Yukawa system (dusty plasma) in one-dimensional external fields

Totsuji, Hiroo; Kishimoto, Tokunari; Inoue, Yoshihiko; Totsuji, Chieko; Nara, Shigetoshi

doi:10.1016/0375-9601(96)00583-x

Cited by 148 publications

(136 citation statements)

References 13 publications

Supporting

Mentioning

131

Contrasting

Order By: Relevance

“…where is the mean counts in the cell, is directly related tō N the angular correlation function (Peebles 1980) (Totsuji & Kihara 1969;Lahav & Saslaw 1992)…”

Section: N(1 S) P A(s/smentioning

confidence: 99%

Imaging Large-Scale Structure in the X-Ray Sky

Yang

Mushotzky

Barger

et al. 2003

The Astrophysical Journal

View full text Add to dashboard Cite

We present the first results from a wide solid angle, moderately deep Chandra survey of the Lockman Hole North-West region. Our nine ACIS-I fields cover an effective solid angle of 0.4 deg 2 and reach a depth of 3 # ergs cm Ϫ2 s Ϫ1 in the 0.4-2 keV band and ergs cm Ϫ2 s Ϫ1 in the 2-8 keV band. The best-fit log N-Ϫ16 Ϫ15 10 3 # 10 log S for the entire field matches well onto that of the Chandra Deep Field-North. We show that the full range of the "cosmic variance" previously seen in different Chandra fields is reproduced in this small region of the sky. A counts-in-cells analysis shows that the hard-band sources are more strongly correlated than the soft-band sources. Subject headings: cosmology: observations -galaxies: nuclei -large-scale structure of universe -X-rays: diffuse background

show abstract

“…where is the mean counts in the cell, is directly related tō N the angular correlation function (Peebles 1980) (Totsuji & Kihara 1969;Lahav & Saslaw 1992)…”

Section: N(1 S) P A(s/smentioning

confidence: 99%

Imaging Large-Scale Structure in the X-Ray Sky

Yang

Mushotzky

Barger

et al. 2003

The Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…Despite the fact that large scale galaxy structures, of size of the order of several hundreds of Mpc/h 1 , have been observed to be the typical feature of the distribution of visible matter in the local universe, the statistical analysis measuring their properties has identified a characteristic scale which has only slightly changed since its discovery fourthy years ago in angular catalogs. This scale, r 0 , was measured to be the one at which fluctuations in the galaxy density field are about twice the value of the sample density and it was indeed determined to be r 0 ≈ 5 Mpc/h in the Shane and Wirtanen angular catalog [5]. Subsequent measurements of this scale -see e.g.…”

mentioning

confidence: 93%

Persistent fluctuations in the distribution of galaxies from the Two-degree Field Galaxy Redshift Survey

Labini¹,

Vasilyev²,

Baryshev³

2009

Europhys. Lett.

View full text Add to dashboard Cite

Abstract. -We apply the scale-length method to several three dimensional samples of the Two degree Field Galaxy Redshift Survey. This method allows us to map in a quantitative and powerful way large scale structures in the distribution of galaxies controlling systematic effects. By determining the probability density function of conditional fluctuations we show that large scale structures are quite typical and correspond to large fluctuations in the galaxy density field. We do not find a convergence to homogeneity up to the samples sizes, i.e. ≈ 75 Mpc/h. We then measure, at scales r ∼ < 40 Mpc/h, a well defined and statistically stable power-law behavior of the average number of galaxies in spheres, with fractal dimension D = 2.2 ± 0.2. We point out that standard models of structure formation are unable to explain the existence of the large fluctuations in the galaxy density field detected in these samples. This conclusion is reached in two ways: by considering the scale, determined by the linear perturbation analysis of a self-gravitating fluid, below which large fluctuations are expected in standard models and through the determination of statistical properties of mock galaxy catalogs generated from cosmological N-body simulations of the Millenium consortitum Introduction. -In the past twenty years observations have provided growing evidences that galaxy distribution is organized in a complex network of structures and voids [1][2][3][4]. Despite the fact that large scale galaxy structures, of size of the order of several hundreds of Mpc/h 1 , have been observed to be the typical feature of the distribution of visible matter in the local universe, the statistical analysis measuring their properties has identified a characteristic scale which has only slightly changed since its discovery fourthy years ago in angular catalogs. This scale, r 0 , was measured to be the one at which fluctuations in the galaxy density field are about twice the value of the sample density and it was indeed determined to be r 0 ≈ 5 Mpc/h in the Shane and Wirtanen angular catalog [5]. Subsequent measurements of this scale -see e.g. [6-13] -found a similar value, although in several samples larger values of r 0 have been found (i.e. r 0 ≈ 6 − 12 Mpc/h). This variation was then ascribed to a luminosity depen-

