Showing papers by "University of Portsmouth published in 2014"
University of Chicago1, Lawrence Berkeley National Laboratory2, Pierre-and-Marie-Curie University3, University of Pennsylvania4, Argonne National Laboratory5, Fermilab6, African Institute for Mathematical Sciences7, University of Cape Town8, Texas A&M University9, University of Portsmouth10, University of Cambridge11, University of Toronto12, Wayne State University13, University of Colorado Boulder14, University of Tokyo15, California Institute of Technology16, University of Victoria17, University of California, Berkeley18, University of Illinois at Urbana–Champaign19, University of Chile20, Autonomous University of Barcelona21, Stockholm University22, University of Texas at Austin23, Princeton University24, University of Oxford25, University of California, Santa Barbara26, Las Cumbres Observatory Global Telescope Network27, Rutgers University28, University of Copenhagen29, Australian Astronomical Observatory30, Instituto Superior Técnico31, University of Utah32, Rochester Institute of Technology33, Johns Hopkins University34, Space Telescope Science Institute35, Pennsylvania State University36, University of the Western Cape37, University of Southampton38
TL;DR: In this article, the authors presented cosmological constraints from a joint analysis of type Ia supernova (SN Ia) observations obtained by the SDSS-II and SNLS collaborations.
Abstract: Aims. We present cosmological constraints from a joint analysis of type Ia supernova (SN Ia) observations obtained by the SDSS-II and SNLS collaborations. The dataset includes several low-redshift samples (z< 0.1), all three seasons from the SDSS-II (0.05
1,939 citations
University of Tasmania1, University of Portsmouth2, Stockholm Resilience Centre3, Charles Darwin Foundation4, Spanish National Research Council5, Wildlife Conservation Society6, Department of Water7, Pontifical Catholic University of Valparaíso8, National Park Service9, Federal University of Rio de Janeiro10, Scripps Institution of Oceanography11, University of Auckland12, University of Bologna13
TL;DR: The results show that global conservation targets based on area alone will not optimize protection of marine biodiversity, and more emphasis is needed on better MPA design, durable management and compliance to ensure that MPAs achieve their desired conservation value.
Abstract: In line with global targets agreed under the Convention on Biological Diversity, the number of marine protected areas (MPAs) is increasing rapidly, yet socio-economic benefits generated by MPAs remain difficult to predict and under debate1, 2. MPAs often fail to reach their full potential as a consequence of factors such as illegal harvesting, regulations that legally allow detrimental harvesting, or emigration of animals outside boundaries because of continuous habitat or inadequate size of reserve3, 4, 5. Here we show that the conservation benefits of 87 MPAs investigated worldwide increase exponentially with the accumulation of five key features: no take, well enforced, old (>10 years), large (>100 km2), and isolated by deep water or sand. Using effective MPAs with four or five key features as an unfished standard, comparisons of underwater survey data from effective MPAs with predictions based on survey data from fished coasts indicate that total fish biomass has declined about two-thirds from historical baselines as a result of fishing. Effective MPAs also had twice as many large (>250 mm total length) fish species per transect, five times more large fish biomass, and fourteen times more shark biomass than fished areas. Most (59%) of the MPAs studied had only one or two key features and were not ecologically distinguishable from fished sites. Our results show that global conservation targets based on area alone will not optimize protection of marine biodiversity. More emphasis is needed on better MPA design, durable management and compliance to ensure that MPAs achieve their desired conservation value.
1,355 citations
Christopher P. Ahn1, Rachael M. Alexandroff2, Carlos Allende Prieto3, Carlos Allende Prieto4 +272 more•Institutions (69)
TL;DR: The 10th public data release (DR10) from the Sloan Digital Sky Survey (SDSS-III) was released in 2013 as mentioned in this paper, which includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopy data from Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July.
Abstract: The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R ~ 22,500 300 fiber spectrograph covering 1.514-1.696 μm. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. DR10 includes a total of 1,507,954 BOSS spectra comprising 927,844 galaxy spectra, 182,009 quasar spectra, and 159,327 stellar spectra selected over 6373.2 deg2.
1,188 citations
University of Tokyo1, University of Wisconsin-Madison2, University of Toronto3, University of Kentucky4, University of Texas at Austin5, University of Washington6, University of St Andrews7, University of Portsmouth8, European Southern Observatory9, University of Nottingham10, National Autonomous University of Mexico11, University of Pittsburgh12, University of Cambridge13, New Mexico State University14, Carnegie Institution for Science15, University of Sydney16, New York University17, University of Utah18, University of Oxford19, University of California, Santa Cruz20, Max Planck Society21, Claude Bernard University Lyon 122, École normale supérieure de Lyon23, Texas Christian University24, University of Iowa25, Princeton University26, Case Western Reserve University27, University of La Laguna28, Chinese Academy of Sciences29, Academia Sinica30, University of Manchester31, Macquarie University32, Australian Astronomical Observatory33, Yale University34, Lawrence Berkeley National Laboratory35, University of Potsdam36, University of Victoria37, University of Groningen38
TL;DR: MaNGA (Mapping Nearby Galaxies at Apache Point Observatory) as mentioned in this paper employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12'' (19 fibers) to 32'' (127 fibers).
