bluuebunny/crossref_metadata_2025_split huggingface dataset:
Clustering of disability pension and socioeconomic disadvantage in Sweden: a geospatial analysis
Authors: Virtanen Marianna , Heikkilä Katriina , Vahtera Jussi , Kivimäki Mika , Halonen Jaana I , Alexanderson Kristina , Rautiainen Simo , Lallukka Tea , Mittendorfer-Rutz Ellenor 
Published: July 2022

Abstract

Background
To characterize geospatial patterning of disadvantage in Sweden, we examined whether municipal-level indicators of socioeconomic disadvantage and disability pension (DP) rate were clustered, whether the different geospatial clusters were overlapping and whether the findings were similar among women and men.

Methods
Administrative national data from all 290 Swedish municipalities were used to determine the prevalence of DP and socioeconomic disadvantage [poverty, long-term unemployment, income inequality (GINI Index) and income inequality between women and men]. Geospatial cold spots (clusters of municipalities with a DP/socioeconomic disadvantage prevalence lower than the nationwide prevalence) and hot spots (clusters of municipalities with a DP/socioeconomic disadvantage higher than the nationwide prevalence) were identified, and whether a hot spot was overlapping with another hot spot and a cold spot overlapping with another cold spot were analysed using the Getis-Ord Gi statistics.

Results
Among women and men, cold spots of DP were most consistently located in the Stockholm area. Hot spots of DP were found in the mid-south Sweden, characterized by mid-sized urban centres in rural territories. High DP rate and socioeconomic disadvantage were overlapping, except for income inequality. Clusters of gender income inequality and women’s high DP rate were observed in mid-south Sweden.

Conclusion
DP and socioeconomic disadvantage are not randomly distributed in Sweden. Geospatial analyses revealed clusters of municipalities with high risk of both DP and socioeconomic disadvantage in certain areas and low risk in other areas. Further research is needed to identify preventive actions to decrease regional inequalities in work capacity.
Outcomes of in-vitro fertilization after bariatric surgery: a national register-based case–control study
Authors: Nilsson-Condori E , Mattsson K , Thurin-Kjellberg A , Hedenbro J L , Friberg B 
Published: July 2022

Abstract

STUDY QUESTION
Does previous bariatric surgery (BS) in women affect cumulative live birth rate in IVF?

SUMMARY ANSWER
Women having had BS seem to have the same cumulative live birth rate as non-operated women of the same BMI at IVF treatment.

WHAT IS KNOWN ALREADY
Because of the perinatal risks of obesity to mother and infant as well as impaired outcomes of IVF, obese women are advised to reduce their weight, but it is not clear whether previous BS could affect IVF results.

STUDY DESIGN, SIZE, DURATION
This national register-based case–control study included all cases of BS (n = 30 436) undergoing IVF (n = 153) from 2007 until 2017.

PARTICIPANTS/MATERIALS, SETTING, METHODS
Swedish women between 18 and 45 years operated with BS, with at least one first started cycle of IVF after surgery, were included. For each woman having IVF after BS (n = 153), up to five non-operated control women (n = 744) starting their first IVF cycle during the study period were matched for age, parity and BMI at treatment. The primary outcome in this study was the cumulative live birth rate (CLBR) after the first IVF cycle, defined as all live births after the first cycle including fresh and frozen embryo transfers.

MAIN RESULTS AND THE ROLE OF CHANCE
There was no significant difference in CLBR between the BS group and the matched controls (29.4% compared to 33.1%), even though the number of retrieved oocytes (7.6 vs 8.9, P = 0.005) and frozen embryos (1.0 vs 1.5, P = 0.041) were significantly fewer in the BS group. There was no association between cumulative live birth and BS, adjusted odds ratio 1.04, 95% CI (0.73, 1.51). However, the birth weight was significantly lower in the children born to mothers with previous BS, mean (SD) 3190 (690) vs 3478 (729) g, P = 0.037.

LIMITATIONS, REASONS FOR CAUTION
Confounders such as age, BMI and previous childbirth were accounted for by the matching design of the study, but there were no data on indication for IVF, anti-Müllerian hormone, smoking or previous comorbidities. The study was exploratory and did not reach sufficient power to detect potential smaller differences in live birth rates.

