The Hercules supercluster. I - Basic data

Tarenghi, M.; Tifft, W. G.; Chincarini, G.; Rood, Herbert J.; Thompson, Laird A.

doi:10.1086/157558

Cited by 64 publications

(40 citation statements)

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“…Perseus-Pisces (Gregory, Thompson & Tifft 1981), the Hercules supercluster (Tarenghi et al 1979, Chincarini, Rood and Thompson 1981, Gregory and Thompson 1984, the Local Supercluster (Yahil et al 1980, Tully 1982, and the early Center for Astrophysics survey work - Huchra et al 1983), the Bootes void (Kirshner, et al 1981), and the Hydra-Centaurus supercluster , most recently thoroughly mapped along with the slightly more distant region of the 'Great Attractor' by Dressler (1988 and1991). All of these efforts to map using magnitude-limited surveys of individual galaxies (and a few other, not complete samplings of some apparent supercluster regions) have identified structures of order 30 -100 h −1 Mpc or more, but they are limited to volumes only about 100 h −1 Mpc deep.…”

Section: Introductionmentioning

confidence: 99%

Discovery of Extreme Examples of Superclustering in Aquarius

Batuski¹,

Miller²,

Slinglend³

et al. 1999

ApJ

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The results of spectroscopic observations of 46 R º 1 clusters of galaxies from the Abell and Abell, Corwin, & Olowin (hereafter ACO) catalogs are presented. The observations were conducted at the ESO 3.6 m telescope with the Meudon-ESO Fibre Optics Spectrograph (MEFOS) multiple-Ðber spectrograph. Thirty-nine of the clusters lie in a 10¡ ] 45¡ strip of sky that contains two supercluster candidates (in Aquarius and Eridanus). These candidates were identiÐed by a percolation analysis of the Abell and ACO catalogs, using estimated redshifts for clusters that had not yet been measured. With our measurements and redshifts from the literature, the target strip is now 85% complete in redshift measurements for R º 1 ACO clusters with Seven other clusters were observed in a supercluster candidate m 10 ¹ 18.3. in the Grus-Indus region. Seven hundred thirty-seven galaxy redshifts were obtained in these 46 cluster Ðelds. We Ðnd that one of the supercluster candidates is a collection of 14 R º 1 ACO/Abell clusters with a spatial number density that is 20 times the average spatial density for rich ACO clusters. This overdensity has a maximum extent of D110 h~1 Mpc, making it the longest supercluster composed only of R º 1 clusters to be identiÐed to date. This Ðlament of clusters runs within 6¡ of the line of sight in the Aquarius region, and, on its high-z end, four R \ 0 ACO clusters (three of which are R \ 1 in the Abell catalog) appear to bridge gaps to other clusters, extending the structure to D150 h~1 Mpc. Our analysis also reveals that another supercluster, consisting of eight rich clusters with an extent of D75 h~1 Mpc, runs roughly perpendicular to Aquarius near its low-redshift end. Both of these superclusters are remarkably Ðlamentary. Fitting ellipsoids to all N º 5 clumps of clusters (at b \ 25 h~1 Mpc) in the measured-z Abell/ACO R º 1 clusters sample, we found two other superclusters with axis ratios º3 (long-to-midlength axis). The frequency of such Ðlaments (D20%) was nearly identical with that found among "" superclusters ÏÏ in Monte Carlo simulations of random and random-clumped cluster samples, however, so the Abell/ACO clusters have no particular tendency toward Ðlamentation. The Aquarius and Aquarius-Cetus superclusters, in this one region of the sky, have axis ratios of 4.3 and 3.0, respectively. The Aquarius Ðlament also contains a "" knot ÏÏ of six R º 1 clusters at z D 0.11, with Ðve of the clusters close enough together to represent an apparent overdensity of 150There are three other n6 . R º 1 cluster density enhancements similar to this knot at lower redshifts : Corona Borealis, the Shapley concentration, and another grouping of seven clusters in Microscopium. All four of these dense superclusters appear near the point of breaking away from the Hubble Ñow, and some may now be in collapse, but there is little indication of any being virialized. With four such objects, studies of them as a class may now lead to much greater insight into large-scale processes.