Abstract: We present an overview of a new integral field spectroscopic survey called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV) that began on 2014 July 1. MaNGA will investigate the internal kinematic structure and composition of gas and stars in an unprecedented sample of 10,000 nearby galaxies. We summarize essential characteristics of the instrument and survey design in the context of MaNGA's key science goals and present prototype observations to demonstrate MaNGA's scientific potential. MaNGA employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12'' (19 fibers) to 32'' (127 fibers). Two dual-channel spectrographs provide simultaneous wavelength coverage over 3600-10300 A at R ~ 2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 (A–1 per 2'' fiber) at 23 AB mag arcsec–2, which is typical for the outskirts of MaNGA galaxies. Targets are selected with M * 109 M ☉ using SDSS-I redshifts and i-band luminosity to achieve uniform radial coverage in terms of the effective radius, an approximately flat distribution in stellar mass, and a sample spanning a wide range of environments. Analysis of our prototype observations demonstrates MaNGA's ability to probe gas ionization, shed light on recent star formation and quenching, enable dynamical modeling, decompose constituent components, and map the composition of stellar populations. MaNGA's spatially resolved spectra will enable an unprecedented study of the astrophysics of nearby galaxies in the coming 6 yr.
1,104 citations
ETH Zurich1, Yale University2, University of Oxford3, University of Minnesota4, University of Hertfordshire5, University of Alabama6, Adler Planetarium7, University of Portsmouth8, University of California, San Diego9, University of Concepción10, Commonwealth Scientific and Industrial Research Organisation11, Yonsei University12
TL;DR: In this article, the authors use SDSS+GALEX+Galaxy Zoo data to study the quenching of star formation in low-redshift galaxies and conclude that the green valley between the blue cloud of star-forming galaxies and the red sequence of quiescent galaxies in the colour-mass diagram is not a single transitional state through which most blue galaxies evolve into red galaxies.
Abstract: We use SDSS+GALEX+Galaxy Zoo data to study the quenching of star formation in low-redshift galaxies. We show that the green valley between the blue cloud of star-forming galaxies and the red sequence of quiescent galaxies in the colour-mass diagram is not a single transitional state through which most blue galaxies evolve into red galaxies. Rather, an analysis that takes morphology into account makes clear that only a small population of blue early-type galaxies move rapidly across the green valley after the morphologies are transformed from disc to spheroid and star formation is quenched rapidly. In contrast, the majority of blue star-forming galaxies have significant discs, and they retain their late-type morphologies as their star formation rates decline very slowly. We summarize a range of observations that lead to these conclusions, including UV-optical colours and halo masses, which both show a striking dependence on morphological type. We interpret these results in terms of the evolution of cosmic gas supply and gas reservoirs. We conclude that late-type galaxies are consistent with a scenario where the cosmic supply of gas is shut off, perhaps at a critical halo mass, followed by a slow exhaustion of the remaining gas over several Gyr, driven by secular and/or environmental processes. In contrast, early-type galaxies require a scenario where the gas supply and gas reservoir are destroyed virtually instantaneously, with rapid quenching accompanied by a morphological transformation from disc to spheroid. This gas reservoir destruction could be the consequence of a major merger, which in most cases transforms galaxies from disc to elliptical morphology, and mergers could play a role in inducing black hole accretion and possibly active galactic nuclei feedback.
629 citations
TL;DR: In this paper, the authors analyzed the anisotropic clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 (DR11) sample, which consists of 690 827 galaxies in the redshift range 0.43 ± 0.7 and has a sky coverage of 8498 deg^2.
Abstract: We analyse the anisotropic clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 (DR11) sample, which consists of 690 827 galaxies in the redshift range 0.43 < z < 0.7 and has a sky coverage of 8498 deg^2. We perform our analysis in Fourier space using a power spectrum estimator suggested by Yamamoto et al. We measure the multipole power spectra in a self-consistent manner for the first time in the sense that we provide a proper way to treat the survey window function and the integral constraint, without the commonly used assumption of an isotropic power spectrum and without the need to split the survey into subregions. The main cosmological signals exploited in our analysis are the baryon acoustic oscillations and the signal of redshift space distortions, both of which are distorted by the Alcock–Paczynski effect. Together, these signals allow us to constrain the distance ratio D_V(z_eff)/r_s(z_d) = 13.89 ± 0.18, the Alcock–Paczynski parameter F_AP(z_eff) = 0.679 ± 0.031 and the growth rate of structure f (z_eff)σ_8(z_eff) = 0.419 ± 0.044 at the effective redshift z_eff = 0.57. We emphasize that our constraints are robust against possible systematic uncertainties. In order to ensure this, we perform a detailed systematics study against CMASS mock galaxy catalogues and N-body simulations. We find that such systematics will lead to 3.1 per cent uncertainty for fσ_8 if we limit our fitting range to k = 0.01–0.20 h Mpc^−1, where the statistical uncertainty is expected to be three times larger. We did not find significant systematic uncertainties for D_V/r_s or F_AP. Combining our data set with Planck to test General Relativity (GR) through the simple γ-parametrization, where the growth rate is given by $f(z) = \Omega ^{\gamma }_{\rm m}(z)$, reveals a ∼2σ tension between the data and the prediction by GR. The tension between our result and GR can be traced back to a tension in the clustering amplitude σ_8 between CMASS and Planck.
