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A precise measurement of the curvature of the Universe is of prime importance for cosmology since it could not only confirm the paradigm of primordial inflation but also help in discriminating between different early-Universe scenarios. Recent observations, while broadly consistent with a spatially flat standard Λ Cold Dark Matter ( Λ CDM) model, show tensions that still allow (and, in some cases, even suggest) a few percent deviations from a flat universe. In particular, the Planck Cosmic Microwave Background power spectra, assuming the nominal likelihood, prefer a closed universe at more than 99% confidence level. While new physics could be at play, this anomaly may be the result of an unresolved systematic error or just a statistical fluctuation. However, since positive curvature allows a larger age of the Universe, an accurate determination of the age of the oldest objects provides a smoking gun in confirming or falsifying the current flat Λ CDM model.

Refereed/Peer-reviewed The present study provides evidence for a valid and reliable tool, the Academic Quality at Work Tool (AQ@workT), to investigate the quality of life at work in academics within the Italian university sector. The AQ@workT was developed by the QoL@Work research team, namely a group of expert academics in the field of work and organizational psychology affiliated with the Italian Association of Psychologists. The tool is grounded in the job demands-resources model and its psychometric properties were assessed in three studies comprising a wide sample of lecturers, researchers, and professors: a pilot study (N = 120), a calibration study (N = 1084), and a validation study (N = 1481). Reliability and content, construct, and nomological validity were supported, as well as measurement invariance across work role (researchers, associate professors, and full professors) and gender. Evidence from the present study shows that the AQ@workT represents a useful and reliable tool to assist university management to enhance quality of life, to manage work-related stress, and to mitigate the potential for harm to academics, particularly during a pandemic. Future studies, such as longitudinal tests of the AQ@workT, should test predictive validity among the variables in the tool.

We discuss axion dark matter detection via two mechanisms: spontaneous decays and resonant conversion in neutron star magnetospheres. For decays, we show that the brightness temperature signal, rather than flux, is a less ambiguous measure for selecting candidate objects. This is owing principally to the finite beam width of telescopes which prevents one from being sensitive to the total flux from the object. With this in mind, we argue that the large surface-mass-density of the galactic centre or the Virgo cluster centre offers the best chance of improving current constraints on the axion-photon coupling via spontaneous decays. For the neutron star case, we first carry out a detailed study of mixing in magnetised plasmas. We derive transport equations for the axion-photon system via a controlled gradient expansion, allowing us to address inhomogeneous mass-shell constraints for arbitrary momenta. We then derive a non-perturbative Landau-Zener formula for the conversion probability valid across the range of relativistic and non-relativistic axions and show that the standard perturbative resonant conversion amplitude is a truncation of this result in the non-adiabatic limit. Our treatment reveals that that infalling dark matter axions typically convert non-adiabatically in magnetospheres. We describe the limitations of one-dimensional mixing equations and explain how three-dimensional effects activate new photon polarisations, including longitudinal modes and illustrate these arguments with numerical simulations in higher dimensions. We find that the bandwidth of the radio signal is dominated by Doppler broadening from the relative motion of the neutron star with respect to the observer. Therefore, we conclude that the radio signal from the resonant decay is weaker than previously thought, which means one relies on local density peaks to probe weaker axion-photon couplings., Comment: 31 pages, 14 figures and 2 tables. Accepted by Phys. Rev. D. Comments welcome

The standard Λ Cold Dark Matter cosmological model provides a wonderful fit to current cosmological data, but a few statistically significant tensions and anomalies were found in the latest data analyses. While these anomalies could be due to the presence of systematic errors in the experiments, they could also indicate the need for new physics beyond the standard model. In this Letter of Interest we focus on the tension between Planck data and weak lensing measurements and redshift surveys, in the value of the matter energy density Ω m and the amplitude σ 8 (or the growth rate f σ 8 ) of cosmic structure. We list a few promising models for solving this tension, and discuss the importance of trying to fit multiple cosmological datasets with complete physical models, rather than fitting individual datasets with a few handpicked theoretical parameters.

Model-independent constraints on modified gravity models hitherto exist mainly on linear scales. A recently developed formalism presented a consistent parameterisation that is valid on all scales. Using this approach, we perform model-independent modified gravity $N$-body simulations on all cosmological scales with a time-dependent $\mu$. We present convergence tests of our simulations, and we examine how well existing fitting functions reproduce the non-linear matter power spectrum of the simulations. We find that although there is a significant variation in the accuracy of all of the fitting functions over the parameter space of our simulations, the ReACT framework delivers the most consistent performance for the matter power spectrum. We comment on how this might be improved to the level required for future surveys such as Euclid and the Vera Rubin Telescope (LSST). We also show how to compute weak-lensing observables consistently from the simulated matter power spectra in our approach, and show that ReACT also performs best when fitting the weak-lensing observables. This paves the way for a full model-independent test of modified gravity using all of the data from such upcoming surveys., Comment: 32 pages, 14 Figures; Comments welcome

Background Recently, comparative trials among biologics in ulcerative colitis (UC) provided conflicting results on their reciprocal superiority or equivalence. Therefore, in patients naive to biologics, the first-choice biological drug is uncertain. Methods In a retrospective, real-life, multicentre inception cohort study involving 11 Italian IBD tertiary centres, all consecutive patients, naive to biologics, treated with adalimumab (ADA), infliximab biosimilar (CTP-13), golimumab (GOL) or vedolizumab (VDZ) after their postmarketing approval (2014–2018) for moderate–severe active UC, were followed up for 1 year or until relapse. All drugs were compared with each other and to naive patients treated with IFX-originator (IFX-O, Remicade) in 2013–2014 as a reference group. A propensity score analysis was performed. The primary endpoint was the 1 year relapse-free, optimisation-free, steroid-free remission, defined as Mayo score ≤2, with bleeding subscore = 0, no relapse after first clinical remission and no optimisation with dose intensification or steroids courses. Multiple further secondary endpoints were analysed (Table 1). Results Two hundred ninety-six naive patients (ADA = 56, CTP-13 = 73, GOL = 60, VDZ = 34, IFX-O = 73) were included. The primary end-point was achieved in similar percentages in all groups, irrespective of optimisation. IFX-O and ADA had similar rates of clinical remission achieved once during the follow-up but higher rates than GOL and VDZ. The 1-year relapse rate, however, was lower with VDZ than ADA, GOL and IFX-O. Treatment failure for primary/secondary no response was higher with GOL than IFX-O and ADA. Treatment failures for intolerance were similar among all drugs. CTP-13 performed differently than the originator for some secondary end-points. Conclusion Based on a strict definition of clinical remission, all biologics appear equally effective at 1 year in patients naive to these drugs. IFX originator and ADA appear more effective in the induction phase, while patients responders to VDZ had more prolonged clinical remission. Some differences on secondary questionable outcomes between IFX biosimilar and originator have been observed.

