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Recently, various pesticides have been employed at different stages of cultivation to protect the oil crop from insect, disease, and weed. Those pesticides, especially lipophilic ones, bio-accumulate in the oilseeds and get co-extracted into edible oils during the refining process. Hence, this study aimed to optimise an extraction method for routine pesticide multi-residue analysis in edible vegetable oil samples using gas chromatography coupled to tandem mass spectrometry (GC – MS/MS). Two parameters were optimised using a factorial design of experiment (solvent type and solvent/sample ratio). In general, the number of pesticides that conformed to our criteria (mean recovery 70–120%) increased as the solvent/sample ratio increased. Each of the three tested solvents had an advantage over the other, ethyl acetate showed the highest capability for non-polar pesticides extraction, acetonitrile had the highest sensitivity, and the ethyl acetate/acetonitrile mixture showed the highest number of pesticides with acceptable criteria. The three solvents were tested using two different cleanup sorbents (EMR, and Z-Sep), the best solvent/cleanup combination was found to be ethyl acetate/acetonitrile mixture in addition to Z-Sep. The final method was validated in accordance with the European guidelines for Analytical Quality Control and Method Validation Procedures for Pesticide Residues Analysis in Food and Feed (SANTE/11312/2021). The precision and trueness of the method were determined from recovery experiments on six replicates of spiked blank corn oil samples at 0.01, 0.025, and 0.05 mg/kg. The number of pesticides that showed accepted criteria were 130, 166, and 182 out of 222 for each spiking level respectively. [ABSTRACT FROM AUTHOR]

Euclid will collect an enormous amount of data during the mission's lifetime, observing billions of galaxies in the extragalactic sky. Along with traditional template-fitting methods, numerous machine learning (ML) algorithms have been presented for computing their photometric redshifts and physical parameters (PPs), requiring significantly less computing effort while producing equivalent performance measures. However, their performance is limited by the quality and amount of input information entering the model (the features), to a level where the recovery of some well-established physical relationships between parameters might not be guaranteed – for example, the star-forming main sequence (SFMS). To forecast the reliability of Euclid photo-zs and PPs calculations, we produced two mock catalogs simulating the photometry with the UNIONS ugriz and Euclid filters. We simulated the Euclid Wide Survey (EWS) and Euclid Deep Fields (EDF), alongside two auxiliary fields. We tested the performance of a template-fitting algorithm (Phosphoros) and four ML methods in recovering photo-zs, PPs (stellar masses and star formation rates), and the SFMS on the simulated Euclid fields. To mimic the Euclid processing as closely as possible, the models were trained with Phosphoros-recovered labels and tested on the simulated ground truth. For the EWS, we found that the best results are achieved with a mixed labels approach, training the models with wide survey features and labels from the Phosphoros results on deeper photometry, that is, with the best possible set of labels for a given photometry. This imposes a prior to the input features, helping the models to better discern cases in degenerate regions of feature space, that is, when galaxies have similar magnitudes and colors but different redshifts and PPs, with performance metrics even better than those found with Phosphoros. We found no more than 3% performance degradation using a COSMOS-like reference sample or removing u band data, which will not be available until after data release DR1. The best results are obtained for the EDF, with appropriate recovery of photo-z, PPs, and the SFMS. [ABSTRACT FROM AUTHOR]

Context. Near- to mid-infrared observations (from Spitzer and JWST) have revealed a hidden population of galaxies at redshift z = 3 − 6 called optically dark objects, which are believed to be massive and dusty star-formers. They contribute substantially to the cosmic star-formation rate (SFR) density at z ∼ 4 − 5 (up to 30 − 40%). Aims. While optically dark sources are widely recognized as a significant component of the stellar mass function, the history of their stellar mass assembly (and the evolution of their interstellar medium) remains unexplored. However, they are thought to be the progenitors of the more massive early-type galaxies found in present-day groups and clusters. It is thus important to examine the possible connection between dark sources and merging events in order to understand the environment in which they live. Methods. Here, we report our search for close companions in a sample of 19 optically-dark objects identified in the SMACS0723 JWST deep field. They were selected in the NIRCam F444W band and undetected below 2 μm. We restricted our analysis to the reddest (i.e., F277W–F444W > 1.3) and brightest (F444W < 26 mag) objects. Results. We identified KLAMA, an optically dark source showing a very close companion (angular distance < 0.5″). The spatially resolved SED fitting procedure indicates that all components lying within 1.5″ of who is it the dark source are indeed at z ∼ 5.7. Tidal features (leading to a whale-shaped morphology) corroborate the hypothesis that KLAMA is the most massive (log(M⋆/M⊙) > 10.3) and dusty (AV ∼ 3 at the core) system of an ongoing merger with a mass ratio of ∼10. Thus, around ten similar merger events would be required to double the stellar mass of KLAMA. Merging systems with properties similar to KLAMA are identified in the SERRA simulations, allowing us to reconstruct their stellar-mass assembly history and predict their molecular gas properties (in particular, the [CII] emission for the simulated system). Conclusions. The discovery of mergers within dark galaxies at the end of the Epoch of Reionization highlights the importance of conducting a statistical search for additional candidates in deep NIRCam fields. Such research will aid in our understanding of the significance of merging processes during the obscured phase of stellar-mass accumulation. [ABSTRACT FROM AUTHOR]

Context. Stellar bars are common morphological structures in the local Universe; according to optical and NIR surveys, they are present in about two-thirds of disc galaxies. These elongated structures are also believed to play a crucial role in secular evolutionary processes, because they are able to efficiently redistribute gas, stars, and angular momentum within their hosts, although it remains unclear as to whether they enhance or suppress star formation. A useful tool to investigate this ambiguity is the main sequence (MS) relation, which tightly links stellar mass (M⋆) and star formation rate (SFR). Aims. The main goal of this work is to explore star-formation processes in barred galaxies in order to assess the relevance of bars in star-formation quenching and whether or not they affect the typical log-linear trend of the resolved MS. Methods. To this purpose, we carried out a spatially resolved analysis on subkiloparsec (subkpc) scales for a sample of six nearby barred galaxies. We collected multi-wavelength photometric data from far-ultraviolet (FUV) to far-infrared (FIR) from the DustPedia database and applied a panchromatic spectral energy distribution (SED) fitting procedure on square apertures of fixed angular size (8″ × 8″) using the magphys code. Results. For each galaxy, we obtain the distributions of stellar mass and SFR surface density and relate them in the log Σ⋆ − log ΣSFR plane, deriving the spatially resolved MS relation. Although significant galaxy-to-galaxy variations are in place, we infer the presence of a common anti-correlation track in correspondence with the bar-hosting region, which shows systematically lower SFRs. This central quiescent signature can be interpreted as the result of a bar-driven depletion of gas reservoirs and a consequent halting of star formation. Our findings appear to support an inside-out quenching scenario. [ABSTRACT FROM AUTHOR]