325 citations
TL;DR: The RTI-IB facilitates a more complete quality assessment than the NOS but is more burdensome; the observed agreement and AC1 statistic in this study were higher than those reported by the RTI’s developers.
Abstract: Background
The study objective was to compare the Newcastle–Ottawa Scale (NOS) and the RTI item bank (RTI-IB) and estimate interrater agreement using the RTI-IB within a systematic review on the cardiovascular safety of glucose-lowering drugs.
313 citations
Institute of Cosmology and Gravitation, University of Portsmouth1, Abastumani Astrophysical Observatory2, Lawrence Berkeley National Laboratory3, University of California, Berkeley4, University of Barcelona5, Yale University6, University of Portsmouth7, University College London8, Paris Diderot University9, New Mexico State University10, University of Utah11, Harvard University12, Carnegie Mellon University13, Ohio State University14, Max Planck Society15, Drexel University16, Pennsylvania State University17, Spanish National Research Council18, University of La Laguna19, New York University20, Open University21, University of Wisconsin-Madison22, Case Western Reserve University23
TL;DR: In this paper, the authors used the observed anisotropic clustering of galaxies in the Baryon Oscillation Spectroscopic Survey Data Release 11 CMASS sample to measure the linear growth rate of structure, the Hubble expansion rate and the comoving distance scale.
Abstract: We use the observed anisotropic clustering of galaxies in the Baryon Oscillation Spectroscopic Survey Data Release 11 CMASS sample to measure the linear growth rate of structure, the Hubble expansion rate and the comoving distance scale. Our sample covers 8498 deg2 and encloses an effective volume of 6 Gpc3 at an effective redshift of z¯=0.57. We find fσ8 = 0.441 ± 0.044, H = 93.1 ± 3.0 km s−1 Mpc−1 and DA = 1380 ± 23 Mpc when fitting the growth and expansion rate simultaneously. When we fix the background expansion to the one predicted by spatially flat Λ cold dark matter (ΛCDM) model in agreement with recent Planck results, we find fσ8 = 0.447 ± 0.028 (6 per cent accuracy). While our measurements are generally consistent with the predictions of ΛCDM and general relativity, they mildly favour models in which the strength of gravitational interactions is weaker than what is predicted by general relativity. Combining our measurements with recent cosmic microwave background data results in tight constraints on basic cosmological parameters and deviations from the standard cosmological model. Separately varying these parameters, we find w = −0.983 ± 0.075 (8 per cent accuracy) and γ = 0.69 ± 0.11 (16 per cent accuracy) for the effective equation of state of dark energy and the growth rate index, respectively. Both constraints are in good agreement with the standard model values of w = −1 and γ = 0.554.
306 citations
INAF1, University of Milan2, Aix-Marseille University3, Roma Tre University4, University of Nice Sophia Antipolis5, Academia Sinica6, University of Geneva7, University of Bologna8, University of Edinburgh9, Institut d'Astrophysique de Paris10, Jan Kochanowski University11, Nagoya University12, Jagiellonian University13, Max Planck Society14, University of Portsmouth15
TL;DR: The VIMOS Public Extragalactic Redshift Survey (VIPERS) as discussed by the authors was designed to address a broad range of problems in large-scale structure and galaxy evolution, thanks to a unique combination of volume and sampling rate, comparable to state-of-the-art surveys of the local Universe, together with extensive multi-band optical and near-infrared photometry.
Abstract: We describe the construction and general features of VIPERS, the VIMOS Public Extragalactic Redshift Survey. This `Large Programme' has been using the ESO VLT with the aim of building a spectroscopic sample of ~100,000 galaxies with i_{AB}<22.5 and 0.5
304 citations
TL;DR: It is proposed that a gold standard deep-body temperature does not exist and the validity of each measurement must be evaluated relative to one's research objectives, whilst satisfying equilibration and positioning requirements.
298 citations
University of Chile1, Centre national de la recherche scientifique2, Lawrence Berkeley National Laboratory3, Max Planck Society4, University of Wyoming5, University of La Laguna6, York University7, Princeton University8, University of Washington9, New Mexico State University10, Pennsylvania State University11, University of Utah12, University of Arizona13, Erciyes University14, University of Zurich15, University of Florida16, University of Cambridge17, Carnegie Mellon University18, University of Barcelona19, Ohio State University20, University of Portsmouth21, Universidade Federal do Rio Grande do Sul22, New York University23, University of Pittsburgh24, University of Chicago25
TL;DR: The Data Release 10 Quasar (DR10Q) catalog from the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey III as discussed by the authors includes all BOSS objects that were targeted as quasar candidates during the first 2.5 years of the survey and that are confirmed as quasars via visual inspection of the spectra.
