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Abstract: The use of headland-breakwater systems along the shore of Chesapeake Bay began in the early 1980s. Properly designed and installed headland breakwaters with beach fill and wetlands plantings provide shore protection and create a “full” coastal profile of beach/backshore/dune which enhances habitat. They create a tertiary buffer for upland runoff and groundwater and provide access and recreation. The wetland grasses also create an erosion resistant turf. The coastal profile accommodates environmental permitting requirements of habitat enhancement for shore protection structures. The Static Equilibrium Bay (SEB) model of Hsu and Sylvester has shown its utility in defining the pocket or embayed beach planform between headland breakwaters. Bay plots for varying wind/wave conditions and water levels define the limits of shoreline change. The embayed beach must be high and wide enough to offer protection, usually for the base of a graded upland bank, under design storm conditions. The embayed beach morphology should emulate nature; the existing beach profile should be assessed first in designing any headland-breakwater system. The design of the beach begins with establishing the minimum design beach width (B m) and profile in the context of stable embayed beaches held by headland breakwaters. With B m established, breakwater length (L b), the breakwater gap (G b) and the bay indentation distance (M b) come into play depending on the wave environment. The empirically derived relationships between these parameters are offered as a guide for breakwater design along the sheltered coasts of Chesapeake Bay. Constructing stable headland/embayed beaches for long-term shore protection can be done cost effectively. The procedures developed over the years to evaluate and design headland breakwaters have been, in retrospect, effective. These installations provide a database of successful headland-breakwater installations, some of which are over 20years old. This database will continue to be used to verify and compare parameters for headland systems in the future as sites continue to mature. [Copyright &y& Elsevier]

The article present a profile of American writer Isaac Asimov along with his science fiction writing. Topics discussed include his novelette "Nightfall" which received a cover story in 'Astounding Science Fiction' journal in 1941; his books, written on topics ranging from the Bible to the human body; and "Foundation" book series which became his first bestseller. Also mentions about his book "Opus 100".

This article discusses writings of playwright Jules Verne. One example of his significance is that his novels are the first science fiction works translated into countries just beginning their industrial transformations, such as China and India. A second is that his work, was featured on the cover of "Amazing Stories," for its first nine issues. A third is the inspiration he provided for a generation of inventors and explorers such as Igor Sikorsky, Simon Lake, Norman Casteret, and Admiral Byrd.

Radial electric fields ( Er) and their role in the establishment of edge transport barriers and improved confinement have been studied in the tokamaks TEXTOR-94 and CASTOR, where Er is externally applied to the plasma in a controlled way using a biased electrode, as well as in the tokamak T-10 where an edge transport barrier (H-mode) is obtained during electron-cyclotron resonance heating (ECRH) of the plasma. The physics of radial currents was studied and the radial conductivity in the edge of TEXTOR-94 ( R = 1.75 m, a = 0.46 m) was found to be dominated by recycling (ion-neutral collisions) at the last closed flux surface (LCFS) and by parallel viscosity inside the LCFS. From a performance point of view (edge engineering), such electrode biasing was shown to induce a particle transport barrier, a reduction of particle transport, and a concomitant increase in energy confinement. An H-mode-like behaviour can be induced both with positive and negative electric fields. Positive as well as negative electric fields were shown to strongly affect the exhaust of hydrogen, helium, and impurities, not only in the H-mode-like regime. The impact of sheared radial electric fields on turbulent structures and flows at the plasma edge is investigated on the CASTOR tokamak ( R = 0.4 m, a = 0.085 m). A non-intrusive biasing scheme that we call "separatrix biasing" is applied whereby the electrode is located in the scrape-off layer (SOL) with its tip just touching the LCFS. There is evidence of strongly sheared radial electric field and E× B flow, resulting in the formation of a transport barrier at the separatrix. Advanced probe diagnosis of the edge region has shown that the E× B shear rate that arises during separatrix biasing is larger than for standard edge plasma biasing. The plasma flows, especially the poloidal E× B drift velocity, are strongly modified in the sheared region, reaching Mach numbers as high as half the sound speed. The corresponding shear rates (≈ 5×106 s-1) derived from both the flow and electric field profiles are in excellent agreement and are at least an order of magnitude higher than the growth rate of unstable turbulent modes as estimated from fluctuation measurements. During ECRH in the tokamak T-10 ( R = 1.5 m, a = 0.3 m), a regime of improved confinement is obtained with features resembling those in the H-mode in other tokamaks. Using a heavy ion beam probe, a narrow potential well is observed near the limiter together with the typical features of the L-H transition. The time evolution of the plasma profiles during L-H and H-L transitions is clearly correlated with that of the density profile and the formation of a transport barrier near the limiter. The edge electric field is initially positive after the onset of ECRH. It changes its sign during the L-H transition and grows till a steady condition is reached. Similar to the biasing experiments in TEXTOR-94 and CASTOR, the experimentally observed transport barrier is a barrier for particles. [ABSTRACT FROM AUTHOR]

