bluuebunny/crossref_metadata_2025_split huggingface dataset:
Convict Labor in Turkey, 1936–1953: A Capitalist Corporation in the State?
Authors: Sipahi Ali 
Published: October 2016

AbstractThe article proposes the institutional analysis of convict labor as an alternative to both (profit-oriented) economic and (discipline-oriented) political explanations. The specialized labor-based prisons in Turkey from 1936 to 1953 are brought to light by archival research and are presented here as a rich case to discuss the experiential/subjective conditions of unfree labor regimes and the structural effects of institutions on the convicts’ experiences. I argue that the state department responsible for prison labor in Turkey was transformed into a capitalist corporation with bureaucratic management, and the target of convict labor system was neither profit nor discipline, but the creation of the corporate bureaucracy itself. As a consequence, both for prisoners and for the prison staff, labor-based prisons appeared as privileged places. Hence, unfree labor was volunteered.
Definitely Not Moralistic: State Political Culture and Support for Donald Trump in the Race for the 2016 Republican Presidential Nomination
Authors: Fisher Patrick I. 
Published: October 2016

ABSTRACTThis study analyzes the important role state political culture played in the race for the 2016 Republican presidential nomination. Donald Trump appealed to demographically distinct types of voters in the 2016 Republican presidential primaries and caucuses that varied considerably from previous Republican presidential nominees. Relative to the demographics of the primary electorates, however, this study finds that state political culture played an outsized role in determining Donald Trump’s relative level of support in a particular state. When state demographics are utilized in ordinary least squares regression models as independent variables with state partisanship and Daniel Elazar’s state political culture typology, political culture proves to be a significant determinant of the level of support given to Trump in a state. States that are characterized by a more moralistic political culture are considerably more likely to have given Trump a lower share of the vote while voters in states that are characterized by a more traditionalistic or individualistic culture were more likely to support Trump.
Becoming a Stop on the Road to the White House: Using a University Protocol to Govern Candidate Visits
Authors: Kedrowski Karen M. , Moyon Katarina Duich 
Published: October 2016

ABSTRACTWinthrop University capitalized upon South Carolina’s early presidential primary to bring 10 US Presidential candidates to campus between August 2015 and February 2016. These events are part of Winthrop University’s intentional commitment to civic engagement. This essay describes and analyzes how Winthrop University developed a campus-wide protocol for hosting visits by public officials and candidates. It also provides best practices that campuses may emulate in future election cycles.
The next generation
Authors: CHURCH KENNETH WARD 
Published: October 2016

AbstractI’m sure you want me to tell you about the next new emerging trend, but I’m not going to do that. It is much easier to suggest where trends come from (the next generation), and how to distinguish passing fads (bubbles) from emerging trends. Young people are often the early adopters, the first to see what is about to happen, but most people don’t see what’s coming until well after the fact. Those with the most to lose (the establishment) tend to be the most resistant to change.
Mis-estimation risk: measurement and impact
Authors: Richards S. J. 
Published: October 2016

AbstractWhen deriving a demographic basis from experience data it is useful to know (i) what uncertainty surrounds that basis, and (ii) the financial impact of that uncertainty. Under the Solvency II regime in the EU, insurers must hold capital against a number of risks. One of these is mis-estimation risk, i.e. the uncertainty over the current rates of mortality and other biometric risks experienced by a portfolio. We propose a general method for assessing mis-estimation risk, and by way of illustration we look at how mis-estimation risk can be assessed for a portfolio of pensions in payment from a UK pension scheme. We find that the impact of mis-estimation risk varies according to the risk factors included in a model, and that the inclusion of some necessary risk factors increases the financial impact of mis-estimation risk. In particular, the inclusion of risk factors which improve the model’s fit and financial applicability can lead to an increase in the mis-estimation risk. We also find that a full-portfolio valuation is preferable to using model points when assessing mis-estimation risk.
Zeldovich's legacy in the Discovery and Understanding of the Cosmic Web
Authors: Shandarin Sergei F. 
Published: October 2016