Background Until 2014, infliximab originator (Remicade, IFX-O) was the only biological treatment approved in Italy for ulcerative colitis (UC), followed by the sequential approval of adalimumab (ADA), infliximab biosimilar (CTP-13), golimumab (GOL) and vedolizumab (VDZ). Recently, comparative trials among these drugs provided conflicting results on their reciprocal superiority or equivalence. Methods In a retrospective, real-life, multicenter inception cohort study involving 11 Italian IBD tertiary centres, all consecutive patients with moderate-to-severe active UC, treated with ADA, CTP-13, GOL or VDZ after their post-marketing approval (2014–2018) were followed-up for 1 year or until relapse. All drugs were compared with each other and to patients treated with Remicade in 2013–2014 (reference group). The 80% power calculation of the study required at least 75 patients in each arm. A propensity score analysis was performed. The primary endpoint was the 1 year relapse-free, optimisation-free, steroid-free remission, defined as Mayo partial score ≤2, with bleeding subscore = 0, no relapse after first clinical remission and no optimisation with dose intensification or steroids courses. Multiple further secondary endpoints were analysed (Table 1). Results 492 patients (ADA=90, CTP-13=105, GOL=79, VDZ=142, IFX-O=76) were included. Overall, 65% achieved clinical remission once during the follow-up, with IFX-O performing better than GOL and VDZ. The relapse rate was 24%, with the lowest rates with VDZ. The primary end-point was achieved in similar percentages in all groups, except for lower rates with GOL than IFX-O. IFX-O performed better than each other drug for other clinical outcomes (Table 1). Discontinuation for intolerance was similar among the drugs, but CTP-13 had more frequent adverse events (mainly infusion reactions) than ADA, VDZ and IFX-O. Conclusion Based on a strict definition of clinical remission, all biologics appear equally effective at 1 year, except for GOL vs. IFX originator. IFX-O appears more effective in multiple questionable clinical outcomes. IFX biosimilar had more adverse events than the other drugs. IFX originator should be used as the reference drug in head to head, controlled, comparison trials for current and future biologics in UC.

Nowadays, data-centers are largely under-utilized because resource allocation is based on reservation mechanisms which ignore actual resource utilization. Indeed, it is common to reserve resources for peak demand, which may occur only for a small portion of the application life time. As a consequence, cluster resources often go under-utilized. In this work, we propose a mechanism that improves compute cluster utilization and their responsiveness, while preventing application failures due to contention in accessing finite resources such as RAM. Our method monitors resource utilization and employs a data-driven approach to resource demand forecasting, featuring quantification of uncertainty in the predictions. Using demand forecast and its confidence, our mechanism modulates cluster resources assigned to running applications, and reduces the turnaround time by more than one order of magnitude while keeping application failures under control. Thus, tenants enjoy a responsive system and providers benefit from an efficient cluster utilization.

We derive the mass-temperature relation using an improved top-hat model and a continuous formation model which takes into account the effects of the ordered angular momentum acquired through tidal-torque interaction between clusters, random angular momentum, dynamical friction, and modifications of the virial theorem to include an external pressure term usually neglected. We show that the mass-temperature relation differs from the classical self-similar behavior, $M \propto T^{3/2}$, and shows a break at $3--4$ keV, and a steepening with a decreasing cluster temperature. We then compare our mass-temperature relation with those obtained in the literature with $N$-body simulations for $f(R)$ and symmetron models. We find that the mass-temperature relation is not a good probe to test gravity theories beyond Einstein's general relativity, because the mass-temperature relation of the $\Lambda$CDM model is similar to that of the modified gravity theories., Comment: 11 pages; 2 figures; matches the published Phys. Rev. D version

We investigate generalized Einstein-Aether theories that are compatible with the Planck Cosmic Microwave Background (CMB) temperature anisotropy, polarisation, and lensing data. For a given dark energy equation of state, $w_{\rm de}$, we formulate a designer approach and we investigate their impact on the CMB temperature anisotropy and matter power spectra. We use the Equation of State approach to parametrize the perturbations and find that this approach is particularly useful in identifying the most suitable and numerically efficient parameters to explore in a Markov chain Monte Carlo (MCMC) analysis. We find the data constrains models with $w_{\rm de} = -1$ to be compatible with $\Lambda$CDM. For $w_{\rm de} \not= -1$ models, which avoid the gravitational waves constraint through the entropy perturbation, we constrain $w_{\rm de}$ to be $w_{\rm de } = -1.06^{+0.08}_{-0.03}$ (CMB) and $w_{\rm de } =-1.04^{+0.05}_{-0.02}$ (CMB+Lensing) at $68\%$C.L., and find that these models can be different from $\Lambda$CDM and still be compatible with the data. We also find that these models can ameliorate some anomalies in $\Lambda$CDM when confronted with data, such as the low-$\ell$ and high-$k$ power in the CMB temperature anisotropy and matter power spectra respectively, but not simultaneously. We also investigate the anomalous lensing amplitude, quantified by $A_{\rm lens}$, and find that that for $w_{\rm de} = -1$ models, $A_{\rm lens} = 1.15^{+0.07}_{-0.08}$ (CMB) and $A_{\rm lens} = 1.12\pm0.05$ (CMB+Lensing) at $68\%$C.L. $\sim$ 2$\sigma$ larger than expected, similar to previous analyses of $\Lambda$CDM., Comment: 20 pages, 9 figures, 4 tables. Public version of the code will be released upon acceptance by PRD

The accelerated expansion of the universe is a rather established fact in cosmology and many different models have been proposed as a viable explanation. Many of these models are based on the standard general relativistic framework of non-interacting fluids or more recently of coupled (interacting) dark energy models, where dark energy (the scalar field) is coupled to the dark matter component giving rise to a fifth-force. An interesting alternative is to couple the scalar field directly to the gravity sector via the Ricci scalar. These models are dubbed non-minimally coupled models and give rise to a time-dependent gravitational constant. In this work we study few models falling into this category and describe how observables depend on the strength of the coupling. We extend recent work on the subject by taking into account also the effects of the perturbations of the scalar field and showing their relative importance on the evolution of the mass function. By working in the framework of the spherical collapse model, we show that perturbations of the scalar field have a limited impact on the growth factor (for small coupling constant) and on the mass function with respect to the case where perturbations are neglected., Comment: 13 pages, 9 figures, accepted in MNRAS

It is known that diabetes is associated with the development of premature atherosclerosis and microvascular complications and consequently increased cardiovascular (CV) morbidity and mortality. In ...