Abstract: We present the Data Release 10 Quasar (DR10Q) catalog from the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey III. The catalog includes all BOSS objects that were targeted as quasar candidates during the first 2.5 years of the survey and that are confirmed as quasars via visual inspection of the spectra, have luminosities M i [z = 2] 0 = 70 km s-1 Mpc-1 , ΩM = 0.3, and ΩΛ = 0.7), and either display at least one emission line with a full width at half maximum (FWHM) larger than 500 km s-1 or, if not, have interesting/complex absorption features. The catalog also includes known quasars (mostly from SDSS-I and II) that were reobserved by BOSS. The catalog contains 166 583 quasars (74 454 are new discoveries since SDSS-DR9) detected over 6373 deg2 with robust identification and redshift measured by a combination of principal component eigenspectra. The number of quasars with z > 2.15 (117 668) is ~5 times greater than the number of z > 2.15 quasars known prior to BOSS. Redshifts and FWHMs are provided for the strongest emission lines (C iv, C iii, Mg ii). The catalog identifies 16 461 broad absorption line quasars and gives their characteristics. For each object, the catalog presents five-band (u , g , r , i , z ) CCD-based photometry with typical accuracy of 0.03 mag and information on the optical morphology and selection method. The catalog also contains X-ray, ultraviolet, near-infrared, and radio emission properties of the quasars, when available, from other large-area surveys. The calibrated digital spectra cover the wavelength region 3600−10 500 A at a spectral resolution in the range 1300 < 2500; the spectra can be retrieved from the SDSS Catalog Archive Server. We also provide a supplemental list of an additional 2376 quasars that have been identified among the galaxy targets of the SDSS-III/BOSS.
University of Washington1, University of Paris2, Lawrence Berkeley National Laboratory3, University of Utah4, New Mexico State University5, Autonomous University of Madrid6, Yale University7, Harvard University8, Carnegie Mellon University9, Ohio State University10, Swinburne University of Technology11, University of California, Irvine12, University of Portsmouth13, Spanish National Research Council14, Max Planck Society15, Institute of Cosmology and Gravitation, University of Portsmouth16, Abastumani Astrophysical Observatory17, Pennsylvania State University18, Princeton University19, New York University20, University of Barcelona21, University of Wisconsin-Madison22
TL;DR: In this article, the angular diameter distance to and Hubble parameter at z = 0:57 from the measurement of the baryon acoustic peak in the correlation of galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey was measured.
Abstract: We present measurements of the angular diameter distance to and Hubble parameter at z = 0:57 from the measurement of the baryon acoustic peak in the correlation of galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey. Our analysis is based on a sample from Data Release 9 of 264,283 galaxies over 3275 square degrees in the redshift range 0:43 < z < 0:70. We use two different methods to provide robust measurement of the acoustic peak position across and along the line of sight in order to measure the cosmological distance scale. We find DA(0:57) = 1408 45 Mpc and H(0:57) = 92:9 7:8 km/s/Mpc for our fiducial value of the sound horizon. These results from the anisotropic fitting are fully consistent with the analysis of the spherically averaged acoustic peak position presented in Anderson et al. (2012). Our distance measurements are a close match to the predictions of the standard cosmological model featuring a cosmological constant and zero spatial curvature.
University of Tokyo1, University of Wisconsin-Madison2, University of Toronto3, University of Kentucky4, University of Texas at Austin5, University of Washington6, University of St Andrews7, University of Portsmouth8, European Southern Observatory9, University of Nottingham10, National Autonomous University of Mexico11, University of Pittsburgh12, University of Cambridge13, New Mexico State University14, Carnegie Institution for Science15, University of Sydney16, New York University17, University of Utah18, University of Oxford19, University of California, Santa Cruz20, Max Planck Society21, Claude Bernard University Lyon 122, École normale supérieure de Lyon23, Texas Christian University24, University of Iowa25, Princeton University26, Case Western Reserve University27, University of La Laguna28, Chinese Academy of Sciences29, Academia Sinica30, University of Manchester31, Australian Astronomical Observatory32, Macquarie University33, Yale University34, Lawrence Berkeley National Laboratory35, University of Potsdam36, University of Victoria37, University of Groningen38
TL;DR: MaNGA (Mapping Nearby Galaxies at Apache Point Observatory) as discussed by the authors employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12" (19 fibers) to 32" (127 fibers).
