bluuebunny/crossref_metadata_2025_split huggingface dataset:
Benefit of linking hospital resource information and patient-level stroke registry data
Authors: Purvis Tara , Cadilhac Dominique A , Hill Kelvin , Gibbs Adele K , Ghuliani Jot , Middleton Sandy , Kilkenny Monique F 
Published: January 2023

AbstractVariation in the delivery of evidence-based care affects outcomes for patients with stroke. A range of hospital (organizational), patient, and clinical factors can affect care delivery. Clinical registries are widely used to monitor stroke care and guide quality improvement efforts within hospitals. However, hospital features are rarely collected. We aimed to explore the influence of hospital resources for stroke, in metropolitan and regional/rural hospitals, on the provision of evidence-based patient care and outcomes. The 2017 National Audit organizational survey (Australia) was linked to patient-level data from the Australian Stroke Clinical Registry (2016–2017 admissions). Regression models were used to assess the associations between hospital resources (based on the 2015 Australian National Acute Stroke Services Framework) and patient care (reflective of national guideline recommendations), as well as 90–180-day readmissions and health-related quality of life. Models were adjusted for patient factors, including the severity of stroke. Fifty-two out of 127 hospitals with organizational survey data were merged with 22 832 Australian Stroke Clinical Registry patients with an admission for a first-ever stroke or transient ischaemic attack (median age 75 years, 55% male, and 66% ischaemic). In metropolitan hospitals (n = 42, 20 977 patients, 1701 thrombolyzed, and 2395 readmitted between 90 and 180 days post stroke), a faster median door-to-needle time for thrombolysis was associated with ≥500 annual stroke admissions [−15.9 minutes, 95% confidence interval (CI) −27.2, −4.7], annual thrombolysis &gt;20 patients (−20.2 minutes, 95% CI −32.0, −8.3), and having specialist stroke staff (dedicated medical lead and stroke coordinator; −12.7 minutes, 95% CI −25.0, −0.4). A reduced likelihood of all-cause readmissions between 90 and 180 days was evident in metropolitan hospitals using care pathways for stroke management (odds ratio 0.82, 95% CI 0.67–0.99). In regional/rural hospitals (n = 10, 1855 patients), being discharged with a care plan was also associated with the use of stroke clinical pathways (odds ratio 3.58, 95% CI 1.45–8.82). No specific hospital resources influenced 90–180-day health-related quality of life. Relevant to all international registries, integrating information about hospital resources with clinical registry data provides greater insights into factors that influence evidence-based care.
Prevalence and genetic characteristics offosB-positiveStaphylococcus aureusin duck farms in Guangdong, China in 2020
Authors: Hu Jianxin , Chen Lin , Li Guihua , Pan Yu , Lu Yixing , Chen Jin , Xiong Wenguang , Zeng Zhenling 
Published: January 2023

AbstractObjectivesTo investigate the epidemiology of fosB-positive Staphylococcus aureus in waterfowl farms in the Pearl River tributaries in Guangdong Province, China in 2020.MethodsA total of 63 S. aureus were recovered from 315 samples collected from six duck farms and one goose farm. PFGE, WGS and analysis were performed on 19 fosB-positive S. aureus.ResultsThe fosfomycin resistance rate of the strains was as high as 52.4% (33/63), and 30.1% (19/63) of the strains carried fosB. Resistance gene prediction results showed that duck farm environment-derived strains contained the oxazolidinone drug resistance gene optrA. All fosB-positive S. aureus were MRSA and most of them were MDR, mainly ST9-t899 and ST164-t899. PFGE showed that fosB-positive S. aureus from humans and ducks could be clustered into the same clade. In addition, core-genome SNP analysis showed that clonal transmission of S. aureus occurred between humans and water. Pan-genome analysis showed that S. aureus had an open pangenome. The fosB gene was located on 2610–2615 bp plasmids, which all contained a broad host-range plasmid replication protein family 13. Small plasmids carrying the fosB gene could be found in different multilocus STs of S. aureus.ConclusionsThis study indicated that duck farms in Guangdong, China could be an important reservoir of fosB-positive S. aureus. The spread of drug-resistant bacteria in waterfowl farms requires further monitoring.
Reporting Peers’ Wrongdoing: Evidence on the Effect of Incentives on Morally Controversial Behavior
Authors: Fiorin Stefano 
Published: January 2023

