Biasing in the Galaxy Distribution

Benoist, Christophe; Maurogordato, S.; Costa, L. N. da; Cappi, A.; Schaeffer, R.

doi:10.1086/178078

Cited by 112 publications

(170 citation statements)

References 33 publications

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“…First of all we notice that r 0 ≈ 16h −1 Mpc is the highest value for the correlation length ever found in a redshift survey, after the results of LEDA [24]. The authors [55] have done several test in order to check if the dependence of r 0 on sample size is due to a luminosity effect or to a depth effect. In the first case it should be due to the so-called luminosity segregation phenomenon, while in the second case it should be attributed to the intrinsic fractal nature of galaxy distribution in this sample.…”

Section: Ssrs2mentioning

confidence: 86%

“…A clear dependence of r 0 on sample size is shown. We stress that the authors [55] fit the ξ(r) with a power law behavior in the wrong region of length scales, i.e. for r ≈ r 0 , and hence they find a higher value for the correlation exponent γ ≈ 1.5 ÷ 1.8 (Sec.2.3).…”

Section: Ssrs2mentioning

confidence: 93%

“…For historical reasons the apparent magnitude m of an object with incoming flux f is m = −2.5 log 10 f + constant, (55) while the absolute magnitude M is instead related to its intrinsic luminosity L by…”

Section: Detailed Analysis Of the Available Catalogsmentioning

confidence: 99%

“…The SSRS2 catalog is a magnitude limited survey that includes ∼ 3600 galaxies and covers Ω = 1.13 sr, complete up to limiting magnitude m B(0) = 15.5 [37,55] (this catalog is not yet published). The characteristics of the VL samples are reported in the Appendix.…”

Section: Ssrs2mentioning

confidence: 99%

“…Benoist et al [55] have measured the "correlation length" r 0 in several VL samples of different depth. We show in Tab.1 the values of r 0 and R ef f for the various VL samples of the SSRS2 survey.…”

Section: Ssrs2mentioning

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: Ssrs2mentioning

confidence: 86%

Section: Ssrs2mentioning

confidence: 93%

Section: Detailed Analysis Of the Available Catalogsmentioning

confidence: 99%

Section: Ssrs2mentioning

confidence: 99%

Section: Ssrs2mentioning

confidence: 99%

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Scale-invariance of galaxy clustering

1998

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Mark Correlations: Relating Physical Properties to Spatial Distributions

Beisbart

Kerscher

Mecke

2002

Morphology of Condensed Matter

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Abstract. Mark correlations provide a systematic approach to look at objects both distributed in space and bearing intrinsic information, for instance on physical properties. The interplay of the objects' properties (marks) with the spatial clustering is of vivid interest for many applications; are, e.g., galaxies with high luminosities more strongly clustered than dim ones? Do neighbored pores in a sandstone have similar sizes? How does the shape of impact craters on a planet depend on the geological surface properties? In this article, we give an introduction into the appropriate mathematical framework to deal with such questions, i.e. the theory of marked point processes. After having clarified the notion of segregation effects, we define universal test quantities applicable to realizations of a marked point processes. We show their power using concrete data sets in analyzing the luminosity-dependence of the galaxy clustering, the alignment of dark matter halos in gravitational N -body simulations, the morphologyand diameter-dependence of the Martian crater distribution and the size correlations of pores in sandstone. In order to understand our data in more detail, we discuss the Boolean depletion model, the random field model and the Cox random field model. The first model describes depletion effects in the distribution of Martian craters and pores in sandstone, whereas the last one accounts at least qualitatively for the observed luminosity-dependence of the galaxy clustering.

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The VIMOS VLT Deep Survey (VVDS)

Pelló

Fèvre

Adami

et al.

Highlights of Spanish Astrophysics IV

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Aims. We present a measurement of the dependence of galaxy clustering on galaxy stellar mass at redshift z ∼ 0.9, based on the first-epoch data from the VVDS-Deep survey. Methods. Concentrating on the redshift interval 0.5 < z < 1.2, we measured the projected correlation function, w p (r p ), within mass-selected subsamples covering the range ∼10 9 and ∼10 11 M . We explored and quantify in detail the observational selection biases due to the flux-limited nature of the survey, both from the data themselves and with a suite of realistic mock samples constructed by coupling the Millennium Simulation to semi-analytic models. We identify the range of masses within which our main conclusions are robust against these effects. Serious incompleteness in mass is present below log (M/M ) = 9.5, with about two thirds of the galaxies in the range 9 < log (M/M ) < 9.5 that are lost due to their low luminosity and high mass-to-light ratio. However, the sample is expected to be 100% complete in mass above log (M/M ) = 10. Results. We present the first direct evidence for a dependence of clustering on the galaxy stellar mass at a redshift as high as z ∼ 0.85. We quantify this by fitting the projected function w p (r p ) with a power-law model. The clustering length increases from r 0 = 2.76 Comparison to the SDSS measurements at z ∼ 0.15 shows that the evolution of w p (r p ) is significant for samples of galaxies with M < 10 10.5 M , while it is negligible for more massive objects. Considering the growth of structure, this implies that the linear bias b L of the most massive galaxies evolves more rapidly between these two cosmic epochs. We quantify this effect by computing the value of b L from the SDSS and VVDS clustering amplitudes and find that b L decreases from 1.5 ± 0.2 at z ∼ 0.85 to 1.33 ± 0.03 at z ∼ 0.15, for the most massive galaxies, while it remains virtually constant (b L ∼ 1.3) for the remaining population. Qualitatively, this is the kind of scenario expected for the clustering of dark-matter halos as a function of their total mass and redshift. Our result therefore seems to indicate that galaxies with the highest stellar mass today were originally central objects of the most massive dark-matter halos at earlier times, whose distribution was strongly biased with respect to the overall mass density field.

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Biasing in the Galaxy Distribution

Cited by 112 publications

References 33 publications

Scale-invariance of galaxy clustering

Scale-invariance of galaxy clustering

Mark Correlations: Relating Physical Properties to Spatial Distributions

The VIMOS VLT Deep Survey (VVDS)

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