We present the first spectroscopic ALMA follow-up for a pilot sample of nine radio-selected near-IR-dark galaxies in the COSMOS field. These sources were initially selected as radio-detected sources (S3 GHz > 12.65 μJy) without an optical or near-IR (NIR) counterpart in the COSMOS2015 catalog (Ks ≳ 24.7 mag), and just three of them were subsequently detected in the deeper COSMOS2020. Several studies highlighted that this selection could provide a population of highly dust-obscured, massive, and star-bursting galaxies. With these new ALMA observations, we assess the spectroscopic redshifts of this pilot sample of sources and improve the quality of the physical properties estimated through SED-fitting. Moreover, we measure the quantity of molecular gas inside these galaxies and forecast their potential evolutionary path, finding that the radio-selected NIR-dark galaxies might likely represent a population of high-z progenitors of the massive and passive galaxies that were discovered at z ∼ 3. Finally, we present some initial constraints on the kinematics of the interstellar medium within the analyzed galaxies, reporting a high fraction (∼55%) of double-peaked lines that can be interpreted as the signature of a rotating structure in our targets or as the presence of major mergers in our sample. The results we present here show the scientific potential of (sub)mm observations for this elusive population of galaxies and highlight the potential contribution of these sources to the evolution of the massive and passive galaxies at high z. [ABSTRACT FROM AUTHOR]

Aims. We provide an in-depth analysis of the COSMOS-Web ring, an Einstein ring at z ≈ 2 that we serendipitously discovered during the data reduction of the COSMOS-Web survey and that could be the most distant lens discovered to date. Methods. We extracted the visible and near-infrared photometry of the source and the lens from more than 25 bands. We combined these observations with far-infrared detections to study the dusty nature of the source and we derived the photometric redshifts and physical properties of both the lens and the source with three different spectral energy distribution (SED) fitting codes. Using JWST/NIRCam images, we also produced two lens models to (i) recover the total mass of the lens, (ii) derive the magnification of the system, (iii) reconstruct the morphology of the lensed source, and (iv) measure the slope of the total mass density profile of the lens. Results. We find the lens to be a very massive elliptical galaxy at z = 2.02 ± 0.02 with a total mass within the Einstein radius of Mtot(<θEin = (3.66 ± 0.36) × 1011M⊙ and a total stellar mass of M⋆ = 1.37−0.11+0.14 × 1011 M⊙. We also estimate it to be compact and quiescent with a specific star formation rate below 10−13 yr. Compared to stellar-to-halo mass relations from the literature, we find that the total mass of the lens within the Einstein radius is consistent with the presence of a dark matter (DM) halo of total mass Mh = 1.09−0.57+1.46 × 1013 M⊙. In addition, the background source is a M⋆ = (1.26 ± 0.17) × 1010M⊙ star-forming galaxy (SFR ≈ (78 ± 15) M⊙ yr) at z = 5.48 ± 0.06. The morphology reconstructed in the source plane shows two clear components with different colors. Dust attenuation values from SED fitting and nearby detections in the far infrared also suggest that the background source could be at least partially dust-obscured. Conclusions. We find the lens at z ≈ 2. Its total, stellar, and DM halo masses are consistent within the Einstein ring, so we do not need any unexpected changes in our description of the lens such as changing its initial mass function or including a non-negligible gas contribution. The most likely solution for the lensed source is at z ≈ 5.5. Its reconstructed morphology is complex and highly wavelength dependent, possibly because it is a merger or a main sequence galaxy with a heterogeneous dust distribution. [ABSTRACT FROM AUTHOR]

We propose that observations of supermassive galaxies contain cosmological statistical constraining power similar to conventional cluster cosmology, and we provide promising indications that the associated systematic errors are comparably easier to control. We consider a fiducial spectroscopic and stellar mass complete sample of galaxies drawn from the Dark Energy Spectroscopic Instrument (DESI) and forecast how constraints on Ωm–σ8 from this sample will compare with those from number counts of clusters based on richness λ. At fixed number density, we find that massive galaxies offer similar constraints to galaxy clusters. However, a mass-complete galaxy sample from DESI has the potential to probe lower halo masses than standard optical cluster samples (which are typically limited to λ ≳ 20 and M halo ≳ 1013.5 M⊙  h −1); additionally, it is straightforward to cleanly measure projected galaxy clustering w p for such a DESI sample, which we show can substantially improve the constraining power on Ωm. We also compare the constraining power of M *-limited samples to those from larger but mass-incomplete samples [e.g. the DESI Bright Galaxy Survey (BGS) sample]; relative to a lower number density M *-limited samples, we find that a BGS-like sample improves statistical constraints by 60 per cent for Ωm and 40 per cent for σ8, but this uses small-scale information that will be harder to model for BGS. Our initial assessment of the systematics associated with supermassive galaxy cosmology yields promising results. The proposed samples have a ∼10 per cent satellite fraction, but we show that cosmological constraints may be robust to the impact of satellites. These findings motivate future work to realize the potential of supermassive galaxies to probe lower halo masses than richness-based clusters and to potentially avoid persistent systematics associated with optical cluster finding. [ABSTRACT FROM AUTHOR]

Context. ALMA observations show that dusty, distant, massive (M* ≳ 1011 M⊙) galaxies usually have a remarkable star-formation activity, contributing of the order of 25% of the cosmic star-formation rate density at z ≈ 3–5, and up to 30% at z ∼ 7. Nonetheless, they are elusive in classical optical surveys, and current near-IR surveys are able to detect them only in very small sky areas. Since these objects have low space densities, deep and wide surveys are necessary to obtain statistically relevant results about them. Euclid will potentially be capable of delivering the required information, but, given the lack of spectroscopic features at these distances within its bands, it is still unclear if Euclid will be able to identify and characterise these objects. Aims. The goal of this work is to assess the capability of Euclid, together with ancillary optical and near-IR data, to identify these distant, dusty, and massive galaxies based on broadband photometry. Methods. We used a gradient-boosting algorithm to predict both the redshift and spectral type of objects at high z. To perform such an analysis, we made use of simulated photometric observations that mimic the Euclid Deep Survey, derived using the state-of-the-art Spectro-Photometric Realizations of Infrared-selected Targets at all-z (SPRITZ) software. Results. The gradient-boosting algorithm was found to be accurate in predicting both the redshift and spectral type of objects within the simulated Euclid Deep Survey catalogue at z > 2, while drastically decreasing the runtime with respect to spectral-energy-distribution-fitting methods. In particular, we studied the analogue of HIEROs (i.e. sources selected on the basis of a red H − [4.5]> 2.25), combining Euclid and Spitzer data at the depth of the Deep Fields. These sources include the bulk of obscured and massive galaxies in a broad redshift range, 3 < z < 7. We find that the dusty population at 3 ≲ z ≲ 7 is well identified, with a redshift root mean squared error and catastrophic outlier fraction of only 0.55 and 8.5% (HE ≤ 26), respectively. Our findings suggest that with Euclid we will obtain meaningful insights into the impact of massive and dusty galaxies on the cosmic star-formation rate over time. [ABSTRACT FROM AUTHOR]