Abstract
I show that offering monetary rewards to whistleblowers can backfire as a moral aversion to being paid for harming others can reverse the effect of financial incentives. I run a field experiment with employees of the Afghan Ministry of Education, who are asked to confidentially report on their colleagues’ attendance. I use a two-by-two design, randomizing whether or not reporting absence carries a monetary incentive as well as the perceived consequentiality of the reports. In the consequential treatment arm, where employees are given examples of the penalties that might be imposed on absentees, 15% of participants choose to denounce their peers when reports are not incentivized. In this consequential group, rewards backfire: Only 10% of employees report when denunciations are incentivized. In the non-consequential group, where participants are guaranteed that their reports will not be forwarded to the government, only 6% of employees denounce absence without rewards. However, when moral concerns of harming others are limited through the guarantee of non-consequentiality, rewards do not backfire: The incentivized reporting rate is 12%.
The accretion history of the Milky Way – I. How it shapes globular clusters and dwarf galaxies
Authors: Hammer Francois , Li Hefan , Mamon Gary A , Pawlowski Marcel S , Bonifacio Piercarlo , Jiao Yongjun , Wang Haifeng , Wang Jianling , Yang Yanbin 
Published: January 2023

ABSTRACT
Halo inhabitants are individual stars, stellar streams, star, and globular clusters, and dwarf galaxies. Here we compare the two last categories that include objects of similar stellar mass, which are often studied as self-dynamical equilibrium systems. We discover that the half-light radius of globular clusters depends on their orbital pericentre and total energy, and that Milky Way (MW) tides may explain the observed correlation. We also suggest that the accretion epoch of stellar systems in the MW halo can be calibrated by the total orbital energy, and that such a relation is due to both the mass growth of the MW and dynamical friction affecting mostly satellites with numerous orbits. This calibration starts from the bulge to Kraken, Gaia Sausage Enceladus, Sagittarius stellar systems, and finally to the new coming dwarfs, either or not linked to the vast-polar structure. The most eccentric globular clusters, and dwarfs have their half-light radius scaling as the inverse of their binding energy, and this over more than two decades. This means that earlier arriving satellites are smaller due to the tidal effects of the MW. Therefore, most halo inhabitants appear to have their structural parameters shaped by MW tides, and also by ram-pressure for the most recent arrivals, the dwarf galaxies. The correlations found in this study can be used as tools to further investigate the origin of globular clusters and dwarfs, as well as the assembly history of our Galaxy.
Empirical constraints on the nucleosynthesis of nitrogen
Authors: Johnson James W , Weinberg David H , Vincenzo Fiorenzo , Bird Jonathan C , Griffith Emily J 
Published: January 2023

ABSTRACT
We derive empirical constraints on the nucleosynthetic yields of nitrogen by incorporating N enrichment into our previously developed and empirically tuned multizone galactic chemical evolution model. We adopt a metallicity-independent (‘primary’) N yield from massive stars and a metallicity-dependent (‘secondary’) N yield from AGB stars. In our model, galactic radial zones do not evolve along the observed [N/O]–[O/H] relation, but first increase in [O/H] at roughly constant [N/O], then move upward in [N/O] via secondary N production. By t ≈ 5 Gyr, the model approaches an equilibrium [N/O]–[O/H] relation, which traces the radial oxygen gradient. Reproducing the [N/O]–[O/H] trend observed in extragalactic systems constrains the ratio of IMF-averaged N yields to the IMF-averaged O yield of core-collapse supernovae. We find good agreement if we adopt $y_\text{N}^\text{CC}/y_\text{O}^\text{CC}=0.024$ and $y_\text{N}^\text{AGB}/y_\text{O}^\text{CC} = 0.062(Z/Z_\odot)$. For the theoretical AGB yields we consider, simple stellar populations release half their N after only ∼250 Myr. Our model reproduces the [N/O]–[O/H] relation found for Milky Way stars in the APOGEE survey, and it reproduces (though imperfectly) the trends of stellar [N/O] with age and [O/Fe]. The metallicity-dependent yield plays the dominant role in shaping the gas-phase [N/O]–[O/H] relation, but the AGB time-delay is required to match the stellar age and [O/Fe] trends. If we add ∼40 per cent oscillations to the star formation rate, the model reproduces the scatter in the gas phase [N/O]–[O/H] relation observed in external galaxies by MaNGA. We discuss implications of our results for theoretical models of N production by massive stars and AGB stars.
The relationship between galaxy and halo sizes in the Illustris and IllustrisTNG simulations
Authors: Karmakar Tathagata , Genel Shy , Somerville Rachel S 
Published: January 2023