We review the Equation of State (EoS) approach to dark sector perturbations and apply it to $f(\mathcal{R})$ gravity models of dark energy. We show that the EoS approach is numerically stable and use it to set observational constraints on designer models. Within the EoS approach we build an analytical understanding of the dynamics of cosmological perturbations for the designer class of $f(\mathcal{R})$ gravity models, characterised by the parameter $B_0$ and the background equation of state of dark energy $w$. When we use the Planck Cosmic Microwave Background (CMB) temperature anisotropy, polarisation and lensing data as well as the Baryonic Acoustic Oscillation (BAO) data from SDSS and WiggleZ, we find $B_0

Until now object storage has not been a first-class citizen of the Apache Hadoop ecosystem including Apache Spark. Hadoop connectors to object storage have been based on file semantics, an impedance mismatch, which leads to low performance and the need for an additional consistent storage system to achieve fault tolerance. In particular, Hadoop depends on its underlying storage system and its associated connector for fault tolerance and allowing speculative execution. However, these characteristics are obtained through file operations that are not native for object storage, and are both costly and not atomic. As a result these connectors are not efficient and more importantly they cannot help with fault tolerance for object storage. We introduce Stocator, whose novel algorithm achieves both high performance and fault tolerance by taking advantage of object storage semantics. This greatly decreases the number of operations on object storage as well as enabling a much simpler approach to dealing with the eventually consistent semantics typical of object storage. We have implemented Stocator and shared it in open source. Performance testing with Apache Spark shows that it can be 18 times faster for write intensive workloads and can perform 30 times fewer operations on object storage than the legacy Hadoop connectors, reducing costs both for the client and the object storage service provider.

We explore the constraints on dark sector models imposed by the recent observation of coincident gravitational waves and gamma rays from a binary neutron star merger, GW170817. Rather than focusing on specific models as has been considered by other authors, we explore this in the context of the equation of state approach of which the specific models are special cases. After confirming the strong constraints found by others for Horndeski, Einstein-Aether and massive gravity models, we discuss how it is possible to construct models which might evade the constraints from GW170817 but still leading to cosmologically interesting modifications to gravity. Possible examples are ``miracle cancellations" such as in $f(R)$ models, nonlocal models and higher-order derivatives. The latter two rely on the dimensionless ratio of the wave number of the observed gravitational waves to the Hubble expansion rate being very large ($\sim10^{19}$) which is used to suppress modifications to the speed of gravitational waves., Comment: 10 pages

The rate of structure formation in the Universe is different in homogeneous and clustered dark energy models. The degree of dark energy clustering depends on the magnitude of its effective sound speed $c^{2}_{\rm eff}$ and for $c_{\rm eff}=0$ dark energy clusters in a similar fashion to dark matter while for $c_{\rm eff}=1$ it stays (approximately) homogeneous. In this paper we consider two distinct equations of state for the dark energy component, $w_{\rm d}=const$ and $w_{\rm d}=w_0+w_1\left(\frac{z}{1+z}\right)$ with $c_{\rm eff}$ as a free parameter and we try to constrain the dark energy effective sound speed using current available data including SnIa, Baryon Acoustic Oscillation, CMB shift parameter ({\em Planck} and {\em WMAP}), Hubble parameter, Big Bang Nucleosynthesis and the growth rate of structures $f\sigma_{8}(z)$. At first we derive the most general form of the equations governing dark matter and dark energy clustering under the assumption that $c_{\rm eff}=const$. Finally, performing an overall likelihood analysis we find that the likelihood function peaks at $c_{\rm eff}=0$, however the dark energy sound speed is degenerate with respect to the cosmological parameters, namely $\Omega_{\rm m}$ and $w_{\rm d}$., Comment: This paper has been accepted for publication in MNRAS 452, 2015, 2930-2939

The purpose of this study was to examine the relationship among adolescents’ indecisiveness, adolescents’ self-esteem, and maternal and paternal psychological control by focusing on the differences in the relationship among these variables across adolescent genders. A total of 381 Italian adolescents (215 boys and 166 girls), aged from 13 to 17years, completed self-report measures of parental psychological control, self-esteem and indecisiveness. Since previous studies have highlighted indirect relations between family characteristics and indecisiveness, structural equation modeling (SEM) methods were used for testing self-esteem as a possible mediator. In particular, a multiple group analysis (based on adolescent genders) was conducted to determine if the resultant model differed for boys and girls. The results showed that self-esteem acted as mediator of the relation between paternal psychological control and boys’ indecisiveness. Moreover, this study shows how maternal and paternal psychological control is differently related to children’s development during early adolescence, emphasizing the important relationship between paternal psychological control and boys’ indecisiveness.

This study attempted to examine the validity of the Italian version of the Career Factors Inventory (CFI), a psychometric tool widely used in the assessment of cognitive and personal–emotional dimensions of career indecision, among a sample of 2,060 Italian students attending high school and university. Recurring to both exploratory and confirmatory factor analyses, the original four-factor structure was confirmed and returned, in line with the literature, satisfactory reliability indices; moreover, CFI subscales showed intercorrelations consistent with previous studies, albeit lower in some cases. Subsequently, convergent validity between the four CFI subscales and other scales via zero-order correlation was tested, confirming previous evidence except for need for career information. In conclusion, consistent with previous studies, the Italian version of the CFI showed to be a valid and reliable instrument for the evaluation of dimensions of career indecision.

