bluuebunny/crossref_metadata_2025_split huggingface dataset:
Prediction of body condition in Jersey dairy cattle from 3D-images using machine learning techniques
Authors: Stephansen Rasmus B , Manzanilla-Pech Coralia I V , Gebreyesus Grum , Sahana Goutam , Lassen Jan 
Published: November 2023

Abstract
The body condition of dairy cows is a crucial health and welfare indicator that is widely acknowledged. Dairy herds with a well-management body condition tend to have more fertile and functional cows. Therefore, routine recording of high-quality body condition phenotypes is required. Automated prediction of body condition from 3D images can be a cost-effective approach to current manual recording by technicians. Using 3D-images, we aimed to build a reliable prediction model of body condition for Jersey cows. The dataset consisted of 808 individual Jersey cows with 2,253 phenotypes from three herds in Denmark. Body condition was scored on a 1 to 9 scale and transformed into a 1 to 5 scale with 0.5-unit differences. The cows’ back images were recorded using a 3D camera (Microsoft Xbox One Kinect v2). We used contour and back height features from 3D-images as predictors, together with class predictors (evaluator, herd, evaluation round, parity, lactation week). The performance of machine learning algorithms was assessed using H2O AutoML algorithm (h2o.ai). Based on outputs from AutoML, DeepLearning (DL; multi-layer feedforward artificial neural network) and Gradient Boosting Machine (GBM) algorithms were implemented for classification and regression tasks and compared on prediction accuracy. In addition, we compared the Partial Least Square (PLS) method for regression. The training and validation data were divided either through a random 7:3 split for 10 replicates or by allocating two herds for training and one herd for validation. The accuracy of classification models showed the DL algorithm performed better than the GBM algorithm. The DL model achieved a mean accuracy of 48.1% on the exact phenotype and 93.5% accuracy with a 0.5-unit deviation. The performances of PLS and DL regression methods were comparable, with mean coefficient of determination of 0.67 and 0.66, respectively. When we used data from two herds for training and the third herd as validation, we observed a slightly decreased prediction accuracy compared to the 7:3 split of the dataset. The accuracies for DL and PLS in the herd validation scenario were &gt; 38% on the exact phenotype and &gt; 87% accuracy with 0.5-unit deviation. This study demonstrates the feasibility of a reliable body condition prediction model in Jersey cows using 3D-images. The approach developed can be used for reliable and frequent prediction of cows’ body condition to improve dairy farm management and genetic evaluations.
Deterministic surface roughness effects on elastic material contact with shear thinning fluid media
Authors: Jang Siyoul 
Published: November 2023

Abstract
The formation of lubrication films is described using the hydrodynamic lubrication theory, which is based on the Reynolds equation that includes shear thinning behaviors of lubricant. Contacting surfaces are considered to undergo elastic deformation owing to concentrated contact pressures that exceed 1.0 GPa in most engineering applications. Under the contact condition of a high load on a relatively small contact area, elastic deformation of contacting bodies directly influences the formation of the lubricated film. Elastohydrodynamic lubrication (EHL) analysis is applied to correctly analyze the lubricated contact. Under an EHL contact, the scale of the lubrication film thickness is frequently less than that of the surface roughness that results from either the manufacturing or running-in processes. In this work, surface roughness is considered in detail, and two-dimensional surface roughness is measured as that characterizing general engineering surface roughness. The deterministic method regarding the surface roughness is considered for computing EHL film formation under several contact conditions such as load, contact velocity, and elasticity of contacting materials.
Lion Localizer: A software tool for inferring the provenance of lions (Panthera leo) using mitochondrial DNA
Authors: Au Wesley C , Dures Simon G , Ishida Yasuko , Green Cory E , Zhao Kai , Ogden Rob , Roca Alfred L 
Published: November 2023