AbstractModeling and understanding the structure of the universe is one the most interesting problems in modern cosmology. It is also an extremely difficult problem. Despite spectacular achievements in observations and computational capabilities at present there is no comprehensive theory of the structure formation. There are successful theoretical models however most of them rely on assumptions and various fits which are not fully physically justified. The Zeldovich Approximation is a rare exception. Suggested more than forty years ago it remains one of the most successful and profound analytic models of structure formation. Some of results stemmed from the Zeldovich Approximation will be briefly reviewed.
Why Planck (the Satellite) could have been Zel'dovich
Authors: Partridge Bruce 
Published: October 2016

AbstractIn this brief paper, I cannot provide an overall review of the Planck results to date. Instead I will focus on a handful of results from both Planck and related cosmic microwave background (CMB) experiments that reflect Ya. B. Zel'dovich's legacy in cosmology. These include the Sunyaev-Zel'dovich effect in clusters of galaxies and in the cosmic web, and a map of the overall distribution of mass in the Universe derived from CMB maps.
Understanding the cosmic web
Authors: Cautun Marius , van de Weygaert Rien , Jones Bernard J. T. , Frenk Carlos S. 
Published: October 2016

AbstractWe investigate the characteristics and the time evolution of the cosmic web from redshift,z=2, to present time, within the framework of the \nexus{} algorithm. This necessitates the introduction of new analysis tools optimally suited to describe the very intricate and hierarchical pattern that is the cosmic web. In particular, we characterising filaments (walls) in terms of their linear (surface) mass density, which is very good in capturing the evolution of these structures. At early times the cosmos is dominated by tenuous filaments and sheets, which, during subsequent evolution, merge together, such that the present day web is dominated by fewer, but much more massive, structures. We show also that voids are more naturally described in terms of their boundaries and not their centres. We illustrate this for void density profiles, which, when expressed as a function of the distance from void boundary, show a universal profile in good qualitative agreement with the theoretical shell-crossing framework of expanding underdense regions.
Non Gaussian Minkowski functionals and extrema counts for CMB maps
Authors: Pogosyan Dmitri , Codis Sandrine , Pichon Christophe 
Published: October 2016

AbstractIn the conference presentation we have reviewed the theory of non-Gaussian geometrical measures for 3D Cosmic Web of the matter distribution in the Universe and 2D sky data, such as Cosmic Microwave Background (CMB) maps that was developed in a series of our papers. The theory leverages symmetry of isotropic statistics such as Minkowski functionals and extrema counts to develop post Gaussian expansion of the statistics in orthogonal polynomials of invariant descriptors of the field, its first and second derivatives. The application of the approach to 2D fields defined on a spherical sky was suggested, but never rigorously developed. In this paper we present such development treating the effects of the curvature and finiteness of the spherical space $S_2$ exactly, without relying on flat-sky approximation. We present Minkowski functionals, including Euler characteristic and extrema counts to the first non-Gaussian correction, suitable for weakly non-Gaussian fields on a sphere, of which CMB is the prime example.
Large-scale structure non-Gaussianities with modal methods
Authors: Schmittfull Marcel 
Published: October 2016

AbstractRelying on a separable modal expansion of the bispectrum, the implementation of a fast estimator for the full bispectrum of a 3d particle distribution is presented. The computational cost of accurate bispectrum estimation is negligible relative to simulation evolution, so the bispectrum can be used as a standard diagnostic whenever the power spectrum is evaluated. As an application, the time evolution of gravitational and primordial dark matter bispectra was measured in a large suite of N-body simulations. The bispectrum shape changes characteristically when the cosmic web becomes dominated by filaments and halos, therefore providing a quantitative probe of 3d structure formation. Our measured bispectra are determined by ∼ 50 coefficients, which can be used as fitting formulae in the nonlinear regime and for non-Gaussian initial conditions. We also compare the measured bispectra with predictions from the Effective Field Theory of Large Scale Structures (EFTofLSS).
The cosmic web: a selective history and outlook
Authors: Peacock John A. 
Published: October 2016