We have carried out Hubble Space Telescope (HST) snapshot observations at 1.1 μm of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel Space Observatory. Our candidates comprise systems with flux densities at |$500\, \mu$| m, S 500 ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnifications of the background sources are consistent with previous studies. However, the background source circularized radii (between 0.34 and 1.30 kpc) are ∼3 times smaller than the ones measured in the sub-millimetre/millimetre for a similarly selected and partially overlapping sample. We compare our lenses with those in the Sloan Lens Advanced Camera for Surveys (ACS) Survey confirming that our lens-independent selection is more effective at picking up fainter and diffuse galaxies and group lenses. This sample represents the first step towards characterizing the near-infrared properties and stellar masses of the gravitationally lensed dusty star-forming galaxies. [ABSTRACT FROM AUTHOR]

The COVID-19 pandemic is having profound effects on college students, and those with mental health conditions are more vulnerable to the impact of this stress. Objective: To study the impact of the COVID-19 pandemic on college students' mental health. Participants: Participants (n=489) were mostly female, undergraduate, and aged 18–25. Methods: Participants completed an online survey assessing symptoms of mental health problems including hopelessness, loneliness, sadness, anxiety, sadness, and anger. Results: Approximately 81.6 % self-reported at least one negative mental health symptom. Students reported increased feelings of hopelessness (+7.8%), loneliness (+6.7%), sadness (+8.8%), depression (+2.6%), anxiety (+5.2%), and anger (+14.6%) during the pandemic than before. LGBTQ students and Black students had significantly more mental health symptoms during the pandemic than straight and White students. Conclusions: Results of this study highlight the negative impact of the pandemic and resultant changes on college students' mental health. [ABSTRACT FROM AUTHOR]

About 12 billion years ago, the Universe was first experiencing light again after the dark ages, and galaxies filled the environment with stars, metals, and dust. How efficient was this process? How fast did these primordial galaxies form stars and dust? We can answer these questions by tracing the star formation rate density (SFRD) back to its widely unknown high-redshift tail, traditionally observed in the near-infrared (NIR), optical, and UV bands. Thus, objects with a large amount of dust were missing. We aim to fill this knowledge gap by studying radio-selected NIR-dark (RS-NIRdark) sources, i.e., sources not having a counterpart at UV-to-NIR wavelengths. We widen the sample of Talia et al. from 197 to 272 objects in the Cosmic Evolution Survey (COSMOS) field, including also photometrically contaminated sources, which were previously excluded. Another important step forward consists in the visual inspection of each source in the bands from u * to MIPS 24 μ m. According to their "environment" in the different bands, we are able to highlight different cases of study and calibrate an appropriate photometric procedure for the objects affected by confusion issues. We estimate that the contribution of RS-NIRdark sources to the cosmic SFRD at 3 < z < 5 is ∼10%–25% of that based on UV-selected galaxies. [ABSTRACT FROM AUTHOR]

In recent years, architectural interactions have become the center of many important reflections. However, there is little agreement on the subject. Some authors consider architecture to be about its relations with human and nonhuman agents. Others consider that buildings have an autonomous presence, which transcends all their interactions. These approaches are generally seen as incompatible. Although at the heart of the debate is the role of relations in architecture, their nature is not addressed. The discussion could gain clarity by recognizing the differences between them. In this paper, we propose a classification of architectural interactions, which may help to better inform further discussion on the topic. A closer look at architectural relations reveals that autonomy and relationality are not opposing, but complementary, aspects. [ABSTRACT FROM AUTHOR]

We introduce a new, multizone chemical evolution model of the DustPedia galaxy M74, calibrated by means of Markov Chain Monte Carlo methods. We take into account the observed stellar and gas density profiles and use Bayesian analysis to constrain two fundamental parameters characterizing the gas accretion and star formation time-scale, i.e. the infall time-scale τ and the SF efficiency ν, respectively, as a function of galactocentric radius R. Our analysis supports an infall time-scale increasing with R and a star formation efficiency decreasing with R , thus supporting an 'Inside-Out' formation for M74. For both τ and ν, we find a weaker radial dependence than in the Milky Way. We also investigate the dust content of M74, comparing the observed dust density profile with the results of our chemical evolution models. Various prescriptions have been considered for two key parameters, i.e. the typical dust accretion time-scale τ0 and the mass of gas cleared out of dust by a supernova remnant, M clear, regulating the dust growth and destruction rate, respectively. Two models with a different current balance between destruction and accretion, i.e. with an equilibrium and a dominion of accretion over destruction, can equally reproduce the observed dust profile of M74. This outlines the degeneracy between these parameters in shaping the interstellar dust content in galaxies. Our methods will be extended to more DustPedia galaxies to shed more light on the relative roles of dust production and destruction. [ABSTRACT FROM AUTHOR]

Exceptional situations allow us to rethink sociocultural dynamics that were previously taken for granted. Architecture is often part of these processes, anticipating with its projects situations that would only occur decades later. This is the case of the Tuscolano III housing project (Rome, 1950), by Adalberto Libera, which introduces a concept of domesticity based on the dissolution between the public and the private. In this project, inhabiting is understood as a phenomenon that occurs on a neighborhood scale; and domesticity as something that expands beyond the walls of a house, and depends on a complex network of social, spatial and political relations. In Tuscolano III Libera proposes an inclusive model of the city, embracing lifestyles that were not widespread at the time, but are so in current times, such as living alone. Through this project, the article aims to investigate the anticipatory capacity of architectural design in periods of great change, as was the period of post-war reconstruction in Italy, and as is the contemporary era, with its continuing economic, political and health crises. [ABSTRACT FROM AUTHOR]

