The size and shape of local voids

Plionis, M.; Basilakos, Spyros

doi:10.1046/j.1365-8711.2002.05069.x

Cited by 84 publications

(92 citation statements)

References 43 publications

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“…Studies of the distribution of sizes of voids in the observed galaxy distribution have been performed (see, for example, Plionis & Basilakos 2002;Muller et al 2000;Muller & Maulbetsch 2004). An analysis of void properties with respect to CDM models and the effects of galaxy/dark matter biasing has been carried out by several authors (e.g., Mathis & White 2002;Benson et al 2003;Tikhonov & Klypin 2009;Tinker & Conroy 2009).…”

Section: Introductionmentioning

confidence: 99%

The Size, Shape, and Orientation of Cosmological Voids in the Sloan Digital Sky Survey

Foster¹,

Nelson²

2009

ApJ

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We present a detailed description of our void finding algorithm which is an extension of the prescription by Hoyle and Vogeley. We include a discussion of the reproducibility and robustness of the algorithm as well as the statistical significance of the detected voids. We apply our void finder to the Data Release 5 of the Sloan Digital Sky Survey and identify 232 cosmological voids. A void catalog which contains the most salient properties of the detected voids is created. We present a statistical analysis of the distribution of the size, shape, and orientation of our identified cosmological voids. We also investigate possible trends with redshift for 0.04 z 0.16. We compare our results to those from an identical analysis of a mock catalog based on the ΛCDM model and find reasonable agreement. However, some statistically significant differences in the overall orientation of cosmological voids are exhibited and will have to be reconciled by further refinement of the simulations.

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Section: Introductionmentioning

confidence: 99%

The Size, Shape, and Orientation of Cosmological Voids in the Sloan Digital Sky Survey

Foster¹,

Nelson²

2009

ApJ

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“…Voids in the galaxy distribution account for about 95% of the total volume (see Kauffmann & Fairall, 1991;El-Ad, Piran & da Costa, 1996;El-Ad & Piran, 1997;Plionis & Basilakos, 2002;Rojas et al, 2005). The typical sizes of voids in the galaxy distribution depend on the galaxy population used to define the voids.…”

Section: Cosmic Depressions: the Voidsmentioning

confidence: 99%

“…Voids defined by galaxies brighter than a typical L * galaxy tend to have diameters of order 10 − 20h −1 Mpc, but voids associated with rare luminous galaxies can be considerably larger; diameters in the range of 20h −1 − 50h −1 Mpc are not uncommon (e.g. Plionis & Basilakos, 2002). These large sizes mean that only now we are beginning to probe a sufficiently large cosmological volume to allow meaningful statistics with voids to be done.…”

Section: Cosmic Depressions: the Voidsmentioning

confidence: 99%

“…Such methods attempt to synthesize voids from the intersection of cubic or spherical elements and do so with varying degrees of success. Because of the vague and different definitions, and the range of different interests in voids, there is a plethora of void identification procedures (Kauffmann & Fairall, 1991;El-Ad & Piran, 1997;Aikio & Mähönen, 1998;Arbabi-Bidgoli & Müller, 2002;Plionis & Basilakos, 2002;Patiri et al, 2006;Colberg et al, 2005b;Shandarin et al, 2006). The "voidfinder" algorithm of El-Ad & Piran (1997) has been at the basis of most voidfinding methods.…”

Section: Void Findingmentioning

confidence: 99%

“…The boundary and identity of voids is therefore mostly a matter of definition. As a consequence there is a variety of voidfinding algorithms (Kauffmann & Fairall, 1991;El-Ad, Piran & da Costa, 1996;Plionis & Basilakos, 2002;Shandarin et al, 2006;Colberg et al, 2005b;Patiri et al, 2006). A recent study (Colberg, Pearce et al, 2007) contains a balanced comparison of the performance of the various void finders with respect to a small region taken from the Millennium simulation Springel et al (2005) …”

Section: The Watershed Void Findermentioning

confidence: 99%

See 2 more Smart Citations

Data Analysis in Cosmology

Martı́nez¹,

Saar²,

Gonzales³

et al. 2009

Lecture Notes in Physics

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The Quest for the Cosmological Parameters

Plionis

2002

Cosmological Crossroads

Self Cite

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Abstract. The following review is based on lectures given in the 1 st Samos Cosmology summer school. It presents an attempt to discuss various issues of current interest in Observational Cosmology, the selection of which as well as the emphasis given, reflects my own preference and biases. After presenting some Cosmological basics, for which I was aided by excellent text-books, I emphasize on attempts to determine some of the important cosmological parameters; the Hubble constant, the curvature and total mass content of the Universe. The outcome of these very recent studies is that the concordance model, that fits the majority of observations, is that with04 and spectral index of primordial fluctuations, the inflationary value n ≃ 1. I apologise before hand for the many important works that I have omitted and for the possible misunderstanding of those presented. Background-PrerequisitesThe main task of Observational Cosmology is to identify which of the idealized models, that theoretical Cosmologists construct, relates to the Universe we live in. One may think that since we cannot perform experiments and study, in a laboratory sense, the Universe as a whole, this is a futile task. Nature however has been graceful, and through the detailed and exhaustive analysis of the detected electromagnetic radiation emitted from the different photon-generating processes, we can do wonders! Among the many important tasks of Observational Cosmology is the determination of the total mass-energy density of the Universe, the rate of its expansion, its age, the amount of ordinary and exotic matter that it contains, as well as to quantify in a objective and bias free manner the large-scale distribution of matter, as traced by galaxies, clusters of galaxies and AGN's for example.However, these tasks are not easy to fulfil. Subjective (instrumentation, available funds, technological limitations etc) as well as objective (observational biases, limitations due to our position in space-time, etc) difficulties exist. Furthermore, we do not know whether the Universe accessible to our observations is representative of the whole Universe. A positive answer to this question is essential in order to meaningfully compare observations with theory. Under the assumption that the Universe is homogeneous and isotropic (in a statistical sense), well separated regions can be viewed as independent realizations of the same formation process. Therefore many of such regions constitute an ensemble and thus we can employ statistical techniques in our study.

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The size and shape of local voids

Cited by 84 publications

References 43 publications

The Size, Shape, and Orientation of Cosmological Voids in the Sloan Digital Sky Survey

The Size, Shape, and Orientation of Cosmological Voids in the Sloan Digital Sky Survey

Data Analysis in Cosmology

The Quest for the Cosmological Parameters

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