AbstractIn the Century since Slipher's first observations, roughly three million galaxy redshifts have been measured. The resulting maps of large-scale structure have taught us much of central importance in cosmology, ranging from the matter content of the universe to the study of the primordial density fluctuations. This talk aims to review some of the key observational and theoretical milestones on this journey, and to speculate about what the future may bring.
Measuring Large-Scale Structure atz∼ 1 with the VIPERS galaxy survey
Authors: Guzzo Luigi 
Published: October 2016

AbstractThe VIMOS Public Extragalactic Redshift Survey (VIPERS) is the largest redshift survey ever conducted with the ESO telescopes. It has used the Very Large Telescope to collect nearly 100,000 redshifts from the general galaxy population at 0.5 <z< 1.2. With a combination of volume and high sampling density that is unique for these redshifts, it allows statistical measurements of galaxy clustering and related cosmological quantities to be obtained on an equal footing with classic results from local redshift surveys. At the same time, the simple magnitude-limited selection and the wealth of ancillary photometric data provide a general view of the galaxy population, its physical properties and the relation of the latter to large-scale structure. This paper presents an overview of the galaxy clustering results obtained so far, together with their cosmological implications. Most of these are based on the ∼ 55,000 galaxies forming the first public data release (PDR-1). As of January 2015, observations and data reduction are complete and the final data set of more than 90,000 redshifts is being validated and made ready for the final investigations.
The place of the Local Group in the cosmic web
Authors: Forero-Romero Jaime E. , González Roberto 
Published: October 2016

AbstractWe use the Bolshoi Simulation to find the most probable location of the Local Group (LG) in the cosmic web. Our LG simulacra are pairs of halos with isolation and kinematic properties consistent with observations. The cosmic web is defined using a tidal tensor approach. We find that the LG's preferred location is regions with a dark matter overdensity close to the cosmic average. This makes filaments and sheets the preferred environment. We also find a strong alignment between the LG and the cosmic web. The orbital angular momentum is preferentially perpendicular to the smallest tidal eigenvector, while the vector connecting the two halos is strongly aligned along the the smallest tidal eigenvector and perpendicular to the largest tidal eigenvector; the pair lies and moves along filaments and sheets. We do not find any evidence for an alignment between the spin of each halo in the pair and the cosmic web.
Galaxy Group Properties in Observations and Simulations
Authors: Nurmi Pasi 
Published: October 2016

AbstractIn this project, we compare different properties of galaxy groups in cosmological N-body simulations and SDSS galaxy group catalogs. In the first part of the project (Nurmi et al. 2013) we compared the basic properties of the groups like the luminosity functions, group richness and velocity dispersion distributions and studied how good is the agreement between the mock group catalog and the SDSS group catalog. Here we continue the earlier study and use updated galaxy group catalog (SDSS DR10) and new simulation data (Guo et al. 2013). We reanalyse earlier group properties and include new properties in the analysis like group environment, star formation rates and group masses. Our analysis show that there are clear differences between the simulated and observed properties of galaxy groups, especially for small groups with a few members. Also, the high luminosities are clearly overestimated in the simulations compared with the SDSS group data.
The Adopted Morphological Types of 247 Rich PF Galaxy Clusters
Authors: Panko Elena , Bajan Katarzyna , Flin Piotr , Gotsulyak Alla 
Published: October 2016

AbstractMorphological types were determined for 247 rich galaxy clusters from the PF Catalogue of Galaxy Clusters and Groups. The adopted types are based on classical morphological schemes and consider concentration to the cluster center, the signs of preferential direction or plane in the cluster, and the positions of the brightest galaxies. It is shown that both concentration and preferential plane are significant and independent morphological criteria.
Quantifying the Cosmic Web using the Shapefinder diagonistic
Authors: Sarkar Prakash 
Published: October 2016