WIDER IMPLICATIONS OF THE FINDINGS
The findings concur with those in previously published smaller studies and provide somewhat reassuring results considering IVF outcomes after BS with a CLBR comparable to that of controls, despite a lower mean birth weight.

STUDY FUNDING/COMPETING INTEREST(S)
This research was funded by grants from the Southern Health Care Region of Sweden. The authors have no competing interests to declare.

TRIAL REGISTRATION NUMBER
N/A.
What Influences Trust in Survey Results? Evidence From a Vignette Experiment
Authors: Stadtmüller Sven , Silber Henning , Beuthner Christoph 
Published: July 2022

Abstract
More survey results are available today than ever before. This increase in survey data has been accompanied by growing concerns about their quality. With the present study, we aim to investigate to what extent the public draws on survey quality information when evaluating the trustworthiness of survey results. We implemented a vignette experiment in an online panel survey (N = 3,313), in which respondents each received four different survey descriptions with varying methodological information. Compared with respondent characteristics, survey quality information had only a minor effect on perceptions of trustworthiness. However, trust in the survey results was significantly influenced by sample size and sample balance. Finally, the relevance of survey quality information increased with the cognitive ability of the respondent.
Corruption and Political Knowledge Erosion. A Cautionary Tale from Latin America
Authors: Bargsted Matías , Bachmann Ingrid , Valenzuela Sebastián 
Published: July 2022

Abstract
Previous research has shown that corruption diminishes citizens’ level of political support and engagement. We extend this line of reasoning and evaluate whether previous levels of perceived corruption can influence subsequent levels of political knowledge. We test this proposition with data from a two-wave panel probability survey applied in Chile between 2016 and 2017, just after a 2-year period in which an avalanche of corruption scandals shook the country. Our estimates confirm that perceived corruption reduces subsequent political knowledge, while controlling for prior knowledge. This pattern is particularly strong among non-ideologues and people ideologically distant from the incumbent government. Given the status of political knowledge as a democratically valuable trait, our results uncover some normatively disturbing consequences of corruption.
Information Architecture: Using K-Means Clustering and the Best Merge Method for Open Card Sorting Data Analysis
Authors: Paea Sione , Katsanos Christos , Bulivou Gabiriele 
Published: July 2022

Abstract
Open card sorting is a well-established method for discovering how people understand and categorize information. This paper addresses the problem of quantitatively analyzing open card sorting data using the K-means algorithm. Although the K-means algorithm is effective, its results are too sensitive to initial category centers. Therefore, many approaches in the literature have focused on determining suitable initial centers. However, this is not always possible, especially when the number of categories is increased. This paper proposes an approach to improve the quality of the solution produced by the K-means for open card sort data analysis. Results show that the proposed initialization approach for K-means outperforms existing initialization methods, such as MaxMin, random initialization and K-means++. The proposed algorithm is applied to a real-world open card sorting dataset, and, unlike existing solutions in the literature, it can be used with any number of participants and cards.
A novel deep convolutional neural network algorithm for surface defect detection
Authors: Zhang Dehua , Hao Xinyuan , Liang Linlin , Liu Wei , Qin Chunbin 
Published: July 2022

Abstract
The surface defect detection (SDD) problem is one of the crucial techniques during production process, so it has become a key research area to control the quality of industrial products, which has been increasingly of greater interest to the researchers especially with the rapid development of artificial neural networks technology in recent years. Therefore, this paper proposes a novel deep convolutional neural network algorithm aiming at SDD. Firstly, a dense cross-stage partial Darknet backbone network is designed for feature extraction by optimizing cross-stage partial Darknet through the idea of dense connections, which can, not only enhance feature reuse but also greatly alleviate the overfitting issue. Secondly, a new cross-stage hierarchy module is presented combining the cross-stage feature fusion strategy and depthwise separable convolution technique for each node of the path aggregated feature pyramid network (PAN). Finally, an efficient channel attention (ECA) mechanism is introduced in PAN to construct a novel ECA PAN. The experimental results on three surface defect datasets show that the mean average precision of this network is 2.63, 5.48, and 1.16$\%$ which is higher than that of the baseline network, respectively. The proposed network outperforms not only the classical models but state-of-the-art models, which indicates the proposed algorithm can achieve higher accuracy and speed with fewer calculation parameters. And what is more, the proposed algorithm also has outstanding generalization ability.
Horizon auto-picking with quantitative uncertainty evaluation by using a modified VQ-VAE framework
Authors: Yuan Cheng , Su Mingjun , Ni Changkuan , Liu Xingye , Xu Yunze , Cui Xiangli 
Published: July 2022