Abstract: We present an overview of a new integral field spectroscopic survey called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV) that began on 2014 July 1. MaNGA will investigate the internal kinematic structure and composition of gas and stars in an unprecedented sample of 10,000 nearby galaxies. We summarize essential characteristics of the instrument and survey design in the context of MaNGA's key science goals and present prototype observations to demonstrate MaNGA's scientific potential. MaNGA employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12" (19 fibers) to 32" (127 fibers). Two dual-channel spectrographs provide simultaneous wavelength coverage over 3600-10300 A at R~2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 (per A, per 2" fiber) at 23 AB mag per sq. arcsec, which is typical for the outskirts of MaNGA galaxies. Targets are selected with stellar mass greater than 1e9 Msun using SDSS-I redshifts and i-band luminosity to achieve uniform radial coverage in terms of the effective radius, an approximately flat distribution in stellar mass, and a sample spanning a wide range of environments. Analysis of our prototype observations demonstrates MaNGA's ability to probe gas ionization, shed light on recent star formation and quenching, enable dynamical modeling, decompose constituent components, and map the composition of stellar populations. MaNGA's spatially resolved spectra will enable an unprecedented study of the astrophysics of nearby galaxies in the coming 6 yr.
TL;DR: If antidepressants affect aquatic invertebrates at concentrations currently found in the environment, there is strong evidence to suggest the answer is yes, and compelling evidence that the effects could be quite multifaceted across a variety of biological systems.
INAF1, University of Milan2, Aix-Marseille University3, Roma Tre University4, Academia Sinica5, University of Bologna6, University of Edinburgh7, Jan Kochanowski University8, Nagoya University9, Institut d'Astrophysique de Paris10, Max Planck Society11, University of Portsmouth12, North Carolina State University13
TL;DR: The first public data release (PDR-1) of the VIMOS Public Extragalactic Survey (VIPERS) is presented in this paper, which comprises 57 204 spectroscopic measurements together with all additional information necessary for optimal scientific exploitation of the data, in particular the associated photometric measurements and quantification of the photometric completeness.
Abstract: We present the first Public Data Release (PDR-1) of the VIMOS Public Extragalactic Survey (VIPERS). It comprises 57 204 spectroscopic measurements together with all additional information necessary for optimal scientific exploitation of the data, in particular the associated photometric measurements and quantification of the photometric and survey completeness. VIPERS is an ESO Large Programme designed to build a spectroscopic sample of ' 100 000 galaxies with iAB < 22.5 and 0.5 < z < 1.5 with high sampling rate (~45%). The survey spectroscopic targets are selected from the CFHTLS-Wide five-band catalogues in the W1 and W4 fields. The final survey will cover a total area of nearly 24 deg2, for a total comoving volume between z = 0.5 and 1.2 of ~4x10^7 h^(-3)Mpc^3 and a median galaxy redshift of z~0.8. The release presented in this paper includes data from virtually the entire W4 field and nearly half of the W1 area, thus representing 64% of the final dataset. We provide a detailed description of sample selection, observations and data reduction procedures; we summarise the global properties of the spectroscopic catalogue and explain the associated data products and their use, and provide all the details for accessing the data through the survey database (http://vipers.inaf.it) where all information can be queried interactively.
TL;DR: In this paper, a consistent theory for a self-interacting vector field, breaking an Abelian symmetry in such a way to obtain an interesting behavior for its longitudinal polarization, was discussed.
Abstract: We discuss a consistent theory for a self-interacting vector field, breaking an Abelian symmetry in such a way to obtain an interesting behavior for its longitudinal polarization. In an appropriate decoupling limit, the dynamics of the longitudinal mode is controlled by Galileon interactions. The full theory away from the decoupling limit does not propagate ghost modes, and can be investigated in regimes where non-linearities become important. When coupled to gravity, this theory provides a candidate for dark energy, since it admits de Sitter cosmological solutions characterized by a technically natural value for the Hubble parameter. We also consider the homogeneous evolution when, besides the vector, additional matter in the form of perfect fluids is included. We find that the vector can have an important role in characterizing the universe expansion.
TL;DR: It is suggested that care be invested in relating measurement to underlying theory or hypotheses, and that summative, theory-free descriptors of integration generally be avoided.
Abstract: Integration and modularity refer to the patterns and processes of trait interaction and independence. Both terms have complex histories with respect to both conceptualization and quantification, resulting in a plethora of integration indices in use. We review briefly the divergent definitions, uses and measures of integration and modularity and make conceptual links to allometry. We also discuss how integration and modularity might evolve. Although integration is generally thought to be generated and maintained by correlational selection, theoretical considerations suggest the relationship is not straightforward. We caution here against uncontrolled comparisons of indices across studies. In the absence of controls for trait number, dimensionality, homology, development and function, it is difficult, or even impossible, to compare integration indices across organisms or traits. We suggest that care be invested in relating measurement to underlying theory or hypotheses, and that summative, theory-free descriptors of integration generally be avoided. The papers that follow in this Theme Issue illustrate the diversity of approaches to studying integration and modularity, highlighting strengths and pitfalls that await researchers investigating integration in plants and animals.