We present a novel simulation-based cosmological analysis of galaxy–galaxy lensing and galaxy redshift-space clustering. Compared to analysis methods based on perturbation theory, our simulation-based approach allows us to probe a much wider range of scales, |$0.4 \, h^{-1} \, \mathrm{Mpc}$| to |$63 \, h^{-1} \, \mathrm{Mpc}$|⁠ , including highly non-linear scales, and marginalizes over astrophysical effects such as assembly bias. We apply this framework to data from the Baryon Oscillation Spectroscopic Survey LOWZ sample cross-correlated with state-of-the-art gravitational lensing catalogues from the Kilo Degree Survey and the Dark Energy Survey. We show that gravitational lensing and redshift-space clustering when analysed over a large range of scales place tight constraints on the growth-of-structure parameter |$S_8 = \sigma _8 \sqrt{\Omega _{\rm m} / 0.3}$|⁠. Overall, we infer S 8 = 0.792 ± 0.022 when analysing the combination of galaxy–galaxy lensing and projected galaxy clustering and S 8 = 0.771 ± 0.027 for galaxy redshift-space clustering. These findings highlight the potential constraining power of full-scale studies over studies analysing only large scales and also showcase the benefits of analysing multiple large-scale structure surveys jointly. Our inferred values for S 8 fall below the value inferred from the CMB, S 8 = 0.834 ± 0.016. While this difference is not statistically significant by itself, our results mirror other findings in the literature whereby low-redshift large-scale structure probes infer lower values for S 8 than the CMB, the so-called S 8-tension. [ABSTRACT FROM AUTHOR]

Using the weak gravitational lensing data from the Hyper Suprime-Cam Subaru Strategic Program (HSC survey), we study the potential of different stellar mass estimates in tracing halo mass. We consider galaxies with log10(M ⋆/M⊙) > 11.5 at 0.2 < z < 0.5 with carefully measured light profiles, and clusters from the redMaPPer and CAMIRA richness-based algorithms. We devise a method (the 'Top- N test') to evaluate the scatter in the halo mass–observable relation for different tracers, and to inter-compare halo mass proxies in four number density bins using stacked galaxy–galaxy lensing profiles. This test reveals three key findings. Stellar masses based on CModel photometry and aperture luminosity within R <30 kpc are poor proxies of halo mass. In contrast, the stellar mass of the outer envelope is an excellent halo mass proxy. The stellar mass within R  = [50, 100] kpc, M ⋆, [50, 100], has performance comparable to the state-of-the-art richness-based cluster finders at log10 M vir ≳ 14.0 and could be a better halo mass tracer at lower halo masses. Finally, using N -body simulations, we find that the lensing profiles of massive haloes selected by M ⋆, [50, 100] are consistent with the expectation for a sample without projection or mis-centring effects. Richness-selected clusters, on the other hand, display an excess at R ∼ 1 Mpc in their lensing profiles, which may suggest a more significant impact from selection biases. These results suggest that M ⋆-based tracers have distinct advantages in identifying massive haloes, which could open up new avenues for cluster cosmology. The codes and data used in this work can be found here: [ABSTRACT FROM AUTHOR]

Human bocaviruses (HBoVs) are recently described as human emergent viruses, especially in young children. In this study, we undertook a systematic review and meta‐analysis to estimate their prevalence in Europe. PubMed, Web of Science and Scopus databases were systematically screened for clinical studies, up to October 2020. Study eligibility criteria were primary full‐text articles from clinical studies, conducted using valid screening test methods and published in peer‐reviewed journals, in English or Spanish and from European countries. The overall pooled prevalence, prevalence by country as well as the prevalence of HBoV as a single or co‐pathogen were estimated using a random‐effects model. Sub‐group and meta‐regression analyses explored potential sources of heterogeneity in the data. A total of 35 studies involving 32,656 subjects from 16 European countries met the inclusion criteria. Heterogeneity (I2 = 97.0%, p <.01) was seen among studies; HBoV prevalence varied from 2.0 to 45.69% with a pooled estimate of 9.57% (95%CI 7.66‐11.91%). The HBoV prevalence both as a single infection (3.99%; 95%CI 2.99‐5.31%) or as co‐infection with other viruses (5.06%; 95%CI 3.88‐6.58%) was also analysed. On a geographic level, prevalence by country did not show statistical differences, ranging from 3.24% (Greece) to 21.05% (Denmark). An odds ratio analysis was also included in order to evaluate the relevance of the variable 'age' as a risk factor of HBoV infection in children <5 years old. The OR value of 1.77 (95%CI 1.13‐2.77; p <.01) indicated that being <5 years old is a risk factor for HBoV infection. This study showed that HBoV has a moderate prevalence among European countries. [ABSTRACT FROM AUTHOR]

Objective: To assess survival of ALS patients in general and in selected demographic and clinical subgroups comparing two periods (1998–2000 vs. 2008–2010). Methods: Newly diagnosed adults resident of Lombardy, Northern Italy from a population-based registry were included. Data were collected on age at diagnosis, sex, site of onset, diagnostic delay, and El-Escorial diagnostic category. Patients were followed until death or last observation. Survival was evaluated using Kaplan–Meier curves and Cox's proportional hazards models. Results: In 2008–2010 (267 patients), median survival was 2.4 years and 1-year, 2-year, 3-year and 5-year survival rates were 79%, 56%, 41% and 24%. Longer survival was associated with male sex, younger age, spinal onset, and longer diagnostic delay. Multivariable analysis confirmed higher death in 65–69yr (HR 2.8; 95% CI 1.4-5.6), 70–74yr (HR 3.2; 95% CI 1.6-6.3) and 75 + yr (HR 6.9; 95% CI 3.5-13.8) categories, compared to ≤49yr, in females (HR 1.4; 95% CI 1.02-1.8), compared to males, and in patients diagnosed after 6–12 months (HR 1.9; 95% CI 1.4-2.7), compared with longer diagnostic delay. In 1998–2000 (235 patients), median survival was 2.2 years. The 1-year, 2-year, 3-year and 5-year survival rates were 77%, 53%, 38% and 20%. When adjusting for demographic and clinical variables, the HR for death in 2008–2010 versus 1998–2000 was 0.80 (95% CI 0.66–0.98). A significant increase of survival in 2008–2010 was found only in patients aged 50–59yr and 70–74yr at diagnosis. Conclusions: Survival of ALS has increased over time in the last decades, especially in middle aged and elderly patients. The benefits of comprehensive care in selected age groups might explain our findings. [ABSTRACT FROM AUTHOR]