Explains the teaching of science fiction. Kinds of subjects that can be taught through science fiction; Teachers of science fiction; Author's own experience in the field.

Describes the installation of arrays of 12 flush-mounted Langmuir plasma probes in the upper and lower outboard divertor plates of Tokamak de Varennes (TdeV). Measurement of electron temperature and density; Validation of the technique by comparing measurements from a cylindrical and a flush probe which are operated simultaneously in the same plasma.

Focuses on the history of science fiction. Early science fiction writers as being influenced by blossoming science and technology; Beginnings of modern science fiction; Relationship between naturalism and science fiction; Science fiction as applying naturalism to the fantastic; Differences between mainstream and science fiction.

A response by James Gunn to a letter to the editor about his article "A Singular Conundrum: How odd is our universe?" in the September 28, 2007 issue is presented.

Presents a letter to the editor reacting to Peter Sanders' letter in the July 2003 issue of 'IEE Review' journal which distinguished between members of Institution of Electrical Engineers, Institution of Mechanical Engineers or British Computer Society.

Symptomatic perineal hernias following abdomino-perineal excision of rectum have been reported to occur uncommonly.We present the case of a 79-year-old gentleman who developed a perineal hernia after laparoscopic-assisted extralevator abdomino-perineal excision (ELAPE) of the rectum. Despite initial myocutaneous flap repair, there was further symptomatic recurrence. Magnetic resonance imaging demonstrated non-compromised bowel extending beneath the gracilis flap with extension into the adductor compartment of the left thigh. Given the recurrent nature, a rectus flap repair was performed and after 15 months, he remains hernia free. There is currently no consensus as to the optimal operative technique in the prevention and management of these hernias; however, primary reconstruction at the time of ELAPE may be preferable. Symptomatic perineal hernias can be severely debilitating and require operative repair.We suggest that surgical options should be discussed and carried out with the input of a Plastic surgeon. [ABSTRACT FROM AUTHOR]

This paper describes the detailed design of the CCD dewar and the camera system which is a part of the wide-field imager Hyper Suprime-Cam (HSC) on the 8.2 m Subaru Telescope. On the 1.°5 diameter focal plane (497 mm in physical size), 116 four-side buttable 2 k × 4 k fully depleted CCDs are tiled with 0.3 mm gaps between adjacent chips, which are cooled down to −100°C by two pulse tube coolers with a capability to exhaust 100 W heat at −100°C. The design of the dewar is basically a natural extension of Suprime-Cam, incorporating some improvements such as (1) a detailed CCD positioning strategy to avoid any collision between CCDs while maximizing the filling factor of the focal plane, (2) a spherical washers mechanism adopted for the interface points to avoid any deformation caused by the tilt of the interface surface to be transferred to the focal plane, (3) the employment of a truncated-cone-shaped window, made of synthetic silica, to save the back focal space, and (4) a passive heat transfer mechanism to exhaust efficiently the heat generated from the CCD readout electronics which are accommodated inside the dewar. Extensive simulations using a finite-element analysis (FEA) method are carried out to verify that the design of the dewar is sufficient to satisfy the assigned errors. We also perform verification tests using the actually assembled CCD dewar to supplement the FEA and demonstrate that the design is adequate to ensure an excellent image quality which is key to the HSC. The details of the camera system, including the control computer system, are described as well as the assembling process of the dewar and the process of installation on the telescope. [ABSTRACT FROM AUTHOR]

