A study of the large voids in the spatial distribution of
 galaxy clusters in the Northern Galactic Hemisphere

Stavrev, K. Y.

doi:10.1051/aas:2000212

Cited by 5 publications

(5 citation statements)

References 55 publications

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“…The size of the void in the Ly forest we detect at 0:0320 < z < 0:0814 (Áv ¼ 14;000 km s À1 , 206 h À1 comoving Mpc) for strong absorbers is on the order of twice the mean size of large voids as traced by R ! 1 Abell/ACO galaxy clusters (Stavrev 2000) and of the same order in the case of voids in our weak absorber survey. Voids in the Ly forest are rare, and the most widely known comparable examples with similar H i column density limits to the ones in our sample are at high redshift.…”

Section: Clustering and Voidssupporting

confidence: 67%

The Low‐Redshift Lyα Forest toward PKS 0405−123

Williger

Heap

Weymann³

et al. 2006

ApJ

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We present results for Ly forest and metal absorbers from $7 km s À1 resolution Space Telescope Imaging Spectrograph data for QSO PKS 0405À123 (z ¼ 0:574). We analyze strong and weak samples of Ly forest lines, containing 60 absorbers with column density log N H i ! 13:3 over 0:002 < z < 0:423 and 44 with log N H i ! 13:1 over 0:020 < z < 0:234, respectively. Seven absorbers contain metals, all with associated O vi and often offset in velocity from Ly. The strong and weak Doppler parameter distributions have hbi ¼ 47 AE 22 and 44 AE 21 km s À1 , respectively. Simulated spectra suggest that line blending and signal-to-noise ratio effects inflate b. For absorbers with 13:1 < log N H i < 14:0, we find a redshift overdensity of $0.2-0.3 dex at 0:127 < z < 0:234, which we attribute to cosmic variance. There is a void in the strong sample at 0:0320 < z < 0:0814 with probability of random occurrence P < 0:0004. We detect Ly-Ly clustering in our sample on a scale of Áv 250 km s À1 for log N H i ! 13:3, consistent with a numerical model of structure evolution. We detect velocity correlations of up to 250 km s À1 between Ly absorbers and 39 galaxies at z < 0:43 out to a transverse distance of 1.6 h À1 70 local frame Mpc. The Ly-galaxy two-point correlation function is significant out to Áv < 250 km s À1 and grows with minimum H i column density. The strongest signal occurs for log N H i k13:5 14:0 absorbers and is similar to the galaxy-galaxy correlation, implying that such Ly absorbers have masses log (M /M ) ¼ 11:3 þ1:0 À0:6 . We find a correlation between local galaxy counts and local summed H i column density, with peak significance on scales of 4000-6000 km s À1 and probability of random occurrence P ¼ 0:0009. Finally, we present column densities for a number of Galactic species.

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Section: Clustering and Voidssupporting

confidence: 67%

The Low‐Redshift Lyα Forest toward PKS 0405−123

Williger

Heap

Weymann³

et al. 2006

ApJ

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“…Only relatively small and moderate size voids are almost completely devoid of galaxies (van de Weygaert 2016). Linear sizes of the present voids exceed 300 Mpc, and are comparable to the largest voids detected in the galaxy distribution (Stavrev 2000). Such large volumes are called voids because of distinctly lower than average number of galaxies.…”

Section: Introductionsupporting

confidence: 56%

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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“…In order to study in an objective manner the distribution of voids and their physical properties it is necessary to develop objective void-finding algorithms and to apply them onto well controlled data. Such attempts were pioneered by Kauffmann & Fairall (1991), Kauffmann & Melott (1992) and more recently by El-Ad, Piran & da Costa (1996 and Stavrev (2000). El-Ad, Piran & da Costa (1997) applied their void-finding algorithm to the IRAS 1.2Jy galaxy catalogue and found, within 80 h −1 Mpc, 15 voids with an average diameter of 40 ± 6h −1 Mpc.…”

Section: Introductionmentioning

confidence: 99%

The size and shape of local voids

Plionis

Basilakos

2002

Monthly Notices of the Royal Astronomical Society

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We study the size and shape of low‐density regions in the local Universe, which we identify in the smoothed density field of the PSCz flux‐limited IRAS galaxy catalogue. After quantifying the systematic biases that enter the detection of voids using our data set and method, we identify, using a smoothing length of 5 h−1 Mpc, 14 voids within 80 h−1 Mpc (having volumes 103 h−3 Mpc3) and, using a smoothing length of 10 h−1 Mpc, eight voids within 130 h−1 Mpc (having volumes 8×103 h−3 Mpc3). We study the void size distribution and morphologies and find that there is roughly an equal number of prolate and oblate‐like spheroidal voids. We compare the measured PSCz void shape and size distributions with those expected in six different cold dark matter (CDM) models and find that only the size distribution can discriminate between models. The models preferred by the PSCz data are those with intermediate values of σ8(≃0.83), independent of cosmology.

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A study of the large voids in the spatial distribution of galaxy clusters in the Northern Galactic Hemisphere

Cited by 5 publications

References 55 publications

The Low‐Redshift Lyα Forest toward PKS 0405−123

The Low‐Redshift Lyα Forest toward PKS 0405−123

Topology of large-scale underdense regions

The size and shape of local voids

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