Secondary halo properties beyond mass, such as the mass accretion rate (MAR), concentration, and the half mass scale, are essential in understanding the formation of large-scale structure and dark matter haloes. In this paper, we study the impact of secondary halo properties on the galaxy-galaxy lensing observable, ΔΣ. We build an emulator trained on N -body simulations to model ΔΣ and quantify the impact of different secondary parameters on the ΔΣ profile. We focus on the impact of MAR on ΔΣ. We show that a 3σ detection of variations in MAR at fixed halo mass could be achieved with the Hyper Suprime Cam survey assuming no baryonic effects and a proxy for MAR with scatter <1.5. We show that the full radial profile of ΔΣ depends on secondary properties at fixed halo mass. Consequently, an emulator that can perform full shape fitting yields better than two times improvement upon the constraints on MAR than only using the outer part of the halo. Finally, we highlight that miscentring and MAR impact the radial profile of ΔΣ in a similar fashion, implying that miscentring and MAR need to be modelled jointly for unbiased estimates of both effects. We show that present-day lensing data sets have the statistical capability to place constraints on halo MAR within our assumptions. Our analysis opens up new possibilities for observationally measuring the assembly history of the dark matter haloes that host galaxies and clusters. [ABSTRACT FROM AUTHOR]

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We investigate the radio/far-infrared (FIR) correlation for a sample of 28 bright high-redshift (1 ≲ z  ≲ 4) star-forming galaxies selected in the FIR from the Herschel -ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated Australia Telescope Compact Array observations at 2.1 GHz or from cross-matches with the FIRST survey at 1.4 GHz. By taking advantage of source brightness possibly enhanced by lensing magnification, we identify a weak evolution with redshift out to z  ≲ 4 of the FIR-to-radio luminosity ratio q FIR. We also find that the q FIR parameter as a function of the radio power |$L_{1.4\, \rm GHz}$| displays a clear decreasing trend, similarly to what is observed for optically/radio-selected lensed quasars found in literature, yet covering a complementary region in the |$q_{\rm FIR}{\!-\!}L_{1.4\, \rm GHz}$| diagram. We interpret such a behaviour in the framework of an in situ galaxy formation scenario, as a result of the transition from an early dust-obscured star-forming phase (mainly pinpointed by our FIR selection) to a late radio-loud quasar phase (preferentially sampled by the optical/radio selection). [ABSTRACT FROM AUTHOR]

The boundaries between domestic and urban environments are increasingly blurred. Until the contemporary era, the house acted as aquite autonomous microcosm and the city as its receptacle, but today this distinction is not so sharp. Various changes are transforming both domestic and urban life. Many activities, events and rituals usually associated with domestic space today take place often outside, scattering the home throughout the city. Meanwhile, domestic environment is increasingly accommodating some urban functions, changing its traditional meaning and giving rise to hybrid situations. Domestic and urban environments are merging in asymbiotic way; it is then necessary to rethink their spaces in order to respond to their contemporary and future evolutions. The paper aims at introducing the main facts about the contemporary blurring of the boundaries of domestic and urban space, explaining how this is currently affecting the architecture of both the house and the city. [ABSTRACT FROM AUTHOR]

Objectives: To determine whether the generic and branded warfarins used as anticoagulants in Brazil are therapeutic equivalents based on their international normalized ratio (INR) results. Methods: This crossover randomized controlled trial had four periods. We used the branded Marevan and two generic versions of warfarin sodium tablets, manufactured by União Química and Teuto laboratories, all purchased from retail drugstores. Eligible participants were outpatients from an anticoagulation clinic at a university hospital in São Paulo, Brazil. They had atrial fibrillation or flutter and had been using warfarin for at least 2 months with an INR therapeutic range of 2.0–3.0. Randomization was by numbered, opaque, sealed envelopes. Healthcare personnel and outcome assessors were blinded to treatments, but patients were not. The primary outcome was the variability in the INR (ΔINR) and secondary outcomes included mean INR. We accepted formulations as equivalent if the 95% confidence interval (CI) of the comparison of ΔINR between branded and generic formulations was within the limit of ±0.49. Results: One hundred patients were recruited and randomized to six sequences of treatment (four sequences with n = 17 and two sequences with n = 16). União Química generic warfarin had equivalent variability in the INR to Marevan (ΔINR +0.09 [95% CI -0.29 to +0.46], n = 84). Comparison between Teuto generic warfarin and Marevan was inconclusive (ΔINR +0.29 [95% CI -0.09 to +0.68], n = 84). Conclusions: Marevan and União Química warfarin had equivalent therapeutic effectiveness and both could be confidently used for anticoagulation. The comparison between Marevan and TW was inconclusive and does not warrant a statement of equivalence. Our methods are especially important for comparing generic and branded drugs that raise concerns and may be subject of future investigations by regulatory agents. Trial registration: ClinicalTrials.gov NCT02017197. [ABSTRACT FROM AUTHOR]

There is still a need to analyze the factors that enhance navigation accuracy. This study aims to examine how success in environment learning relates to task goals and WM. A total of 90 undergraduates (46 females) learned a route from a virtual navigation experience after being given a goal that involved tracing the route (a route-based goal) or finding a shortcut (a survey-based goal). The two groups thus formed were each divided into three subgroups according to the dual-task paradigm: one only navigated (control condition); the other two did so while simultaneously performing a visuo-spatial or verbal secondary task. Afterwards, participants traced the previously seen route and found a shortcut. Several visuo-spatial and verbal WM tasks were also administered. The results showed that participants given a route-based goal performed better in the route-tracing task; and those given a survey-based goal were better at finding shortcuts. An influence of WM was also shown: higher WM (visuo-spatial and verbal) ability significantly reduced the number of route-tracing errors made while performing a secondary visuo-spatial task, regardless of the goal, whereas no such effects emerged for shortcut finding. These results offer new insight on how task goals and WM support successful navigation. [ABSTRACT FROM AUTHOR]

In this paper, we present an attempt to estimate the redshift evolution of the molecular to neutral gas mass ratio within galaxies (at fixed stellar mass). For a sample of five nearby grand design spirals located on the main-sequence (MS) of star-forming galaxies, we exploit maps at 500 pc resolution of stellar mass and star formation rate (M ⋆ and SFR). For the same cells, we also have estimates of the neutral (M H  i ) and molecular (⁠|$M_{\rm H_2}$|⁠) gas masses. To compute the redshift evolution, we exploit two relations: (i) one between the molecular-to-neutral mass ratio and the total gas mass (M gas), whose scatter shows a strong dependence with the distance from the spatially resolved MS, and (ii) the one between |$\log (M_{\rm {H_2}}/M_{\star })$| and log (M H  i / M ⋆). For both methods, we and that |$M_{\rm H_2}$| / M H  i within the optical radius slightly decreases with redshift, contrary to common expectations of galaxies becoming progressively more dominated by molecular hydrogen at high redshifts. We discuss possible implications of this trend on our understanding of the internal working of high-redshift galaxies. [ABSTRACT FROM AUTHOR]