AbstractOne of the most successful method in quantifying the structures in the Cosmic Web is the Minkowski Functionals. In 3D, there are four minkowski Functionals: Area, Volume, Integrated Mean Curvature and the Integrated Gaussian Curvature. For defining the Minkowski Functionals one should define a surface. We have developed a method based on Marching cube 33 algorithm to generate a surface from a discrete data sets. Next we calculate the Minkowski Functionals and Shapefinder from the triangulated polyhedral surface. Applying this methodology to different data sets , we obtain interesting results related to geometry, morphology and topology of the large scale structure
Identification of Extremely Large Scale Structures in SDSS-III
Authors: Sankhyayan Shishir , Bagchi J. , Sarkar P. , Sahni V. , Jacob J. 
Published: October 2016

AbstractWe have initiated the search and detailed study of large scale structures present in the universe using galaxy redshift surveys. In this process, we take the volume-limited sample of galaxies from Sloan Digital Sky Survey III and find very large structures even beyond the redshift of 0.2. One of the structures is even greater than 600 Mpc which raises a question on the homogeneity scale of the universe. The shapes of voids-structures (adjacent to each other) seem to be correlated, which supports the physical existence of the observed structures. The other observational supports include galaxy clusters' and QSO distribution's correlation with the density peaks of the volume limited sample of galaxies.
Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field
Authors: Hudson Michael J. , Carrick Jonathan , Turnbull Stephen J. , Lavaux Guilhem 
Published: October 2016

AbstractUsing redshifts from the 2M++ redshift compilation, we reconstruct the density of galaxies within 200 h−1 Mpc, and compare the predicted peculiar velocities Tully-Fisher and SNe peculiar velocities. The comparison yields a best-fit value of β ≡ Ωm0.55/b* = 0.431 ± 0.021, suggesting Ωm0.55σ8,lin = 0.401 ± 0.024, in good agreement with other probes. The predicted peculiar velocity of the Local Group from sources within the 2M++ volume is 540 ± 40 km s−1, towards l = 268° ± 4°, b = 38° ± 6°, which is misaligned by only 10° with the Cosmic Microwave Background dipole. To account for sources outside the 2M++ volume, we fit simultaneously for β* and an external bulk flow in our analysis. The external bulk flow has a velocity of 159 ± 23 km s−1 towards l = 304° ± 11°, b6° ± 13°.
The disks and spheroid of LTGs in the light of their early web-like organization
Authors: Domínguez-Tenreiro R. , Obreja A. , Brook C. , Martínez-Serrano F. J. , Serna A. 
Published: October 2016

AbstractCosmological hydrodynamical simulations show that the baryonic elements that at z = 0 form the stellar populations of late-type galaxies (LTGs), display, at high z, a gaseous web-like organization, where different singular structures (walls, filaments, nodes) show up. The analysis also shows that the spheroid-to-be elements are the first to be involved in the singular structures, while thick and thin disk-to-be elements chronologically follow them. We discuss how these differences at high z can explain the differences among these three components at z = 0.
Satellites are the main drivers of environmental effects at least to z = 0.7
Authors: Kovač Katarina ,   the zCOSMOS team
Published: October 2016