Data is the natural resource of the 21st century. It is being produced at dizzying rates, e.g., for genomics, for media and entertainment, and for Internet of Things. Object storage systems such as Amazon S3, Azure Blob storage, and IBM Cloud Object Storage, are highly scalable distributed storage systems that offer high capacity, cost effective storage. But it is not enough just to store data; we also need to derive value from it. Apache Spark is the leading big data analytics processing engine combining MapReduce, SQL, streaming, and complex analytics. We present Stocator, a high performance storage connector, enabling Spark to work directly on data stored in object storage systems, while providing the same correctness guarantees as Hadoop's original storage system, HDFS. Current object storage connectors from the Hadoop community, e.g., for the S3 and Swift APIs, do not deal well with eventual consistency, which can lead to failure. These connectors assume file system semantics, which is natural given that their model of operation is based on interaction with HDFS. In particular, Spark and Hadoop achieve fault tolerance and enable speculative execution by creating temporary files, listing directories to identify these files, and then renaming them. This paradigm avoids interference between tasks doing the same work and thus writing output with the same name. However, with eventually consistent object storage, a container listing may not yet include a recently created object, and thus an object may not be renamed, leading to incomplete or incorrect results. Solutions such as EMRFS [1] from Amazon, S3mper [4] from Netflix, and S3Guard [2], attempt to overcome eventual consistency by requiring additional strongly consistent data storage. These solutions require multiple storage systems, are costly, and can introduce issues of consistency between the stores. Current object storage connectors from the Hadoop community are also notorious for their poor performance for write workloads. This, too, stems from their use of the rename operation, which is not a native object storage operation; not only is it not atomic, but it must be implemented using a costly copy operation, followed by delete. Others have tried to improve the performance of object storage connectors by eliminating rename, e.g., the Direct-ParquetOutputCommitter [5] for S3a introduced by Databricks, but have failed to preserve fault tolerance and speculation. Stocator takes advantage of object storage semantics to achieve both high performance and fault tolerance. It eliminates the rename paradigm by writing each output object to its final name. The name includes both the part number and the attempt number, so that multiple attempts to write the same part use different objects. Stocator proposes to extend an already existing success indicator object written at the end of a Spark job, to include a manifest with the names of all the objects that compose the final output; this ensures that a subsequent job will correctly read the output, without resorting to a list operation whose results may not be consistent. By leveraging the inherent atomicity of object creation and using a manifest we obtain fault tolerance and enable speculative execution; by avoiding the rename paradigm we greatly decrease the complexity of the connector and the number of operations on the object storage. We have implemented our connector and shared it in open source [3]. We have compared its performance with the S3a and Hadoop Swift connectors over a range of workloads and found that it executes many fewer operations on the object storage, in some cases as few as one thirtieth. Since the price for an object storage service typically includes charges based on the number of operations executed, this reduction in operations lowers the costs for clients in addition to reducing the load on client software. It also reduces costs and load for the object storage provider since it can serve more clients with the same amount of processing power. Stocator also substantially increases performance for Spark workloads running over object storage, especially for write intensive workloads, where it is as much as 18 times faster.

We present Stocator, a high performance object store connector for Apache Spark, that takes advantage of object store semantics. Previous connectors have assumed file system semantics, in particular, achieving fault tolerance and allowing speculative execution by creating temporary files to avoid interference between worker threads executing the same task and then renaming these files. Rename is not a native object store operation; not only is it not atomic, but it is implemented using a costly copy operation and a delete. Instead our connector leverages the inherent atomicity of object creation, and by avoiding the rename paradigm it greatly decreases the number of operations on the object store as well as enabling a much simpler approach to dealing with the eventually consistent semantics typical of object stores. We have implemented Stocator and shared it in open source. Performance testing shows that it is as much as 18 times faster for write intensive workloads and performs as much as 30 times fewer operations on the object store than the legacy Hadoop connectors, reducing costs both for the client and the object storage service provider.

This work addresses the problem of scheduling user-defined analytic applications, which we define as high-level compositions of frameworks, their components, and the logic necessary to carry out work. The key idea in our application definition, is to distinguish classes of components, including rigid and elastic types: the first being required for an application to make progress, the latter contributing to reduced execution times. We show that the problem of scheduling such applications poses new challenges, which existing approaches address inefficiently. Thus, we present the design and evaluation of a novel, flexible heuristic to schedule analytic applications, that aims at high system responsiveness, by allocating resources efficiently. Our algorithm is evaluated using trace-driven simulations, with large-scale real system traces: our flexible scheduler outperforms a baseline approach across a variety of metrics, including application turnaround times, and resource allocation efficiency. We also present the design and evaluation of a full-fledged system, which we have called Zoe, that incorporates the ideas presented in this paper, and report concrete improvements in terms of efficiency and performance, with respect to prior generations of our system.

This study aims to evaluate the factor structure of Career Decision Self-Efficacy scale-short form in a sample of Italian high school adolescents. confirmatory factor analysis (CFA) was used to test the degree to which a one-factor structure and a five-factor structure provided the best fit. In view of available research the five-factor structure was expected to provide the best fit. Moreover, factorial invariance in males and females was tested. It was expected to be invariant across groups. As expected the five-factor structure showed a better fit than the one-factor model and the factorial invariance resulted invariant across boys and girls.

We study the nature of potentials in scalar field based models for dark energy - with both canonical and noncanonical kinetic terms. We calculate numerically, and using an analytic approximation around $a\approx 1$, potentials for models with constant equation-of-state parameter, $w_{\phi}$. We find that for a wide range of models with canonical and noncanonical kinetic terms there is a simple approximation for the potential that holds when the scale factor is in the range $0.6\lesssim a\lesssim 1.4$. We discuss how this form of the potential can also be used to represent models with non-constant $w_{\phi}$ and, hence, how it could be used in reconstruction from cosmological data., Comment: 17 pages, 6 figures. Accepted by Phys. Rev. D

An increasing number of Analytics-as-a-Service solutions has recently seen the light, in the landscape of cloud-based services. These services allow flexible composition of compute and storage components, that create powerful data ingestion and processing pipelines. This work is a first attempt at an experimental evaluation of analytic application performance executed using a wide range of storage service configurations. We present an intuitive notion of data locality, that we use as a proxy to rank different service compositions in terms of expected performance. Through an empirical analysis, we dissect the performance achieved by analytic workloads and unveil problems due to the impedance mismatch that arise in some configurations. Our work paves the way to a better understanding of modern cloud-based analytic services and their performance, both for its end-users and their providers., Comment: Longer version of the paper in Submission at IEEE CLOUD'16

