bluuebunny/crossref_metadata_2025 huggingface dataset:
Motion of a spherical capsule in branched tube flow with finite inertia
Authors: Wang Z. , Sui Y. , Salsac A.-V. , Barthès-Biesel D. , Wang W.
Published: October 2016

We computationally study the transient motion of an initially spherical capsule flowing through a right-angled tube bifurcation, composed of tubes having the same diameter. The capsule motion and deformation is simulated using a three-dimensional immersed-boundary lattice Boltzmann method. The capsule is modelled as a liquid droplet enclosed by a hyperelastic membrane following the Skalak’s law (Skalak et al., Biophys. J., vol. 13(3), 1973, pp. 245–264). The fluids inside and outside the capsule are assumed to have identical viscosity and density. We mainly focus on path selection of the capsule at the bifurcation as a function of the parameters of the problem: the flow split ratio, the background flow Reynolds number $Re$, the capsule-to-tube size ratio $a/R$ and the capillary number $Ca$, which compares the viscous fluid force acting on the capsule to the membrane elastic force. For fixed physical properties of the capsule and of the tube flow, the ratio $Ca/Re$ is constant. Two size ratios are considered: $a/R=0.2$ and 0.4. At low $Re$, the capsule favours the branch which receives most flow. Inertia significantly affects the background flow in the branched tube. As a consequence, at equal flow split, a capsule tends to flow straight into the main branch as $Re$ is increased. Under significant inertial effects, the capsule can flow into the downstream main tube even when it receives much less flow than the side branch. Increasing $Ca$ promotes cross-stream migration of the capsule towards the side branch. The results are summarized in a phase diagram, showing the critical flow split ratio for which the capsule flows into the side branch as a function of size ratio, $Re$ and $Ca/Re$. We also provide a simplified model of the path selection of a slightly deformed capsule and explore its limits of validity. We finally discuss the experimental feasibility of the flow system and its applicability to capsule sorting.
DYNAMICS ON SUPERSINGULAR K3 SURFACES AND AUTOMORPHISMS OF SALEM DEGREE 22
Authors: BRANDHORST SIMON
Published: October 2016

In this paper, we exhibit explicit automorphisms of maximal Salem degree 22 on the supersingular K3 surface of Artin invariant one for all primes $p\equiv 3~\text{mod}\,4$ in a systematic way. Automorphisms of Salem degree 22 do not lift to any characteristic zero model.
BEST PROXIMITY POINT THEOREMS FOR CYCLIC QUASI-CONTRACTION MAPS IN UNIFORMLY CONVEX BANACH SPACES
Authors: VAN DUNG NGUYEN , LE HANG VO THI
Published: October 2016

In this paper we first give a negative answer to a question of Amini-Harandi [‘Best proximity point theorems for cyclic strongly quasi-contraction mappings’, J. Global Optim.56 (2013), 1667–1674] on a best proximity point theorem for cyclic quasi-contraction maps. Then we prove some new results on best proximity point theorems that show that results of Amini-Harandi for cyclic strongly quasi-contractions are true under weaker assumptions.
Parental and perinatal risk factors for sexual offending in men: a nationwide case-control study
Authors: Babchishin K. M. , Seto M. C. , Sariaslan A. , Lichtenstein P. , Fazel S. , Långström N.
Published: October 2016

Background

Prior studies suggest parental and perinatal risk factors are associated with later offending. It remains uncertain, however, if such risk factors are similarly related to sexual offending.

Method

We linked socio-demographic, family relations, and perinatal (obtained at birth) data from the nationwide Swedish registers from 1973 to 2009 with information on criminal convictions of cases and control subjects. Male sex offenders (n = 13 773) were matched 1:5 on birth year and county of birth in Sweden to male controls without sexual or non-sexual violent convictions. To examine risk-factor specificity for sexual offending, we also compared male violent, non-sexual offenders (n = 135 953) to controls without sexual or non-sexual violent convictions. Predictors included parental (young maternal or paternal age at son's birth, educational attainment, violent crime, psychiatric disorder, substance misuse, suicide attempt) and perinatal (number of older brothers, low Apgar score, low birth weight, being small for gestational age, congenital malformations, small head size) variables.

Results

Conditional logistic regression models found consistent patterns of statistically significant, small to moderate independent associations of parental risk factors with sons’ sexual offending and non-sexual violent offending. For perinatal risk factors, patterns varied more; small for gestational age and small head size exhibited similar risk effects for both offence types whereas a higher number of older biological brothers and any congenital malformation were small, independent risk factors only for non-sexual violence.