show abstract

“…From the statistical point of view, the problem is whether these structures are compatible with the very small characteristic length scale of the galaxy distribution of about ten Mpc. This is the scale at which the two-point correlation function is equal to unity, and it has been measured to be in the range of 5−15 Mpc/h in different (angular and three-dimensional) catalogs (Totsuji & Kihara 1969;Davis & Peebles 1983;Davis et al 1988;Park et al 1994;Benoist et al 1996;Norberg et al 2001Norberg et al , 2002Zehavi et al 2002Zehavi et al , 2005. The essence of the problem is not whether these measurements have been properly made as indeed they have been, but whether the statistical methods used to get this result are consistent with the properties of the galaxy distribution in these samples (see Gabrielli et al 2005;Sylos Labini et al 2009c).…”

Section: Introductionmentioning

confidence: 99%

Breaking the self-averaging properties of spatial galaxy fluctuations in the Sloan Digital Sky Survey – Data release six

Labini

Vasilyev

Baryshev

2009

A&A

View full text Add to dashboard Cite

Statistical analyses of finite sample distributions usually assume that fluctuations are self-averaging, i.e. statistically similar in different regions of the given sample volume. By using the scale-length method, we test whether this assumption is satisfied in several samples of the Sloan Digital Sky Survey Data Release Six. We find that the probability density function (PDF) of conditional fluctuations, if filtered on large enough spatial scales (i.e., r > 30 Mpc/h), shows relevant systematic variations in different subvolumes of the survey. Instead for scales of r < 30 Mpc/h, the PDF is statistically stable, and its first moment presents scaling behavior with a negative exponent around one. Thus while up to 30 Mpc/h galaxy structures have well-defined power-law correlations, on larger scales it is not possible to consider whole sample average quantities as meaningful and useful statistical descriptors. This situation stems from galaxy structures corresponding to density fluctuations that are too large in amplitude and too extended in space to be self-averaging on such large scales inside the sample volumes: galaxy distribution is inhomogeneous up to the largest scales, i.e. r ≈ 100 Mpc/h probed by the SDSS samples. We show that cosmological corrections, such as K-corrections and standard evolutionary corrections, do not qualitatively change the relevant behaviors. We consider in detail the relation between several statistical measurements generally used to quantify galaxy fluctuations and the scale-length analysis by discussing how the breaking of self-averaging properties makes it impossible to have a reliable estimation of average fluctuations amplitude, variance, and correlations for r > 30 Mpc/h. Finally we show that the large-amplitude galaxy fluctuations observed in the SDSS samples are at odds with the predictions of the standard ΛCDM model of structure formation.

show abstract

Yukawa system (dusty plasma) in one-dimensional external fields

Cited by 148 publications

References 13 publications

Imaging Large-Scale Structure in the X-Ray Sky

Imaging Large-Scale Structure in the X-Ray Sky

Persistent fluctuations in the distribution of galaxies from the Two-degree Field Galaxy Redshift Survey

Breaking the self-averaging properties of spatial galaxy fluctuations in the Sloan Digital Sky Survey – Data release six

Contact Info

Product

Resources

About