{abridged} We study the imprints on the formation and evolution of cosmic structures of dynamical dark energy models, characterized by an oscillating equation of state. The redshift evolution of the equation of state parameter w(z) for dark energy is characterized by two parameters, describing the amplitude and the frequency of the oscillations. We consider six different oscillating dark energy models, each characterized by a different set of parameter values. Under the common assumption that dark energy is not clustering on the scales of interest, we study different aspects of cosmic structure formation. In particular, we self-consistently solve the spherical collapse problem. We then estimate the behavior of several cosmological observables, such as the linear growth factor, the Integrated Sachs-Wolfe (ISW) effect, the number counts of massive structures, and the matter and cosmic shear power spectra. We show that, independently of the amplitude and the frequency of the dark energy oscillations, none of the aforementioned observables show an oscillating behavior as a function of redshift. This is a consequence of the said observables' being integrals over some functions of the expansion rate over cosmic history. We also notice that deviations with respect to the expectations for a fiducial LambdaCDM cosmology are generically small, and in the majority of the cases distinguishing an oscillating dark energy model would be difficult. Exceptions to this conclusion are provided by the cosmic shear power spectrum, which for some of the models shows a difference at the level of \sim 10% over a wide range of angular scales, and the abundance of galaxy clusters, which is modified at the $\sim 10-20%$ level at $z \gtrsim 0.6$ for future wide weak lensing surveys.

(abridged) We explore the imprints of deviations from Gaussian primordial density fluctuations on the skeleton of the large-scale matter distribution as mapped through cosmological weak lensing. We computed the skeleton length of simulated effective convergence maps covering $\sim 35$ sq. deg each, extracted from a suite of cosmological $n-$body runs with different levels of local primordial non-Gaussianity. The latter is expected to alter the structure formation process with respect to the fiducial Gaussian scenario, and thus to leave a signature on the cosmic web. We found that alterations of the initial conditions consistently modify both the cumulative and the differential skeleton length, although the effect is generically smaller than the cosmic variance and depends on the smoothing of the map prior to the skeleton computation. Nevertheless, the qualitative shape of these deviations is rather similar to their primordial counterparts, implying that skeleton statistics retain good memory of the initial conditions. We performed a statistical analysis in order to find out at what Confidence Level primordial non-Gaussianity could be constrained by the skeleton test on cosmic shear maps of the size we adopted. At 68.3% Confidence Level we found an error on the measured level of primordial non-Gaussianity of $\Delta f_\mathrm{NL}\sim 300$, while at 90% Confidence Level it is of $\Delta f_\mathrm{NL}\sim 500$. While these values by themselves are not competitive with the current constraints, weak lensing maps larger than those used here would have a smaller field-to-field variance, and thus would likely lead to tighter constraints. A rough estimate indicates $\Delta f_\mathrm{NL} \sim$ a few tens at 68.3% Confidence Level for an all-sky weak lensing survey.

While usually cosmological initial conditions are assumed to be Gaussian, inflationary theories can predict a certain amount of primordial non-Gaussianity which can have an impact on the statistical properties of the lensing observables. In order to evaluate this effect, we build a large set of realistic maps of different lensing quantities starting from light-cones extracted from large dark-matter only N-body simulations with initial conditions corresponding to different levels of primordial local non-Gaussianity strength $f_{\rm NL}$. Considering various statistical quantities (PDF, power spectrum, shear in aperture, skewness and bispectrum) we find that the effect produced by the presence of primordial non-Gaussianity is relatively small, being of the order of few per cent for values of $|f_{\rm NL}|$ compatible with the present CMB constraints and reaching at most 10-15 per cent for the most extreme cases with $|f_{\rm NL}|=1000$. We also discuss the degeneracy of this effect with the uncertainties due to the power spectrum normalization $\sigma_8$ and matter density parameter $\Omega_{\rm m}$, finding that an error in the determination of $\sigma_8$ ($\Omega_{\rm m}$) of about 3 (10) per cent gives differences comparable with non-Gaussian models having $f_{\rm NL}=\pm 1000$. These results suggest that the possible presence of an amount of primordial non-Gaussianity corresponding to $|f_{\rm NL}|=100$ is not hampering a robust determination of the main cosmological parameters in present and future weak lensing surveys, while a positive detection of deviations from the Gaussian hypothesis is possible only breaking the degeneracy with other cosmological parameters and using data from deep surveys covering a large fraction of the sky.

Mobile devices are among the most disruptive technologies of the last years, gaining even more diffusion and success in the daily life of a wide range of people categories. Unfortunately, while the number of mobile devices implicated in crime activities is relevant and growing, the capability to perform the forensic analysis of such devices is limited both by technological and methodological problems. In this paper, we focus on Anti-Forensic techniques applied to mobile devices, presenting some fully automated instances of such techniques to Android devices. Furthermore, we tested the effectiveness of such techniques versus both the cursory examination of the device and some acquisition tools.

Purpose: To compare new-generation multifocal intraocular lenses (IOLs) with monofocal IOLs. Design: Randomized prospective clinical trial. Participants: Sixty-two consecutive patients with cataract, seen between January of 2005 and January of 2006 at the Department of Ophthalmology of Palermo University Hospital in Italy, were bilaterally implanted with monofocal (AR 40, Advanced Medical Optics [AMO], Santa Ana, CA; 15 patients), multifocal refractive (Array SA40N, AMO; 16 patients), multifocal refractive (ReZoom, AMO; 15 patients), or multifocal diffractive pupil-independent (Tecnis ZM900, AMO; 16 patients) IOLs. Intervention: Bimanual phacoemulsification. Main Outcome Measures: Primary outcomes were far, near, and intermediate visual acuity of the 4 IOL-implanted groups. Secondary outcomes were defocusing curves, contrast sensitivity, patients' quality of life (7-item visual function questionnaire [VF-7], halos and glare presence, overall satisfaction), and spectacle independence. Snellen visual acuity was measured as uncorrected visual acuity (UCVA), best corrected visual acuity (BCVA), uncorrected near visual acuity (UCNVA), best distance corrected near visual acuity (BDCNVA), best corrected near visual acuity (BCNVA), uncorrected intermediate visual acuity (UCIVA), and best distance corrected intermediate visual acuity (BDCIVA). Results: UCNVA was 20/50 in the monofocal IOL group, compared with 20/32 or better in the multifocal IOL groups (P