We perform a consistent comparison of the mass and mass profiles of massive (M ⋆ > 1011.4 M⊙) central galaxies at z ∼ 0.4 from deep Hyper Suprime-Cam (HSC) observations and from the Illustris, TNG100, and Ponos simulations. Weak lensing measurements from HSC enable measurements at fixed halo mass and provide constraints on the strength and impact of feedback at different halo mass scales. We compare the stellar mass function (SMF) and the Stellar-to-Halo Mass Relation (SHMR) at various radii and show that the radius at which the comparison is performed is important. In general, Illustris and TNG100 display steeper values of α where |$M_{\star } \propto M_{\rm vir}^{\alpha }$|⁠. These differences are more pronounced for Illustris than for TNG100 and in the inner rather than outer regions of galaxies. Differences in the inner regions may suggest that TNG100 is too efficient at quenching in situ star formation at M vir ≃ 1013 M⊙ but not efficient enough at M vir ≃ 1014 M⊙. The outer stellar masses are in excellent agreement with our observations at M vir ≃ 1013 M⊙, but both Illustris and TNG100 display excess outer mass as M vir ≃ 1014 M⊙ (by ∼0.25 and ∼0.12 dex, respectively). We argue that reducing stellar growth at early times in |$M_\star \sim 10^{9-10} \, \mathrm{M}_{\odot }$| galaxies would help to prevent excess ex-situ growth at this mass scale. The Ponos simulations do not implement AGN feedback and display an excess mass of ∼0.5 dex at r < 30 kpc compared to HSC which is indicative of overcooling and excess star formation in the central regions. The comparison of the inner profiles of Ponos and HSC suggests that the physical scale over which the central AGN limits star formation is r ≲ 20 kpc. Joint comparisons between weak lensing and galaxy stellar profiles are a direct test of whether simulations build and deposit galaxy mass in the correct dark matter haloes and thereby provide powerful constraints on the physics of feedback and galaxy growth. Our galaxy and weak lensing profiles are publicly available to facilitate comparisons with other simulations. [ABSTRACT FROM AUTHOR]

The splashback radius (R sp) of dark matter haloes has recently been detected using weak gravitational lensing and cross-correlations with galaxies. However, different methods have been used to measure R sp and to assess the significance of its detection. In this paper, we use simulations to study the precision and accuracy to which we can detect the splashback radius with 3D density, 3D subhalo, and weak lensing profiles. We study how well various methods and tracers recover R sp by comparing it with the value measured directly from particle dynamics. We show that estimates of R sp from density and subhalo profiles correspond to different percentiles of the underlying R sp distribution of particle orbits. At low accretion rates, a second caustic appears and can bias results. Finally, we show that upcoming lensing surveys may be able to constrain the R sp–Γdyn relation directly. [ABSTRACT FROM AUTHOR]

Stiff person syndrome (SPS) is a rare neurologic disorder, characterized by muscle rigidity and spasms. Anti-glutamic acid decarboxylase (anti-GAD) antibodies are associated with the classic form of SPS, while antibodies against amphiphysin are associated with the paraneoplastic form of the disease. We present the case of a patient with paraneoplastic SPS, presenting with muscle cramps of lower extremities that progressed to severe muscle rigidity and spasms, associated with a right breast tumor and positive anti-amphiphysin antibodies. Paraneoplastic SPS is a rare neurological disorder, challenging for the physicians both to diagnose and treat. [ABSTRACT FROM AUTHOR]

We use dust masses (M dust) derived from far-infrared data and molecular gas masses (M mol) based on CO luminosity to calibrate proxies based on a combination of the galaxy Balmer decrement, disc inclination, and gas metallicity. We use such proxies to estimate M dust and M mol in the local SDSS sample of star-forming galaxies (SFGs). We study the distribution of M dust and M mol along and across the main sequence (MS) of SFGs. We find that M dust and M mol increase rapidly along the MS with increasing stellar mass (M *), and more marginally across the MS with increasing SFR (or distance from the relation). The dependence on M * is sub-linear for both M dust and M mol. Thus, the fraction of dust (f dust) and molecular gas mass (f mol) decreases monotonically towards large M *. The star formation efficiency (SFE, inverse of the molecular gas depletion time) depends strongly on the distance from the MS and it is constant along the MS. As nearly all galaxies in the sample are central galaxies, we estimate the dependence of f dust and f gas on the host halo mass and find a tight anticorrelation. As the region where the MS is bending is numerically dominated by massive haloes, we conclude that the bending of the MS is due to a lower availability of molecular gas mass in massive haloes rather than a lower efficiency in forming stars. [ABSTRACT FROM AUTHOR]

Background and Purpose: Poor dietary practices are linked to many chronic diseases. The purpose of this validation study was to develop a psychometrically sound instrument that can be administered by health practitioners to measure dietary barriers. Methods: The Dietary Health Status (DHS) instrument, designed to measure dietary barriers is comprised of items in the National Health and Nutrition Examination Survey-What We Eat in America datasets. Content validity was established for DHS using an expert review process. Principal component analysis (PCA) was then used to assess validity and reliability as determined by Cronbach's alpha values. Results: The PCA supported a 10-component solution, explaining 61% of the total variance. Cronbach's alpha was.67 for the entire instrument, ranging from.55 to.87 for the 10 subscales. Conclusion: Results suggest the instrument had sufficient construct and internal validity. This exploratory study is an important first step in validating the DHS instrument. [ABSTRACT FROM AUTHOR]