We present spectroscopic identification of 32 new quasars and luminous galaxies discovered at 5.7 < z ≤ 6.8. This is the second in a series of papers presenting the results of the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, which exploits the deep multi-band imaging data produced by the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. The photometric candidates were selected by a Bayesian probabilistic algorithm, and then observed with spectrographs on the Gran Telescopio Canarias and the Subaru Telescope. Combined with the sample presented in the previous paper of this series, we have now identified 64 HSC sources over about 430 deg2, which include 33 high-z quasars, 14 high-z luminous galaxies, two [O III] emitters at z ∼ 0.8, and 15 Galactic brown dwarfs. The new quasars have considerably lower luminosity (M1450 ∼ −25 to −22 mag) than most of the previously known high-z quasars. Several of these quasars have luminous (>1043 erg s−1) and narrow (< 500 km s−1) Lyα lines, and also a possible mini broad-absorption-line system of N V λ1240 in the composite spectrum, which clearly separate them from typical quasars. On the other hand, the high-z galaxies have extremely high luminosities (M1450 ∼ −24 to −22 mag) compared to other galaxies found at similar redshifts. With the discovery of these new classes of objects, we are opening up new parameter spaces in the high-z Universe. Further survey observations and follow-up studies of the identified objects, including the construction of the quasar luminosity function at z ∼ 6, are ongoing. [ABSTRACT FROM AUTHOR]

Understanding heat flux deposition processes is essential for the design of the plasma facing component allowing reliable high power steady state plasma operations. Misalignments up to δ = 0.2 mm between two adjacent CFC tiles have been reported on the Toroidal Pump Limiter of Tore Supra. Heat flux impinging the top and leading edge of the protruding tile are characterized with both IR thermographic system and numerical modelling using 2D particle-in-cell simulations that accounts for the Larmor radius smoothing effect of incident ions. Numerical heat loads are coupled with a 2D thermal model of the tile and with a specific sensor correction to simulate spatial-resolution related effects (necessary here since the tile misalignment is smaller than the spatial resolution of the IR system). In the experiment depicted here, with a misalignment smaller than an ion gyro-radius, the Larmor radius smoothing effect is maximum and overheating of the leading edge is reduced by a factor of two. [ABSTRACT FROM AUTHOR]

Purposes: Several reports have described a relationship between tumor volume and oncological outcomes for certain cancers. There is paucity of similar data for rectal cancer. We conducted this study to establish whether tumor volume, mesorectal volume, and the tumor volume to mesorectal volume ratio (TV/MRV), evaluated by magnetic resonance imaging (MRI), affect the oncological outcomes of patients with rectal cancer. Methods: We performed volumetric analysis of rectal tumors from magnetic resonance imaging (MRI) images and assessed their correlation with oncological outcomes, using clinical and radiological databases. Results: The subjects of this study were 25 of 35 patients who underwent rectal cancer surgery after staging with MRI, after the exclusion of 7 patients for whom MRI images could not be retrieved and 3 patients who had metastases identified at diagnosis. Tumor volume (TV) was a significant predictor of overall survival hazard ratio (95 % CI); 5.8 (1.2-29), ( P = 0.03). Mesorectal volume (MRV) and TV/MRV did not correlate with oncological outcomes. Conclusions: We found a direct relationship between tumor volume and overall survival, which may be used to stratify rectal tumors for neoadjuvant therapy. A larger prospective study is required to confirm this correlation. [ABSTRACT FROM AUTHOR]

In this paper, we report results of a dedicated experiment that gives the plasma penetration profiles inside a gap of a tokamak castellated plasma-facing component. A specially designed probe that recreates a gap between two tiles has been built for the purpose of this study. It allows to measure ion saturation profiles along the 2 sides and at the bottom of the gap for both poloidal and toroidal orientations. The novelty of such experiment is the real time measurement of the plasma flux inside the gap during a tokamak D-shaped discharge compared to previous experimental studies which were mainly post-mortem. This experiment was performed in the COMPASS tokamak and results are compared with particle-in-cell simulations. The plasma deposition is found to be asymmetric in both orientations with a stronger effect in poloidal gaps. The Larmor radius of the incoming ions plays a role in the plasma penetration only in poloidal gaps but seems to have little impact in toroidal gaps. Profiles are qualitatively well reproduced by simulations. Ion current is recorded at the bottom of a toroidal gap under certain conditions. [ABSTRACT FROM AUTHOR]