Conclusions

This nationwide study suggests substantial commonalities in parental and perinatal risk factors for the onset of sexual and non-sexual violent offending.
Naam, Kaam, Gaam: Educating Women for Self-Employment, Cooperation and Struggle
Authors: Bali Namrata
Published: October 2016

The following is a detailed description of a training program offered by the Self-Employed Women's Association (SEWA) Academy to introduce new members to the organization and its work. SEWA describes its main goals as “to organize women workers for full employment,” by which it means “employment whereby workers obtain work security, income security, food security, and social security (at least health care, child care and shelter).” The organization works to achieve its goals “through the strategy of struggle and development. The struggle is against the many constraints and limitations imposed on them by society and the economy, while development activities strengthen women's bargaining power and offer them new alternatives.” SEWA describes itself as “both an organisation and a movement,” which is enhanced by “the sangama or confluence of three movements: the labour movement, the cooperative movement and the women's movement.” SEWA also describes itself as a Gandhian movement: “Gandhian thinking is the guiding force for SEWA's poor, self-employed members in organising for social change. We follow the principles of satya (truth), ahimsa (nonviolence), sarvadharma (integrating all faiths, all people) and khadi (propagation of local employment and self-reliance).” In practical terms, SEWA carries out its strategy “through the joint action of union and cooperatives.” As a trade union, it has nearly two million members, half of whom are in the organization's home state of Gujarat, India. It also operates or is affiliated with nearly two dozen sister organizations and cooperatives.
Political Training and Social Change in the 1960s and 1970s: The Educational Activities of the Latin American Central of Workers (CLAT)
Authors: Scodeller Gabriela
Published: October 2016

This article reconstructs the educational policies of the Latin American Confederation of Christian Trade Unions (CLASC)—the name of which was later changed to the Latin American Central of Workers (CLAT) —in the context of the Latin American Cold War. It provides an empirical description of its pedagogical praxis, showing how it was shaped in constant dialogue with the region's conflictive context. It explores how they viewed political training in relation to both their organizing efforts and struggles, applying a conception that brought together “action, organization and training” as integrated elements, in the run to foster class awareness, build up a “new society,” and “workers’ organized power”.
The Cooperative Movement and the Education of Working Men and Women: Provision by a Local Society in Lincoln, England, 1861–1914
Authors: Jackson Andrew J.H.
Published: October 2016

In the second half of the nineteenth century the provision of better education for working-class men and women became one of the various and broad-ranging set of preoccupations of the cooperative movement in Britain. Much early cooperation was economic, concerning alternative means of production and distribution. However, local societies also turned themselves toward other forms of societal improvement, including creating the facilities and contexts that would promote and support the education and learning of adults. The archive of the Lincoln Equitable Co-operative Industrial Society offers a rich body of source material for a microhistorical investigation of the expansion and diversification of one local cooperative up to the First World War. The members’ magazine of this local society in particular records the evolution of its purpose—economic, political, social, and cultural. This included achieving progress through various forms of educational provision—although the opportunities for men contrasted with those made available for women. This research illuminates what is a relatively underresearched area—that is, exploration of the complexities, dynamism, and phenomenology of local cooperative adult education and the significance of what it had to offer the development of the labor movement in particular places.
Class Formation in Sweden and Britain: Educating Workers
Authors: Jansson Jenny
Published: October 2016

The European labor movements developed in different directions during the twentieth century. The class formation literature has tried to explain these differences but left unexplored the internal dynamics of the labor movement and, above all, the differences in ideological schooling. Workers’ education constitutes a forum for ideological schooling of members, and these educational settings can be identity constitutive and thus play an important part in the class formation process. In this article I analyze the institutions for workers’ education in Sweden and Britain and I suggest that the variation of the design and practices of workers’ education had an impact on the movements’ developments in terms of identity formation and cohesiveness.
Watching Election 2016 with a Gender Lens
Authors: Dittmar Kelly
Published: October 2016

The presence of women candidates in both major parties’ presidential primaries, including a likely woman Democratic nominee, has increased the attention paid to gender dynamics in the 2016 US presidential election. However, the presumption that previous presidential elections—without female prominent contenders—were gender neutral is false: gender dynamics have been at play in all US presidential elections to date. The nation’s top executive office is arguably the most masculine in American politics. Duerst-Lahti (1997) describes the presidency as a gendered space in which masculine norms and images are reified as the ideal, adding, “the masculinist assumption-made-normal is strong and is made even stronger when it goes unnoticed for its gendered aspects” (22). Presidents and presidential contenders, whether male or female, are expected to meet the masculine expectations of the office through words and actions, and those around them—family, spouses, and advisors—often play a role in shaping the degree to which they are successful. In navigating American politics, candidates also face gendered treatment by opponents, voters, and media, reminding us that presidential politics is far from gender neutral. These gender dynamics have been detailed by scholars, particularly in analyses of the presidential candidacies of women (Beail and Longworth 2013; Carlin and Winfrey 2009; Carroll and Dittmar 2009; Dittmar and Carroll 2013; Duerst-Lahti 2013; Falk 2010; Han and Heldman 2007; Heldman, Carroll, and Olson 2005; Lawrence and Rose 2009; McClain, Carter, and Brady 2005). However, the depth and nuance in scholarly analyses are rarely evident in popular dialogue about the ways in which gender shapes presidential elections.
The Accuracy of Microtargeted Policy Positions
Authors: Endres Kyle
Published: October 2016