Abstract
In this paper, we propose a novel approach of deep-learning-based seismic horizon auto-picking that introduces a modified vector quantized variational autoencoder (VQ-VAE) framework to improve the accuracy of seismic horizon interpretation and, for the first time, quantitatively evaluate the uncertainty of the auto-picked horizon by exploiting the concept of entropy. Compared with the conventional VQ-VAE approach, the proposed method not only modifies the VQ-VAE model with more deep-learning channels at each layer of the network to enhance the performance of horizon auto-picking within the VQ-VAE framework, but also extends the 1D seismic labels with more continuous samplings within a single trace to boost the stability of auto-picked horizon in geologically complex settings and also significantly suppress the resulting uncertainty. To further improve the resulting accuracy in geologically complex settings, we introduce the directional structure tensor to extract a more reliable initial horizon and, moreover, a dilated horizon searching strategy to extend the capacity of the proposed method in dealing with the large fault displacement and reducing the computational cost simultaneously. Additionally, the resulting uncertainty quantitatively measured by entropy can also serve as an effective indicator to enable a further refinement of the auto-picked result accordingly. Both 2D example and 3D field applications are carried out to validate the effectiveness of the proposed method.
Identifying the carbonate interlayer using the horn response of electromagnetic wave resistivity logging while drilling combined with drilling and mud-logging data during geo-steering
Authors: Shao Cairui , Zhang Pangfei , Ji Jiaqi , Chang Lunjie 
Published: July 2022

Abstract
The electromagnetic wave propagation resistivity (EWPR) and natural gamma rays (GR) are commonly used in logging while drilling (LWD) to identify the formation interface and for geo-steering. Because the GR logging value of a carbonate reservoir does not change significantly or not change at all, the horn effect of the EWPR is the main basis for identifying the formation interface. However, many factors influence the horn effect, so it is sometimes difficult to determine whether the sharper response of the EWPR is the horn signal or the real value of the thin interlayer. Therefore, based on a review of existing research results, in this paper, the EWR-PHASE4 LWD tool is taken as an example, and using a numerical forward simulation, the influences of different resistivity ratios of the surrounding rock to the target layers, the different transmitter spacings on the EWPR for different angles between the borehole trajectory and formation are investigated. The conditions required to generate horn signals at the formation interfaces and the influencing rules of the main influencing factors are summarized, providing a theoretical basis for correctly determining the formation occurrence. Since the drilling and mud-logging data can be used to determine the formation's properties directly, through application examples, this study provides a reference for identifying the carbonate interlayer and formation occurrence using a combination of EWPR with drilling and mud-logging data, which has a smaller uncertainty than the application of only EWPR.
Reionization time of the Local Group and Local-Group-like halo pairs
Authors: Sorce Jenny G , Ocvirk Pierre , Aubert Dominique , Gottlöber Stefan , Shapiro Paul R , Dawoodbhoy Taha , Yepes Gustavo , Ahn Kyungjin , Iliev Ilian T , Lewis Joseph S W 
Published: July 2022