The W -for tungsten- environment in steady-state tokamak (WEST) project consists in transforming the French tokamak Tore Supra into an X-point divertor one and aims at testing the ITER technology of actively cooled high heat flux tungsten components during ITER-relevant long pulses. In addition to the integration in the vacuum vessel of a lower divertor and an upper one, this metamorphosis has a strong impact on diagnostics initially present in Tore Supra. Indeed, the introduction of a divertor in the upper part of the machine leads to block the lines of sight (LOS) of diagnostics previously installed in the upper ports. Therefore, new diagnostics playing a paramount role for the safe tokamak operation need to be implemented, such as an infrared (IR) thermography diagnostic for the protection of plasma-facing components (PFCs) and heating antennas, and a visible spectroscopy system for the protection of tungsten PFCs. Besides, several existing diagnostics need to be modified to adapt their LOS to the new divertor targets and plasma shape. This paper presents the main issues linked to the integration of diagnostics deriving from the WEST project. First, the changes involved by the upgrade on the set of diagnostics currently implemented in Tore Supra are described. Then, a particular focus is put on the integration of the two new optical systems, namely the IR system and the visible spectroscopy one. These two systems being located within the vacuum vessel, a special care must be paid to their design, to allow them to withstand their harsh environmental conditions. Other new or updated fundamental diagnostics are also briefly presented. Finally, the resulting new implementation of diagnostics envisaged to reach the scientific and technological goals of the WEST project is described. [ABSTRACT FROM PUBLISHER]

The Subaru Prime Focus Spectrograph (PFS) is a massively multiplexed fiber-fed optical and near-infrared three-arm spectrograph (Nfiber = 2400, 380 ≤ λ ≤ 1260 nm, 1 $_{.}^{\circ}$3 diameter field of view). Here, we summarize the science cases in terms of provisional plans for a 300-night Subaru survey. We describe plans to constrain the nature of dark energy via a survey of emission line galaxies spanning a comoving volume of 9.3 h−3 Gpc3 in the redshift range 0.8 < z < 2.4. In each of six redshift bins, the cosmological distances will be measured to 3% precision via the baryonic acoustic oscillation scale, and redshift-space distortion measures will constrain structure growth to 6% precision. In the near-field cosmology program, radial velocities and chemical abundances of stars in the Milky Way and M 31 will be used to infer the past assembly histories of spiral galaxies and the structure of their dark matter halos. Data will be secured for 106 stars in the Galactic thick-disk, halo, and tidal streams as faint as V ∼ 22, including stars with V < 20 to complement the goals of the Gaia mission. A medium-resolution mode with R = 5000 to be implemented in the red arm will allow the measurement of multiple α-element abundances and more precise velocities for Galactic stars. For the galaxy evolution program, our simulations suggest the wide wavelength range of PFS will be powerful in probing the galaxy population and its clustering over a wide redshift range. We plan to conduct a color-selected survey of 1 < z < 2 galaxies and AGN over 16 deg2 to J ≃ 23.4, yielding a fair sample of galaxies with stellar masses above ∼1010 M⊙ at z ≃ 2. A two-tiered survey of higher redshift Lyman break galaxies and Lyman alpha emitters will quantify the properties of early systems close to the reionization epoch. [ABSTRACT FROM AUTHOR]

We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions σ* ≳ 150 km s–1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼10 Gyr), relatively metal-poor ([Fe/H] ≈ –0.5), and α-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). [ABSTRACT FROM AUTHOR]

Abstract: We report on the first full 3D EMC3-Eirene simulations of the bulk plasma, neutral gas and W impurity transport in Tore Supra (TS). Three configurations are addressed: (A) the high field side-, (B) bottom- and (C) low field side limited case and compared to Mach probe measurements at the top of the device. As in previous 2D simulations the 3D modelling also showed a strong discrepancy between the measured and simulated Mach number in case B. In order to investigate the finite size of the Mach probe we included this object as a plasma limiting structure in the simulation and found that the probe indeed perturbs the plasma, which explains the discrepancy only partly. The W transport simulation was found to have a rather weak dependence on the magnetic configuration and the simulated tungsten confinement time shows a similar behavior as those measured recently by Meyer et al. The absolute value, however, differs by a factor of 10. [Copyright &y& Elsevier]

