Segregation of metals-containing wastewater by pH

Taylor, P.A.; McTaggart, D.

doi:10.2172/6460486

Cited by 9 publications

(18 citation statements)

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“…To measure the 3D gravitational potential, we must first calculate the lensing potential, φ, which we consider as a 3D field (cf. Taylor 2001;. This is related to the shear field (in the limit of a flat sky) by…”

Section: Lensing Potentialmentioning

confidence: 99%

“…We measure transverse positions θ in units of radians, leading to dimensionless lensing quantities. Equation (6) reconstructs the lensing potential up to an arbitrary function of comoving distance (Taylor 2001;:…”

Section: Lensing Potentialmentioning

confidence: 99%

“…where we have assumed a spatially flat universe and the Born approximation. Treating φ(r , r θ) as a 3D variable, we can invert equation (13) to arrive at an estimate of the 3D gravitational potential (Taylor 2001):…”

Section: Gravitational Potentialmentioning

confidence: 99%

“…A further significant development has been the realization that a full reconstruction of the 3D gravitational potential and dark-matter density field is possible using just weak shear and redshifts (Taylor 2001). A 3D gravitational lensing analysis is clearly of importance for cosmology.…”

Section: Introductionmentioning

confidence: 99%

“…Following Taylor (2001), Hu & Keeton (2002) subsequently developed a pixelized version of the 3D reconstruction, while examined the practical implementation of Taylor's (2001) method. demonstrated that one can hope to reconstruct the gravitational potential on cluster mass-scales with ground-based shear surveys to a depth of z = 1 by including photometric redshifts with accuracy z 0.05.…”

Section: Introductionmentioning

confidence: 99%

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Mapping the 3D dark matter with weak lensing in COMBO-17

Taylor

Bacon

Gray

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present a three‐dimensional (3D) lensing analysis of the z= 0.16 supercluster A901/2, resulting in a 3D map of the dark matter distribution within a 3 × 105 [h−1 Mpc]3 volume. This map is generated from a combined catalogue of 3D galaxy coordinates together with shear estimates, using R‐band imaging and photometric redshifts from the COMBO‐17 survey. We perform a χ2 fit of isothermal spheres to the tangential shear pattern around each cluster as a function of redshift to estimate the 3D positions and masses of the main clusters in the supercluster from lensing alone. Motivated by the appearance of a second cluster behind A902 in galaxy number density, we also fit a two‐cluster model to A902. We then present the first 3D map of the dark‐matter gravitational potential field, Φ, from weak lensing using the Kaiser–Squires and Taylor inversion methods. These maps clearly show the potential wells of the main supercluster components, including the new cluster behind A902, and demonstrate the applicability of 3D dark‐matter mapping and projection‐free, mass‐selected cluster finding to current data. Finally, we develop the halo model of dark matter and galaxy clustering and compare this with the auto‐ and cross‐correlation functions of the 3D gravitational potential, galaxy number densities and galaxy luminosity densities measured in the A901/2 field. We find significant anticorrelations between the gravitational potential field and the galaxy number density and luminosities, as expected due to baryonic infall into dark‐matter concentrations. We find good agreement with the halo model for the number densities and luminosity correlation functions, but some disagreement with the shape of the gravitational potential correlation function, which we attribute to finite‐field effects.

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Section: Lensing Potentialmentioning

confidence: 99%

Section: Lensing Potentialmentioning

confidence: 99%

Section: Gravitational Potentialmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mapping the 3D dark matter with weak lensing in COMBO-17

Taylor

Bacon

Gray

et al. 2004

Monthly Notices of the Royal Astronomical Society

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Bounds on anomalous magnetic and electric moments of tau lepton from LEP and lepton flavor violation

1999

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The most stringent bounds on the anomalous magnetic and electric dipole moments of the tau lepton was derived by Escribano and Massó[6] from the Z width at LEP in an effective lagrangian approach to the new physics. In this paper we point out that the higher dimensional operators introduced by Escribano and Massó not only modify the neutral currents of the tau lepton to Z gauge boson and the photon, but also induce lepton flavor violation (LFV). The size of the LFV effect depends crucially on the dynamics of the lepton mass generation. Assuming the lepton mass matrices in the form of an Fritzsch ansatz, we point out that the experimental limit on µ → eγ will push the anomalous magnetic and electric dipole moments of the tau lepton down to 10 −11 and 10 −25 e cm respectively.

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Microlensing Halo Models with Abundant Brown Dwarfs

Kerins

Evans

1998

The Astrophysical Journal

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All previous attempts to understand the microlensing results toward the Large Magellanic Cloud (LMC) have assumed homogeneous present-day mass functions (PDMFs) for the lensing populations. Here, we present an investigation into the microlensing characteristics of halos with spatially varying PDMFs and anisotropic velocity dispersion tensors. One attractive possibility-suggested by baryonic dark cluster formation in pregalactic and protogalactic cooling flows-is that the inner halo is dominated by stellar mass objects, whereas low-mass brown dwarfs become more prevalent on moving outward. The contribution to the microlensing rate must be dominated by dark remnants (∼0.5 M , ) to recover the observed timescales of the microlensing experiments. But, even though stellar remnants control the rate, they do not dominate the mass of the baryonic halo, and so the wellknown enrichment and mass budget problems are much less severe. Using a simple Ansatz for the spatial variation of the PDMF, models are constructed in which the contribution of brown dwarfs to the mass of the baryonic halo is ∼55% and to the total halo is ∼30%. An unusual property of the models is that they predict that the average timescale of events toward M31 is shorter than the average timescale toward the LMC. This is because the longer line of sight toward M31 probes more of the far halo in which brown dwarfs are the most common constituent.

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Segregation of metals-containing wastewater by pH

Cited by 9 publications

References 0 publications

Mapping the 3D dark matter with weak lensing in COMBO-17

Mapping the 3D dark matter with weak lensing in COMBO-17

Bounds on anomalous magnetic and electric moments of tau lepton from LEP and lepton flavor violation

Microlensing Halo Models with Abundant Brown Dwarfs

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