Background Clinical studies comparing trabeculectomy augmented with Ologen implant (OLO) versus trabeculectomy plus mitomycin-C (MMC) show contradictory results. To obtain long-term data, we report an extended 5-year follow-up trial evaluating the safety and efficacy of OLO as adjuvant compared to low-dosage MMC in trabeculectomy. Methods Forty glaucoma patients (40 eyes) assigned to trabeculectomy with MMC or Ologen. Primary outcome: target IOP at ≤21, ≤17 and ≤15 mmHg; complete and qualified success endpoint rates. Secondary outcomes: visual acuity (VA), mean deviation (MD), bleb evaluation, according to Moorfields Bleb Grading System (MBGS); spectral domain OCT (SD-OCT) bleb examination; number of glaucoma medications; frequency of postoperative complications. Results The mean preoperative IOP was 26.7(±5.2) in MMC and 27.3(±6.0) in OLO eyes. Mean 60-month percentage reduction in IOP was significant in both groups [40.9 (±14.2) and 42.1(±13.3) P = 0.01], with an endpoint value of 15.2 (±3.2) and 15.8 (±2.3) mmHg in MMC and OLO, respectively. Complete success rates at ≤ 21 mmHg target IOP were 65 % and 70 %, at ≤17 mm Hg 60 % and 55 %, and at the ≤15 mm Hg target IOP 35 % and 45 % in MMC and OLO, respectively. The Kaplan–Meier curves did not differ both for complete and qualified success at any target IOP, with no significant endpoint intergroup difference at ≤ 15 mm Hg (log-rank P = 0.595).The intergroup MBGS scores differed due to reduced central and peripheral vascularity in MMC group (P = 0.027; P = 0.041). SD-OCT analysis denied differences in bleb height between MMC vs OLO (140.5 ± 20.3 μ vs 129.2 ± 19.3 μ respectively; P =0.079). Mean antiglaucoma medications were significantly reduced (P

In the present paper, we compare the predictions of two well known mechanisms considered able to solve the cusp/core problem (a. supernova feedback; b. baryonic clumps-DM interaction) by comparing their theoretical predictions to recent observations of the inner slopes of galaxies with masses ranging from dSphs to normal spirals. We compare the $\alpha$-$V_{\rm rot}$ and the $\alpha$-$M_{\ast}$ relationships, predicted by the two models with high resolution data coming from \citep{Adams2014,Simon2005}, LITTLE THINGS \citep{Oh2015}, THINGS dwarves \citep{Oh2011a,Oh2011b}, THINGS spirals \citep{Oh2015}, Sculptor, Fornax and the Milky Way. The comparison of the theoretical predictions with the complete set of data shows that the two models perform similarly, while when we restrict the analysis to a smaller subsample of higher quality, we show that the method presented in this paper (baryonic clumps-DM interaction) performs better than the one based on supernova feedback. We also show that, contrarily to the first model prediction, dSphs of small mass could have cored profiles. This means that observations of cored inner profiles in dSphs having a stellar mass $, Comment: 22 pages, 5 figures, accepted by A&SS

In this work we study the relevance of the cosmic web and substructures on the matter and lensing power spectra measured from halo mock catalogues extracted from the N-body simulations. Since N-body simulations are computationally expensive, it is common to use faster methods that approximate the dark matter field as a set of halos. In this approximation, we replace mass concentrations in N-body simulations by a spherically symmetric Navarro-Frenk-White halo density profile. We also consider the full mass field as the sum of two distinct fields: dark matter halos ($M>9\times 10^{12}~M_{\odot}$/h) and particles not included into halos. Mock halos reproduce well the matter power spectrum, but underestimate the lensing power spectrum on large and small scales. For sources at $z_{\rm s}=1$ the lensing power spectrum is underestimated by up to 40% at $\ell\approx 10^4$ with respect to the simulated halos. The large scale effect can be alleviated by combining the mock catalogue with the dark matter distribution outside the halos. In addition, to evaluate the contribution of substructures we have smeared out the intra-halo substructures in a N-body simulation while keeping the halo density profiles unchanged. For the matter power spectrum the effect of this smoothing is only of the order of 5%, but for lensing substructures are much more important: for $\ell\approx 10^4$ the internal structures contribute 30% of the total spectrum. These findings have important implications in the way mock catalogues have to be created, suggesting that some approximate methods currently used for galaxy surveys will be inadequate for future weak lensing surveys., 16 pages, 18 figures, submitted to MNRAS

In this work we investigate the spherical collapse model in flat FRW dark energy universes. We consider the Holographic Dark Energy (HDE) model as a dynamical dark energy scenario with a slowly time-varying equation-of-state (EoS) parameter $w_{\rm de}$ in order to evaluate the effects of the dark energy component on structure formation in the universe. We first calculate the evolution of density perturbations in the linear regime for both phantom and quintessence behavior of the HDE model and compare the results with standard Einstein-de Sitter (EdS) and $\Lambda$CDM models. We then calculate the evolution of two characterizing parameters in the spherical collapse model, i.e., the linear density threshold $\delta_{\rm c}$ and the virial overdensity parameter $\Delta_{\rm vir}$. We show that in HDE cosmologies the growth factor $g(a)$ and the linear overdensity parameter $\delta_{\rm c}$ fall behind the values for a $\Lambda$CDM universe while the virial overdensity $\Delta_{\rm vir}$ is larger in HDE models than in the $\Lambda$CDM model. We also show that the ratio between the radius of the spherical perturbations at the virialization and turn-around time is smaller in HDE cosmologies than that predicted in a $\Lambda$CDM universe. Hence the growth of structures starts earlier in HDE models than in $\Lambda$CDM cosmologies and more concentrated objects can form in this case. It has been shown that the non-vanishing surface pressure leads to smaller virial radius and larger virial overdensity $\Delta_{\rm vir}$. We compare the predicted number of halos in HDE cosmologies and find out that in general this value is smaller than for $\Lambda$CDM models at higher redshifts and we compare different mass function prescriptions. Finally, we compare the results of the HDE models with observations., Comment: accepted in MNRAS