ABSTRACT We present measurements of galaxy clustering from the Baryon Oscillation Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey III (SDSS-III). These use the Data Release 9 (DR9) CMASS sample, which contains 264 283 massive galaxies covering 3275 square degrees with an effective redshift z = 0.57 and redshift range 0.43 < z < 0.7. Assuming a concordance ΛCDM cosmological model, this sample covers an effective volume of 2.2 Gpc3, and represents the largest sample of the Universe ever surveyed at this density [ABSTRACT FROM AUTHOR]

ABSTRACT We analyse the anisotropic clustering of massive galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) sample, which consists of 264 283 galaxies in the redshift range 0.43 < z < 0.7 spanning 3275 deg2. Both peculiar velocities and errors in the assumed redshift-distance relation ('Alcock-Paczynski effect') generate correlations between clustering amplitude and orientation with respect to the line of sight. Together with the sharp baryon acoustic oscillation (BAO) standard ruler, our measurements of the broad-band shape of the monopole and quadrupole correlation functions simultaneously constrain the comoving angular diameter distance (2190 ± 61 Mpc) to z = 0.57, the Hubble expansion rate at z = 0.57 (92.4 ± 4.5 km s−1 Mpc−1) and the growth rate of structure at that same redshift (dσ8/d ln a = 0.43 ± 0.069). Our analysis provides the best current direct determination of both DA and H in galaxy clustering data using this technique. If we further assume a Λcold dark matter expansion history, our growth constraint tightens to dσ8/d ln a = 0.415 ± 0.034. In combination with the cosmic microwave background, our measurements of DA, H and dσ8/d ln a all separately require dark energy at z > 0.57, and when combined imply ΩΛ = 0.74 ± 0.016, independent of the Universe's evolution at z < 0.57. All of these constraints assume scale-independent linear growth, and assume general relativity to compute both [ABSTRACT FROM AUTHOR]

Abstract: We present the ensemble properties of 31 comets (27 resolved and 4 unresolved) observed by the Sloan Digital Sky Survey (SDSS). This sample of comets represents about 1 comet per 10million SDSS photometric objects. Five-band (u, g, r, i, z) photometry is used to determine the comets’ colors, sizes, surface brightness profiles, and rates of dust production in terms of the Afρ formalism. We find that the cumulative luminosity function for the Jupiter Family Comets in our sample is well fit by a power law of the form N(

We measure the luminosity and color dependence of galaxy clustering in the largest-ever galaxy redshift survey, the main galaxy sample of the Sloan Digital Sky Survey Seventh Data Release. We focus on the projected correlation function wp(rp) of volume-limited samples, extracted from the parent sample of ~700,000 galaxies over 8000 deg², extending up to redshift of 0.25. We interpret our measurements using halo occupation distribution (HOD) modeling assuming a ACDM cosmology (inflationary cold dark matter with a cosmological constant). The amplitude of wp (rp) grows slowly with luminosity for L < L* and increases sharply at higher luminosities, with a large-scale bias factor b(>L) x (σ8/0.8) = 1.06 + 0.21(L/L*)1.12, where L is the sample luminosity threshold. At fixed luminosity, redder galaxies exhibit a higher amplitude and steeper correlation function, a steady trend that runs through the "blue cloud" and "green valley" and continues across the "red sequence." The cross-correlation of red and blue galaxies is close to the geometric mean of their autocorrelations, dropping slightly below at rp < 1 h-1 Mpc. The luminosity trends for the red and blue galaxy populations separately are strikingly different. Blue galaxies show a slow but steady increase of clustering strength with luminosity, with nearly constant shape of wp(rp). The large-scale clustering of red galaxies shows little luminosity dependence until a sharp increase at L > 4 L*, but the lowest luminosity red galaxies (0.044).25 L*) show very strong clustering on small scales (rp < 2 h-1 Mpc). Most of the observed trends can be naturally understood within the ACDM+HOD framework. The growth of wp(rp) for higher luminosity galaxies reflects an overall shift in the mass scale of their host dark matter halos, in particular an increase in the minimum host halo mass Mmin. The mass at which a halo has, on average, one satellite galaxy brighter than L is M1 ≈ 17 Mmin(L) over most of the luminosity range, with a smaller ratio above L,. The growth and steepening of wp(rp) for redder galaxies reflects the increasing fraction of galaxies that are satellite systems in high-mass halos instead of central systems in low-mass halos, a trend that is especially marked at low luminosities. Our extensive measurements, provided in tabular form, will allow detailed tests of theoretical models of galaxy formation, a firm grounding of semiempirical models of the galaxy population, and new constraints on cosmological parameters from combining real-space galaxy clustering with mass-sensitive statistics such as redshift-space distortions, cluster mass-to-light ratios, and galaxy-galaxy lensing. [ABSTRACT FROM AUTHOR]