Abstract
The illegal poaching of lions for their body parts poses a severe threat to lion populations across Africa. Poaching accounts for 35% of all human-caused lion deaths, with 51% attributed to retaliatory killings following livestock predation. In nearly half of the retaliatory killings, lion body parts are removed, suggesting that high demand for lion body parts may fuel killings attributed to human-lion conflict. Trafficked items are often confiscated in transit or destination countries far from their country of origin. DNA from lion parts may in some cases be the only available means for examining their geographic origins. In this paper, we present the Lion Localizer, a full-stack software tool that houses a comprehensive database of lion mitochondrial DNA (mtDNA) sequences sourced from previously published studies. The database covers 146 localities from across the African continent and India, providing information on the potential provenance of seized lion body parts. Lion mtDNA sequences of 350 or 1,140 bp corresponding to the cytochrome b region can be generated from lion products and queried against the Lion Localizer database. Using the query sequence, the Lion Localizer generates a listing of exact or partial matches, which are displayed on an interactive map of Africa. This allows for the rapid identification of potential regions and localities where lions have been or are presently being targeted by poachers. By examining the potential provenance of lion samples, the Lion Localizer serves as a valuable resource in the fight against lion poaching. The software is available at https://lionlocalizer.org.
Significance of tumor size and number of positive nodes in patients with FIGO 2018 stage IIIC1 cervical cancer
Authors: Maeda Michihide , Mabuchi Seiji , Sakata Mina , Deguchi Satoki , Kakubari Reisa , Matsuzaki Shinya , Hisa Tsuyoshi , Kamiura Shoji 
Published: November 2023

Abstract

Objective
This study aimed to investigate the prognostic significance of tumor size and number of positive pelvic lymph nodes (PLN) in International Federation of Gynecology and Obstetrics (FIGO) 2018 stage IIIC1 cervical cancer patients.

Methods
Clinical data from 626 women with cervical cancer treated at Osaka International Cancer Center in 2010–2020 were retrospectively reviewed. Using the cutoff value obtained on the receiver operating characteristic analysis, the prognostic significance of tumor size and number of positive PLN in stage IIIC1 patients was first evaluated via uni- and multivariate analyses. Then, the impact of incorporating tumor size and number of positive PLN into the FIGO staging system was investigated using the Kaplan–Meier method.

Results
Among 196 women with Stage IIIC1 disease, larger tumors (&gt;4 cm) and multiple PLN metastases (≥4) were independent predictors of progression-free survival (PFS) in patients with stage IIIC1 cervical cancer. The PFS of patients with stage IIIC1 disease was inversely associated with the number of risk factors. Although patients with stage IIIC1 disease had significantly increased survival rates compared to those with stage IIIA or IIIB disease in the original FIGO 2018 staging system, this reversal phenomenon was resolved by incorporating larger tumors (&gt;4 cm) and multiple PLN metastases (≥4) into the revised staging system.

Conclusions
Incorporating tumor size and number of metastatic lymph nodes into the FIGO staging system allows additional risk stratification for women with stage IIIC1 cervical cancer and improves survival prediction performance.
Bayesian kernel machine regression for count data: modelling the association between social vulnerability and COVID-19 deaths in South Carolina
Authors: Mutiso Fedelis , Li Hong , Pearce John L , Benjamin-Neelon Sara E , Mueller Noel T , Neelon Brian 
Published: November 2023

