Voids in the distribution of galaxies: an assessment of their significance and derivation of a void spectrum

Kauffmann, Guinevere; Fairall, A. P.

doi:10.1093/mnras/248.2.313

Cited by 92 publications

(98 citation statements)

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“…This distance corresponds to ∼80% of the radius of the smallest voids identified by Kauffmann & Fairall (1991). Note, that almost all BCGs are low-mass galaxies and are substantially fainter than L * .…”

Section: Sample Descriptionmentioning

confidence: 79%

Studies of galaxies in voids

Pustilnik¹,

Martin²,

Huchtmeier³

et al. 2002

A&A

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Abstract. We present here results of studies of the properties of galaxies located in very low density environments. We observed 26 blue compact galaxies (BCGs) from the Second Byurakan (SBS) and Case surveys located in voids with the radial velocities V hel . 11 000 km s −1 , two BCGs in the void behind the Virgo cluster and 11 BCGs in denser environments. H i fluxes and profile widths, as well as estimates of total H i masses, are presented for the 27 detected galaxies (of which 6 are in three galaxy pairs and are not resolved by the radiotelescope beam). Preliminary comparisons of void BCGs with similar objects from intermediate density regions -in the general field and the Local Supercluster (sub-samples of BCGs in the SBS zone) and in the dense environment of the Virgo Cluster (a BCD sample) -are performed using the hydrogen-to-blue-luminosity ratio M (H i)/LB. We find that for the same blue luminosity, for MB > −18. m 0, BCGs in lower density environment have on average more H i. The slope β of the M (H i)/LB _ L β for BCGs shows a trend of steepening with decreasing bright galaxy density, being very close to zero for the densest environment considered here and reaching β = −0.4 for voids.

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Section: Sample Descriptionmentioning

confidence: 79%

Studies of galaxies in voids

Pustilnik¹,

Martin²,

Huchtmeier³

et al. 2002

A&A

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“…Several authors [22,73,76,72] have investigated the shape and the dimension of voids determined by rich clusters and superclusters. The dimension of a void can be defined as diameter of empty sphere containing no clusters.…”

Section: Analysis Of Clusters Catalogsmentioning

confidence: 99%

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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“…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%

“…Moreover, void finders are often predicated on building void structures out of cubic cells (Kauffmann & Fairall, 1991) or out of spheres (e.g. Patiri et al, 2006).…”

Section: Void Findingmentioning

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%

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