TL;DR: In this article, the authors present details of the construction and characterization of the coaddition of the Sloan Digital Sky Survey (SDSS) Stripe 82 ugriz imaging data, which consists of 275 deg2 of repeated scanning by the SDSS camera over −50° ≤ α ≤ 60° and −125 ≤ δ ≤ +125 centered on the Celestial Equator.
Abstract: We present details of the construction and characterization of the coaddition of the Sloan Digital Sky Survey (SDSS) Stripe 82 ugriz imaging data. This survey consists of 275 deg2 of repeated scanning by the SDSS camera over –50° ≤ α ≤ 60° and –125 ≤ δ ≤ +125 centered on the Celestial Equator. Each piece of sky has ~20 runs contributing and thus reaches ~2 mag fainter than the SDSS single pass data, i.e., to r ~ 23.5 for galaxies. We discuss the image processing of the coaddition, the modeling of the point-spread function (PSF), the calibration, and the production of standard SDSS catalogs. The data have an r-band median seeing of 11 and are calibrated to ≤1%. Star color-color, number counts, and PSF size versus modeled size plots show that the modeling of the PSF is good enough for precision five-band photometry. Structure in the PSF model versus magnitude plot indicates minor PSF modeling errors, leading to misclassification of stars as galaxies, as verified using VVDS spectroscopy. There are a variety of uses for this wide-angle deep imaging data, including galactic structure, photometric redshift computation, cluster finding and cross wavelength measurements, weak lensing cluster mass calibrations, and cosmic shear measurements.
University of Otago1, Stonehill College2, Mount Saint Vincent University3, University of Würzburg4, State University of New York at Brockport5, University of Nebraska–Lincoln6, Erasmus University Rotterdam7, Università degli Studi Suor Orsola Benincasa8, University of Leeds9, George Fox University10, Texas A&M University–Commerce11, University of Social Sciences and Humanities12, Lehigh Carbon Community College13, University of Warwick14, Flinders University15, University of Münster16, Rochester Institute of Technology17, University of Virginia18, Victoria University of Wellington19, Goldsmiths, University of London20, University of North Dakota21, College of Charleston22, University of Stirling23, Kent State University24, University of Tasmania25, University of Oxford26, University of Düsseldorf27, Ohio State University28, University of Central Lancashire29, University of Maine30, Iowa State University31, Nebraska Wesleyan University32, University of Navarra33, University of Wyoming34, Masaryk University35, University of Portsmouth36, University of Texas at El Paso37, Niagara University38, Charles University in Prague39, Arkansas State University40
TL;DR: This article found that participants who described the robber were 25% worse at identifying the robber in a lineup than were participants who instead listed U.S. states and capitals, which has been termed the verbal overshadowing effect.
Abstract: Trying to remember something now typically improves your ability to remember it later. However, after watching a video of a simulated bank robbery, participants who verbally described the robber were 25% worse at identifying the robber in a lineup than were participants who instead listed U.S. states and capitals—this has been termed the “verbal overshadowing” effect (Schooler & Engstler-Schooler, 1990). More recent studies suggested that this effect might be substantially smaller than first reported. Given uncertainty about the effect size, the influence of this finding in the memory literature, and its practical importance for police procedures, we conducted two collections of preregistered direct replications (RRR1 and RRR2) that differed only in the order of the description task and a filler task. In RRR1, when the description task immediately followed the robbery, participants who provided a description were 4% less likely to select the robber than were those in the control condition. In RRR2, when the description was delayed by 20 min, they were 16% less likely to select the robber. These findings reveal a robust verbal overshadowing effect that is strongly influenced by the relative timing of the tasks. The discussion considers further implications of these replications for our understanding of verbal overshadowing.
TL;DR: The authors used the latest generation of 3D printer to create a model, with an inbuilt pathological entity, of varying consistency and density, which was able to take trainees through the basic steps of neurosurgical procedures, from navigation and planning of skin flap to performing initial steps in a craniotomy and simple tumor excision.
Abstract: The advent of multimaterial 3D printers allows the creation of neurosurgical models of a more realistic nature, mimicking real tissues. The authors used the latest generation of 3D printer to create a model, with an inbuilt pathological entity, of varying consistency and density. Using this model the authors were able to take trainees through the basic steps, from navigation and planning of skin flap to performing initial steps in a craniotomy and simple tumor excision. As the technology advances, models of this nature may be able to supplement the training of neurosurgeons in a simulated operating theater environment, thus improving the training experience.
TL;DR: In this article, a consistent theory for a self-interacting vector field, breaking an Abelian symmetry in such a way to obtain an interesting behavior for its longitudinal polarization, was discussed.
Abstract: We discuss a consistent theory for a self-interacting vector field, breaking an Abelian symmetry in such a way to obtain an interesting behavior for its longitudinal polarization. In an appropriate decoupling limit, the dynamics of the longitudinal mode is controlled by Galileon interactions. The full theory away from the decoupling limit does not propagate ghost modes, and can be investigated in regimes where non-linearities become important. When coupled to gravity, this theory provides a candidate for dark energy, since it admits de Sitter cosmological solutions characterized by a technically natural value for the Hubble parameter. We also consider the homogeneous evolution when, besides the vector, additional matter in the form of perfect fluids is included. We find that the vector can have an important role in characterizing the universe expansion.