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Section: Introductionmentioning

confidence: 99%

Discovery of Extreme Examples of Superclustering in Aquarius

Batuski¹,

Miller²,

Slinglend³

et al. 1999

ApJ

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“…Rapid developments in the mapping of various filaments and voids include the studies of Tarenghi et al (1979), Gregory et al (1981), Kirshner et al (1981), Gregory and Thompson (1982), Chincarini et al (1983), andHuchra et al (1983). A general review is given by Oort (1983).…”

Section: Large Scale Structurementioning

confidence: 99%

Observational Cosmology 1920–1985: An Introduction to the Conference

Sandage¹

1987

Symp. - Int. Astron. Union

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ABSTRACT. The history of modern cosmology has been divided into two periods, The primary discovery phase extended from 1920 to ^1950 when most of the classical tests were developed. The subsequent consolidation period from 1950 to ^1980 saw a deeper understanding of the tests and the introduction of concepts of stellar populations that led to estimates of evolutionary trends with look-back time. The only test not affecte^ by evolutionary effects is the comparison of the Hubble time, Η , with independent estimates of the age of the Universe. The N(m), m(z), θ(ζ), θ(m), and HT (q ,Λ) tests are reviewed as they have been discussed in the archive literature. The problem of observational bias is emphasized, as is the difficult recent search for secular evolutionary effects. Current problems which have prospects for solutions in the next decades are set out in the final section. PREVIEWCosmology is now a dominant field of modern astronomy, carrying a principal theme in its own right, but also being the background motivation for much of the present work in even traditional astronomical fields from astrometry, to stellar atmospheres and interiors, to galactic structure, and the interstellar medium. The present cosmological thrust is to devise methods for calibrating various cosmological parameters such as Η , the time scale, the 3°K flux, etc., but ultimately to reach back to tße origins of everything from stars, to galaxies, to the Universe itself; the borders of cosmology and cosmogony here being blurred.The connection of cosmology to nearly all other parts of astronomy, and the fact that a good fraction of the young astronomers now take cosmology to be their subject, has not always been. As late as 1938, the last year before the war, there were probably less than 30 cosmologists in the world, and of these perhaps only ^15 had the status of builders of the foundations. Today there are ^1000 cosmologists, of which V30% are at this conference. This rapid growth corresponds to a doubling time of ^10 years, or a 7% growth per year. At this rate, in 1AU.

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“…Early 3D maps show pronounced filaments and voids extending over 50 and more Mpc (Tarenghi et al 1979;Chincarini et al 1983;Huchra et al 1983;de Lapparent et al 1986). Still larger structures based on the SDSS have been reported; in particular, the Sloan Great Wall 420 Mpc long (Gott et al 2005), and the largest filamentary structure extending above 1 Gpc found in the DR7QSO catalogue (Clowes et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Topology of large-scale underdense regions

Sołtan

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the large scale matter distribution adopting QSOs as matter tracer. The quasar catalogue based on the SDSS DR7 is used. The void finding algorithm is presented and statistical properties of void sizes and shapes are determined. Number of large voids in the quasar distribution is greater than the number of the same size voids found in the random distribution. The largest voids with diameters exceeding 300 Mpc indicate an existence of comparable size areas of lower than the average matter density. No void-void space correlations have been detected, and no larger scale deviations from the uniform distribution are revealed. The average CMB temperature in the directions of the largest voids is lower than in the surrounding areas by 0.0046 ± 0.0028 mK. This figure is compared to the amplitude of the expected temperature depletion caused by the Integrated Sachs-Wolfe effect.

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The Hercules supercluster. I - Basic data

Cited by 64 publications

References 0 publications

Discovery of Extreme Examples of Superclustering in Aquarius

Discovery of Extreme Examples of Superclustering in Aquarius

Observational Cosmology 1920–1985: An Introduction to the Conference

Topology of large-scale underdense regions

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