ABSTRACT
Patchy cosmic reionization resulted in the ionizing UV background asynchronous rise across the Universe. The latter might have left imprints visible in present-day observations. Several numerical simulation-based studies show correlations between the reionization time and overdensities and object masses today. To remove the mass from the study, as it may not be the sole important parameter, this paper focuses solely on the properties of paired haloes within the same mass range as the Milky Way. For this purpose, it uses CoDaII, a fully coupled radiation hydrodynamics reionization simulation of the local Universe. This simulation holds a halo pair representing the Local Group, in addition to other pairs, sharing similar mass, mass ratio, distance separation, and isolation criteria but in other environments, alongside isolated haloes within the same mass range. Investigations of the paired halo reionization histories reveal a wide diversity although always inside-out, given our reionization model. Within this model, haloes in a close pair tend to be reionized at the same time but being in a pair does not bring to an earlier time their mean reionization. The only significant trend is found between the total energy at z = 0 of the pairs and their mean reionization time: Pairs with the smallest total energy (bound) are reionized up to 50 Myr earlier than others (unbound). Above all, this study reveals the variety of reionization histories undergone by halo pairs similar to the Local Group, that of the Local Group being far from an average one. In our model, its reionization time is ∼625 Myr against 660 ± 4 Myr (z ∼ 8.25 against 7.87 ± 0.02) on average.
Comprehensive listing of 156 reliable orbital periods for novae, including 49 new periods
Authors: Schaefer Bradley E 
Published: July 2022

ABSTRACT
I report on a large-scale search for the orbital periods (P) of most known nova systems, by looking for significant, coherent, and stable optical photometric modulation in two or more independent light curves taken mostly from the large surveys of TESS, Kepler, AAVSO, SMARTS, OGLE, ASAS, and ZTF. I have discovered 31 new orbital periods. Further, I have measured new periods for 18 novae with evolved companions, to 30 per cent accuracy, as based on their spectral energy distribution. Also, I have confirmed, improved, and rejected prior claims for P in 46 novae. (As part of this effort, I recognize that 5 novae display 1–3 coherent, significant, and transient periodicities 0.12–4.1 d, with these being mysterious as not being the orbital, spin, or superhump periods). In all, I have compiled a comprehensive list of 156 reliable P values for novae. The histogram of nova periods shows a minimum P at 0.059 h (85 min), and a Period Gap from 0.071 to 0.111 d (1.70–2.66 h). The upper edge of the Period Gap is significantly different between novae (0.111 d), nova-like systems (0.131 d), and dwarf novae (0.141 d). A further issue from the histogram is that 31 per cent of nova systems have evolved companions, for which there has been no models or understanding for their current state or evolution. For the novae with red giant companions, 15-out-of-20 are in the bulge population, despite novae with main-sequence and subgiant companions having bulge fractions near 0.11–0.32.
Dust, CO, and [C i]: cross-calibration of molecular gas mass tracers in metal-rich galaxies across cosmic time
Authors: Dunne L , Maddox S J , Papadopoulos P P , Ivison R J , Gomez H L 
Published: July 2022

ABSTRACT
We present a self-consistent cross-calibration of the three main molecular gas mass tracers in galaxies, namely the 12CO(1–0), [C i](3P1–3P0) lines, and the submm dust continuum emission, using a sample of 407 galaxies, ranging from local discs to submillimetre-selected galaxies (SMGs) up to z ≈ 6. A Bayesian statistical method is used to produce galaxy-scale universal calibrations of these molecular gas indicators, that hold over 3–4 orders of magnitude in infrared luminosity, LIR. Regarding the dust continuum, we use a mass-weighted dust temperature, Tmw, determined using new empirical relations between temperature and luminosity. We find the average L/Mmol gas mass conversion factors (including He) to be ${\alpha _{850}}=6.9\times 10^{12}\, \rm W\, Hz^{-1}\, M_{\odot }^{-1}$, αCO = 4.0 M⊙ (κ km s−1 pc2)−1, and $\alpha _{\rm C\, I}$ = 17.0 M⊙ (κ km s−1 pc2)−1, based on the assumption that the mean dust properties of the sample (κH = gas-to-dust ratio/dust emissivity) will be similar to those of local metal rich galaxies and the Milky Way. The tracer with the least intrinsic scatter is [C i](1–0), while CO(1–0) has the highest. The conversion factors show a weak but significant correlation with LIR which is not apparent when Tmw is held constant. Assuming dust properties typical of metal-rich galaxies, we infer a neutral carbon abundance ${X_{\rm C\, I}}=\rm [C^0/\rm{H_2}]=1.6\times 10^{-5}$, similar to that in the Milky Way. We find no evidence for bi-modality of αCO between main-sequence (MS) galaxies and those with extreme star-formation intensity, i.e. ultraluminous infrared galaxies (ULIRGs) and SMGs. The means of the three conversion factors are found to be similar between MS galaxies and ULIRGs/SMGs, to within 10–20 per cent. The overarching conclusion of our work is that, for metal-rich galaxies, near-universal average values for αCO, $X_{\rm C\, I}$, and κH are adequate for global molecular gas estimates within the expected uncertainties. The 1σ scatter in our optimized values for αCO, $X_{\rm C\, I}$, and κH are 0.14, 0.11, and 0.15 dex, respectively.
Energy balance and Alfvén Mach numbers in compressible magnetohydrodynamic turbulence with a large-scale magnetic field
Authors: Beattie James R , Krumholz Mark R , Skalidis Raphael , Federrath Christoph , Seta Amit , Crocker Roland M , Mocz Philip , Kriel Neco 
Published: July 2022