We examine the dynamics of scalar perturbations in closed Friedmann-Lema\^itre-Robertson- Walker (FLRW) universes in the framework of Brane World theory with a timelike extra dimension. In this scenario, the unperturbed Friedmann equations contain additional terms arising from the bulk-brane interaction that implement non-singular bounces in the models with a cosmological constant and non-interacting perfect fluids. The structure of the phase-space of the models allows for two basic configurations, namely, one bounce solutions or eternal universes. Assuming that the matter content of the model is given by dust and radiation, we derive the dynamical field equations for scalar hydrodynamical perturbations considering either a conformally flat (de Sitter) bulk or a perturbed bulk. We perform a numerical analysis which can shed some light on the study of cosmological scalar perturbations in bouncing brane world models. From a mathematical point of view we show that although the bounce enhances the amplitudes of scalar perturbations for one bounce models in the case of a de Sitter bulk, the amplitudes of the perturbations remain sufficiently small and bounded relative to the background values up to a certain scale. For one bounce models in the case of a perturbed bulk the amplitudes of all perturbations (apart from the Weyl fluid energy density) remain sufficiently small and bounded relative to the background values for any scale of the perturbations. We also discuss and compare the stability and bounded behaviour of the perturbations in the late accelerated phase of one bounce solutions. For eternal universes we argue that some of these features are maintained only for early times (typically of the order of the first bounce). In this sense we show that eternal solutions are highly unstable configurations considering the background model of this paper., Comment: 15 pages, 29 figures. Accepted for publication in Physical Review D

We study, for the first time, how shear and angular momentum modify typical parameters of the spherical collapse model, in dark energy dominated universes. In particular, we study the linear density threshold for collapse $\delta_\mathrm{c}$ and the virial overdensity $\Delta_\mathrm{V}$, for several dark-energy models and its influence on the cumulative mass function. The equations of the spherical collapse are those obtained in Pace et al. (2010), who used the fully nonlinear differential equation for the evolution of the density contrast derived from Newtonian hydrodynamics, and assumed that dark energy is present only at the background level. With the introduction of the shear and rotation terms, the parameters of the spherical collapse model are now mass-dependant. The results of the paper show, as expected, that the new terms considered in the spherical collapse model oppose the collapse of perturbations on galactic scale giving rise to higher values of the linear overdensity parameter with respect to the non-rotating case. We find a similar effect also for the virial overdensity parameter. For what concerns the mass function, we find that its high mass tail is suppressed, while the low mass tail is slightly affected except in some cases, e.g. the Chaplygin gas case., Comment: 10 pages, 5 figures; MNRAS accepted

We study the impact of Early Dark Energy fluctuations in the linear and non-linear regimes of structure formation. In these models the energy density of dark energy is non-negligible at high redshifts and the fluctuations in the dark energy component can have the same order of magnitude of dark matter fluctuations. Since two basic approximations usually taken in the standard scenario of quintessence models, that both dark energy density during the matter dominated period and dark energy fluctuations on small scales are negligible, are not valid in such models, we first study approximate analytical solutions for dark matter and dark energy perturbations in the linear regime. This study is helpful to find consistent initial conditions for the system of equations and to analytically understand the effects of Early Dark Energy and its fluctuations, which are also verified numerically. In the linear regime we compute the matter growth and variation of the gravitational potential associated with the Integrated Sachs-Wolf effect, showing that these observables present important modifications due to Early Dark Energy fluctuations, though making them more similar to $\Lambda$CDM model. We also make use of the Spherical Collapse model to study the influence of Early Dark Energy fluctuations in the nonlinear regime of structure formation, especially on $\delta_c$ parameter, and their contribution to the halo mass, which we show can be of the order of 10%. We finally compute how the number density of halos is modified in comparison to $\Lambda$CDM model and address the problem of how to correct the mass function in order to take into account the contribution of clustered dark energy. We conclude that the inhomogeneous Early Dark Energy models are more similar to $\Lambda$CDM model than its homogeneous counterparts., Comment: 26 pages and 12 figures, improved discussion, matches the accepted by JCAP

Background Ocular syphilis is often difficult to diagnose because of the wide variation in clinical features. HIV co-infection may further complicate the picture. Case presentation Herein the authors report an unusual primary syphilitic ocular lesion in a 45-year-old Italian HIV-infected bisexual man who presented with a unilateral eyelid lesion. Associated precocious signs and symptoms in the posterior segment of both eyes, bilateral chorioretinitis and uveitis, are described. Intravenous penicillin and steroid treatment produced a rapid improvement in clinical status and complete resolution. Conclusions Careful questioning about sexual behavior is crucial for unmasking unusual features of ocular syphilis in HIV-infected subjects.

Objective: To evaluate the biomechanical scenario of platform switching geometric implant-abutment configuration relative to standard configurations by means of finite element analysis.Study Design: A 3D Finite Element Analysis (FEA) was performed on 3 different implant-abutment configurations: a 3.8 mm implant with a matching diameter abutment (Standard Control Design, SCD), a 5.5 mm implant with matching diameter abutment (Wider Control Design, WCD), and a 5.5mm implant with a 3.8 mm abutment (Experimental Design, ED). All the different experimental groups were discretized to over 60000 elements and 100000 nodes, and 130N vertical (axial) and 90N horizontal loads were applied on the coronal portion of the abutment. Von Mises stresses were evaluated and maximum and minimum values were acquired for each implantabutment configuration. Results: The load-induced Von Mises stress (maximum to minumum ranges) on the implant ranged from 150 MPa to 58 Pa (SCD); 45 MPa to 55 Pa (WCD); 190 MPa to 64 Pa (ED). The Von Mises stress on the abutment ranged from 150 MPa to 52 MPa (SCD); 70 MPa to 55 MPa (WCD), and 85 MPa to 42 MPa respectively (ED). The maximum stresses transmitted from the implant-abutment system to the cortical and trabecular bone were 67 Pa and 52 MPa (SCD); 54 Pa and 27 MPa (WCD); 64 Pa and 42 MPa (ED), respectively. When the implant body was evaluated for stresses, a substantial decrease in their levels were observed at the threaded implant region due to the diametral mismatch between implant and abutment for the ED configuration. Conclusion: The platform switching configuration led to not only to a relative decrease in stress levels compared to narrow and wide standard configurations, but also to a notable stress field shift from bone towards the implant system, potentially resulting in lower crestal bone overloading. © Medicina Oral S. L.