Identifying voters who share policy positions with the candidates has become an important component of modern political campaigns as they rely on microtargeted estimates to guide targeting decisions. Using survey data and microtargeted estimates from the 2012 election, I conduct one of the first independent examinations of the accuracy of microtargeting. The estimates are the most accurate in Florida, a state that requests information on the race of voters when they register and has party registration. The estimates are less accurate in the other battleground states that do not collect as much information. The accuracy rates range from 36% to 82% depending on the issue and state.
Twitter Taunts and Tirades: Negative Campaigning in the Age of Trump
Authors: Gross Justin H. , Johnson Kaylee T.
Published: October 2016

What drives candidates to “go negative” and against which opponents? Using a unique dataset consisting of all inter-candidate tweets by the 17 Republican presidential candidates in the 2016 primaries, we assess predictors of negative affect online. Twitter is a free platform, and candidates therefore face no resource limitations when using it; this makes Twitter a wellspring of information about campaign messaging, given a level playing-field. Moreover, Twitter’s 140-character limit acts as a liberating constraint, leading candidates to issue sound bites ready for potential distribution not only online, but also through conventional media, as tweets become news. We find tweet negativity and overall rate of tweeting increases as the campaign season progresses. Unsurprisingly, the front-runner and eventual nominee, Donald Trump, sends and receives the most negative tweets and is more likely than his opponents to strike out against even those opponents who are polling poorly. However, candidates overwhelmingly “punch upwards” against those ahead of them in the polls, and this pattern goes beyond attacks against those near the top. Sixty of 136 dyads are characterized by lopsided negativity in one direction and only one of these 60 involves a clearly higher status candidate on the offensive.
Bias, guess and expert judgement in actuarial work
Authors: Tredger E. R. W. , Lo J. T. H. , Haria S. , Lau H. H. K. , Bonello N. , Hlavka B. , Scullion C.
Published: October 2016

Expert judgement is frequently used within general insurance. It tends to be a method of last resort and used where data is sparse, non-existent or non-applicable to the problem under consideration. Whilst such judgements can significantly influence the end results, their quality is highly variable. The use of the term “expert judgement” itself can lend a generous impression of credibility to what may be a little more than a guess. Despite the increased emphasis placed on the importance of robust expert judgements in regulation, actuarial research to date has focussed on the more technical or data-driven methods, with less emphasis on how to use and incorporate softer information or how best to elicit judgements from others in a way that reduces cognitive biases. This paper highlights the research that the Getting Better Judgement Working Party has conducted in this area. Specifically, it covers the variable quality of expert judgement, both within and outside the regulatory context, and presents methods that may be applied to improve its formation. The aim of this paper is to arm the insurance practitioner with tools to distinguish between low-quality and high-quality judgements and improve the robustness of judgements accordingly, particularly for highly material circumstances.
An Origami Approximation to the Cosmic Web
Authors: Neyrinck Mark C.
Published: October 2016

The powerful Lagrangian view of structure formation was essentially introduced to cosmology by Zel'dovich. In the current cosmological paradigm, a dark-matter-sheet 3D manifold, inhabiting 6D position-velocity phase space, was flat (with vanishing velocity) at the big bang. Afterward, gravity stretched and bunched the sheet together in different places, forming a cosmic web when projected to the position coordinates.

Here, I explain some properties of an origami approximation, in which the sheet does not stretch or contract (an assumption that is false in general), but is allowed to fold. Even without stretching, the sheet can form an idealized cosmic web, with convex polyhedral voids separated by straight walls and filaments, joined by convex polyhedral nodes. The nodes form in ‘polygonal’ or ‘polyhedral’ collapse, somewhat like spherical/ellipsoidal collapse, except incorporating simultaneous filament and wall formation. The origami approximation allows phase-space geometries of nodes, filaments, and walls to be more easily understood, and may aid in understanding spin correlations between nearby galaxies. This contribution explores kinematic origami-approximation models giving velocity fields for the first time.
Disentangling the Cosmic Web with Lagrangian Submanifold
Authors: Shandarin Sergei F. , Medvedev Mikhail V.
Published: October 2016

The Cosmic Web is a complicated highly-entangled geometrical object. Remarkably it has formed from practically Gaussian initial conditions, which may be regarded as the simplest departure from exactly uniform universe in purely deterministic mapping. The full complexity of the web is revealed neither in configuration no velocity spaces considered separately. It can be fully appreciated only in six-dimensional (6D) phase space. However, studies of the phase space is complicated by the fact that every projection of it on a three-dimensional (3D) space is multivalued and contained caustics. In addition phase space is not a metric space that complicates studies of geometry. We suggest to use Lagrangian submanifold i.e., x = x(q), where both x and q are 3D vectors instead of the phase space for studies the complexity of cosmic web in cosmological N-body dark matter simulations. Being fully equivalent in dynamical sense to the phase space it has an advantage of being a single valued and also metric space.
Beyond single-stream with the Schrödinger method
Authors: Uhlemann Cora , Kopp Michael
Published: October 2016