ABSTRACT
Abundance matching studies have shown that the average relationship between galaxy radius and dark matter halo virial radius remains nearly constant over many orders of magnitude in halo mass, and over cosmic time since about z = 3. In this work, we investigate the predicted relationship between galaxy radius re and halo virial radius Rh in the numerical hydrodynamical simulations Illustris and IllustrisTNG from z ∼ 0–3, and compare with the results from the abundance matching studies. We find that Illustris predicts much higher re/Rh values than the constraints obtained by abundance matching, at all redshifts, as well as a stronger dependence on halo mass. In contrast, IllustrisTNG shows very good agreement with the abundance matching constraints. In addition, at high redshift it predicts a strong dependence of re/Rh on halo mass on mass scales below those that are probed by existing observations. We present the predicted re/Rh relations from Illustris and IllustrisTNG for galaxies divided into star forming and quiescent samples, and quantify the scatter in re/Rh for both simulations. Further, we investigate whether this scatter arises from the dispersion in halo spin parameter and find no significant correlation between re/Rh and halo spin. We investigate the paths in re/Rh traced by individual haloes over cosmic time, and find that most haloes oscillate around the median re/Rh relation over their formation history.
The resolved chemical composition of the starburst dwarf galaxy CGCG007-025: direct method versus photoionization model fitting
Authors: Fernández V , Amorín R , Sanchez-Janssen R , del Valle-Espinosa M G , Papaderos P 
Published: January 2023

ABSTRACTThis work focuses on the gas chemical composition of CGCG007-025. This compact dwarf is undergoing a galaxy wide star-forming burst, whose spatial behaviour has been observed by VLT/MUSE. We present a new line measurement library to treat almost 7800 voxels. The direct method chemical analysis is limited to 484 voxels with good detection of the $[\mathrm{S}\, {\small III}]6312\, \mathring{\rm A}$ temperature diagnostic line. The recombination fluxes are corrected for stellar absorption via a population synthesis. Additionally, we discuss a new algorithm to fit photoionization models via neural networks. The eight ionic abundances analysed show a spatial normal distribution with a $\sigma \sim 0.1\, {\rm dex}$, where only half this value can be explained by the uncertainty in the measurements. The oxygen abundance distribution is 12 + log(O/H) = 7.88 ± 0.11. The ${\it T}_{e}[\mathrm{S}\, {\small III}]$ and ne[S ii] are also normally distributed. However, in the central and brightest region, the ne[S ii] is almost thrice the mean galaxy value. This is also reflected in the extinction measurements. The ionization parameter has a distribution of ${\rm log}(U) = -2.52^{0.17}_{0.19}$. The parameter spatial behaviour agrees with the S2+/S+ map. Finally, the discrepancies between the direct method and the photoionization model fitting are discussed. In the latter technique, we find that mixing lines with uneven uncertainty magnitudes can impact the accuracy of the results. In these fittings, we recommend overestimating the minimum flux uncertainty one order below the maximum line flux uncertainty. This provides a better match with the direct method.
Investigating the variability of Swift-BAT blazars with NICER
Authors: Mundo Sergio A , Mushotzky Richard 
Published: January 2023