University of Chicago1, Lawrence Berkeley National Laboratory2, Pierre-and-Marie-Curie University3, University of Pennsylvania4, Argonne National Laboratory5, Fermilab6, African Institute for Mathematical Sciences7, University of Cape Town8, Texas A&M University9, University of Cambridge10, University of Portsmouth11, University of Toronto12, Wayne State University13, University of Colorado Boulder14, University of Tokyo15, California Institute of Technology16, University of Victoria17, University of California, Berkeley18, University of Illinois at Urbana–Champaign19, University of Chile20, Autonomous University of Barcelona21, Stockholm University22, University of Texas at Austin23, Princeton University24, University of Oxford25, Las Cumbres Observatory Global Telescope Network26, University of California, Santa Barbara27, Rutgers University28, University of Copenhagen29, Australian Astronomical Observatory30, Instituto Superior Técnico31, University of Utah32, Rochester Institute of Technology33, Johns Hopkins University34, Space Telescope Science Institute35, Pennsylvania State University36, University of the Western Cape37, University of Southampton38
TL;DR: In this article, cosmological constraints from a joint analysis of type Ia supernova (SN Ia) observations obtained by the SDSS-II and SNLS collaborations are presented.
Abstract: We present cosmological constraints from a joint analysis of type Ia supernova (SN Ia) observations obtained by the SDSS-II and SNLS collaborations. The data set includes several low-redshift samples (z<0.1), all 3 seasons from the SDSS-II (0.05 < z < 0.4), and 3 years from SNLS (0.2
Lawrence Berkeley National Laboratory1, Institute for the Physics and Mathematics of the Universe2, University of Tokyo3, University of Utah4, Autonomous University of Madrid5, University of Barcelona6, University of Portsmouth7, Drexel University8, Pennsylvania State University9, Max Planck Society10, Ohio State University11, New York University12
TL;DR: In this paper, the robustness of the cosmological constraints from the baryon acoustic oscillation (BAO) scale, the Alcock-Paczynski effect and redshift-space distortions (DV/rs, FAP, fsigma8) of Beutler et al., when introducing a neutrino mass in the power spectrum template was examined.
Abstract: We investigate the cosmological implications of the latest growth of structure measurement from the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 with particular focus on the sum of the neutrino masses, ∑mnu. We examine the robustness of the cosmological constraints from the baryon acoustic oscillation (BAO) scale, the Alcock-Paczynski effect and redshift-space distortions (DV/rs, FAP, fsigma8) of Beutler et al., when introducing a neutrino mass in the power spectrum template. We then discuss how the neutrino mass relaxes discrepancies between the cosmic microwave background (CMB) and other low-redshift measurements within Lambda cold dark matter. Combining our cosmological constraints with 9-year Wilkinson Microwave Anisotropy Probe (WMAP9) yields ∑mnu = 0.36 ± 0.14 eV (68 per cent c.l.), which represents a 2.6sigma preference for non-zero neutrino mass. The significance can be increased to 3.3sigma when including weak lensing results and other BAO constraints, yielding ∑mnu = 0.35 ± 0.10 eV (68 per cent c.l.). However, combining CMASS with Planck data reduces the preference for neutrino mass to ?2sigma. When removing the CMB lensing effect in the Planck temperature power spectrum (by marginalizing over AL), we see shifts of ?1sigma in sigma8 and Omegam, which have a significant effect on the neutrino mass constraints. In the case of CMASS plus Planck without the AL lensing signal, we find a preference for a neutrino mass of ∑mnu = 0.34 ± 0.14 eV (68 per cent c.l.), in excellent agreement with the WMAP9+CMASS value. The constraint can be tightened to 3.4sigma yielding ∑mnu = 0.36 ± 0.10 eV (68 per cent c.l.) when weak lensing data and other BAO constraints are included.
TL;DR: Adaptations for a semiaquatic lifestyle in the dinosaur Spinosaurus aegyptiacus are described, including retraction of the fleshy nostrils to a position near the mid-region of the skull and an elongate neck and trunk that shift the center of body mass anterior to the knee joint.
Abstract: We describe adaptations for a semiaquatic lifestyle in the dinosaur Spinosaurus aegyptiacus. These adaptations include retraction of the fleshy nostrils to a position near the mid-region of the skull and an elongate neck and trunk that shift the center of body mass anterior to the knee joint. Unlike terrestrial theropods, the pelvic girdle is downsized, the hindlimbs are short, and all of the limb bones are solid without an open medullary cavity, for buoyancy control in water. The short, robust femur with hypertrophied flexor attachment and the low, flat-bottomed pedal claws are consistent with aquatic foot-propelled locomotion. Surface striations and bone microstructure suggest that the dorsal “sail” may have been enveloped in skin that functioned primarily for display on land and in water.
