davis, M.; Latham, David W.; Tonry, J.

doi:10.1086/190860

Cited by 472 publications

(351 citation statements)

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“…At first these irregular structures appeared to be in contradiction with the picture derived from the angular catalogs and, as we discuss in what follows, they really are. However, in 1983, a correlation analysis of the 3-d distribution CfA1 catalog [17] was performed by Davis & Peebles [18] and the result was again that the correlation length was r 0 = 5h −1 Mpc as for the angular catalogs. This seemed to resolve the puzzle, because it was interpreted as if a relatively small correlation length can be consistent with the observation of large structures.…”

Section: Statistical Methods and Correlation Propertiesmentioning

confidence: 99%

“…Several recent galaxy redshift surveys such as CfA1 [17], CfA2 [36][37][38], SSRS1 [39], SSRS2 [37], Perseus Pisces [40], LCRS [41], IRAS [42], pencil beams surveys [43] and ESP [44,45], have uncovered remarkable structures such as filaments, sheets, superclusters and voids ( Fig.1 and Fig.3). These galaxy catalogs probe scales from ∼ 100 ÷ 200h −1 Mpc for the wide angle surveys, up to ∼ 1000h −1 Mpc for the deeper pencil beam surveys, and show that the Large-Scale Structures (LSS) are the characteristic features of the visible matter distribution.…”

Section: Why a Small Correlation Length Is Not Compatible With Large mentioning

confidence: 99%

“…The CfA1 catalog has been the first wide angle redshift survey (Ω = 1.83 sr) available in the literature [17]. Coleman, Pietronero and Sanders in 1988 [21] have analyzed this catalog with the methods of modern statistical mechanics.…”

Section: Cfa1mentioning

confidence: 99%

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Scale-invariance of galaxy clustering

1998

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Some years ago we proposed a new approach to the analysis of galaxy and cluster correlations based on the concepts and methods of modern statistical Physics. This led to the surprising result that galaxy correlations are fractal and not homogeneous up to the limits of the available catalogs. The usual statistical methods, which are based on the assumption of homogeneity, are therefore inconsistent for all the length scales probed so far, and a new, more general, conceptual framework is necessary to identifythe real physical properties of these structures. In the last few years the 3-d catalogs have been significatively improved and we have extended our methods to the analysis of number counts and angular catalogs. This has led to a complete analysis of all the available data that we present in this review. The result is that galaxy structures are highly irregular and self-similar: all the available data are consistent with each other and show fractal correlations (with dimension $D \simeq 2$) up to the deepest scales probed so far ($1000 \hmp$) and even more as indicated from the new interpretation of the number counts. The evidence for scale-invariance of galaxy clustering is very strong up to $150 \hmp$ due to the statistical robustness of the data but becomes progressively weaker (statistically) at larger distances due to the limited data. In These facts lead to fascinating conceptual implications about our knowledge of the universe and to a new scenario for the theoretical challenge in this field.Comment: Latex file 165 pages, 106 postscript figures. This paper is also available at http://www.phys.uniroma1.it/DOCS/PIL/pil.html To appear in Physics Report (Dec. 1997

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Section: Statistical Methods and Correlation Propertiesmentioning

confidence: 99%

Section: Why a Small Correlation Length Is Not Compatible With Large mentioning

confidence: 99%

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Scale-invariance of galaxy clustering

1998

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“…Although differing in details, many of these investigations have adopted the so-called friends-of-friends (FoF) method, which identifies galaxy systems as member galaxies that are linked by some adopted linkage criteria. For example, Postman & Geller (1984) identified galaxy groups from the CfA redshift survey (Huchra et al 1983) by applying the FoF algorithm, developed by Huchra & Geller (1982), which uses two linking criteria, one on projected separation and the other on redshift difference, to link galaxies. With modifications, the FoF algorithm has been applied to various redshifts surveys of galaxies, including the Two Degree Field Galaxy Redshift Survey (2dFGRS; e.g.…”

Section: Introductionmentioning

confidence: 99%

Galaxy groups in the low-redshift Universe

Lim

et al. 2017

Monthly Notices of the Royal Astronomical Society

133

179

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We apply a halo-based group finder to four large redshift surveys, the 2MRS, 6dFGS, SDSS and 2dFGRS, to construct group catalogs in the low-redshift Universe. The group finder is based on that of Yang et al. but with an improved halo mass assignment so that it can be applied uniformly to various redshift surveys of galaxies. Halo masses are assigned to groups according to proxies based on the stellar mass/luminosity of member galaxies. The performances of the group finder in grouping galaxies according to common halos and in halo mass assignments are tested using realistic mock samples constructed from hydrodynamical simulations and empirical models of galaxy occupation in dark matter halos. Our group finder finds ∼ 94% of the correct true member galaxies for 90 − 95% of the groups in the mock samples; the halo masses assigned by the group finder are un-biased with respect to the true halo masses, and have a typical uncertainty of ∼ 0.2 dex. The properties of group catalogs constructed from the observational samples are described and compared with other similar catalogs in the literature.

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“…where φ i is the type-dependent galaxy luminosity function at z = 0, for which we adopted the Schechter parameters derived by Efstathiou, Ellis, & Peterson (1988) using the catalog of the Center for Astrophysics (CfA) Redshift Survey (Huchra et al 1983). We have to determine the overall normalization of extinction, κ, for which we use the average V extinction of the Milky Way (Sbc type, L B = 1.4 × 10 10 L B⊙ ) at z = 0: A V MW .…”

Section: Average Extinction Evolution Towards High Redshiftsmentioning

confidence: 99%

Dust versus Supernova Cosmology

Totani

2001

Sources and Detection of Dark Matter and Dark Energy in the Universe

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Abstract. Here we present some critical discussions about the systematic uncertainty by dust extinction in the recent cosmological results of high-redshift Type Ia supernovae. First we argue that the currently available data do not robustly exclude the cosmologically significant extinction either by the reddening check or the dispersion argument because of the observational uncertainties, even in the case of ordinary dust that reddens. Then we discuss two theoretical possibilities that high-z supernovae have larger extinction and hence they are fainter than local supernovae: the intergalactic dust and host galaxy evolution. Optical and near-infrared observations for a large number of supernovae with improved photometric accuracy are required to reject these possibilities and derive a compelling cosmological result.

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A survey of galaxy redshifts. IV - The data

Cited by 472 publications

References 0 publications

Scale-invariance of galaxy clustering

Scale-invariance of galaxy clustering

Galaxy groups in the low-redshift Universe

Dust versus Supernova Cosmology

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