ABSTRACT
We present results of X-ray spectral and time-domain variability analyses of four faint, ‘quiescent’ blazars from the Swift-BAT 105-month catalogue. We use observations from a recent, 5-month long NICER campaign, as well as archival BAT data. Variations in the 0.3–2 keV flux are detected on minute, ∼weekly, and monthly time-scales, but we find that the fractional variability Fvar on these time-scales is &lt;25 per cent and decreases on longer time-scales, implying generally low-amplitude variability across all sources and showing very low variability on monthly time-scales ($F_{\rm var}\lesssim 13{{\ \rm per\ cent}}$), which is at odds with previous studies that show that blazars are highly variable in the X-rays on a wide range of time-scales. Moreover, we find that the flux variability on very short time-scales appears to be characterized by long periods of relative quiescence accompanied by occasional short bursts, against the relatively time-stationary nature of the variability of most other AGN light curves. Our analysis also shows that the broadband X-ray spectra (0.3–195 keV) of our sources can be described with different power-law models. As is the case with most blazars, we find that two sources (2MASS J09343014-1721215 and PKS 0312-770) are well-modelled with a simple power law, while the remaining two (1RXS J225146.9-320614 and PKS 2126-15) exhibit curvature in the form of a log-parabolic power law. We also find that, in addition to the continuum, PKS 2126-15 requires significant absorption at the soft X-rays (≲1 keV) to fully describe the observed curvature, possibly due to absorption from the intergalactic medium.
Revised constraints on the photon mass from well-localized fast radio bursts
Authors: Lin Hai-Nan , Tang Li , Zou Rui 
Published: January 2023

ABSTRACT
We constrain the photon mass from well-localized fast radio bursts (FRBs) using Bayes inference method. The probability distributions of dispersion measures (DMs) of host galaxy and intergalactic medium are properly taken into account. The photon mass is tightly constrained from 17 well-localized FRBs in the redshift range 0 &lt; z &lt; 0.66. Assuming that there is no redshift evolution of host DM, the 1σ and 2σ upper limits of photon mass are constrained to be mγ &lt; 4.8 × 10−51 kg and mγ &lt; 7.1 × 10−51 kg, respectively. Monte Carlo simulations show that even enlarging the FRB sample to 200 and extending the redshift range to 0 &lt; z &lt; 3 could not significantly improve the constraining ability on photon mass. This is because of the large uncertainty on the DM of intergalactic medium.
Enabling discovery of gravitationally lensed explosive transients: a new method to build an all-sky watch list of groups and clusters of galaxies
Authors: Ryczanowski Dan , Smith Graham P , Bianconi Matteo , McGee Sean , Robertson Andrew , Massey Richard , Jauzac Mathilde 
Published: January 2023

ABSTRACT
Cross-referencing a watch list of galaxy groups and clusters with transient detections from real-time streams of wide-field survey data is a promising method for discovering gravitationally lensed explosive transients, including supernovae, kilonovae, gravitational waves, and gamma-ray bursts in the next 10 yr. However, currently there exists no catalogue of objects with both sufficient angular extent and depth to adequately perform such a search. In this study, we develop a cluster-finding method capable of creating an all-sky list of galaxy group- and cluster-scale objects out to z ≃ 1 based on their lens-plane properties and using only existing data from wide-field infrared surveys such as VISTA Hemisphere Survey and UKIRT Hemisphere Survey, and all-sky WISE (Wide-field Infrared Survey Explorer) data. In testing this method, we recover 91 per cent of a sample containing known and candidate lensing objects with Einstein radii of θE ≥ 5 arcsec. We also search the surrounding regions of this test sample for other groups and clusters using our method and verify the existence of any significant findings by visual inspection, deriving estimates of the false positive rate that are as low as 6 per cent. The method is also tested on simulated Rubin data from their Data Preview 0 programme, which yields complementary results of a good recovery rate of ≳80 per cent for M200 ≥ 7 × 1013 M⊙ clusters and with no false positives produced in our test region. Importantly, our method is positioned to create a watch list in advance of Rubin’s LSST, as it utilizes only existing data, therefore enabling the discovery of lensed transients early within the survey’s lifetime.
Cloudy with a chance of rain: accretion braking of cold clouds
Authors: Tan Brent , Oh S Peng , Gronke Max 
Published: January 2023