We study the spherical collapse model for several dark energy scenarios using the fully nonlinear differential equation for the evolution of the density contrast within homogeneous spherical overdensities derived from Newtonian hydrodynamics. While mathematically equivalent to the more common approach based on the differential equation for the radius of the perturbation, this approach has substantial conceptual as well as numerical advantages. Among the most important are that no singularities at early times appear, which avoids numerical problems in particular in applications to cosmologies with dynamical and early dark energy, and that the assumption of time-reversal symmetry can easily be dropped where it is not strictly satisfied. We use this approach to derive the two parameters characterising the spherical-collapse model, i.e.~the linear density threshold for collapse $\delta_\mathrm{c}$ and the virial overdensity $\Delta_\mathrm{V}$, for a broad variety of dark-energy models and to reconsider these parameters in cosmologies with early dark energy. We find that, independently of the model under investigation, $\delta_\mathrm{c}$ and $\Delta_\mathrm{V}$ are always very close to the values obtained for the standard $\Lambda$CDM model, arguing that the abundance of and the mean density within non-linear structures are quite insensitive to the differences between dark-energy cosmologies. Regarding early dark energy, we thus arrive at a different conclusion than some earlier papers, including one from our group, and we explain why.

We study the reliability of dark-matter halo detections with three different linear filters applied to weak-lensing data. We use ray-tracing in the multiple lens-plane approximation through a large cosmological simulation to construct realizations of cosmic lensing by large-scale structures between redshifts zero and two. We apply the filters mentioned above to detect peaks in the weak-lensing signal and compare them with the true population of dark matter halos present in the simulation. We confirm the stability and performance of a filter optimized for suppressing the contamination by large-scale structure. It allows the reliable detection of dark-matter halos with masses above a few times 1e13 M_sun/h with a fraction of spurious detections below ~10%. For sources at redshift two, 50% of the halos more massive than ~7e13 M_sun/h are detected, and completeness is reached at ~2e14 M_sun/h., Comment: 14 pages, 13 figures, accepted on A&A

Purpose: To compare the efficacy of non-penetrating deep sclerectomy without implant with Crozafon-De Laage punch trabeculectomy, and to evaluate the effect of simultaneous temporal approach phacoemulsification on both techniques. Patients and Methods: Setting: Department of Ophthalmology of the University of Palermo. Design: Prospective randomized clinical trial. Patients and intervention procedures: Sixty-five patients (65 eyes) with primary open angle glaucoma (POAG) or pseudoexfoliative glaucoma (PEXG): 32 eyes underwent non-penetrating deep sclerectomy (NPDS), 17 as single procedure and 15 combined with phacoemulsification (phaco- NPDS), and 33 eyes underwent punch trabeculectomy (PT), 18 single and 15 with phaco (phaco-PT). The patients were randomly assigned to each procedure. No adjuvants, such as Nd: YAG laser goniopuncture, laser suturelysis, and antimetabolites were used. Main Outcome Measures: Postoperative complications, number of antiglaucoma medications, and IOP level were checked at each control. Complete success indicated the achievement of the target IOP without antiglaucoma medications, while qualified success indicated the same goal with or without medications. These categories were assessed at two target IOP levels, namely #21 mm Hg and #17 mm Hg in all four groups. Results: The mean follow-up period was 22.5 6 2.5 months. The mean preoperative IOP was 30.2 mm Hg in NPDS eyes, 26.8 in phaco-NPDS eyes, 32.1 in PT eyes, and 27.0 in phaco-PT ones, without significant intergroup difference. At the end point the mean IOP was 17.7 6 0.8, 15.7 6 0.9, 14.2 6 1.1, and 13.8 6 1.1 mm Hg respectively with postoperative IOP significantly lower (P = 0.005)than preoperative IOP in all groups. No difference was observed among groups at any observation time when simple and combined surgery were compared. Significant difference at the end point was found between NPDS and PT (P = 0.030). As for complete and qualified success with a #21 and #17 mm Hg target IOP no significant differences were noticed in all groups. Among postoperative complications, hypotony was significantly more frequent in both PT groups when compared with the NPDS groups. The same was true, but relating only to the single procedures, for shallow anterior chamber and choroidal detachment. The Kaplan-Meier cumulative survival curves relating to the qualified success rate in the four surgical groups for a #21 mm Hg target IOP (log rank, P = 0.564)and for a #17 mm Hg target IOP (log rank, P = 0.591) showed no significant intergroup differences. When the #21 mm Hg target IOP was considered, a mild positive trend in combined procedures (both phaco-NPDS and phaco-PT) was found in comparison with simple procedures. At lower IOP target (ie, #17 mm Hg) a better trend was found in favor of simple or combined PT procedure. Conclusions: Both techniques, NPDS and PT, without enhancements (ie, implants or antimetabolites) control IOP efficaciously at our end point. Phacoemulsification combined with penetrating and non-penetrating procedures does not seem to interfere with final results. When a lower target IOP and probability of success over time are considered, PT, single or combined, exhibits a better trend. PT, therefore, could be more suitable for higher IOP levels or longer life expectancies.

Prevalence of cataract was studied in a population based survey performed in adults aged 40 years or more living in Casteldaccia, a small Sicilian town. Lens opacities of moderate or severe grade (type II or worse, according to the Lens Opacity Classification System II) were found at the following rates: nuclear opalescence in 18.5%, cortical cataract in 12.9%, posterior subcapsular cataract in 10.8%. All these types of cataract were much more frequent in the elderly population and were about 1.5 times more common in women than in men. Late cataract was found in about 1/3 of subjects aged 60 to 69 years, in 2/3 of subjects aged 70 or more, but rarely under 60 years of age. However, early cataract was rather common among younger subjects. Cataracts causing a reduction of visual acuity under 0.7 in the worst eye were found in 4%, 8.7% and 21.5% respectively in the three age groups ranging from 40 to 49, 50 to 59 and 60 to 69 years and in 54.4% of subjects 70 years old or over.