We investigate large scale structure formation of collisionless dark matter in the phase space description based on the Vlasov-Poisson equation. We present the Schrödinger method, originally proposed by \cite{WK93} as numerical technique based on the Schrödinger Poisson equation, as an analytical tool which is superior to the common standard pressureless fluid model. Whereas the dust model fails and develops singularities at shell crossing the Schrödinger method encompasses multi-streaming and even virialization.
Higher-order Lagrangian perturbative theory for the Cosmic Web
Authors: Tatekawa Takayuki , Mizuno Shuntaro
Published: October 2016

Zel'dovich proposed Lagrangian perturbation theory (LPT) for structure formation in the Universe. After this, higher-order perturbative equations have been derived. Recently fourth-order LPT (4LPT) have been derived by two group. We have shown fifth-order LPT (5LPT) In this conference, we notice fourth- and more higher-order perturbative equations. In fourth-order perturbation, because of the difference in handling of spatial derivative, there are two groups of equations. Then we consider the initial conditions for cosmological N-body simulations. Crocce, Pueblas, and Scoccimarro (2007) noticed that second-order perturbation theory (2LPT) is required for accuracy of several percents. We verify the effect of 3LPT initial condition for the simulations. Finally we discuss the way of further improving approach and future applications of LPTs.
Structure and kinematics of the Bootes filament
Authors: Nasonova O. , Karachentsev I. , Karachentseva V.
Published: October 2016

Bootes filament of galaxies is a dispersed chain of groups residing on sky between the Local Void and the Virgo cluster. We consider a sample of 361 galaxies inside the sky area of RA = 13h0...18h.5 and Dec = .5°... + 10° with radial velocities VLG < 2000 km/s to clarify its structure and kinematics. In this region, 161 galaxies have individual distance estimates. We use these data to draw the Hubble relation for galaxy groups, pairs as well as the field galaxies, and to examine the galaxy distribution on peculiar velocities. Our analysis exposes the known Virgo-centric infall at RA < 14h and some signs of outflow from the Local Void at RA > 17h. According to the galaxy grouping criterion, this complex contains the members of 13 groups, 11 pairs and 140 field galaxies. The most prominent group is dominated by NGC 5846. The Bootes filament contains the total stellar mass of 2.7 ×1012M⊙ and the total virial mass of 9.07×1013M⊙, having the average density of dark matter to be Ωm = 0.09, i.e. a factor three lower than the global cosmic value.
Characterising large-scale structure with the REFLEX II cluster survey
Authors: Chon Gayoung
Published: October 2016

We study the large-scale structure with superclusters from the REFLEX X-ray cluster survey together with cosmological N-body simulations. It is important to construct superclusters with criteria such that they are homogeneous in their properties. We lay out our theoretical concept considering future evolution of superclusters in their definition, and show that the X-ray luminosity and halo mass functions of clusters in superclusters are found to be top-heavy, different from those of clusters in the field. We also show a promising aspect of using superclusters to study the local cluster bias and mass scaling relation with simulations.
The structural elements of the cosmic web
Authors: Jones Bernard J.T. , van de Weygaert Rien
Published: October 2016

In 1970 Zel'dovich published a far-reaching paper presenting a simple equation describing the nonlinear growth of primordial density inhomogeneities. The equation was remarkably successful in explaining the large scale structure in the Universe that we observe: a Universe in which the structure appears to be delineated by filaments and clusters of galaxies surrounding huge void regions. In order to concretise this impression it is necessary to define these structural elements through formal techniques with which we can compare the Zel'dovich model and N-body simulations with the observational data.

We present an overview of recent efforts to identify voids, filaments and clusters in both the observed galaxy distribution and in numerical simulations of structure formation. We focus, in particular, on methods that involve no fine-tuning of parameters and that handle scale dependence automatically. It is important that these techniques should result in finding structures that relate directly to the dynamical mechanism of structure formation.
Filamentary pattern in the cosmic web: galaxy filaments as pearl necklaces
Authors: Tempel Elmo , Bussov Maarja
Published: October 2016

Galaxies form chains (filaments) that connect groups and clusters of galaxies. The filamentary network includes nearly half of the galaxies and is visually the most striking feature in cosmological maps. We study the distribution of galaxies along such a filamentary network, trying to find specific patterns. Our galaxy filaments are defined using the Bisous process. We use the two-point correlation function and the Rayleigh $Z$-squared statistic to study how the galaxies are distributed along the filaments. We show that galaxies and galaxy groups are not uniformly distributed along filaments, but tend to form a regular pattern. The characteristic length of the pattern is 7~$h^{-1}$Mpc. A slightly smaller characteristic length 4~$h^{-1}$Mpc can also be found, using the $Z$-squared statistic. One can say that galaxy filaments are like pearl necklaces, where the pearls are galaxy groups distributed more or less regularly along the filaments. We propose that this well defined characteristic scale could be used as a cosmological test.
Adaptive density estimator for galaxy surveys
Authors: Saar Enn
Published: October 2016