Abstract
The COVID-19 pandemic created an unprecedented global health crisis. Recent studies suggest that socially vulnerable communities were disproportionately impacted, although findings are mixed. To quantify social vulnerability in the US, many studies rely on the Social Vulnerability Index (SVI), a county-level measure comprising 15 census variables. Typically, the SVI is modelled in an additive manner, which may obscure non-linear or interactive associations, further contributing to inconsistent findings. As a more robust alternative, we propose a negative binomial Bayesian kernel machine regression (BKMR) model to investigate dynamic associations between social vulnerability and COVID-19 death rates, thus extending BKMR to the count data setting. The model produces a ‘vulnerability effect’ that quantifies the impact of vulnerability on COVID-19 death rates in each county. The method can also identify the relative importance of various SVI variables and make future predictions as county vulnerability profiles evolve. To capture spatio-temporal heterogeneity, the model incorporates spatial effects, county-level covariates, and smooth temporal functions. For Bayesian computation, we propose a tractable data-augmented Gibbs sampler. We conduct a simulation study to highlight the approach and apply the method to a study of COVID-19 deaths in the US state of South Carolina during the 2021 calendar year.
Tidal disruption rate suppression by the event horizon of spinning black holes
Authors: Huang Hao-Tse , Lu Wenbin 
Published: November 2023

ABSTRACT
The rate of observable tidal disruption events (TDEs) by the most massive (≳ few × 107 M⊙) black holes (BHs) is suppressed due to direct capture of stars. This suppression effect depends on the space–time geometry and holds the promise of probing the spin distribution of dormant BHs at the centres of galaxies. By extending the frozen-in approximation commonly used in the Newtonian limit, we propose a general relativistic criterion for the tidal disruption of a star of given interior structure. The rate suppression factor is then calculated for different BH masses, spins, and realistic stellar populations. We find that either a high-BH spin (≳ 0.5) or a young stellar population (≲1 Gyr) allows TDEs to be observed from BHs significantly more massive than $10^8\, \mathrm{M}_{\odot }$. We call this spin-age degeneracy (SAD). This limits our utility of the TDE rate to constrain the BH spin distribution, unless additional constraints on the age of the stellar population or the mass of the disrupted star can be obtained by modelling the TDE radiation or the stellar spectral energy distribution near the galactic nuclei.
Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations
Authors: Borsato E , Marchetti L , Negrello M , Corsini E M , Wake D , Amvrosiadis A , Baker A J , Bakx T J L C , Beelen A , Berta S , Beyer A , Clements D L , Cooray A , Cox P , Dannerbauer H , de Zotti G , Dye S , Eales S A , Enia A , Farrah D , Gonzalez-Nuevo J , Hughes D H , Ismail D , Jin S , Lapi A , Lehnert M D , Neri R , Pérez-Fournon I , Riechers D A , Rodighiero G , Scott D , Serjeant S , Stanley F , Urquhart S , van der Werf P , Vaccari M , Wang L , Yang C , Young A 
Published: November 2023

ABSTRACT
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, S500 ≥ 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.
Galactic ‘Snake’ IRDC G11.11−0.12: a site of multiple hub–filament systems and colliding filamentary clouds
Authors: Dewangan L K , Bhadari N K , Maity A K , Eswaraiah C , Sharma Saurabh , Jadhav O R 
Published: November 2023

ABSTRACT
To probe star formation processes, we present a multiscale and multiwavelength investigation of the ‘Snake’ nebula/infrared dark cloud G11.11−0.12 (hereafter, G11; length ∼27 pc). Spitzer images hint at the presence of subfilaments (in absorption), and reveal four infrared-dark hub–filament system (HFS) candidates (extent &lt; 6 pc) towards G11, where massive clumps (&gt; 500 M⊙) and protostars are identified. The 13CO(2–1), C18O(2–1), and NH3(1,1) line data reveal a noticeable velocity oscillation towards G11, as well as its left part (or part-A) around Vlsr of 31.5 km s−1, and its right part (or part-B) around Vlsr of 29.5 km s−1. The common zone of these cloud components is investigated towards the centre of G11 housing one HFS. Each cloud component hosts two subfilaments. In comparison to part-A, more APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) clumps are observed towards part-B. The JWST near-infrared images discover one infrared-dark HFS candidate (extent ∼0.55 pc) around the massive protostar G11P1 (i.e. G11P1-HFS). Hence, the infrared observations reveal multiple infrared-dark HFS candidates at multiscale in G11. The Atacama Large Millimeter/submillimeter Array (ALMA) 1.16-mm continuum map shows multiple finger-like features (extent ∼3500–10 000 au) surrounding a dusty envelope-like feature (extent ∼18 000 au) towards the central hub of G11P1-HFS. Signatures of forming massive stars are found towards the centre of the envelope-like feature. The ALMA H13CO+ line data show two cloud components with a velocity separation of ∼2 km s−1 towards G11P1. Overall, the collision process, the ‘fray and fragment’ mechanism, and the ‘global non-isotropic collapse’ scenario seem to be operational in G11.
Core-collapse supernova inside the core of a young massive star cluster: 3D MHD simulations
Authors: Badmaev D V , Bykov A M , Kalyashova M E 
Published: November 2023