We present the power spectrum of the reconstructed halo density field derived from a sample of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) Seventh Data Release (DR7). The halo power spectrum has a direct connection to the underlying dark matter power for , well into the quasi-linear regime. This enables us to use a factor of ∼8 more modes in the cosmological analysis than an analysis with , as was adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for is well fitted by our model: for 40 degrees of freedom for the best-fitting Λ cold dark matter (ΛCDM) model. We find for a power-law primordial power spectrum with spectral index ns and fixed, consistent with cosmic microwave background measurements. The halo power spectrum also constrains the ratio of the comoving sound horizon at the baryon-drag epoch to an effective distance to . Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe ( WMAP) 5 year results, for the flat ΛCDM model we find and . Allowing for massive neutrinos in ΛCDM, we find eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species Neff as a free parameter, we find . Combining also with the Kowalski et al. supernova sample, we find and for an open cosmology with constant dark energy equation of state w. The power spectrum and a module to calculate the likelihoods are publicly available at . [ABSTRACT FROM AUTHOR]

Plasma deposition in narrow gaps between tiles of ITER plasma-facing components during ELMs is simulated by means of particle-in-cell technique. The particle and power loads onto and between the divertor tiles are estimated for a multispecies plasma. We simulate an equal mixture of deuterium and tritium (T) for the main plasma with one impurity, the carbon (C). The aim of this paper is to know whether the C ions can enter the narrow gaps between tiles and with which energy. Due to its radioactivity, the T deposition in the gaps is also of high interest and is estimated. The two basic orientations of the gap with respect to the magnetic field lines, poloidal and toroidal, have been studied. The global penetration of the two hydrogen species into the gap is on the order of the gap width (~0.5 mm), and their own contribution on the total heat flux to the gap is given. The main impurity penetrates into the gap in between 50% to 70% of the total plasma-deposition length but with a power deposited representing less than 1% of the total deposited power. [ABSTRACT FROM AUTHOR]

Abstract: Using a sample of serendipitously discovered active comets in the Sloan Digital Sky Survey (SDSS), we develop well-controlled selection criteria for greatly increasing the efficiency of comet identification in the SDSS catalogs. After follow-up visual inspection of images to reject remaining false positives, the total sample of SDSS comets presented here contains 19 objects, roughly one comet per 10 million other SDSS objects. The good understanding of selection effects allows a study of the population statistics, and we estimate the apparent magnitude distribution to , the ecliptic latitude distribution, and the comet distribution in SDSS color space. The most surprising results are the extremely narrow range of colors for comets in our sample (e.g. root-mean-square scatter of only ∼0.06mag for the color), and the similarity of comet colors to those of jovian Trojans. We discuss the relevance of our results for upcoming deep multi-epoch optical surveys such as the Dark Energy Survey, Pan-STARRS, and the Large Synoptic Survey Telescope (LSST), and estimate that LSST may produce a sample of about 10,000 comets over its 10-year lifetime. [Copyright &y& Elsevier]

The spectroscopic Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) galaxy sample represents the final set of galaxies observed using the original SDSS target selection criteria. We analyse the clustering of galaxies within this sample, including both the luminous red galaxy and main samples, and also include the 2-degree Field Galaxy Redshift Survey data. In total, this sample comprises 893 319 galaxies over 9100 deg2. Baryon acoustic oscillations (BAO) are observed in power spectra measured for different slices in redshift; this allows us to constrain the distance–redshift relation at multiple epochs. We achieve a distance measure at redshift , of (2.7 per cent accuracy), where is the comoving sound horizon at the baryon-drag epoch, is the angular diameter distance and is the Hubble parameter. We find an almost independent constraint on the ratio of distances , which is consistent at the 1.1σ level with the best-fitting Λ cold dark matter model obtained when combining our distance constraint with the Wilkinson Microwave Anisotropy Probe 5-year ( WMAP5) data. The offset is similar to that found in previous analyses of the SDSS DR5 sample, but the discrepancy is now of lower significance, a change caused by a revised error analysis and a change in the methodology adopted, as well as the addition of more data. Using WMAP5 constraints on and , and combining our BAO distance measurements with those from the Union supernova sample, places a tight constraint on and that is robust to allowing and . This result is independent of the behaviour of dark energy at redshifts greater than those probed by the BAO and supernova measurements. Combining these data sets with the full WMAP5 likelihood constraints provides tight constraints on both and for a constant dark energy equation of state. [ABSTRACT FROM AUTHOR]