Galaxy number or luminosity density serves as a basis for many structure classification algorithms. Several methods are used to estimate this density. Among them kernel methods have probably the best statistical properties and allow also to estimate the local sample errors of the estimate. We introduce a kernel density estimator with an adaptive data-driven anisotropic kernel, describe its properties and demonstrate the wealth of additional information it gives us about the local properties of the galaxy distribution.
Bayesian inference of the initial conditions from large-scale structure surveys
Authors: Leclercq Florent
Published: October 2016

Analysis of three-dimensional cosmological surveys has the potential to answer outstanding questions on the initial conditions from which structure appeared, and therefore on the very high energy physics at play in the early Universe. We report on recently proposed statistical data analysis methods designed to study the primordial large-scale structure via physical inference of the initial conditions in a fully Bayesian framework, and applications to the Sloan Digital Sky Survey data release 7. We illustrate how this approach led to a detailed characterization of the dynamic cosmic web underlying the observed galaxy distribution, based on the tidal environment.
Bayesian Cosmic Web Reconstruction: BARCODE for Clusters
Authors: Patrick Bos E. G. , van de Weygaert Rien , Kitaura Francisco , Cautun Marius
Published: October 2016

We describe the Bayesian \barcode\ formalism that has been designed towards the reconstruction of the Cosmic Web in a given volume on the basis of the sampled galaxy cluster distribution. Based on the realization that the massive compact clusters are responsible for the major share of the large scale tidal force field shaping the anisotropic and in particular filamentary features in the Cosmic Web. Given the nonlinearity of the constraints imposed by the cluster configurations, we resort to a state-of-the-art constrained reconstruction technique to find a proper statistically sampled realization of the original initial density and velocity field in the same cosmic region. Ultimately, the subsequent gravitational evolution of these initial conditions towards the implied Cosmic Web configuration can be followed on the basis of a proper analytical model or an N-body computer simulation. The BARCODE formalism includes an implicit treatment for redshift space distortions. This enables a direct reconstruction on the basis of observational data, without the need for a correction of redshift space artifacts. In this contribution we provide a general overview of the the Cosmic Web connection with clusters and a description of the Bayesian BARCODE formalism. We conclude with a presentation of its successful workings with respect to test runs based on a simulated large scale matter distribution, in physical space as well as in redshift space.
Dynamics of pairwise motions in the Cosmic Web
Authors: Hellwing Wojciech A.
Published: October 2016

We present results of analysis of the dark matter (DM) pairwise velocity statistics in different Cosmic Web environments. We use the DM velocity and density field from the Millennium 2 simulation together with the NEXUS+ algorithm to segment the simulation volume into voxels uniquely identifying one of the four possible environments: nodes, filaments, walls or cosmic voids. We show that the PDFs of the mean infall velocities v12 as well as its spatial dependence together with the perpendicular and parallel velocity dispersions bear a significant signal of the large-scale structure environment in which DM particle pairs are embedded. The pairwise flows are notably colder and have smaller mean magnitude in wall and voids, when compared to much denser environments of filaments and nodes. We discuss on our results, indicating that they are consistent with a simple theoretical predictions for pairwise motions as induced by gravitational instability mechanism. Our results indicate that the Cosmic Web elements are coherent dynamical entities rather than just temporal geometrical associations. In addition it should be possible to observationally test various Cosmic Web finding algorithms by segmenting available peculiar velocity data and studying resulting pairwise velocity statistics.
Measuring the cosmic bulk flow with 6dFGSv
Authors: Magoulas Christina , Springob Christopher , Colless Matthew , Mould Jeremy , Lucey John , Erdoğdu Pirin , Jones D. Heath
Published: October 2016

While recent years have seen rapid growth in the number of galaxy peculiar velocity measurements, disagreements remain about the extent to which the peculiar velocity field - a tracer of the large-scale distribution of mass - agrees with both ΛCDM expectations and with velocity field models derived from redshift surveys. The 6dF Galaxy Survey includes peculiar velocities for nearly 9 000 early-type galaxies (6dFGSv), making it the largest and most homogeneous galaxy peculiar velocity sample to date. We have used the 6dFGS velocity field to determine the amplitude and scale of large-scale cosmic flows in the local universe and test standard cosmological models. We also compare the galaxy density and peculiar velocity fields to establish the distribution of dark and luminous matter and better constrain key cosmological parameters such as the redshift-space distortion parameter.
Lyα Forest Tomography of the z > 2 Cosmic Web
Authors: Lee Khee-Gan
Published: October 2016

The hydrogen Lyα forest is an important probe of the z > 2 Universe that is otherwise challenging to observe with galaxy redshift surveys, but this technique has traditionally been limited to 1D studies in front of bright quasars. However, by pushing to faint magnitudes (g > 23) with 8-10m large telescopes it becomes possible to exploit the high area density of high-redshift star-forming galaxies to create 3D tomographic maps of large-scale structure in the foreground. I describe the first pilot observations using this technique, as well discuss future surveys and the resulting science possibilities for galaxy evolution and cosmology.
Radiative Feedback Effects during Cosmic Reionization
Authors: Sullivan David , Iliev Ilian T.
Published: October 2016