ABSTRACT
Young massive stars in compact stellar clusters could end their evolution as core-collapse supernovae a few million years after the cluster was built. The blast wave of a supernova propagates through the inner cluster region with multiple stellar winds of young luminous stars. We present the results of 3D magnetohydrodynamic simulations of the plasma flows produced by a supernova event inside a cluster with a population of massive stars similar to that in Westerlund 1. We followed its evolution over a few thousand years (i.e. a few shock crossing times). The plasma temperature, density, and magnetic field, which are highly disturbed by supernova event, relax to values close to the initial over the studied period. The relaxation time of a cluster is a few thousand years, which is a sizeable fraction of the period between the successive supernova events for a massive cluster of a few million years age. The spectra of the cluster diffuse X-ray emission simulated here should be representative for the galactic and extragalactic young massive clusters. The resultant magnetic fields are highly intermittent, so we derived the volume filling factors for a set of magnetic field ranges. Highly amplified magnetic fields of magnitude well above 100 µG fill in a few per cent of the cluster volume, but still dominate the magnetic energy. The structure of the magnetic fields and high-velocity plasma flows with shocks in the system are favourable for both proton and electron acceleration to energies well above TeV.
Physics-informed neural networks in the recreation of hydrodynamic simulations from dark matter
Authors: Dai Zhenyu , Moews Ben , Vilalta Ricardo , Davé Romeel 
Published: November 2023

ABSTRACT
Physics-informed neural networks have emerged as a coherent framework for building predictive models that combine statistical patterns with domain knowledge. The underlying notion is to enrich the optimization loss function with known relationships to constrain the space of possible solutions. Hydrodynamic simulations are a core constituent of modern cosmology, while the required computations are both expensive and time-consuming. At the same time, the comparatively fast simulation of dark matter requires fewer resources, which has led to the emergence of machine learning algorithms for baryon inpainting as an active area of research; here, recreating the scatter found in hydrodynamic simulations is an ongoing challenge. This paper presents the first application of physics-informed neural networks to baryon inpainting by combining advances in neural network architectures with physical constraints, injecting theory on baryon conversion efficiency into the model loss function. We also introduce a punitive prediction comparison based on the Kullback–Leibler divergence, which enforces scatter reproduction. By simultaneously extracting the complete set of baryonic properties for the simba suite of cosmological simulations, our results demonstrate improved accuracy of baryonic predictions based on dark matter halo properties and successful recovery of the fundamental metallicity relation, and retrieve scatter that traces the target simulation’s distribution.
Studying the variability of fluorescence emission and the presence of clumpy wind in HMXB GX 301−2 using XMM–Newton
Authors: Roy Kinjal , Manikantan Hemanth , Paul Biswajit 
Published: November 2023