ABSTRACT
Energy equipartition is a powerful theoretical tool for understanding astrophysical plasmas. It is invoked, for example, to measure magnetic fields in the interstellar medium (ISM), as evidence for small-scale turbulent dynamo action, and, in general, to estimate the energy budget of star-forming molecular clouds. In this study, we motivate and explore the role of the volume-averaged root-mean-squared (rms) magnetic coupling term between the turbulent, $\delta {\boldsymbol{B}}$ , and large-scale, ${\boldsymbol{B}}_0$, fields, ${\left\langle (\delta \mathrm{{\boldsymbol {\mathit {B}}}}\cdot {\mathrm{{\boldsymbol {\mathit {B}}}}_0})^{2} \right\rangle ^{1/2}_{\mathcal {V}}}$. By considering the second moments of the energy balance equations we show that the rms coupling term is in energy equipartition with the volume-averaged turbulent kinetic energy for turbulence with a sub-Alfvénic large-scale field. Under the assumption of exact energy equipartition between these terms, we derive relations for the magnetic and coupling term fluctuations, which provide excellent, parameter-free agreement with time-averaged data from 280 numerical simulations of compressible magnetohydrodynamic (MHD) turbulence. Furthermore, we explore the relation between the turbulent mean field and total Alfvén Mach numbers, and demonstrate that sub-Alfvénic turbulence can only be developed through a strong, large-scale magnetic field, which supports an extremely super-Alfvénic turbulent magnetic field. This means that the magnetic field fluctuations are significantly subdominant to the velocity fluctuations in the sub-Alfvénic large-scale field regime. Throughout our study, we broadly discuss the implications for observations of magnetic fields and understanding the dynamics in the magnetized ISM.
The magnetic field of the chemically peculiar star V352 Peg
Authors: Fréour L , Neiner C , Landstreet J D , Folsom C P , Wade G A 
Published: July 2022

ABSTRACTWe present a spectropolarimetric analysis of the hot star V352 Peg. We have acquired 18 spectropolarimetric observations of the star with ESPaDOnS at the CFHT between 2018 and 2019 and completed our data set with one archival ESPaDOnS measurement obtained in 2011. Our analysis of the spectra shows that the star is on the main sequence and chemically peculiar, i.e. it is a Bp star, with overabundances of iron peak elements (Ti, Cr, and Fe) and underabundance of He and O. Through a Least-Square Deconvolution of each spectrum, we extracted the mean Zeeman signature and mean line profile of thousands of spectral lines and detected a magnetic field in V352 Peg. By modelling the Stokes I and V profiles and using the Oblique Rotator Model, we determined the geometrical configuration of V352 Peg. We also performed Zeeman–Doppler Imaging (ZDI) to provide a more detailed characterization of the magnetic field of V352 Peg and its surface chemical distributions. We find a magnetic field that is mainly dipolar, dominantly poloidal, and largely non-axisymmetric with a dipole field strength of ∼9 kG and a magnetic axis almost perpendicular to the rotation axis. The strong variability of Stokes I profiles also suggests the presence of chemical spots at the stellar surface.