We present coupled radiation hydrodynamical simulations of the epoch of reionization, aimed at probing self-feedback on galactic scales. Unlike previous works, which assume a (quasi) homogeneous UV background, we self-consistently evolve both the radiation field and the gas to model the impact of previously unresolved processes such as spectral hardening and self-shielding. We find that the characteristic halo mass with a gas fraction half the cosmic mean,Mc(z), a quantity frequently used in semi-analytical models of galaxy formation, is significantly larger than previously assumed. While this results in an increased suppression of star formation in the early Universe, our results are consistent with the extrapolated stellar abundance matching models from Mosteret al.2013.
Zeldovich and the Missing Baryons, Results from Gravitational Lensing
Authors: Schild Rudolph E.
Published: October 2016

Central to Zeldovich's attempts to understand the origin of cosmological structure was his exploration of the fluid dynamical effects in the primordial gas, and how the baryonic dark matter formed. Unfortunately microlensing searches for condensed objects in the foreground of the Magellanic Clouds were flawed by the assumption that the objects would be uniformly (Gaussian) distributed, and because the cadence of daily observations strongly disfavored detection of planet mass microlenses. But quasar microlensing showed them to exist at planetary mass at the same time that a hydro-gravitational theory predicted the planet-mass population as fossils of turbulence at the time of recombination (z = 1100; Gibson 1996, 2001). Where the population has now been detected from MACHO searches to the LMC (Sumi et al. 2011) we compare the quasar microlensing results to the recent determination of the mass distribution function measured for the planetary mass function, and show that the population can account for the baryonic dark matter.
The origin of the galaxy color bimodality
Authors: Aragón-Calvo M. A. , Neyrinck Mark C. , Silk Joseph
Published: October 2016

The star formation history of galaxies is a complex process usually considered to be stochastic in nature, for which we can only give average descriptions such as the color-density relation. In this work we follow star-forming gas particles in a hydrodynamical N-body simulation back in time in order to study their initial spatial configuration. By keeping record of the time when a gas particle started forming stars we can produce Lagrangian gas-star isochrone surfaces delineating the surfaces of accreting gas that begin producing stars at different times. These surfaces form a complex a network of filaments in Eulerian space from which galaxies accrete cold gas. Lagrangian accretion surfaces are closely packed inside dense regions, intersecting each other, and as a result galaxies inside proto-clusters stop accreting gas early, naturally explaining the color dependence on density. The process described here has a purely gravitational / geometrical origin, arguably operating at a more fundamental level than complex processes such as AGN and supernovae, and providing a conceptual origin for the color-density relation.
The role of cold and hot gas flows in feeding early-type galaxy formation
Authors: Johansson Peter H.
Published: October 2016

We study the evolution of the gaseous components in massive simulated galaxies and show that their early formation is fuelled by cold, low entropy gas streams. At lower redshifts of z ≲ 3 the simulated galaxies are massive enough to support stable virial shocks resulting in a transition from cold to hot gas accretion. The gas accretion history of early-type galaxies is directly linked to the formation of their stellar component in the two phased formation scenario, in which the central parts of the galaxy assemble rapidly through in situ star formation and the later assembly is dominated primarily by minor stellar mergers.
Large-scale structure and the intrinsic alignment of galaxies
Authors: Blazek Jonathan , Seljak Uroš , Mandelbaum Rachel
Published: October 2016

Coherent alignments of galaxy shapes, often called“intrinsic alignments” (IA), are the most significant source of astrophysical uncertainty in weak lensing measurements. We develop the tidal alignment model of IA and demonstrate its success in describing observational data. We also describe a technique to separate IA from galaxy-galaxy lensing measurements. Applying this technique to luminous red galaxy lenses in the Sloan Digital Sky Survey, we constrain potential IA contamination from associated sources to be below a few percent.
The beaming of subhalo accretion
Authors: Libeskind Noam I.
Published: October 2016

We examine the infall pattern of subhaloes onto hosts in the context of the large-scale structure. We find that the infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that its always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼ 10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group.
The effect of environment on the fundamental plane of elliptical galaxies
Authors: Kipper R. , Tamm A. , Tenjes P. , Tempel E.
Published: October 2016

We study the effect of environment to fundamental relation of elliptical galaxies. We find that superclusters, filaments and groups give noticeable effect to slope of velocity dispersions while little to luminosity slope.
Kinematics, structure and environment of three dwarf spheroidal galaxies
Authors: Sharina M. E. , Karachentsev I. D. , Karachentseva V. E.
Published: October 2016