ABSTRACT
We present the results from an analysis of data from an XMM–Newton observation of the accreting high-mass X-ray binary pulsar GX 301−2. Spectral analysis in the non-flaring segment of the observation revealed that the equivalent width of the iron fluorescence emission is correlated with the observed absorption column density and the ratio of the iron Kβ and Kα line strength varied with the flux of the source. Coherent pulsations were detected with the spin period of the pulsar of 687.9 ± 0.1 s, and a secondary pulsation was also detected with a period of 671.8 ± 0.2 s, most prominent in the energy band of the iron line. At the spin period of the neutron star, the pulsation of the iron line has a low amplitude and the profile is different from the continuum. Pulse phase-resolved spectroscopy also revealed pulsations of the iron emission line during the non-flaring segment of the light curve. At the secondary period, both the iron line and the continuum have nearly identical pulse fraction and pulse profile. The additional periodicity can be attributed to the beat frequency between the spin of the neutron star and the Keplerian frequency of a stellar wind clump in retrograde motion around the neutron star. Reprocessed X-ray emissions originating from the clump can produce the observed secondary pulsations both in the continuum and the iron fluorescence line. The clump rotating around the neutron star is estimated to be approximately five lt-s away from the neutron star.
Probing the disc–jet coupling in S4 0954+65, PKS 0903−57, and 4C +01.02 with γ-rays
Authors: Sharma Ajay , Kamaram Sushanth Reddy , Prince Raj , Khatoon Rukaiya , Bose Debanjan 
Published: November 2023

ABSTRACT
We present a comprehensive variability study on three blazars, S4 0954+65, PKS 0903−57, and 4C +01.02, covering a mass range of log(M/M⊙) = 8–9, by using ∼15-yr-long γ-ray LCs from Fermi-LAT. The variability level is characterized by the fractional variability amplitude that is higher for γ-rays compared with optical/UV and X-rays emissions. A power spectral density (PSD) study and damped random walk (DRW) modelling are done to probe the characteristic time-scale. The PSD is fitted with a single power law (PL) and bending PL models and the corresponding success fraction was estimated. In the case of PKS 0903−57, We observed a break in the γ-ray PSD at 256 d, which is comparable to the viscous time-scale in the accretion disc, suggesting a possible disc–jet coupling. The non-thermal damping time-scale from the DRW modelling is compared with the thermal damping time-scale for AGNs including our three sources. Our sources lie on the best fit of the $\mathrm{\tau ^{\rm rest}_{\rm damping}}\!-\!M_{\rm BH}$ plot derived for AGN, suggesting a possible accretion disc–jet connection. If the jet’s variability is linked to the disc’s variability, we expect a log-normal flux distribution, often connected to the accretion disc’s multiplicative processes. Our study observed a double log-normal flux distribution, possibly linked to long- and short-term variability from the accretion disc and the jet. In summary, PSD and DRW modelling results for these three sources combined with blazars and AGNs studied in literature favour a disc–jet coupling scenario. However, more such studies are needed to refine this understanding.
Studying the radiation characteristics of rotating radio transient J1913 + 1330 with FAST
Authors: Zhong Wenqian , Zhi Qijun , Lu Jiguang , Dang Shijun , Bai Juntao , Tian Jie , Xu Xin , Shang Lunhua , Zhang Dandan , Dong Aijun , Zhao Rushuang , Du Changrong , Yuen Rai 
Published: November 2023

ABSTRACT
We report a high-resolution study of the radio radiation properties of RRAT J1913 + 1330 based on data obtained from three observing epochs over 4 months using the Five-hundred-meter Aperture Spherical Radio telescope (FAST). Segments of bursts and nulls are detected from the RRAT, which are in agreement with earlier results. From our observations, we identify nine burst segments, and the pulse profile is different for burst segments. We obtain polarization profile for the RRAT J1913 + 1330, and study the polarization, energy distribution, and the wait time distribution between pulses for different burst states. The results show that there are significant differences in the polarization profiles and linear polarization position angle (PA) across different burst states. In addition, pulses in the burst states are discontinuous, and there is no short-term correlation of the arrival time of single pulses in our observations. More interestingly, we find that the PA from some single pulses with high linear polarization demonstrates very different characteristics. The unique radiation characteristics of RRAT J1913 + 1330 will provide important clues for studying its radiation mechanism.