TL;DR: The anisotropic electronic densities of covalently-bonded Group IV-VII atoms frequently give rise to regions of positive electrostatic potential on the extensions ofcovalent bonds to these atoms, through which positive "σ-holes" can interact attractively and highly directionally with negative sites.
Abstract: The anisotropic electronic densities of covalently-bonded Group IV–VII atoms frequently give rise to regions of positive electrostatic potential on the extensions of covalent bonds to these atoms. Through such positive “σ-holes,” the atoms can interact attractively and highly directionally with negative sites such as the lone pairs of Lewis bases, anions, π electrons, etc. In the case of Group VII this is called “halogen bonding.” Hydrogen bonding can be viewed as a less directional subset of σ-hole interactions. Since positive σ-holes often exist in conjunction with regions of negative potential, the atoms can also interact favorably with positive sites. In accordance with the Hellmann–Feynman theorem, all of these interactions are purely Coulombic in nature (which encompasses polarization and dispersion). The strength of σ-hole bonding increases with the magnitudes of the potentials of the positive σ-hole and the negative site; their polarizabilities must sometimes also be taken explicitly into account.
TL;DR: The findings suggest that emotional self-regulation resource impairment affects perceived exertion, pacing and sport performance and extends previous research examining the regulation of persistence on physical tasks.
Abstract: This study used a single-blind, within-participant, counterbalanced, repeated-measures design to examine the relationship between emotional self-regulation and sport performance. Twenty competitive athletes completed four laboratory-based conditions; familiarization, control, emotion suppression, and nonsuppression. In each condition participants completed a 10-km cycling time trial requiring self-regulation. In the experimental conditions participants watched an upsetting video before performing the cycle task. When participants suppressed their emotional reactions to the video (suppression condition) they completed the cycling task slower, generated lower mean power outputs, and reached a lower maximum heart rate and perceived greater physical exertion than when they were given no self-regulation instructions during the video (nonsuppression condition) and received no video treatment (control condition). The findings suggest that emotional self-regulation resource impairment affects perceived exertion, pacing and sport performance and extends previous research examining the regulation of persistence on physical tasks. The results are discussed in line with relevant psychophysiological theories of self-regulation and fatigue and pertinent potential implications for practice regarding performance and well-being are suggested.
TL;DR: It is shown that mangrove forests are strong candidates for PES projects, particularly well suited to the generation of carbon credits, because of their unrivaled potential as carbon sinks, their resistance and resilience to natural hazards, and their extensive provision of Ecosystem Services other than carbon sequestration.
Abstract: In this review paper, we aim to describe the potential for, and the key challenges to, applying PES projects to mangroves. By adopting a “carbocentric approach,” we show that mangrove forests are strong candidates for PES projects. They are particularly well suited to the generation of carbon credits because of their unrivaled potential as carbon sinks, their resistance and resilience to natural hazards, and their extensive provision of Ecosystem Services other than carbon sequestration, primarily nursery areas for fish, water purification and coastal protection, to the benefit of local communities as well as to the global population. The voluntary carbon market provides opportunities for the development of appropriate protocols and good practice case studies for mangroves at a small scale, and these may influence larger compliance schemes in the future. Mangrove habitats are mostly located in developing countries on communally or state-owned land. This means that issues of national and local governance, land ownership and management, and environmental justice are the main challenges that require careful planning at the early stages of mangrove PES projects to ensure successful outcomes and equitable benefit sharing within local communities.
Electronic supplementary material
The online version of this article (doi:10.1007/s13280-014-0530-y) contains supplementary material, which is available to authorized users.
TL;DR: A new hybrid method based on AHP and the K-means algorithm is introduced: AHP-K-Veto, which provides a clearly higher clustering validity index than previous sorting methods, but is a full compensatory method.
TL;DR: Fluoxetine and sertraline have a significant impact on the behaviour and neurophysiology of this amphipod at environmentally relevant concentrations with effects observed after relatively short periods of time.
TL;DR: In this article, the authors examined the hypothesis that liars will report their activities strategically and will, if possible, avoid mentioning details that can be verified by the investigator, and they compared their verifiability approach with other theoretical approaches as to why differences in detail between truth tellers and liars emerge.
Abstract: Background We examined the hypothesis that liars will report their activities strategically and will, if possible, avoid mentioning details that can be verified by the investigator. Method A total of 38 participants wrote a statement in which they told the truth or lied about their activities during a recent 30-minute period. Two coders counted the frequency of occurrence of details that can be verified and that cannot be verified. Results Liars, compared with truth tellers, included fewer details that can be verified and an equal number of details that cannot be verified in their statement, and the ratio between verifiable and unverifiable details was smaller in liars compared with truth tellers. High percentages of truth tellers and liars were classified correctly based on the frequency counting of verifiable details (79%) or the ratio between verifiable and unverifiable details (71%). Those percentages were higher than the percentage that could be classified correctly (63%) based on verifiable and unverifiable detail combined. We compared our verifiability approach with other theoretical approaches as to why differences in detail between truth tellers and liars emerge.