We present the 3D real-space clustering power spectrum of a sample of ∼600 000 luminous red galaxies measured by the Sloan Digital Sky Survey, using photometric redshifts. These galaxies are old, elliptical systems with strong 4000-Å breaks, and have accurate photometric redshifts with an average error of Δ z= 0.03. This sample of galaxies ranges from redshift z= 0.2 to 0.6 over 3528 deg2 of the sky, probing a volume of 1.5 h−3 Gpc3, making it the largest volume ever used for galaxy clustering measurements. We measure the angular clustering power spectrum in eight redshift slices and use well-calibrated redshift distributions to combine these into a high-precision 3D real-space power spectrum from k= 0.005 to k= 1 h Mpc−1. We detect power on gigaparsec scales, beyond the turnover in the matter power spectrum, at a ∼2σ significance for k < 0.01 h Mpc−1, increasing to 5.5σ for k < 0.02 h Mpc−1. This detection of power is on scales significantly larger than those accessible to current spectroscopic redshift surveys. We also find evidence for baryonic oscillations, both in the power spectrum, as well as in fits to the baryon density, at a 2.5 σ confidence level. The large volume and resulting small statistical errors on the power spectrum allow us to constrain both the amplitude and the scale dependence of the galaxy bias in cosmological fits. The statistical power of these data to constrain cosmology is ∼1.7 times better than previous clustering analyses. Varying the matter density and baryon fraction, we find ΩM= 0.30 ± 0.03, and Ωb/ΩM= 0.18 ± 0.04, for a fixed Hubble constant of 70 km s−1 Mpc−1 and a scale-invariant spectrum of initial perturbations. The detection of baryonic oscillations also allows us to measure the comoving distance to z= 0.5; we find a best-fitting distance of 1.73 ± 0.12 Gpc, corresponding to a 6.5 per cent error on the distance. These results demonstrate the ability to make precise clustering measurements with photometric surveys. [ABSTRACT FROM AUTHOR]

We have used the Two-Degree Field (2dF) instrument on the Anglo-Australian Telescope (AAT) to obtain redshifts of a sample of and quasars selected from Sloan Digital Sky Survey (SDSS) imaging. These data are part of a larger joint programme between the SDSS and 2dF communities to obtain spectra of faint quasars and luminous red galaxies, namely the 2dF–SDSS LRG and QSO (2SLAQ) Survey. We describe the quasar selection algorithm and present the resulting number counts and luminosity function of 5645 quasars in 105.7 deg2. The bright-end number counts and luminosity functions agree well with determinations from the 2dF QSO Redshift Survey (2QZ) data to. However, at the faint end, the 2SLAQ number counts and luminosity functions are steeper (i.e. require more faint quasars) than the final 2QZ results from Croom et al., but are consistent with the preliminary 2QZ results from Boyle et al. Using the functional form adopted for the 2QZ analysis (a double power law with pure luminosity evolution characterized by a second-order polynomial in redshift), we find a faint-end slope of if we allow all of the parameters to vary, and if we allow only the faint-end slope and normalization to vary (holding all other parameters equal to the final 2QZ values). Over the magnitude range covered by the 2SLAQ survey, our maximum-likelihood fit to the data yields 32 per cent more quasars than the final 2QZ parametrization, but is not inconsistent with other deep surveys for quasars. The 2SLAQ data exhibit no well-defined‘break’ in the number counts or luminosity function, but do clearly flatten with increasing magnitude. Finally, we find that the shape of the quasar luminosity function derived from 2SLAQ is in good agreement with that derived from Type I quasars found in hard X-ray surveys. [ABSTRACT FROM AUTHOR]