We explore the environmental status of three low surface brightness
dwarf spheroidal galaxies (dSphs) KKH65, KK180 and KK227 using the results of our long slit
spectroscopic observations at the 6m telescope of the Russian Academy of Sciences and surface
photometry on the Sloan Digital Sky Survey (SDSS) images.
The objects were selected by Karachentseva in 2010 as presumably isolated galaxies.
The obtained surface brightness profiles demonstrate that our sample dSphs are less
centrally concentrated than the objects of the same morphological type in the Virgo cluster (VC).
Using the derived kinematic data we searched for possible neighbours of the dSphs within
the projected distances from them Rproj > 500 kpc and with the differences in radial velocities |Δ V| > 500 kms−1. We applied the group finding algorithm by
Makarov and Karachentsev to the selected sample.
Our analysis shows that the dwarf galaxies of our study are not isolated.
KKH65 and KK227 belong to the groups NGC3414
and NGC5371, respectively. KK180 is in the VC infall region. We conclude that
it is not possible at the moment to justify the existence of isolated dSphs outside
the Local Volume. The searches are complicated due to the lack of the accurate
distances to the galaxies farther than 10 Mpc.
The Binggeli effect
Authors: Biernacka M. , Panko E. , Godłowski W. , Bajan K. , Flin P.
Published: October 2016

We found the alignement of elongated clusters of BM type I and III (the excess of small values of the Δθ angles is observed), having range till about 60 h−1Mpc. The first one is probably connected with the origin of supergiant galaxy, while the second one with environmental effects in clusters, originated on the long filament or plane.
Co–evolution of black holes and galaxies: the role of selection biases
Authors: Portinari Laura
Published: October 2016

Quasars are tracers of the cosmological evolution of the Black Hole mass
– host galaxy relation, and indicate that the formation of BH
anticipated that of the host galaxies. We find that selection effects and
statistical biases dominate the interpretation of the observational results;
and co-evolution (= constant BH/galaxy mass ratio) is still compatible
with observations.
Answers from the Void: VIDE and its Applications
Authors: Sutter P. M. , Hamaus N. , Pisani A. , Lavaux G. , Wandelt B. D.
Published: October 2016

We discuss various applications ofvide, the Void IDentification and Examination toolkit, an open-source Python/C++ code for finding cosmic voids in galaxy redshift surveys and $N$-body simulations. Based on a substantially enhanced version ofZOBOV,videnot only finds voids, but also summarizes their properties, extracts statistical information, and provides a Python-based platform for more detailed analysis, such as manipulating void catalogs and particle members, filtering, plotting, computing clustering statistics, stacking, comparing catalogs, and fitting density profiles.videalso provides significant additional functionality for pre-processing inputs: for example,videcan work with volume- or magnitude-limited galaxy samples with arbitrary survey geometries, or dark matter particles or halo catalogs in a variety of common formats. It can also randomly subsample inputs and includes a Halo Occupation Distribution model for constructing mock galaxy populations.videhas been used for a wide variety of applications, from discovering a universal density profile to estimating primordial magnetic fields, and is publicly available athttp://bitbucket.org/cosmicvoids/vide\_publicandhttp://www.cosmicvoids.net.
Void asymmetries in the cosmic web: a mechanism for bulk flows
Authors: Bland-Hawthorn J. , Sharma S.
Published: October 2016

Bulk flows of galaxies moving with respect to the cosmic microwave background are well established observationally and seen in the most recent ΛCDM simulations. With the aid of an idealised Gadget-2 simulation, we show that void asymmetries in the cosmic web can exacerbate local bulk flows of galaxies. The {\it Cosmicflows-2} survey, which has mapped in detail the 3D structure of the Local Universe, reveals that the Local Group resides in a “local sheet” of galaxies that borders a “local void” with a diameter of about 40 Mpc. The void is emptying out at a rate of 16 km s-1Mpc-1. In a co-moving frame, the Local Sheet is found to be moving away from the Local Void at ∼ 260 km s-1. Our model shows how asymmetric collapse due to unbalanced voids on either side of a developing sheet or wall can lead to a systematic movement of the sheet. We conjectured that asymmetries could lead to a large-scale separation of dark matter and baryons, thereby driving a dependence of galaxy properties with environment, but we do {\it not} find any evidence for this effect.
The cosmic web in CosmoGrid void regions
Authors: Rieder Steven , van de Weygaert Rien , Cautun Marius , Beygu Burcu , Zwart Simon Portegies
Published: October 2016

We study the formation and evolution of the cosmic web, using the high-resolution CosmoGrid ΛCDM simulation. In particular, we investigate the evolution of the large-scale structure around void halo groups, and compare this to observations of the VGS-31 galaxy group, which consists of three interacting galaxies inside a large void.