AbstractWe study the role of environment in the evolution of galaxies up to z = 0.7 using the final zCOSMOS-bright data set. We use the colour as a proxy for the quenched population, and measure the dependence of the red fraction of galaxies on stellar mass and two environmental indicators: the local overdensity of galaxies δ and a demarcation of galaxies to centrals and satellites. The analysis is carried out by quantifying the role of different quenching processes. We find that the measured dependence of the red fraction of galaxies on stellar mass and environment can be well described by two quenching processes: one related only to stellar mass (mass quenching) and the other related to the local environment (environment quenching). Within the errors, these processes are independent of each other, and consistent with the z ~ 0 measurement. Moreover, the red fraction of centrals fr,cen (both singleton centrals and centrals in the groups) does not show any trend with δ and more than 95% of fr,cen is consistent with being produced through the mass quenching alone. The satellite galaxies are redder than the centrals at the same stellar mass and δ, requiring additional environment quenching. Given the observed fractional distribution of satellites at different overdensities, the normalized excess in the red fraction of satellites with respect to the red fraction of centrals is consistent with a scenario in which the satellites account for most of the δ-dependences observed in the overall population of galaxies covering 0.1 < z < 0.7.
It takes a supercluster to raise a galaxy
Authors: Lietzen Heidi , Einasto Maret 
Published: October 2016

AbstractThe properties of galaxies depend on their environment: red, passive elliptical galaxies are usually located in denser environments than blue, star-forming spiral galaxies. This difference in galaxy populations can be detected at all scales from groups of galaxies to superclusters. In this paper, we will discuss the effect of the large-scale environment on galaxies. Our results suggest that galaxies in superclusters are more likely to be passive than galaxies in voids even when they belong to groups with the same richness. In addition, the galaxies in superclusters are also affected by the morphology of the supercluster: filament-type superclusters contain relatively more red, passive galaxies than spider-type superclusters. These results suggest that the evolution of a galaxy is not determined by its local environment alone, but the large-scale environment also affects.
How the cosmic web induces intrinsic alignments of galaxies
Authors: Codis S. , Dubois Y. , Pichon C. , Devriendt J. , Slyz A. 
Published: October 2016

AbstractIntrinsic alignments are believed to be a major source of systematics for future generation of weak gravitational lensing surveys like Euclid or LSST. Direct measurements of the alignment of the projected light distribution of galaxies in wide field imaging data seem to agree on a contamination at a level of a few per cent of the shear correlation functions, although the amplitude of the effect depends on the population of galaxies considered. Given this dependency, it is difficult to use dark matter-only simulations as the sole resource to predict and control intrinsic alignments. We report here estimates on the level of intrinsic alignment in the cosmological hydrodynamical simulation Horizon-AGN that could be a major source of systematic errors in weak gravitational lensing measurements. In particular, assuming that the spin of galaxies is a good proxy for their ellipticity, we show how those spins are spatially correlated and how they couple to the tidal field in which they are embedded. We will also present theoretical calculations that illustrate and qualitatively explain the observed signals.
Spin Alignment in Analogues of The Local Sheet
Authors: Conidis George J. 
Published: October 2016

AbstractTidal torque theory and simulations of large scale structure predict spin vectors of massive galaxies should be coplanar with sheets in the cosmic web. Recently demonstrated, the giants (Ks⩽ -22.5 mag) in the Local Volume beyond the Local Sheet have spin vectors directed close to the plane of the Local Supercluster, supporting the predictions of Tidal Torque Theory. However, the giants in the Local Sheet encircling the Local Group display a distinctly different arrangement, suggesting that the mass asymmetry of the Local Group or its progenitor torqued them from their primordial spin directions. To investigate the origin of the spin alignment of giants locally, analogues of the Local Sheet were identified in the SDSS DR9. Similar to the Local Sheet, analogues have an interacting pair of disk galaxies isolated from the remaining sheet members. Modified sheets in which there is no interacting pair of disk galaxies were identified as a control sample.Galaxies in face-on control sheets do not display axis ratios predominantly weighted toward low values, contrary to the expectation of tidal torque theory. For face-on and edge-on sheets, the distribution of axis ratios for galaxies in analogues is distinct from that in controls with a confidence of 97.6% & 96.9%, respectively. This corroborates the hypothesis that an interacting pair can affect spin directions of neighbouring galaxies.