We report the serendipitous discovery of a dust-obscured galaxy observed as part of the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [C  ii ] at Early times (ALPINE). While this galaxy is detected both in line and continuum emissions in ALMA Band 7, it is completely dark in the observed optical/near-infrared bands and only shows a significant detection in the UltraVISTA K s band. We discuss the nature of the observed ALMA line, that is [C  ii ] at |$z$| ∼ 4.6 or high- J CO transitions at |$z$| ∼ 2.2. In the first case, we find a [C  ii ]/FIR luminosity ratio of |$\mathrm{log}{(L_{[\mathrm{ C}\, \rm {\small {II}}]}/L_{\mathrm{ FIR}})} \sim -2.5$|⁠ , consistent with the average value for local star-forming galaxies (SFGs). In the second case instead, the source would lie at larger CO luminosities than those expected for local SFGs and high- z submillimetre galaxies. At both redshifts, we derive the star formation rate (SFR) from the ALMA continuum and the physical parameters of the galaxy, such as the stellar mass (M *), by fitting its spectral energy distribution. Exploiting the results of this work, we believe that our source is a 'main-sequence', dusty SFG at |$z$|  = 4.6 (i.e. [C  ii ] emitter) with |$\mathrm{log(SFR/M_{\odot }\, yr^{-1})}\sim 1.4$| and log(M */M⊙) ∼ 9.9. As a support to this scenario our galaxy, if at this redshift, lies in a massive protocluster recently discovered at |$z$| ∼ 4.57, at only ∼1 proper Mpc from its centre. This work underlines the crucial role of the ALPINE survey in making a census of this class of objects, in order to unveil their contribution to the global SFR density at the end of the Reionization epoch. [ABSTRACT FROM AUTHOR]

We analyse the spatially resolved relation between stellar mass (M ⋆) and star formation rate (SFR) in disc galaxies (i.e. the main sequence, MS). The studied sample includes eight nearby face-on grand-design spirals, e.g. the descendant of high-redshift, rotationally supported star-forming galaxies. We exploit photometric information over 23 bands, from the UV to the far-IR, from the publicly available DustPedia data base to build spatially resolved maps of stellar mass and SFRs on sub-galactic scales of 0.5–1.5 kpc, by performing a spectral energy distribution fitting procedure that accounts for both the observed and obscured star formation processes, over a wide range of internal galaxy environments (bulges, spiral arms, and outskirts). With more than 30 000 physical cells, we have derived a definition of the local spatially resolved MS per unit area for discs, log (ΣSFR) = 0.82log (Σ*) − 8.69. This is consistent with the bulk of recent results based on optical IFU, using the H α line emission as an SFR tracer. Our work extends the analysis at lower sensitivities in both M ⋆ and SFR surface densities, up to a factor of ∼10. The self-consistency of the MS relation over different spatial scales, from sub-galactic to galactic, as well as with a rescaled correlation obtained for high-redshift galaxies, clearly proves its universality. [ABSTRACT FROM AUTHOR]

Copyright of Brazilian Journal of Surgery & Clinical Research is the property of Master Editora and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Background: A poor quality diet is a well-known risk factor for many chronic diseases. However, eating a healthful diet is not always simple as many underlying factors can impede adherence. Individuals with fewer barriers are more likely to eat a healthful diet than those who have more barriers. Accurately measuring barriers to eating a healthful diet could inform personalized interventions, particularly those aiming to prevent chronic diseases. The aim of this study was to establish content validity for selected items obtained from the National Health and Nutrition Examination Survey (NHANES) database to be considered for inclusion as items on the conceptualized Dietary Health Status (DHS) instrument, which is designed to measure barriers to eating a healthful diet in adults.Methods: The Behavioral Change Wheel hub COM-B and the Theoretical Domains Framework (TDF) were the two theoretical frameworks underpinning the development of the DHS instrument. Seven steps were conducted to create the instrument: 1) development of operational definitions for each TDF domain; 2) identification of items from the NHANES database 2011-2012; 3) screening of items to ensure inclusion of all relevant items; 4) assigning items to a theory-based domain; 5) evaluation of the items against inclusion/exclusion criteria; 6) solicitation of feedback from expert reviewers to reach consensus on inclusion into a domain; and 7) validation of items.Results: A total of 170 items representing twelve domains were identified as potential barriers to eating a healthful diet-- knowledge, optimism, beliefs about consequences, beliefs about capabilities, reinforcement, memory, attention and decision processes, environmental context and resources, social influences, emotion, behavioral regulation, health identity, and functional status.Conclusion: Expert review consultation and a consensus approach established content validity for 12 theory-based domains comprised of 170 items identified as potential barriers to eating a healthful diet. The use of these explanatory domains may: assist researchers to better understand barriers to adult dietary practices; inform the development of a screening tool that could be used in a community setting to measure barriers to eating a healthful diet; and inform individualized interventions. [ABSTRACT FROM AUTHOR]

Brightest cluster galaxies (BCGs) residing in cool-core clusters are known to be the stage of intricate baryon cycle phenomena (e.g. gas inflows, AGN outflows, star formation feedback). The scenarios describing the observed properties of these galaxies are still controversial, suffering from limitations due to the spatial resolving power of the instruments, specifically for galaxies beyond the Local Universe. However, the dramatic improvements introduced by the integral-field unit instruments (e.g. MUSE) could shed light on the physical processes driving the evolution of these galaxies. We present an extensive analysis of the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud BCG sitting at the centre of the X-ray luminous cool-core cluster Abell 2667 (z = 0.23), based on MUSE data. Our results indicate that the BCG is a massive elliptical, hosting an AGN that is possibly undergoing accretion of cold star-forming clouds of ICM or galactic cannibalism. [ABSTRACT FROM AUTHOR]

Brightest cluster galaxies (BCGs) residing in cool-core clusters are known to be the stage of intricate baryon cycle phenomena (e.g. gas inflows, AGN outflows, star formation feedback). The scenarios describing the observed properties of these galaxies are still controversial, suffering from limitations due to the spatial resolving power of the instruments, specifically for galaxies beyond the Local Universe. However, the dramatic improvements introduced by the integral-field unit instruments (e.g. MUSE) could shed light on the physical processes driving the evolution of these galaxies. We present an extensive analysis of the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud BCG sitting at the centre of the X-ray luminous cool-core cluster Abell 2667 (z = 0.23), based on MUSE data. Our results indicate that the BCG is a massive elliptical, hosting an AGN that is possibly undergoing accretion of cold star-forming clouds of ICM or galactic cannibalism. [ABSTRACT FROM AUTHOR]

Copyright of Revista Habanera de Ciencias Médicas is the property of Universidad de Ciencias Medicas de La Habana and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Based on HST and MUSE data, we probe the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud brightest cluster galaxy (BCG) located at the centre of the X-ray-luminous cool-core cluster Abell 2667 (z  = 0.2343). The bi-dimensional modelling of the BCG surface brightness profile reveals the presence of a complex system of substructures extending all around the galaxy. Clumps of different size and shape plunged into a more diffuse component constitute these substructures, whose intense 'blue' optical colour hints at the presence of a young stellar population. Our results depict the BCG as a massive (M ⋆ ≃ 1.38 × 1011 M⊙) dispersion-supported spheroid (Δ v ⋆ ≤ 150 km s−1, σ0 ∼ 216 km s−1) hosting an active supermassive black hole (M SMBH ≃ 3.8 × 109 M⊙) whose optical features are typical of low-ionization nuclear emission line regions. Although the velocity pattern of the stars in the BCG is irregular, the stellar kinematics in the regions of the clumps show a positive velocity of ∼100 km s−1, similarly to the gas component. An analysis of the mechanism giving rise to the observed lines in the clumps through empirical diagnostic diagrams points out that the emission is composite , suggesting contribution from both star formation and an active galactic nucleus. We conclude our analysis describing how scenarios of both chaotic cold accretion and merging with a gas-rich disc galaxy can efficaciously explain the phenomena the BCG is undergoing. [ABSTRACT FROM AUTHOR]