ABSTRACT
Understanding the survival, growth, and dynamics of cold gas is fundamental to galaxy formation. While there has been a plethora of work on ‘wind tunnel’ simulations that study such cold gas in winds, the infall of this gas under gravity is at least equally important, and fundamentally different since cold gas can never entrain. Instead, velocity shear increases and remains unrelenting. If these clouds are growing, they can experience a drag force due to the accretion of low-momentum gas, which dominates over ram pressure drag. This leads to subvirial terminal velocities, in line with observations. We develop simple analytic theory and predictions based on turbulent radiative mixing layers. We test these scalings in 3D hydrodynamic simulations, both for an artificial constant background and a more realistic stratified background. We find that the survival criterion for infalling gas is more stringent than in a wind, requiring that clouds grow faster than they are destroyed ($t_{\rm grow} \lt 4\, t_{\rm cc}$). This can be translated to a critical pressure, which for Milky Way-like conditions is $P \sim 3000 \, {k}_\mathrm{ B} \, {\rm K}\, {\rm cm}^{-3}$. Cold gas that forms via linear thermal instability (tcool/tff &lt; 1) in planar geometry meets the survival threshold. In stratified environments, larger clouds need only survive infall until cooling becomes effective. We discuss applications to high-velocity clouds and filaments in galaxy clusters.
Radiative turbulent mixing layers at high Mach numbers
Authors: Yang Yanhui , Ji Suoqing 
Published: January 2023

ABSTRACTRadiative turbulent mixing layers (TMLs) are ubiquitous in astrophysical environments, for example the circumgalactic medium (CGM), and are triggered by the shear velocity at interfaces between different gas phases. To understand the shear velocity dependence of TMLs, we perform a set of 3D hydrodynamic simulations with an emphasis on the TML properties at high Mach numbers $\mathcal {M}$. Since the shear velocity in mixing regions is limited by the local sound speed of mixed gas, high-Mach number TMLs develop into a two-zone structure: a Mach number-independent mixing zone traced by significant cooling and mixing, plus a turbulent zone with large-velocity dispersions which expands with greater $\mathcal {M}$. Low-Mach number TMLs do not have distinguishable mixing and turbulent zones. The radiative cooling of TMLs at low and high Mach numbers is predominantly balanced by enthalpy consumption and turbulent dissipation, respectively. Both the TML surface brightness and column densities of intermediate-temperature ions (e.g. O vi) scale as $\propto \mathcal {M}^{0.5}$ at $\mathcal {M} \lesssim 1$, but reach saturation ($\propto \mathcal {M}^0$) at $\mathcal {M} \gtrsim 1$. Inflow velocities and hot gas entrainment into TMLs are substantially suppressed at high Mach numbers, and strong turbulent dissipation drives the evaporation of cold gas. This is in contrast to low-Mach number TMLs where the inflow velocities and hot gas entrainment are enhanced with greater $\mathcal {M}$, and cold gas mass increases due to the condensation of entrained hot gas.
The SQUALO project (Star formation in QUiescent And Luminous Objects) I: clump-fed accretion mechanism in high-mass star-forming objects
Authors: Traficante A , Jones B M , Avison A , Fuller G A , Benedettini M , Elia D , Molinari S , Peretto N , Pezzuto S , Pillai T , Rygl K L J , Schisano E , Smith R J 
Published: January 2023

ABSTRACT
The formation mechanism of the most massive stars is far from completely understood. It is still unclear if the formation is core-fed or clump-fed, i.e. if the process is an extension of what happens in low-mass stars, or if the process is more dynamical such as a continuous, multiscale accretion from the gas at parsec (or even larger) scales. In this context, we introduce the SQUALO project, an ALMA 1.3 and 3 mm survey designed to investigate the properties of 13 massive clumps selected at various evolutionary stages, with the common feature that they all show evidence for accretion at the clump scale. In this work, we present the results obtained from the 1.3 mm continuum data. Our observations identify 55 objects with masses in the range 0.4 ≤ M ≤ 309 M⊙, with evidence that the youngest clumps already present some degree of fragmentation. The data show that physical properties such as mass and surface density of the fragments and their parent clumps are tightly correlated. The minimum distance between fragments decreases with evolution, suggesting a dynamical scenario in which massive clumps first fragment under the influence of non-thermal motions driven by the competition between turbulence and gravity. With time gravitational collapse takes over and the fragments organize themselves into more thermally supported objects while continuing to accrete from their parent clump. Finally, one source does not fragment, suggesting that the support of other mechanisms (such as magnetic fields) is crucial only in specific star-forming regions.