Suppression of Mn photoluminescence in ferromagnetic state of Mn-doped ZnS nanocrystals

Sarkar, Indranil; Sanyal, M. K.; Takeyama, S.; Kar, Soumitra; Hirayama, Hiroyuki; Mino, H.; Komori, Fumio; Biswas, Subhajit

doi:10.1103/physrevb.79.054410

Cited by 25 publications

(19 citation statements)

References 35 publications

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“…Results disagree as to whether recent redshift surveys have approached the depths required to describe the universe as statistically homogeneous. Studies of the fractal dimension of the galaxy distribution typically report a homogeneity scale of ≈ 70h −1 Mpc (Sarkar et al 2009;Scrimgeour et al 2012;Hogg et al 2005). However, other studies instead find the presence of LSS beyond these scales and indeed persisting to the relevant survey depths (Sylos Labini 2011;Célérier & Thieberger 2005).…”

Section: Scale Of Homogeneitymentioning

confidence: 99%

The local hole revealed by galaxy counts and redshifts

Whitbourn¹,

Shanks²

2013

Monthly Notices of the Royal Astronomical Society

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The redshifts of ≈ 250000 galaxies are used to study the Local Hole and its associated peculiar velocities. The sample, compiled from 6dF Galaxy Redshift Survey (6dFGS) and Sloan Digital Sky Survey (SDSS), provides wide sky coverage to a depth of ≈ 300h −1 Mpc. We have therefore examined K and r limited galaxy redshift distributions and number counts to map the local density field. Comparing observed galaxy n(z) distributions to homogeneous models in three large regions of the high latitude sky, we find evidence for under-densities ranging from ≈4-40% in these regions to depths of ≈150h −1 Mpc with the deepest under-density being over the Southern Galactic cap. Using the Galaxy and Mass Assembly (GAMA) survey we then establish the normalisation of galaxy counts at fainter magnitudes and thus confirm that the underdensity over all three fields at K < 12.5 is ≈ 15 ± 3%. Finally, we further use redshift catalogues to map sky-averaged peculiar velocities over the same areas using the average redshift -magnitude, z(m), technique of Soneira (1979). After accounting for the direct effect of large-scale structure on z(m) we can then search for peculiar velocities. Taking all three regions into consideration the data reject at the ≈ 4σ level the idea that we have recovered the CMB rest frame in the volume probed. We therefore conclude that there is some consistent evidence from both counts and Hubble diagrams for a 'Local Hole' with a ≈ 150h −1 Mpc under-density that deeper counts and redshifts in the Northern Galactic cap suggest may extend to ≈ 300h −1 Mpc.

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Section: Scale Of Homogeneitymentioning

confidence: 99%

The local hole revealed by galaxy counts and redshifts

Whitbourn¹,

Shanks²

2013

Monthly Notices of the Royal Astronomical Society

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“…Fractal analysis can also be used to determine the transition to homogeneity in a statistical sense. The analysis has been applied to redshift galaxy surveys: Pan & Coles (2000) to PSCz; Hogg et al (2005) to SDSS LRG; Sarkar et al (2009) to SDSS DR6; Scrimgeour et al (2012) to WiggleZ;Chacón-Cardona & Casas-Miranda (2012b) to SDSS DR9) and to N-Body simulations (Gaite (2010), Chacón-Cardona & Casas-Miranda (2012a)). The quantities of interest are the number of objects within a sphere of radius r, n(< r), and its scaling with r. This is known as a 'counts-in-cells' method.…”

Section: Introductionmentioning

confidence: 99%

Characterizing cosmic inhomogeneity with anomalous diffusion

Kraljić

2015

Mon. Not. R. Astron. Soc.

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Dark matter (DM) clustering at the present epoch is investigated from a fractal viewpoint in order to determine the scale where the self-similar scaling property of the DM halo distribution transits to homogeneity. Methods based on well-established 'countsin-cells' as well as new methods based on anomalous diffusion and random walks are investigated. Both are applied to DM halos of the biggest N-Body simulation in the 'Dark Sky Simulations' (DS) catalogue and an equivalent randomly distributed catalogue. Results based on the smaller 'Millennium Run' (MR) simulation are revisited and improved. It is found that the MR simulation volume is too small and prone to bias to reliably identify the onset of homogeneity. Transition to homogeneity is defined when the fractal dimension of the clustered and random distributions cannot be distinguished within the associated uncertainties. The 'counts-in-cells' method applied to the DS simulation then yields a homogeneity scale roughly consistent with previous work (∼ 150 h −1 Mpc). The characteristic length-scale for anomalous diffusion to behave homogeneously is found to be at about 250 h −1 Mpc. The behaviour of the fractal dimensions for a halo catalogue with the same two-point function as the original but with shuffled Fourier phases is investigated. The methods based on anomalous diffusion are shown to be sensitive to the phase information, whereas the 'counts-in-cells' methods are not.

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“…There have been considerable applications in the area of nanostructures, such as nano-wires, thin films, quantum dot lasers as well as those related to passivating the surface of other materials to create confined particles [19][20][21], etc. There have been many empirical and ab initio calculations of the electronic and optical properties for these compounds [22][23][24][25][26][27][28][29][30][31][32]. Reshak and Auluck [32] analyzed the electronic and optical properties of ZnX compounds within local density approximation (LDA) and generalized gradient approximation (GGA).…”

Section: Introductionmentioning

confidence: 99%

Structural, electronic and optical properties of ZnX and CdX compounds (X=Se, Te and S) under hydrostatic pressure

Nourbakhsh

2010

Journal of Alloys and Compounds

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Suppression of Mn photoluminescence in ferromagnetic state of Mn-doped ZnS nanocrystals

Cited by 25 publications

References 35 publications

The local hole revealed by galaxy counts and redshifts

The local hole revealed by galaxy counts and redshifts

Characterizing cosmic inhomogeneity with anomalous diffusion

Structural, electronic and optical properties of ZnX and CdX compounds (X=Se, Te and S) under hydrostatic pressure

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