We quantify the star formation (SF) in the inner cores (⁠|$\mathcal {R}$| / R 200 ≤0.3) of 24 massive galaxy clusters at 0.2≲ z ≲0.9 observed by the Herschel Lensing Survey and the Cluster Lensing and Supernova survey with Hubble. These programmes, covering the rest-frame ultraviolet to far-infrared regimes, allow us to accurately characterize stellar mass-limited (⁠|$\mathcal {M}_{*}\gt 10^{10}$|   M ⊙) samples of star-forming cluster members (not)-detected in the mid- and/or far-infrared. We release the catalogues with the photometry, photometric redshifts, and physical properties of these samples. We also quantify the SF displayed by comparable field samples from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We find that in intermediate- z cluster cores, the SF activity is suppressed with respect the field in terms of both the fraction (⁠|$\mathcal {F}$|⁠) of star-forming galaxies (SFGs) and the rate at which they form stars (⁠|$\mathcal {SFR}$| and |$s\mathcal {SFR} = \mathcal {SFR}/\mathcal {M}_{*}$|⁠). On average, the |$\mathcal {F}$| of SFGs is a factor ∼2 smaller in cluster cores than in the field. Furthermore, SFGs present average |$\mathcal {SFR}$| and |$s\mathcal {SFR}$| typically ∼0.3 dex smaller in the clusters than in the field along the whole redshift range probed. Our results favour long time-scale quenching physical processes as the main driver of SF suppression in the inner cores of clusters since z ∼0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population. [ABSTRACT FROM AUTHOR]

Brightest cluster galaxies (BCGs) residing in cool-core clusters are known to be the stage of intricate baryon cycle phenomena (e.g. gas inflows, AGN outflows, star formation feedback). The scenarios describing the observed properties of these galaxies are still controversial, suffering from limitations due to the spatial resolving power of the instruments, specifically for galaxies beyond the Local Universe. However, the dramatic improvements introduced by the integral-field unit instruments (e.g. MUSE) could shed light on the physical processes driving the evolution of these galaxies. We present an extensive analysis of the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud BCG sitting at the centre of the X-ray luminous cool-core cluster Abell 2667 (z = 0.23), based on MUSE data. Our results indicate that the BCG is a massive elliptical, hosting an AGN that is possibly undergoing accretion of cold star-forming clouds of ICM or galactic cannibalism. [ABSTRACT FROM AUTHOR]

Proxima Centauri, our closest stellar neighbour, is a low-mass M5 dwarf orbiting in a triple system. An Earth-mass planet with an 11 d period has been discovered around this star. The star's mass has been estimated only indirectly using a mass–luminosity relation, meaning that large uncertainties affect our knowledge of its properties. To refine the mass estimate, an independent method has been proposed: gravitational microlensing. By taking advantage of the close passage of Proxima Cen in front of two background stars, it is possible to measure the astrometric shift caused by the microlensing effect due to these close encounters and estimate the gravitational mass of the lens (Proxima Cen). Microlensing events occurred in 2014 and 2016 with impact parameters, the closest approach of Proxima Cen to the background star, of 1.6 ± 0.1 and 0.5 ± 0.1 arcsec, respectively. Accurate measurements of the positions of the background stars during the last 2 yr have been obtained with Hubble Space Telescope /Wide Field Camera 3, and with Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) from the ground. The SPHERE campaign started on 2015 March, and continued for more than 2 yr, covering nine epochs. The parameters of Proxima Centauri's motion on the sky, along with the pixel scale, true North, and centring of the instrument detector were readjusted for each epoch using the background stars visible in the IRDIS field of view. The experiment has been successful and the astrometric shift caused by the microlensing effect has been measured for the second event in 2016. We used this measurement to derive a mass of 0.150 $$^{\textrm{+}0.062}_{-0.051}$$ (an error of ∼ 40 per cent) M⊙ for Proxima Centauri acting as a lens. This is the first and the only currently possible measurement of the gravitational mass of Proxima Centauri. [ABSTRACT FROM AUTHOR]

Copyright of ESTOA: Revista de la Facultad de Arquitectura y Urbanismo de la Universidad de Cuenca is the property of ESTOA Revista de la Facultad de Arquitectura y Urbanismo de la Universidad de Cuenca and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Background: Atrial fibrillation (AF) is the most common cardiac arrhythmia. Some evidence shows that gastroesophageal reflux disease (GERD) may be a trigger for paroxysmal AF (PAF). Most of the previous studies that correlated GERD and AF used questionnaires to diagnose GERD, not an objective evaluation. This study aims to evaluate in patients with PAF: (a) accuracy of symptoms to diagnose GERD; (b) prevalence of GERD; and (c) temporal correlation between cardiac arrhythmia and reflux.Methods: Twenty-two patients (59% females, mean age 68 years) with PAF underwent esophageal manometry followed by ambulatory pH monitoring and concurrent Holter. Eight (36%) patients had GERD symptoms. Patients were grouped as GERD+ or GERD− based on the DeMeester score. Temporal correlation between arrhythmia and reflux was recorded.Results: Six (27%) patients were GERD+. Symptoms had sensitivity and specificity of 50 and 70%, respectively, for the diagnosis of GERD. Episodic AF occurred in one patient only (GERD−). There were 23 episodes of AF during the test with 14% correlation with reflux. Persistent AF during the period of the test was found in five patients (60% GERD+).Conclusions: Our results show: (a) Symptoms have a low accuracy for the diagnosis of GERD; (b) the prevalence of GERD in patients with PAF is low; and (c) temporal correlation between episodes of reflux and cardiac arrhythmia is low. [ABSTRACT FROM AUTHOR]

We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500μm in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single Sérsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5σ. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff ~ 1.77 kpc and a median Gaussian full width at half-maximum ~1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) ~ 900-3500M☉ yr-1, resulting in a median SFR surface density ΣSFR ~ 132M☉ yr-1 kpc-2 (or ~218M☉ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst. [ABSTRACT FROM AUTHOR]