Gundestrup is a Langmuir/Mach probe array which measures the flow velocity in the scrape-off layer of Tokamak de Varennes (TdeV). It is based on the concept of a Mach probe where presheaths extending upstream and downstream from the probe, parallel to the magnetic field, attract charge to a circular array of collecting pins. The polar distribution of ion saturation currents to the circular array is used to compute the components of flow velocity in the plasma. With Gundestrup, there is an assumed flow perpendicular to the magnetic field as well as parallel to it. Equations representing the collection of charge by individual pins on the probe are presented and sample flow patterns from the scrape-off layer are shown. [ABSTRACT FROM AUTHOR]

Although general relativity underlies modern cosmology, its applicability on cosmological length scales has yet to be stringently tested. Such a test has recently been proposed, using a quantity, EG, that combines measures of large-scale gravitational lensing, galaxy clustering and structure growth rate. The combination is insensitive to ‘galaxy bias’ (the difference between the clustering of visible galaxies and invisible dark matter) and is thus robust to the uncertainty in this parameter. Modified theories of gravity generally predict values of EG different from the general relativistic prediction because, in these theories, the ‘gravitational slip’ (the difference between the two potentials that describe perturbations in the gravitational metric) is non-zero, which leads to changes in the growth of structure and the strength of the gravitational lensing effect. Here we report that EG = 0.39 ± 0.06 on length scales of tens of megaparsecs, in agreement with the general relativistic prediction of EG ≈ 0.4. The measured value excludes a model within the tensor–vector–scalar gravity theory, which modifies both Newtonian and Einstein gravity. However, the relatively large uncertainty still permits models within f() theory, which is an extension of general relativity. A fivefold decrease in uncertainty is needed to rule out these models. [ABSTRACT FROM AUTHOR]

• Layout of the designated cubicle and components dissipation is proposed. • Probe power supply based on a full-bridge converter concept, using a PWM technique is relatively simple and adopted. • Probe operation mode switching strategy was proposed. • Probe measurement signal reference potential and signal conditioning comprehensive design are innovative. An electronics system for Langmuir probes to be used on ITER has been developing. The electronics system should meet the physics measurement requirements, which means that the electronics system should include power supply for driving probes, single and double probes operation mode switching circuit, measurement signal conditioning circuit, control and long cable transmission. It would make sense to use a single power supply to control a probe pair, which could be configured for one of the two operating modes foreseen and reduce costs while minimizing risk. The R&D of power supply is most critical activity. The power supply is characterized by 2.5 A, 175 V rating. At the same time, the power supply has been designed to ensure output waveforms ripple, high frequency, four quadrant and compatibility with the electromagnetic noise close to the components and with the plasma etc., which behaves as a nonlinear rapidly varying load. For reducing risk of R&D and exploring different technical prototype, one of the technical prototypes based on a full-bridge converter concept, using a pulse width modulation (PWM) technique is relatively simple and adopted first. Relays array circuit and adequate voltage and current signal conditioning circuit are also effective guarantee for data acquisitioning and drawing the probe current-voltage characteristic. The main design activities of electronics system are presented as detailed as possible in this paper. Besides, the detailed design activities should be continuously optimized and changed based on the results of the future relevant tests and changed requirements. [ABSTRACT FROM AUTHOR]

Gravitational lensing is a powerful tool for the study of the distribution of dark matter in the Universe. The cold-dark-matter model of the formation of large-scale structures (that is, clusters of galaxies and even larger assemblies) predicts the existence of quasars gravitationally lensed by concentrations of dark matter so massive that the quasar images would be split by over 7?arcsec. Numerous searches for large-separation lensed quasars have, however, been unsuccessful. All of the roughly 70 lensed quasars known, including the first lensed quasar discovered, have smaller separations that can be explained in terms of galaxy-scale concentrations of baryonic matter. Although gravitationally lensed galaxies with large separations are known, quasars are more useful cosmological probes because of the simplicity of the resulting lens systems. Here we report the discovery of a lensed quasar, SDSS J1004 + 4112, which has a maximum separation between the components of 14.62?arcsec. Such a large separation means that the lensing object must be dominated by dark matter. Our results are fully consistent with theoretical expectations based on the cold-dark-matter model. [ABSTRACT FROM AUTHOR]