The structure around such haloes shows a great deal of tenuous structure, with most of such systems being embedded in intra-void filaments and walls. We use the Nexus+} algorithm to detect walls and filaments in CosmoGrid, and find them to be present and detectable at every scale. The void regions embed tenuous walls, which in turn embed tenuous filaments. We hypothesize that the void galaxy group of VGS-31 formed in such an environment.
The ISW imprints of voids and superclusters on the CMB
Authors: Hotchkiss S. , Nadathur S. , Gottlöber S. , Iliev I. T. , Knebe A. , Watson W. A. , Yepes G.
Published: October 2016

We examine the stacked integrated Sachs-Wolfe (ISW) imprints on the CMB along the lines of sight of voids and superclusters in galaxy surveys, using the Jubilee ISW simulation and mock luminous red galaxy (LRG) catalogues. We show that the expected signal in the concordance \Lam CDM model is much smaller than the primary anisotropies arising at the last scattering surface and therefore any currently claimed detections of such an imprint cannot be caused by the ISW effect in \Lam CDM. We look for the existence of such a signal in the Planck CMB using a catalogue of voids and superclusters from the Sloan Digital Sky Survey (SDSS), but find a result completely consistent with \Lam CDM – i.e., a null detection.
The Void Galaxy Survey: Galaxy Evolution and Gas Accretion in Voids
Authors: Kreckel Kathryn , van Gorkom Jacqueline H. , Beygu Burcu , van de Weygaert Rien , van der Hulst J. M. , Aragon-Calvo Miguel A. , Peletier Reynier F.
Published: October 2016

Voids represent a unique environment for the study of galaxy evolution, as the lower density environment is expected to result in shorter merger histories and slower evolution of galaxies. This provides an ideal opportunity to test theories of galaxy formation and evolution. Imaging of the neutral hydrogen, central in both driving and regulating star formation, directly traces the gas reservoir and can reveal interactions and signs of cold gas accretion. For a new Void Galaxy Survey (VGS), we have carefully selected a sample of 59 galaxies that reside in the deepest underdensities of geometrically identified voids within the SDSS at distances of ∼100 Mpc, and pursued deep UV, optical, Hα, IR, and HI imaging to study in detail the morphology and kinematics of both the stellar and gaseous components. This sample allows us to not only examine the global statistical properties of void galaxies, but also to explore the details of the dynamical properties. We present an overview of the VGS, and highlight key results on the HI content and individually interesting systems. In general, we find that the void galaxies are gas rich, low luminosity, blue disk galaxies, with optical and HI properties that are not unusual for their luminosity and morphology. We see evidence of both ongoing assembly, through the gas dynamics between interacting systems, and significant gas accretion, seen in extended gas disks and kinematic misalignments. The VGS establishes a local reference sample to be used in future HI surveys (CHILES, DINGO, LADUMA) that will directly observe the HI evolution of void galaxies over cosmic time.
Molecular Gas and Star Formation in Void Galaxies
Authors: Das M. , Saito T. , Iono D. , Honey M. , Ramya S.
Published: October 2016

We present the detection of molecular gas using CO(1–0) line emission and followup Hα imaging observations of galaxies located in nearby voids. The CO(1–0) observations were done using the 45m telescope of the Nobeyama Radio Observatory (NRO) and the optical observations were done using the Himalayan Chandra Telescope (HCT). Although void galaxies lie in the most underdense parts of our universe, a significant fraction of them are gas rich, spiral galaxies that show signatures of ongoing star formation. Not much is known about their cold gas content or star formation properties. In this study we searched for molecular gas in five void galaxies using the NRO. The galaxies were selected based on their relatively higher IRAS fluxes or Hα line luminosities. CO(1–0) emission was detected in four galaxies and the derived molecular gas masses lie between (1 - 8)×109M⊙. The Hα imaging observations of three galaxies detected in CO emission indicates ongoing star formation and the derived star formation rates vary between from 0.2 – 1.0 M7odot; yr-1, which is similar to that observed in local galaxies. Our study shows that although void galaxies reside in underdense regions, their disks may contain molecular gas and have star formation rates similar to galaxies in denser environments.
Führungskräfte-Coaching bei Change Prozessen
Authors: Bickerich Katrin , Michel Alexandra
Published: October 2016

Zusammenfassung. Ziel dieser Längsschnittstudie ist es, die Wirkung von Führungskräfte-Coaching bei organisationalen Change Prozessen auf die berufliche Selbstwirksamkeitserwartung, das Führungsverhalten und den Affekt von Führungskräften zu evaluieren. Dabei wird der Einfluss von Autonomie und Managementunterstützung als moderierende Kontextbedingungen berücksichtigt. Den theoretischen Rahmen bildet das Job Demands-Resources Model ( Demerouti, Bakker, Nachreiner & Schaufeli, 2001 ). Mit einem quasi-experimentellen Kontrollgruppendesign wurden 66 Führungskräfte im mittleren Management unterschiedlicher Organisationen während laufender Change Prozesse (NEG= 28; NKG= 38) zu drei Messzeitpunkten befragt. Die Multilevel-Analysen ergaben signifikante Dreifach-Interaktionseffekte, die zeigen, dass Führungskräfte mit Coaching (EG) bei hoher Autonomie bzw. hoher Managementunterstützung nach sechs Monaten (T3) höhere Werte hinsichtlich beruflicher Selbstwirksamkeitserwartung, Führungsverhalten und positivem Affekt sowie niedrigere Werte im negativen Affekt aufweisen als Führungskräfte ohne Coaching (KG). Basierend auf den Ergebnissen werden praxisorientierte Handlungsempfehlungen für Führungskräfte, Coaches und Personalentwickler abgeleitet, damit Coaching bei organisationalen Veränderungen wirksam werden kann.